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D." } }, { "id": "Umilt\u00e0-Ccaterina", "name": { "family": "Umilta", "given": "C." }, "orcid": "0000-0002-6805-6188" }, { "id": "Verg\u00e8s-Clara", "name": { "family": "Verg\u00e8s", "given": "C." }, "orcid": "0000-0002-3942-1609" }, { "id": "Vieregg-Abigail-G", "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert-K", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "id": "Wiebe-Donald-V", "name": { "family": "Wiebe", "given": "D. V." }, "orcid": "0000-0002-6669-3159" }, { "id": "Willmert-Justin", "name": { "family": "Willmert", "given": "J." }, "orcid": "0000-0002-6452-4693" }, { "id": "Wu-W-L-Kimmy", "name": { "family": "Wu", "given": "W. L. K." }, "orcid": "0000-0001-5411-6920" }, { "id": "Yang-E", "name": { "family": "Yang", "given": "E." } }, { "id": "Yoon-K-W", "name": { "family": "Yoon", "given": "K. W." } }, { "id": "Young-E-T", "name": { "family": "Young", "given": "E. T." } }, { "id": "Yu-C-J", "name": { "family": "Yu", "given": "C. J." } }, { "id": "Zeng-Lingzhen", "name": { "family": "Zeng", "given": "L." }, "orcid": "0000-0001-6924-9072" }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" }, { "id": "Zhang-Silvia", "name": { "family": "Zhang", "given": "S." } } ] }, "title": "Plastic Laminate Antireflective Coatings for Millimeter-Wave Optics in BICEP Array", "ispublished": "pub", "full_text_status": "public", "keywords": "Condensed Matter Physics; General Materials Science; Atomic and Molecular Physics, and Optics", "note": "\u00a9 2023 Springer Nature. \n\nThe BICEP/Keck projects have been made possible through a series of grants from the National Science Foundation including Grants No. 0742818, No. 0742592, No. 1044978, No. 1110087, No. 1145172, No. 1145143, No. 1145248, No. 1639040, No. 1638957, No. 1638978 and No. 1638970, and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund, and by NASA Grants No. 06-ARPA206-0040, No. 10-SAT10-0017, No. 12- SAT12-0031, No. 14-SAT14-0009 and No. 16-SAT-16- 0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Support for quasioptical filtering was provided by UK STFC Grant No. ST/N000706/1. The computations in this work were run on the Odyssey/Cannon cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and S. L. A. C. is partially supported by the U.S. DOE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed past efforts to the BICEP/Keck series of experiments, including the BICEP1 team.", "abstract": "The BICEP/Keck series of experiments target the cosmic microwave background at degree-scale resolution from the South Pole. Over the next few years, the \"Stage-3\" BICEP Array (BA) telescope will improve the program's frequency coverage and sensitivity to primordial B-mode polarization by an order of magnitude. The first receiver in the array, BA1, began observing at 30/40 GHz in early 2020. The next two receivers, BA2 and BA3, are currently being assembled and will map the southern sky at frequencies ranging from 95 to 150 GHz. Common to all BA receivers is a refractive, on-axis, cryogenic optical design that focuses microwave radiation onto a focal plane populated with antenna-coupled bolometers. High-performance antireflective coatings up to 760 mm in aperture are needed for each element in the optical chain, and must withstand repeated thermal cycles down to 4 K. Here, we present the design and fabrication of the 30/40 GHz anti-reflection coatings for the recently deployed BA1 receiver, with indices matched to its various polyethylene, nylon and alumina optical components. We describe an epoxy coating technique designed for alumina optics, which achieves better than 80% transmission at room temperature. For polyethylene optical elements, we present a new heat-compression approach that allows low-density polytetrafluoroethylene AR layers to reach sub-percent reflected power. We describe the planned use of these methods for the next BA cryostats, which may inform technological choices for future small-aperture telescopes of the CMB-S4 experiment.", "date": "2023-06-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "publisher": "Springer", "id_number": "CaltechAUTHORS:20230602-251655000.30", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230602-251655000.30", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "OPP-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12- SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT-16- 0002" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000706/1" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-023-02967-1", "resource_type": "article", "pub_year": "2023", "author_list": "Dierickx, M.; Ade, P. A. 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St." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." }, "orcid": "0000-0001-6544-7469" }, { "name": { "family": "Sudiwala", "given": "R. V." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } }, { "name": { "family": "Thompson", "given": "K. L." } }, { "name": { "family": "Tolan", "given": "J. E." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Verg\u00e8s", "given": "C." }, "orcid": "0000-0002-3942-1609" }, { "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Willmert", "given": "J." }, "orcid": "0000-0002-6452-4693" }, { "name": { "family": "Wong", "given": "C. L." } }, { "name": { "family": "Wu", "given": "W. L. K." } }, { "name": { "family": "Yang", "given": "H." } }, { "name": { "family": "Yoon", "given": "K. W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "name": { "family": "Zeng", "given": "L." }, "orcid": "0000-0001-6924-9072" }, { "id": "Zhang-C", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" }, { "id": "Zhang-S", "name": { "family": "Zhang", "given": "S." } } ] }, "title": "BICEP/Keck. XVII. Line-of-sight Distortion Analysis: Estimates of Gravitational Lensing, Anisotropic Cosmic Birefringence, Patchy Reionization, and Systematic Errors", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "The BICEP/Keck projects have been made possible through a series of grants from the National Science Foundation, including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, and 1638970, and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and NASA grants 06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031, 14-SAT14-0009, and 16-SAT-16-0002. The development and testing of focal planes was supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Support for quasi-optical filtering was provided by UK STFC grant ST/N000706/1. The computations in this paper were run on the Odyssey/Cannon cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. DOE Office of Science. We thank the staff of the U.S. Antarctic Program, in particular the South Pole Station, without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz, Steffen Richter, Sam Harrison, Grantland Hall, and Hans Boenish. We thank all of those who have contributed past efforts to the BICEP/Keck series of experiments, including the BICEP1 team. We also thank the Planck and WMAP teams for the use of their data and are grateful to the Planck team for helpful discussions.", "abstract": "We present estimates of line-of-sight distortion fields derived from the 95 and 150 GHz data taken by BICEP2, BICEP3, and the Keck Array up to the 2018 observing season, leading to cosmological constraints and a study of instrumental and astrophysical systematics. Cosmological constraints are derived from three of the distortion fields concerning gravitational lensing from large-scale structure, polarization rotation from magnetic fields or an axion-like field, and the screening effect of patchy reionization. We measure an amplitude of the lensing power spectrum A^(\u03d5\u03d5)_(L) = 0.95 \u00b1 0.20. We constrain polarization rotation, expressed as the coupling constant of a Chern\u2013Simons electromagnetic term g_(\u03b1\u03b3) \u2264 2.6 \u00d7 10\u207b\u00b2/H_\u026a, where H_\u026a is the inflationary Hubble parameter, and an amplitude of primordial magnetic fields smoothed over 1 Mpc B_(1Mpc) \u2264 6.6 nG at 95 GHz. We constrain the rms of optical depth fluctuations in a simple \"crinkly surface\" model of patchy reionization, finding A^\u03c4 < 0.19 (2\u03c3) for the coherence scale of L_c = 100. We show that all of the distortion fields of the 95 and 150 GHz polarization maps are consistent with simulations including lensed \u039bCDM, dust, and noise, with no evidence for instrumental systematics. In some cases, the EB and TB quadratic estimators presented here are more sensitive than our previous map-based null tests at identifying and rejecting spurious B-modes that might arise from instrumental effects. Finally, we verify that the standard deprojection filtering in the BICEP/Keck data processing is effective at removing temperature to polarization leakage.", "date": "2023-06-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "949", "number": "2", "publisher": "American Astronomical Society", "pagerange": "43", "id_number": "CaltechAUTHORS:20230705-476466000.4", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230705-476466000.4", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "National Science Foundation", "grant_number": "742818" }, { "agency": "NASA \u2223 Jet Propulsion Laboratory", "grant_number": "06-ARPA206- 0040" }, { "agency": "UKRI \u2223 Science and Technology Facilities Council", "grant_number": "ST/N000706/1" } ] }, "corp_creators": { "items": [ "BICEP/Keck Collaboration" ] }, "doi": "10.3847/1538-4357/acc85c", "resource_type": "article", "pub_year": "2023", "author_list": "Ade, P. A. R.; Ahmed, Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/39pmg-hwk69", "eprint_id": 120687, "eprint_status": "archive", "datestamp": "2023-08-22 20:19:27", "lastmod": "2023-10-18 17:57:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." }, "orcid": "0000-0002-9957-448X" }, { "name": { "family": "Amiri", "given": "M." }, "orcid": "0000-0001-6523-9029" }, { "name": { "family": "Barkats", "given": "D." }, "orcid": "0000-0002-8971-1954" }, { "id": "Basu-Thakur-Ritoban", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C. A." }, "orcid": "0000-0001-9185-6514" }, { "name": { "family": "Beck", "given": "D." }, "orcid": "0000-0003-0848-2756" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." }, "orcid": "0000-0002-1345-4322" }, { "name": { "family": "Cheshire", "given": "J. R." }, "orcid": "0000-0002-1630-7854" }, { "name": { "family": "Clark", "given": "S. E." }, "orcid": "0000-0002-7633-3376" }, { "name": { "family": "Connors", "given": "J." }, "orcid": "0000-0002-6094-2943" }, { "name": { "family": "Cornelison", "given": "J." }, "orcid": "0000-0002-2088-7345" }, { "name": { "family": "Crumrine", "given": "M." } }, { "id": "Cukierman-Ari", "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Denison", "given": "E. V." } }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Eiben", "given": "M." } }, { "name": { "family": "Fatigoni", "given": "S." }, "orcid": "0000-0002-3790-7314" }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fliescher", "given": "S." } }, { "name": { "family": "Giannakopoulos", "given": "C." } }, { "name": { "family": "Goeckner-Wald", "given": "N." } }, { "name": { "family": "Goldfinger", "given": "D. C." }, "orcid": "0000-0001-5268-8423" }, { "name": { "family": "Grayson", "given": "J." } }, { "name": { "family": "Grimes", "given": "P." }, "orcid": "0000-0001-9292-6297" }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halal", "given": "G." }, "orcid": "0000-0003-2221-3018" }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Hand", "given": "E." } }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hubmayr", "given": "J." }, "orcid": "0000-0002-2781-9302" }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." }, "orcid": "0000-0001-5812-1903" }, { "name": { "family": "Irwin", "given": "K. D." }, "orcid": "0000-0002-2998-9743" }, { "id": "Kang-Jae-Hwan", "name": { "family": "Kang", "given": "J." }, "orcid": "0000-0002-3470-2954" }, { "name": { "family": "Karkare", "given": "K. S." }, "orcid": "0000-0002-5215-6993" }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kernasovskiy", "given": "S. A." } }, { "name": { "family": "Kovac", "given": "J. M." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Lau", "given": "K." }, "orcid": "0000-0002-6445-2407" }, { "name": { "family": "Leitch", "given": "E. M." }, "orcid": "0000-0001-8553-9336" }, { "name": { "family": "Lennox", "given": "A." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Minutolo-Lorenzo", "name": { "family": "Minutolo", "given": "L." }, "orcid": "0000-0002-4876-112X" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Nakato", "given": "Y." } }, { "name": { "family": "Namikawa", "given": "T." }, "orcid": "0000-0003-3070-9240" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger-C", "name": { "family": "O'Brient", "given": "R." }, "orcid": "0000-0002-4987-6375" }, { "name": { "family": "Ogburn", "given": "R. W., IV" }, "orcid": "0000-0002-1343-2684" }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Petroff", "given": "M. A." }, "orcid": "0000-0002-4436-4215" }, { "name": { "family": "Prouve", "given": "T." }, "orcid": "0000-0001-5562-6690" }, { "name": { "family": "Pryke", "given": "C." }, "orcid": "0000-0003-3983-6668" }, { "name": { "family": "Racine", "given": "B." }, "orcid": "0000-0001-8861-3052" }, { "name": { "family": "Reintsema", "given": "C. D." } }, { "name": { "family": "Richter", "given": "S." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schwarz", "given": "R." }, "orcid": "0000-0001-8227-1020" }, { "name": { "family": "Schmitt", "given": "B. L." } }, { "name": { "family": "Sheehy", "given": "C. D." } }, { "name": { "family": "Singari", "given": "B." }, "orcid": "0000-0001-7387-0881" }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." }, "orcid": "0009-0007-9335-1326" }, { "name": { "family": "St. Germaine", "given": "T." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." }, "orcid": "0000-0001-6544-7469" }, { "name": { "family": "Sudiwala", "given": "R. V." } }, { "id": "Teply-Grant-P", "name": { "family": "Teply", "given": "G. P." } }, { "name": { "family": "Thompson", "given": "K. L." } }, { "name": { "family": "Tolan", "given": "J. E." }, "orcid": "0000-0002-2755-4404" }, { "name": { "family": "Tucker", "given": "C." }, "orcid": "0000-0002-1851-3918" }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." }, "orcid": "0000-0002-6805-6188" }, { "name": { "family": "Verg\u00e8s", "given": "C." }, "orcid": "0000-0002-3942-1609" }, { "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert-K", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." }, "orcid": "0000-0002-6669-3159" }, { "name": { "family": "Willmert", "given": "J." }, "orcid": "0000-0002-6452-4693" }, { "name": { "family": "Wong", "given": "C. L." } }, { "name": { "family": "Wu", "given": "W. L. K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "H." } }, { "name": { "family": "Yoon", "given": "K. W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." }, "orcid": "0000-0002-8542-232X" }, { "name": { "family": "Zeng", "given": "L." }, "orcid": "0000-0001-6924-9072" }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" }, { "id": "Zhang-Silvia", "name": { "family": "Zhang", "given": "S." } } ] }, "title": "BICEP/Keck. XVI. Characterizing Dust Polarization through Correlations with Neutral Hydrogen", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nWe thank the anonymous referee for a thoughtful review. \n\nThis work was supported by the National Science Foundation under grant No. AST-2106607. \n\nThe BICEP/Keck projects have been made possible through a series of grants from the National Science Foundation including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, and 1638970, and by the Keck Foundation. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station and the heroic winter-overs without whose help this research would not have been possible. We also thank all those who have contributed past efforts to the BICEP/Keck series of experiments.\n\nThis publication utilizes data from Planck, an ESA science mission funded by ESA Member States, NASA, and Canada. \n\nThis work makes use of data from the H i4PI Survey, which is constructed from the Effelsberg\u2013Bonn H i Survey (EBHIS), made with the 100 m radio telescope of the MPIfR at Effelsberg/Germany, and the Galactic All-Sky Survey (GASS), observed with the Parkes Radio Telescope, part of the Australia Telescope National Facility, which is funded by the Australian Government for operation as a National Facility managed by CSIRO. EBHIS was funded by the Deutsche Forschungsgemein-schaft (DFG) under the grants KE757/7-1 to 7\u20133. \n\nThe computations in this paper were run on the Sherlock cluster, supported by the Stanford Research Computing Center at Stanford University, and on the Odyssey/Cannon cluster, supported by the FAS Science Division Research Computing Group at Harvard University. \n\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018), Healpix 22 (G\u00f3rski et al. 2005), healpy (Zonca et al. 2019), matplotlib (Hunter 2007), numpy (Oliphant 2015), cobaya (Torrado & Lewis 2019, 2021), GetDist (Lewis 2019).\n\n
Published - Ade_2023_ApJ_945_72.pdf
", "abstract": "We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H i) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H i is strongly correlated with the dust and partly organized into filaments that are aligned with the local magnetic field. We analyze the deep BICEP/Keck data at 95, 150, and 220 GHz, over the low-column-density region of sky where BICEP/Keck has set the best limits on primordial gravitational waves. We separate the H i emission into distinct velocity components and detect dust polarization correlated with the local Galactic H i but not with the H i associated with Magellanic Stream i. We present a robust, multifrequency detection of polarized dust emission correlated with the filamentary H i morphology template down to 95 GHz. For assessing its utility for foreground cleaning, we report that the Hi morphology template correlates in B modes at a \u223c10%\u201365% level over the multipole range 20 \u2113 < 200 with the BICEP/Keck maps, which contain contributions from dust, CMB, and noise components. We measure the spectral index of the filamentary dust component spectral energy distribution to be \u03b2 = 1.54 \u00b1 0.13. We find no evidence for decorrelation in this region between the filaments and the rest of the dust field or from the inclusion of dust associated with the intermediate velocity H i. Finally, we explore the morphological parameter space in the H i-based filamentary model.", "date": "2023-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "945", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 72", "id_number": "CaltechAUTHORS:20230404-289763500.9", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20230404-289763500.9", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-2106607" }, { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "OPP-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "KE757/7-1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "KE757/7-2" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "KE757/7-3" }, { "agency": "Harvard University" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/acb64c", "primary_object": { "basename": "Ade_2023_ApJ_945_72.pdf", "url": "https://authors.library.caltech.edu/records/39pmg-hwk69/files/Ade_2023_ApJ_945_72.pdf" }, "resource_type": "article", "pub_year": "2023", "author_list": "Ade, P. A. R.; Ahmed, Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/hfvre-fw847", "eprint_id": 118303, "eprint_status": "archive", "datestamp": "2023-08-22 18:23:53", "lastmod": "2023-10-24 23:16:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Yun-Ting" }, "orcid": "0000-0002-5437-0504" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Near-infrared Extragalactic Background Light Fluctuations on Nonlinear Scales", "ispublished": "pub", "full_text_status": "public", "keywords": "Space and Planetary Science; Astronomy and Astrophysics", "note": "We are grateful to Mike Zemcov for providing analysis on refitting our model to CIBER data. We thank Asantha Cooray, Tzu-Ching Chang, and the CIBER and SPHEREx collaborations for helpful discussions. We thank Mike Zemcov, Shuji Matsuura, and Richard Feder for valuable comments that improve the manuscript. This work was supported by NASA grants NNX16AJ69G and 80NSSC20K0595. This work has made use of CosmoHub. CosmoHub has been developed by the Port d'Informaci\u00f3 Cient\u00edfica (PIC), maintained through a collaboration of the Institut de F\u00edsica d'Altes Energies (IFAE) and the Centro de Investigaciones Energ\u00e9ticas, Medioambientales y Tecnol\u00f3gicas (CIEMAT) and the Institute of Space Sciences (CSIC & IEEC), and was partially funded by the \"Plan Estatal de Investigaci\u00f3n Cient\u00edfica y T\u00e9cnica y de Innovaci\u00f3n\" program of the Spanish government.", "abstract": "Several fluctuation studies on the near-infrared extragalactic background light (EBL) find an excess power at tens of arcminute scales (\u2113 \u223c 10\u00b3). Emission from the intra-halo light (IHL) has been proposed as a possible explanation for the excess signal. In this work, we investigate the emission from the integrated galaxy light (IGL) and IHL in the power spectrum of EBL fluctuations using the simulated galaxy catalog MICECAT. We find that at \u2113 \u223c 10\u00b3, the one-halo clustering from satellite galaxies has comparable power to the two-halo term in the IGL power spectrum. In some previous EBL analyses, the IGL model assumed a small one-halo clustering signal, which may result in overestimating the IHL contribution to the EBL. We also investigate the dependence of the IGL+IHL power spectrum on the IHL distribution as a function of redshift and halo mass, and the spatial profile within the halo. Our forecast suggests that the upcoming SPHEREx deep field survey can distinguish different IHL models considered in this work with high significance. Finally, we quantify the bias in the power spectrum from the correlation of the mask and the signal, which has not been accounted for in previous analyses.", "date": "2022-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "940", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 115", "id_number": "CaltechAUTHORS:20221212-795726500.6", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221212-795726500.6", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX16AJ69G" }, { "agency": "NASA", "grant_number": "80NSSC20K0595" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac9a51", "resource_type": "article", "pub_year": "2022", "author_list": "Cheng, Yun-Ting and Bock, James J." }, { "id": "https://authors.library.caltech.edu/records/8gfk2-me258", "eprint_id": 114500, "eprint_status": "archive", "datestamp": "2023-08-22 15:01:40", "lastmod": "2023-10-24 15:00:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Leung-Jason-S-Y", "name": { "family": "Leung", "given": "J. S.-Y." }, "orcid": "0000-0001-7116-3710" }, { "name": { "family": "Hartley", "given": "J." } }, { "name": { "family": "Nagy", "given": "J. M." }, "orcid": "0000-0002-2036-7008" }, { "name": { "family": "Netterfield", "given": "C. B." } }, { "name": { "family": "Shariff", "given": "J. A." } }, { "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Benton", "given": "S. J." }, "orcid": "0000-0002-4214-9298" }, { "name": { "family": "Bergman", "given": "A. S." } }, { "name": { "family": "Bihary", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Bonetti-J-A", "name": { "family": "Bonetti", "given": "J. A." } }, { "name": { "family": "Bryan", "given": "S. A." } }, { "name": { "family": "Chiang", "given": "H. C." }, "orcid": "0000-0002-4098-9533" }, { "name": { "family": "Contaldi", "given": "C. R." }, "orcid": "0000-0001-7285-0707" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e8", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "name": { "family": "Duivenvoorden", "given": "A. J." }, "orcid": "0000-0003-2856-2382" }, { "name": { "family": "Eriksen", "given": "H. K." } }, { "name": { "family": "Farhang", "given": "M." } }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fraisse", "given": "A. A." } }, { "name": { "family": "Freese", "given": "K." } }, { "name": { "family": "Galloway", "given": "M." } }, { "name": { "family": "Gambrel", "given": "A. E." } }, { "name": { "family": "Gandilo", "given": "N. N." } }, { "name": { "family": "Ganga", "given": "K." } }, { "name": { "family": "Gualtieri", "given": "R." }, "orcid": "0000-0003-4245-2315" }, { "name": { "family": "Gudmundsson", "given": "J. E." }, "orcid": "0000-0003-1760-0355" }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Hasselfield", "given": "M." } }, { "name": { "family": "Hilton", "given": "G." } }, { "id": "Holmes-Warren-A", "name": { "family": "Holmes", "given": "W." } }, { "id": "Hristov-Viktor-V", "name": { "family": "Hristov", "given": "V. V." } }, { "name": { "family": "Huang", "given": "Z." }, "orcid": "0000-0002-1506-1063" }, { "name": { "family": "Irwin", "given": "K. D." } }, { "name": { "family": "Jones", "given": "W. C." }, "orcid": "0000-0002-3636-1241" }, { "name": { "family": "Karakci", "given": "A." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Kermish", "given": "Z. D." } }, { "name": { "family": "Li", "given": "S." }, "orcid": "0000-0002-8896-911X" }, { "name": { "family": "Mak", "given": "D. S. Y." } }, { "id": "Mason-Peter-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-Tracy-A", "name": { "family": "Morford", "given": "T. A." } }, { "name": { "family": "Nolta", "given": "M." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Osherson", "given": "B." } }, { "name": { "family": "Padilla", "given": "I. L." }, "orcid": "0000-0002-0024-2662" }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Rahlin", "given": "A. S." }, "orcid": "0000-0003-3953-1776" }, { "name": { "family": "Reintsema", "given": "C." } }, { "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Runyan-Marcus-C", "name": { "family": "Runyan", "given": "M. C." } }, { "name": { "family": "Ruud", "given": "T. M." }, "orcid": "0000-0002-7615-1900" }, { "name": { "family": "Shaw", "given": "E. C." }, "orcid": "0000-0001-5644-8750" }, { "name": { "family": "Shiu", "given": "C." } }, { "name": { "family": "Soler", "given": "J. D." }, "orcid": "0000-0002-0294-4465" }, { "name": { "family": "Song", "given": "X." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "van der List", "given": "J. F." } }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wehus", "given": "I. K." }, "orcid": "0000-0003-3821-7275" }, { "name": { "family": "Wen", "given": "S." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Young", "given": "E. Y." } } ] }, "title": "A Simulation-based Method for Correcting Mode Coupling in CMB Angular Power Spectra", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmic microwave background radiation; Observational cosmology; Astronomy data analysis; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 November 2; revised 2022 February 1; accepted 2022 February 11; published 2022 March 30. \n\nSpider is supported in the U.S. by the National Aeronautics and Space Administration under grant Nos. NNX07AL64G, NNX12AE95G, NNX17AC55G, and 80NSSC21K1986 issued through the Science Mission Directorate and by the National Science Foundation through PLR-1043515. Logistical support for the Antarctic deployment and operations is provided by the NSF through the U.S. Antarctic Program. Support in Canada is provided by the Natural Sciences and Engineering Research Council and the Canadian Space Agency. Support in Norway is provided by the Research Council of Norway. Support in Sweden is provided by the Swedish Research Council through the Oskar Klein Centre (Contract No. 638-2013-8993) as well as a grant from the Swedish Research Council (dnr. 2019-93959) and a grant from the Swedish Space Agency (dnr. 139/17). The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. The multiplexing readout electronics were developed with support from the Canada Foundation for Innovation and the British Columbia Knowledge Development Fund. K.F. holds the Jeff & Gail Kodosky Endowed Chair at UT Austin and is grateful for that support. W.C.J. acknowledges the generous support of the David and Lucile Packard Foundation, which has been crucial to the success of the project. C.R.C. was supported by UKRI Consolidated grant Nos. ST/P000762/1, ST/N000838/1, and ST/T000791/1. \n\nSome of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). The computations described in this paper were performed on four computing clusters: Hippo at the University of KwaZulu-Natal, Feynman at Princeton University, and the GPC and Niagara supercomputers at the SciNet HPC Consortium (Loken et al. 2010; Ponce et al. 2019). SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund\u2014Research Excellence, and the University of Toronto. \n\nThe collaboration is grateful to the British Antarctic Survey, particularly Sam Burrell, and to the Alfred Wegener Institute and the crew of R.V. Polarstern for invaluable assistance with the recovery of the data and payload after the 2015 flight. Brendan Crill and Tom Montroy made significant contributions to Spider's development. Paul Steinhardt provided very helpful comments regarding the status of early universe models. This project, like so many others that he founded and supported, owes much to the vision and leadership of the late Professor Andrew E. Lange.\n\nPublished - Leung_2022_ApJ_928_109.pdf
Accepted Version - 2111.01113.pdf
", "abstract": "Modern cosmic microwave background (CMB) analysis pipelines regularly employ complex time-domain filters, beam models, masking, and other techniques during the production of sky maps and their corresponding angular power spectra. However, these processes can generate couplings between multipoles from the same spectrum and from different spectra, in addition to the typical power attenuation. Within the context of pseudo-C_\u2113 based, MASTER-style analyses, the net effect of the time-domain filtering is commonly approximated by a multiplicative transfer function, F_\u2113, that can fail to capture mode mixing and is dependent on the spectrum of the signal. To address these shortcomings, we have developed a simulation-based spectral correction approach that constructs a two-dimensional transfer matrix, J_u, which contains information about mode mixing in addition to mode attenuation. We demonstrate the application of this approach on data from the first flight of the SPIDER balloon-borne CMB experiment.", "date": "2022-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "928", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 109", "id_number": "CaltechAUTHORS:20220427-719784600", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220427-719784600", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NASA", "grant_number": "NNX17AC55G" }, { "agency": "NASA", "grant_number": "80NSSC21K1986" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Research Council of Norway" }, { "agency": "Swedish Research Council", "grant_number": "638-2013-8993" }, { "agency": "Swedish Research Council", "grant_number": "2019-93959" }, { "agency": "Swedish Research Council", "grant_number": "139/17" }, { "agency": "David Dunlap Family" }, { "agency": "University of Toronto" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "British Columbia Knowledge Development Fund" }, { "agency": "University of Texas at Austin" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000762/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000838/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/T000791/1" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac562f", "primary_object": { "basename": "2111.01113.pdf", "url": "https://authors.library.caltech.edu/records/8gfk2-me258/files/2111.01113.pdf" }, "related_objects": [ { "basename": "Leung_2022_ApJ_928_109.pdf", "url": "https://authors.library.caltech.edu/records/8gfk2-me258/files/Leung_2022_ApJ_928_109.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Leung, J. S.-Y.; Hartley, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/cehe0-7s274", "eprint_id": 108675, "eprint_status": "archive", "datestamp": "2023-08-22 14:32:03", "lastmod": "2023-10-23 17:14:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Benton", "given": "S. J." } }, { "name": { "family": "Bergman", "given": "A. S." } }, { "name": { "family": "Bihary", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Bond", "given": "J. R." } }, { "id": "Bonetti-J-A", "name": { "family": "Bonetti", "given": "J. A." } }, { "name": { "family": "Bryan", "given": "S. A." } }, { "name": { "family": "Chiang", "given": "H. C." } }, { "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "name": { "family": "Duivenvoorden", "given": "A. J." } }, { "name": { "family": "Eriksen", "given": "H. K." } }, { "name": { "family": "Farhang", "given": "M." } }, { "name": { "family": "Filippini", "given": "J. P." } }, { "name": { "family": "Fraisse", "given": "A. A." } }, { "name": { "family": "Freese", "given": "K." } }, { "name": { "family": "Galloway", "given": "M." } }, { "name": { "family": "Gambrel", "given": "A. E." } }, { "name": { "family": "Gandilo", "given": "N. N." } }, { "name": { "family": "Ganga", "given": "K." } }, { "name": { "family": "Gualtieri", "given": "R." } }, { "name": { "family": "Gudmundsson", "given": "J. E." } }, { "name": { "family": "Halpern", "given": "M." } }, { "name": { "family": "Hartley", "given": "J." } }, { "name": { "family": "Hasselfield", "given": "M." } }, { "name": { "family": "Hilton", "given": "G." } }, { "id": "Holmes-Warren-A", "name": { "family": "Holmes", "given": "W." } }, { "id": "Hristov-Viktor-V", "name": { "family": "Hristov", "given": "V. V." } }, { "name": { "family": "Huang", "given": "Z." } }, { "name": { "family": "Irwin", "given": "K. D." } }, { "name": { "family": "Jones", "given": "W. C." } }, { "name": { "family": "Karakci", "given": "A." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Kermish", "given": "Z. D." } }, { "name": { "family": "Leung", "given": "J. S. -Y." } }, { "name": { "family": "Li", "given": "S." } }, { "name": { "family": "Mak", "given": "D. S. Y." } }, { "id": "Mason-Peter-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-Tracy-A", "name": { "family": "Morford", "given": "T. A." } }, { "name": { "family": "Nagy", "given": "J. M." } }, { "name": { "family": "Netterfield", "given": "C. B." } }, { "name": { "family": "Nolta", "given": "M." } }, { "id": "O'Brient-Roger-C", "name": { "family": "O'Brient", "given": "R." }, "orcid": "0000-0002-4987-6375" }, { "name": { "family": "Osherson", "given": "B." } }, { "name": { "family": "Padilla", "given": "I. L." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Rahlin", "given": "A. S." } }, { "name": { "family": "Reintsema", "given": "C." } }, { "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Runyan-Marcus-C", "name": { "family": "Runyan", "given": "M. C." } }, { "name": { "family": "Ruud", "given": "T. M." } }, { "name": { "family": "Shariff", "given": "J. A." } }, { "name": { "family": "Shaw", "given": "E. C." } }, { "name": { "family": "Shiu", "given": "C." } }, { "name": { "family": "Soler", "given": "J. D." } }, { "name": { "family": "Song", "given": "X." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "van der List", "given": "J. F." } }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wehus", "given": "I. K." } }, { "name": { "family": "Wen", "given": "S." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Young", "given": "E. Y." } } ] }, "title": "A Constraint on Primordial B-modes from the First Flight of the Spider Balloon-borne Telescope", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmic microwave background radiation; Observational cosmology; Cosmological parameters; Interstellar emissions", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 April 6; revised 2021 August 5; accepted 2021 August 15; published 2022 March 14. \n\nSpider is supported in the U.S. by the National Aeronautics and Space Administration under grants NNX07AL64G, NNX12AE95G, and NNX17AC55G issued through the Science Mission Directorate and by the National Science Foundation through PLR-1043515. Logistical support for the Antarctic deployment and operations is provided by the NSF through the U.S. Antarctic Program. Support in Canada is provided by the Natural Sciences and Engineering Research Council and the Canadian Space Agency. Support in Norway is provided by the Research Council of Norway. Support in Sweden is provided by the Swedish Research Council through the Oskar Klein Centre (Contract No. 638-2013-8993) as well as a grant from the Swedish Research Council (dnr. 2019-93959) and a grant from the Swedish Space Agency (dnr. 139/17). The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. The multiplexing readout electronics were developed with support from the Canada Foundation for Innovation and the British Columbia Knowledge Development Fund. KF holds the Jeff & Gail Kodosky Endowed Chair at UT Austin and is grateful for that support. W.C.J. acknowledges the generous support of the David and Lucile Packard Foundation, which has been crucial to the success of the project. C.R.C. was supported by UKRI Consolidated Grants, ST/P000762/1, ST/N000838/1, and ST/T000791/1. \n\nSome of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). The computations described in this paper were performed on four computing clusters: Hippo at the University of KwaZulu-Natal, Feynman at Princeton University, and the GPC and Niagara supercomputers at the SciNet HPC Consortium (Loken et al. 2010; Ponce et al. 2019). SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund\u2014Research Excellence, and the University of Toronto. \n\nThis collaboration is grateful to the British Antarctic Survey, particularly Sam Burrell, and to the Alfred Wegener Institute and the crew of R.V. Polarstern for invaluable assistance with the recovery of the data and payload after the 2015 flight. Brendan Crill and Tom Montroy made significant contributions to Spider's development. Paul Steinhardt provided very helpful comments regarding the status of early-universe models. This project, like so many others that he founded and supported, owes much to the vision and leadership of the late Professor Andrew E. Lange.\n\nPublished - Ade_2022_ApJ_927_174.pdf
Submitted - 2103.13334.pdf
", "abstract": "We present the first linear polarization measurements from the 2015 long-duration balloon flight of Spider, which is an experiment that is designed to map the polarization of the cosmic microwave background (CMB) on degree angular scales. The results from these measurements include maps and angular power spectra from observations of 4.8% of the sky at 95 and 150 GHz, along with the results of internal consistency tests on these data. While the polarized CMB anisotropy from primordial density perturbations is the dominant signal in this region of sky, Galactic dust emission is also detected with high significance. Galactic synchrotron emission is found to be negligible in the Spider bands. We employ two independent foreground-removal techniques to explore the sensitivity of the cosmological result to the assumptions made by each. The primary method uses a dust template derived from Planck data to subtract the Galactic dust signal. A second approach, which constitutes a joint analysis of Spider and Planck data in the harmonic domain, assumes a modified-blackbody model for the spectral energy distribution of the dust with no constraint on its spatial morphology. Using a likelihood that jointly samples the template amplitude and r parameter space, we derive 95% upper limits on the primordial tensor-to-scalar ratio from Feldman\u2013Cousins and Bayesian constructions, finding r < 0.11 and r < 0.19, respectively. Roughly half the uncertainty in r derives from noise associated with the template subtraction. New data at 280 GHz from Spider's second flight will complement the Planck polarization maps, providing powerful measurements of the polarized Galactic dust emission.", "date": "2022-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "927", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 174", "id_number": "CaltechAUTHORS:20210409-121742575", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210409-121742575", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NASA", "grant_number": "NNX17AC55G" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Research Council of Norway" }, { "agency": "Swedish Research Council", "grant_number": "638-2013-8993" }, { "agency": "Swedish Research Council", "grant_number": "2019-93959" }, { "agency": "Swedish Space Agency", "grant_number": "139/17" }, { "agency": "David Dunlap Family" }, { "agency": "University of Toronto" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "British Columbia Knowledge Development Fund" }, { "agency": "University of Texas at Austin" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000762/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000838/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/T000791/1" }, { "agency": "Compute Canada" }, { "agency": "Ontario Research Fund-Research Excellence" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "SPIDER Collaboration" ] }, "doi": "10.3847/1538-4357/ac20df", "primary_object": { "basename": "2103.13334.pdf", "url": "https://authors.library.caltech.edu/records/cehe0-7s274/files/2103.13334.pdf" }, "related_objects": [ { "basename": "Ade_2022_ApJ_927_174.pdf", "url": "https://authors.library.caltech.edu/records/cehe0-7s274/files/Ade_2022_ApJ_927_174.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Ade, P. A. R.; Amiri, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/31q20-j2g51", "eprint_id": 113770, "eprint_status": "archive", "datestamp": "2023-08-22 14:28:12", "lastmod": "2023-10-23 23:13:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Thakur-Ritoban-Basu", "name": { "family": "Thakur", "given": "R. Basu" } }, { "name": { "family": "Bischoff", "given": "C. A." }, "orcid": "0000-0001-9185-6514" }, { "name": { "family": "Beck", "given": "D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." }, "orcid": "0000-0002-1345-4322" }, { "name": { "family": "Cheshire", "given": "J. R., IV" } }, { "name": { "family": "Connors", "given": "J." }, "orcid": "0000-0002-6094-2943" }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Denison", "given": "E. V." } }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Eiben", "given": "M." } }, { "name": { "family": "Fatigoni", "given": "S." }, "orcid": "0000-0002-3790-7314" }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fliescher", "given": "S." } }, { "name": { "family": "Goeckner-Wald", "given": "N." } }, { "name": { "family": "Goldfinger", "given": "D. C." } }, { "name": { "family": "Grayson", "given": "J." } }, { "name": { "family": "Grimes", "given": "P." } }, { "name": { "family": "Hall", "given": "G." }, "orcid": "0000-0002-6299-8385" }, { "name": { "family": "Halal", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Hand", "given": "E." } }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G. C." }, "orcid": "0000-0003-4247-467X" }, { "name": { "family": "Hubmayr", "given": "J." }, "orcid": "0000-0002-2781-9302" }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." }, "orcid": "0000-0001-5812-1903" }, { "name": { "family": "Irwin", "given": "K. D." }, "orcid": "0000-0002-2998-9743" }, { "id": "Kang-Jae-Hwan", "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K. S." }, "orcid": "0000-0002-5215-6993" }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kernasovskiy", "given": "S. A." } }, { "name": { "family": "Kovac", "given": "J. M." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Lau", "given": "K." }, "orcid": "0000-0002-6445-2407" }, { "name": { "family": "Leitch", "given": "E. M." } }, { "name": { "family": "Lennox", "given": "A." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Minutolo-Lorenzo", "name": { "family": "Minutolo", "given": "L." }, "orcid": "0000-0002-4876-112X" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Nakato", "given": "Y." } }, { "name": { "family": "Namikawa", "given": "T." }, "orcid": "0000-0003-3070-9240" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Ogburn", "given": "R. W., IV" } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Prouve", "given": "T." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." }, "orcid": "0000-0001-8861-3052" }, { "name": { "family": "Reintsema", "given": "C. D." } }, { "name": { "family": "Richter", "given": "S." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Schmitt", "given": "B. L." } }, { "name": { "family": "Sheehy", "given": "C. D." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "St. Germaine", "given": "T." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." }, "orcid": "0000-0001-6544-7469" }, { "name": { "family": "Sudiwala", "given": "R. V." } }, { "id": "Teply-Grant-P", "name": { "family": "Teply", "given": "G. P." } }, { "name": { "family": "Thompson", "given": "K. L." } }, { "name": { "family": "Tolan", "given": "J. E." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Verg\u00e8s", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert-K", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wong", "given": "C. L." } }, { "name": { "family": "Wu", "given": "W. L. K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "H." } }, { "name": { "family": "Yoon", "given": "K. W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "name": { "family": "Zeng", "given": "L." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" }, { "id": "Zhang-Silvia", "name": { "family": "Zhang", "given": "S." } } ] }, "title": "Bicep/Keck XV: The Bicep3 Cosmic Microwave Background Polarimeter and the First Three-year Data Set", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmic microwave background radiation; Polarimeters; Gravitational waves; Cosmic inflation; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 September 30; revised 2021 December 22; accepted 2022 January 3; published 2022 March 7. \n\nBicep/Keck has been made possible through a series of grants from the National Science Foundation including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, 1638970, and 1836010 and by the Keck Foundation. The construction of the Bicep3 receiver was supported by the Department of Energy, Laboratory Directed Research and Development program at SLAC National Accelerator Laboratory, under contract DE-AC02-76SF00515. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grant Nos. 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Cannon cluster supported by the FAS Science Division Research Computing Group at Harvard University. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Sam Harrison, Hans Boenish, Grantland Hall, Ta-Lee Shue, Paula Crock, and Calvin Tsai. We thank all those who have contributed past efforts to the Bicep/Keck series of experiments, including the Bicep1 team. We would also like to thank Jonathon Hunacek at JPL/Caltech for exchange of information regarding detector readout and laboratory housekeeping design, and Aritoki Suzuki, Oliver Jeong, Yuki Inoue, and Tomotake Matsumura at Berkeley and in Japan for discussions regarding alumina optics and AR coatings.\n\nPublished - Ade_2022_ApJ_927_77.pdf
Submitted - 2110.00482.pdf
", "abstract": "We report on the design and performance of the Bicep3 instrument and its first three-year data set collected from 2016 to 2018. Bicep3 is a 52 cm aperture refracting telescope designed to observe the polarization of the cosmic microwave background (CMB) on degree angular scales at 95 GHz. It started science observation at the South Pole in 2016 with 2400 antenna-coupled transition-edge sensor bolometers. The receiver first demonstrated new technologies such as large-diameter alumina optics, Zotefoam infrared filters, and flux-activated SQUIDs, allowing \u223c10\u00d7 higher optical throughput compared to the Keck design. Bicep3 achieved instrument noise equivalent temperatures of 9.2, 6.8, and 7.1 \u03bcK_(CMB) \u221as and reached Stokes Q and U map depths of 5.9, 4.4, and 4.4 \u03bcK arcmin in 2016, 2017, and 2018, respectively. The combined three-year data set achieved a polarization map depth of 2.8 \u03bcK arcmin over an effective area of 585 square degrees, which is the deepest CMB polarization map made to date at 95 GHz.", "date": "2022-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "927", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 77", "id_number": "CaltechAUTHORS:20220307-188876000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220307-188876000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "NSF", "grant_number": "AST-1836010" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "BICEP/Keck Collaboration" ] }, "doi": "10.3847/1538-4357/ac4886", "primary_object": { "basename": "2110.00482.pdf", "url": "https://authors.library.caltech.edu/records/31q20-j2g51/files/2110.00482.pdf" }, "related_objects": [ { "basename": "Ade_2022_ApJ_927_77.pdf", "url": "https://authors.library.caltech.edu/records/31q20-j2g51/files/Ade_2022_ApJ_927_77.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Ade, P. A. R.; Ahmed, Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/x8w5r-c9963", "eprint_id": 113532, "eprint_status": "archive", "datestamp": "2023-08-22 14:05:06", "lastmod": "2023-10-23 23:06:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Korngut-Phillip-M", "name": { "family": "Korngut", "given": "P. M." } }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Arai-Toshiaki", "name": { "family": "Arai", "given": "T." } }, { "id": "Bangale-Priyadarshini", "name": { "family": "Bangale", "given": "P." }, "orcid": "0000-0002-3886-3739" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-Asantha", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Y. T." }, "orcid": "0000-0002-5437-0504" }, { "id": "Feder-Richard-M", "name": { "family": "Feder", "given": "R." }, "orcid": "0000-0002-9330-8738" }, { "id": "Hristov-Viktor-V", "name": { "family": "Hristov", "given": "V." } }, { "id": "Lanz-Alicia", "name": { "family": "Lanz", "given": "A." }, "orcid": "0000-0003-2565-1558" }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Levenson-Louis-R", "name": { "family": "Levenson", "given": "L." } }, { "id": "Matsumoto-Toshio", "name": { "family": "Matsumoto", "given": "T." }, "orcid": "0000-0001-6066-5221" }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Nguyen-C", "name": { "family": "Nguyen", "given": "C." } }, { "id": "Sano-Kei", "name": { "family": "Sano", "given": "K." }, "orcid": "0000-0002-6468-8532" }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." }, "orcid": "0000-0001-7143-6520" }, { "id": "Zemcov-Michael", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Inferred Measurements of the Zodiacal Light Absolute Intensity through Fraunhofer Absorption Line Spectroscopy with CIBER", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmology; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 March 31; revised 2021 November 18; accepted 2021 December 17; published 2022 February 18. \n\nThe data presented here would not have been possible without the support of the NSROC staff at Wallops Flight Facility and White Sands Missile Range. Insight from Kalevi Mattila and Roland dePutter improved the quality of the manuscript. We thank Ned Wright for providing us with his model predictions and Leo Girardi for his star count code. P.K. and M.Z. acknowledge support from the NASA postdoctoral program. We would also like to thank the late Keith Lykke, whose work along with Steven Brown and Allan Smith on the calibration program made this work possible. We acknowledge the contributions of collaboration members working early in the project that were important to acquiring the data in this paper, including Ian Sullivan, Brian Keating, and Tom Renbarger. This work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, NNX10AE12G, and NNX16AJ69G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. Japanese participation in CIBER was supported by KAKENHI (20\u00b734, 18204018, 19540250, 21340047, and 21111004) from Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports, Science and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from Korea Astronomy and Space Science Institute (KASI).\n\nPublished - Korngut_2022_ApJ_926_133.pdf
Submitted - 2104.07104.pdf
", "abstract": "Scattered sunlight from the interplanetary dust (IPD) cloud in our solar system presents a serious foreground challenge for spectrophotometric measurements of the extragalactic background light (EBL). In this work, we report on inferred measurements of the absolute intensity of the zodiacal light (ZL) using the novel technique of Fraunhofer line spectroscopy on the deepest 8542 \u00c5 line of the near-infrared Ca ii absorption triplet. The measurements are performed with the narrow band spectrometer (NBS) on board the Cosmic Infrared Background Experiment sounding rocket instrument. We use the NBS data to test the accuracy of two ZL models widely cited in the literature, the Kelsall and Wright models, which have been used in foreground removal analyses that produce high and low EBL results respectively. We find a mean reduced \u03c7\u00b2 = 3.5 for the Kelsall model and \u03c7\u00b2 = 2.0 for the Wright model. The best description of our data is provided by a simple modification to the Kelsall model, which includes a free ZL offset parameter. This adjusted model describes the data with a reduced \u03c7\u00b2 = 1.5 and yields an inferred offset amplitude of 46 \u00b1 19 nW m\u207b\u00b2 sr\u207b\u00b9 extrapolated to 12500 \u00c5. These measurements elude to the potential existence of a dust cloud component in the inner solar system whose intensity does not strongly modulate with the Earth's motion around the Sun.", "date": "2022-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "926", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 133", "id_number": "CaltechAUTHORS:20220222-707075000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220222-707075000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "NASA", "grant_number": "NNX16AJ69G" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20\u00b734" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac44ff", "primary_object": { "basename": "2104.07104.pdf", "url": "https://authors.library.caltech.edu/records/x8w5r-c9963/files/2104.07104.pdf" }, "related_objects": [ { "basename": "Korngut_2022_ApJ_926_133.pdf", "url": "https://authors.library.caltech.edu/records/x8w5r-c9963/files/Korngut_2022_ApJ_926_133.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Korngut, P. M.; Kim, M. 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L. Kimmy" }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Xu", "given": "Zhilei" }, "orcid": "0000-0001-5112-2567" }, { "name": { "family": "Yang", "given": "H. Y. Eric" } }, { "name": { "family": "Yasini", "given": "Siavash" } }, { "name": { "family": "Yefremenko", "given": "Volodymyr G." } }, { "name": { "family": "Won Yoon", "given": "Ki" } }, { "name": { "family": "Young", "given": "Edward" } }, { "name": { "family": "Yu", "given": "Cyndia" } }, { "name": { "family": "Zonca", "given": "Andrea" }, "orcid": "0000-0001-6841-1058" } ] }, "title": "CMB-S4: Forecasting Constraints on Primordial Gravitational Waves", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmic background radiation; Cosmological parameters; Gravitational waves; Cosmic inflation; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2020 August 26; revised 2021 June 15; accepted 2021 July 8; published 2022 February 11. \n\nThe CMB-S4 collaboration (https://cmb-s4.org/) is working to plan, construct, and operate a next-generation, multisite CMB experiment in the 2020s. The collaboration is led by an elected Governing Board, Spokespeople, Committee Chairs, and Executive Team. Funding for the CMB-S4 Integrated Project Office is provided by the Department of Energy's Office of Science (project level CD-0) and by the National Science Foundation through the Mid-Scale Research Infrastructure-R1 award OPP-1935892. This research used resources of Argonne National Laboratory, a U.S. Department of Energy (DOE) Office of Science User Facility operated under Contract No. DE-AC02-06CH11357. This document was prepared by the CMB-S4 collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract No. DE-AC02-07CH11359. Work at Lawrence Berkeley National Laboratory was supported by the Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Work at SLAC National Accelerator Laboratory is supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences under Contract No. DE-AC02-76SF00515. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. In the United States, work on CMB-S4 by individual investigators has been supported by the National Science Foundation (awards 1248097, 1255358, 1815887, 1835865, 1852617, 2009469), the Department of Energy (awards DE-SC0009919, DE-SC0009946, DE-SC0010129, DE-SC0011784), and the National Aeronautics and Space Administration (award ATP-80NSSC20K0518). In Australia, the Melbourne authors acknowledge support from an Australian Research Council Future Fellowship (FT150100074). In Canada, R.H. is supported by the Discovery Grants program from NSERC, and acknowledges funding from CIFAR, the Sloan Foundation, and the Dunlap family. In Italy, C.B. acknowledges support under the ASI COSMOS and INFN INDARK programs. In the Netherlands, D.M. acknowledges NWO VIDI award number 639.042.730. In Switzerland, J.C. is supported by an SNSF Eccellenza Professorial Fellowship (No. 186879). In the United Kingdom, A.L., G.F., and J.C. are supported by the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC grant Agreement No. [616170]. A.L. also acknowledges STFC award ST/P000525/1. S.M. is supported by the research program Innovational Research Incentives Scheme (Vernieuwingsimpuls), which is financed by the Netherlands Organization for Scientific Research through the NWO VIDI grant No. 639.042.612-Nissanke and the Labex ILP (reference ANR-10-LABX-63) part of the Idex SUPER, received financial state aid managed by the Agence Nationale de la Recherche, as part of the program Investissements d'avenir under the reference ANR-11-IDEX-0004-02. Some computations in this paper were run on the Odyssey cluster, supported by the FAS Science Division Research Computing Group at Harvard University.\n\nPublished - Abazajian_2022_ApJ_926_54.pdf
Submitted - 2008.12619.pdf
", "abstract": "CMB-S4\u2014the next-generation ground-based cosmic microwave background (CMB) experiment\u2014is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the universe. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semianalytic projection tool, targeted explicitly toward optimizing constraints on the tensor-to-scalar ratio, r, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2\u20133 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments, given a desired scientific goal. To form a closed-loop process, we couple this semianalytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for r > 0.003 at greater than 5\u03c3, or in the absence of a detection, of reaching an upper limit of r < 0.001 at 95% CL.", "date": "2022-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "926", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 54", "id_number": "CaltechAUTHORS:20220216-400348865", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220216-400348865", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-06CH11357" }, { "agency": "NSF", "grant_number": "OPP-1935892" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-07CH11359" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "NSF", "grant_number": "OPP-1248097" }, { "agency": "NSF", "grant_number": "AST-1255358" }, { "agency": "NSF", "grant_number": "AST-1815887" }, { "agency": "NSF", "grant_number": "OAC-1835865" }, { "agency": "NSF", "grant_number": "OPP-1852617" }, { "agency": "NSF", "grant_number": "2009469" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0009919" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0009946" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0010129" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0011784" }, { "agency": "NASA", "grant_number": "80NSSC20K0518" }, { "agency": "Australian Research Council", "grant_number": "FT150100074" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Dunlap Institute for Astronomy and Astrophysics" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Istituto Nazionale di Fisica Nucleare (INFN)" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.042.730" }, { "agency": "Swiss National Science Foundation (SNSF)", "grant_number": "186879" }, { "agency": "European Research Council (ERC)", "grant_number": "616170" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000525/1" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.042.612-Nissanke" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-10-LABX-63" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-11-IDEX-0004-02" }, { "agency": "Harvard University" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "CMB-S4 Collaboration" ] }, "doi": "10.3847/1538-4357/ac1596", "primary_object": { "basename": "2008.12619.pdf", "url": "https://authors.library.caltech.edu/records/fqakr-f1296/files/2008.12619.pdf" }, "related_objects": [ { "basename": "Abazajian_2022_ApJ_926_54.pdf", "url": "https://authors.library.caltech.edu/records/fqakr-f1296/files/Abazajian_2022_ApJ_926_54.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Abazajian, Kevork; Addison, Graeme E.; et el." }, { "id": "https://authors.library.caltech.edu/records/vjaav-0m371", "eprint_id": 113351, "eprint_status": "archive", "datestamp": "2023-08-22 13:56:38", "lastmod": "2023-10-23 23:03:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Takimoto-Kohji", "name": { "family": "Takimoto", "given": "Kohji" }, "orcid": "0000-0002-8405-9549" }, { "id": "Arai-Toshiaki", "name": { "family": "Arai", "given": "Toshiaki" } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "Shuji" }, "orcid": "0000-0002-5698-9634" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-Asantha", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Feder-Richard-M", "name": { "family": "Feder", "given": "Richard M." }, "orcid": "0000-0002-9330-8738" }, { "id": "Korngut-Phillip-M", "name": { "family": "Korngut", "given": "Phillip M." } }, { "id": "Lanz-Alicia", "name": { "family": "Lanz", "given": "Alicia" }, "orcid": "0000-0003-2565-1558" }, { "id": "Lee-Dae-Hee", "name": { "family": "Lee", "given": "Dae Hee" } }, { "id": "Matsumoto-Toshio", "name": { "family": "Matsumoto", "given": "Toshio" }, "orcid": "0000-0001-6066-5221" }, { "id": "Nguyen-Chi-H", "name": { "family": "Nguyen", "given": "Chi H." }, "orcid": "0000-0001-9368-3186" }, { "id": "Onishi-Yosuke", "name": { "family": "Onishi", "given": "Yosuke" } }, { "id": "Sano-Kei", "name": { "family": "Sano", "given": "Kei" }, "orcid": "0000-0002-6468-8532" }, { "id": "Shirahata-Mai", "name": { "family": "Shirahata", "given": "Mai" } }, { "id": "Takahashi-Aoi", "name": { "family": "Takahashi", "given": "Aoi" }, "orcid": "0000-0003-3881-3202" }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "Kohji" }, "orcid": "0000-0001-7143-6520" }, { "id": "Zemcov-Michael", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Polarization Spectrum of Near-Infrared Zodiacal Light Observed with CIBER", "ispublished": "pub", "full_text_status": "public", "keywords": "Infrared astronomy; Zodiacal cloud; Interplanetary dust; Spectropolarimetry; Cosmic background radiation; Diffuse radiation; Space and Planetary Science; Astronomy and Astrophysics", "note": "\u00a9 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2021 October 20; revised 2021 November 20; accepted 2021 December 7; published 2022 February 8. \n\nThis work was supported by NASA APRA research grant Nos. NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. CIBER was supported by KAKENHI (20.34, 18204018, 19540250, 21340047, 21111004, 2111717, 26800112, and 15H05744) from the Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports, Science and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from the Korea Astronomy and Space science Institute (KASI). \n\nWe would like to acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range, and also thank Dr. Allan Smith, Dr. Keith Lykke, and Dr. Steven Brown (NIST) for the laboratory calibration of LRS. P.K. and M.Z. acknowledge support from a NASA Postdoctoral Fellowship, T.A. acknowledges support from the JSPS Research Fellowship for Young Scientists, and A.C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.\n\nPublished - Takimoto_2022_ApJ_926_6.pdf
Accepted Version - 2112.05350.pdf
", "abstract": "We report the first measurement of the zodiacal light (ZL) polarization spectrum in the near-infrared between 0.8 and 1.8 \u03bcm. Using the low-resolution spectrometer on board the Cosmic Infrared Background Experiment, calibrated for absolute spectrophotometry and spectropolarimetry, we acquire long-slit polarization spectral images of the total diffuse sky brightness toward five fields. To extract the ZL spectrum, we subtract the contribution of other diffuse radiation, such as the diffuse galactic light, the integrated starlight, and the extragalactic background light. The measured ZL polarization spectrum shows little wavelength dependence in the near-infrared, and the degree of polarization clearly varies as a function of the ecliptic coordinates and solar elongation. Among the observed fields, the North Ecliptic Pole shows the maximum degree of polarization of \u223c20%, which is consistent with an earlier observation from the Diffuse Infrared Background Experiment on board on the Cosmic Background Explorer. The measured degree of polarization and its solar elongation dependence are reproduced by an empirical scattering model in the visible band and also by a Mie scattering model for large absorptive particles, while a Rayleigh scattering model is ruled out. All of our results suggest that the interplanetary dust is dominated by large particles.", "date": "2022-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "926", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 6", "id_number": "CaltechAUTHORS:20220209-266289000", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220209-266289000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "JPL Director's Research and Development Fund" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20.34" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "2111717" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26800112" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H05744" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac416f", "primary_object": { "basename": "2112.05350.pdf", "url": "https://authors.library.caltech.edu/records/vjaav-0m371/files/2112.05350.pdf" }, "related_objects": [ { "basename": "Takimoto_2022_ApJ_926_6.pdf", "url": "https://authors.library.caltech.edu/records/vjaav-0m371/files/Takimoto_2022_ApJ_926_6.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Takimoto, Kohji; Arai, Toshiaki; et el." }, { "id": "https://authors.library.caltech.edu/records/wwjnc-gqg85", "eprint_id": 113319, "eprint_status": "archive", "datestamp": "2023-09-15 07:30:32", "lastmod": "2023-10-23 21:35:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P.\u2009A.\u2009R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-Ritoban", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C.\u2009A." } }, { "name": { "family": "Beck", "given": "D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Cheshire", "given": "J.\u2009R." } }, { "name": { "family": "Connors", "given": "J." } }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Denison", "given": "E.\u2009V." } }, { "name": { "family": "Dierickx", "given": "M." } }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Eiben", "given": "M." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "name": { "family": "Filippini", "given": "J.\u2009P." } }, { "name": { "family": "Fliescher", "given": "S." } }, { "name": { "family": "Goeckner-Wald", "given": "N." } }, { "name": { "family": "Goldfinger", "given": "D.\u2009C." } }, { "name": { "family": "Grayson", "given": "J." } }, { "name": { "family": "Grimes", "given": "P." } }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halal", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." } }, { "name": { "family": "Hand", "given": "E." } }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G.\u2009C." } }, { "name": { "family": "Hubmayr", "given": "J." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." }, "orcid": "0000-0001-5812-1903" }, { "name": { "family": "Irwin", "given": "K.\u2009D." } }, { "id": "Kang-Jae-Hwan", "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K.\u2009S." } }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kernasovskiy", "given": "S.\u2009A." } }, { "name": { "family": "Kovac", "given": "J.\u2009M." } }, { "name": { "family": "Kuo", "given": "C.\u2009L." } }, { "name": { "family": "Lau", "given": "K." } }, { "name": { "family": "Leitch", "given": "E.\u2009M." } }, { "name": { "family": "Lennox", "given": "A." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Minutolo-Lorenzo", "name": { "family": "Minutolo", "given": "L." }, "orcid": "0000-0002-4876-112X" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Nakato", "given": "Y." } }, { "name": { "family": "Namikawa", "given": "T." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger-C", "name": { "family": "O'Brient", "given": "R." }, "orcid": "0000-0002-4987-6375" }, { "name": { "family": "Ogburn", "given": "R.\u2009W." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Prouve", "given": "T." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C.\u2009D." } }, { "name": { "family": "Richter", "given": "S." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Schmitt", "given": "B.\u2009L." } }, { "name": { "family": "Sheehy", "given": "C.\u2009D." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "St. Germaine", "given": "T." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." }, "orcid": "0000-0001-6544-7469" }, { "name": { "family": "Sudiwala", "given": "R.\u2009V." } }, { "id": "Teply-Grant-P", "name": { "family": "Teply", "given": "G. P." } }, { "name": { "family": "Thompson", "given": "K.\u2009L." } }, { "name": { "family": "Tolan", "given": "J.\u2009E." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Verg\u00e8s", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A.\u2009G." } }, { "id": "Wandui-Albert-K", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D.\u2009V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wong", "given": "C.\u2009L." } }, { "name": { "family": "Wu", "given": "W.\u2009L.\u2009K." } }, { "name": { "family": "Yang", "given": "H." } }, { "name": { "family": "Yoon", "given": "K.\u2009W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "name": { "family": "Zeng", "given": "L." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" }, { "id": "Zhang-Silvia", "name": { "family": "Zhang", "given": "S." } } ] }, "title": "BICEP/Keck XIV: Improved constraints on axionlike polarization oscillations in the cosmic microwave background", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2022 American Physical Society. \n\n(Received 13 August 2021; accepted 11 January 2022; published 28 January 2022) \n\nThe BICEP/Keck Array projects have been made possible through a series of grants from the National Science Foundation including Grants No. 0742818, No. 0742592, No. 1044978, No. 1110087, No. 1145172, No. 1145143, No. 1145248, No. 1639040, No. 1638957, No. 1638978, No. 1638970, and No. 1836010 and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and S.\u2009L.\u2009A.\u2009C. was partially supported by the Department of Energy, Contract No. DE-AC02-76SF00515. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP/Keck Array series of experiments.\n\nPublished - PhysRevD.105.022006.pdf
Submitted - 2108.03316.pdf
", "abstract": "We present an improved search for axionlike polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. An all-sky, temporally sinusoidal rotation of CMB polarization, equivalent to a time-variable cosmic birefringence, is an observable manifestation of a local axion field and potentially allows a CMB polarimeter to detect axionlike dark matter directly. We describe improvements to the method presented in previous work, and we demonstrate the updated method with an expanded dataset consisting of the 2012\u20132015 observing seasons. We set limits on the axion-photon coupling constant for mass m in the range 10\u207b\u00b2\u00b3\u201310\u207b\u00b9\u2078 eV, which corresponds to oscillation periods on the order of hours to years. Our results are consistent with the background model. For periods between 1 and 30 d (1.6 \u00d7 10\u207b\u00b2\u00b9 \u2264 m \u2264 4.8 \u00d7 10\u207b\u00b2\u2070 eV), the 95%-confidence upper limits on rotation amplitude are approximately constant with a median of 0.27\u00b0, which constrains the axion-photon coupling constant to g_(\u03d5\u03b3) < (4.5 \u00d7 10\u207b\u00b9\u00b2 GeV\u207b\u00b9)m/(10\u207b\u00b2\u00b9 eV), if axionlike particles constitute all of the dark matter. More than half of the collected BICEP dataset has yet to be analyzed, and several current and future CMB polarimetry experiments can apply the methods presented here to achieve comparable or superior constraints. In the coming years, oscillation measurements can achieve the sensitivity to rule out unexplored regions of the axion parameter space.", "date": "2022-01-15", "date_type": "published", "publication": "Physical Review D", "volume": "105", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 022006", "id_number": "CaltechAUTHORS:20220207-90398000", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220207-90398000", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "NSF", "grant_number": "AST-1836010" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "BICEP/Keck Collaboration" ] }, "doi": "10.1103/physrevd.105.022006", "primary_object": { "basename": "2108.03316.pdf", "url": "https://authors.library.caltech.edu/records/wwjnc-gqg85/files/2108.03316.pdf" }, "related_objects": [ { "basename": "PhysRevD.105.022006.pdf", "url": "https://authors.library.caltech.edu/records/wwjnc-gqg85/files/PhysRevD.105.022006.pdf" } ], "resource_type": "article", "pub_year": "2022", "author_list": "Ade, P.\u2009A.\u2009R.; Ahmed, Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/kannx-arh81", "eprint_id": 108678, "eprint_status": "archive", "datestamp": "2023-08-22 12:39:25", "lastmod": "2023-10-23 17:14:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gambrel-A-E", "name": { "family": "Gambrel", "given": "A. E." } }, { "name": { "family": "Rahlin", "given": "A. S." } }, { "name": { "family": "Song", "given": "X." } }, { "name": { "family": "Contaldi", "given": "C. R." } }, { "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Benton", "given": "S. J." } }, { "name": { "family": "Bergman", "given": "A. S." }, "orcid": "0000-0002-4331-1357" }, { "name": { "family": "Bihary", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Bonetti-J-A", "name": { "family": "Bonetti", "given": "J. A." } }, { "name": { "family": "Bryan", "given": "S. A." } }, { "name": { "family": "Chiang", "given": "H. C." } }, { "name": { "family": "Duivenvoorden", "given": "A. J." } }, { "name": { "family": "Eriksen", "given": "H. K." }, "orcid": "0000-0003-2332-5281" }, { "name": { "family": "Farhang", "given": "M." } }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fraisse", "given": "A. A." } }, { "name": { "family": "Freese", "given": "K." } }, { "name": { "family": "Galloway", "given": "M. M." }, "orcid": "0000-0002-8518-1888" }, { "name": { "family": "Gandilo", "given": "N. N." } }, { "name": { "family": "Gualtieri", "given": "R." } }, { "name": { "family": "Gudmundsson", "given": "J. E." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Hartley", "given": "J." } }, { "name": { "family": "Hasselfield", "given": "M." } }, { "name": { "family": "Hilton", "given": "G." }, "orcid": "0000-0003-4247-467X" }, { "id": "Holmes-Warren-A", "name": { "family": "Holmes", "given": "W." } }, { "id": "Hristov-Viktor-V", "name": { "family": "Hristov", "given": "V. V." } }, { "name": { "family": "Huang", "given": "Z." }, "orcid": "0000-0003-0592-028X" }, { "name": { "family": "Irwin", "given": "K. D." }, "orcid": "0000-0002-2998-9743" }, { "name": { "family": "Jones", "given": "W. C." } }, { "name": { "family": "Karakci", "given": "A." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Kermish", "given": "Z. D." } }, { "name": { "family": "Leung", "given": "J. S.-Y." } }, { "name": { "family": "Li", "given": "S." } }, { "name": { "family": "Mak", "given": "D. S. Y." } }, { "id": "Mason-Peter-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-Tracy-A", "name": { "family": "Morford", "given": "T. A." } }, { "name": { "family": "Nagy", "given": "J. M." }, "orcid": "0000-0002-2036-7008" }, { "name": { "family": "Netterfield", "given": "C. B." } }, { "name": { "family": "Nolta", "given": "M." } }, { "id": "O'Brient-Roger-C", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Osherson", "given": "B." }, "orcid": "0000-0001-7596-2536" }, { "name": { "family": "Padilla", "given": "I. L." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C." } }, { "name": { "family": "Ruhl", "given": "J. E." } }, { "name": { "family": "Ruud", "given": "T. M." } }, { "name": { "family": "Shariff", "given": "J. A." } }, { "name": { "family": "Shaw", "given": "E. C." } }, { "name": { "family": "Shiu", "given": "C." } }, { "name": { "family": "Soler", "given": "J. D." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "name": { "family": "Tucker", "given": "C." }, "orcid": "0000-0002-1851-3918" }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "van der List", "given": "J. F." } }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wehus", "given": "I. K." }, "orcid": "0000-0003-3821-7275" }, { "name": { "family": "Wen", "given": "S." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Young", "given": "E. Y." } } ] }, "title": "The XFaster Power Spectrum and Likelihood Estimator for the Analysis of Cosmic Microwave Background Maps", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmic microwave background radiation; Maximum likelihood estimation; Observational cosmology", "note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 May 21; revised 2021 August 24; accepted 2021 August 24; published 2021 November 25. \n\nWe acknowledge the contribution to the development of the XFaster pipeline by all members of the BOOMERanG, Planck, and Spider collaborations. Spider is supported in the U.S. by the National Aeronautics and Space Administration under grants NNX07AL64G, NNX12AE95G, and NNX17AC55G issued through the Science Mission Directorate and by the National Science Foundation through PLR-1043515. Logistical support for the Antarctic deployment and operations is provided by the NSF through the U.S. Antarctic Program. Support in Canada is provided by the Natural Sciences and Engineering Research Council and the Canadian Space Agency. Support in Norway is provided by the Research Council of Norway. Support in Sweden is provided by the Swedish Research Council through the Oskar Klein Centre (contract No. 638-2013-8993), as well as a grant from the Swedish Research Council (dnr. 2019-93959) and a grant from the Swedish Space Agency (dnr. 139/17). The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. The multiplexing readout electronics were developed with support from the Canada Foundation for Innovation and the British Columbia Knowledge Development Fund. A.E.G. is supported by the Kavli Institute for Cosmological Physics at the University of Chicago through an endowment from the Kavli Foundation and its founder, Fred Kavli. C.R.C. was supported by UKRI consolidated grants ST/P000762/1, ST/N000838/1, and ST/T000791/1. K.F. holds the Jeff and Gail Kodosky Endowed Chair at UT Austin and is grateful for that support. W.C.J. acknowledges the generous support of the David and Lucile Packard Foundation, which has been crucial to the success of the project. \n\nSome of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005). The computations described in this paper were performed on four computing clusters: Hippo at the University of KwaZulu-Natal, Feynman at Princeton University, and the GPC and Niagara supercomputers at the SciNet HPC Consortium (Loken et al. 2010; Ponce et al. 2019). SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, Ontario Research Fund\u2013Research Excellence, and the University of Toronto. \n\nThe collaboration is grateful to the British Antarctic Survey, particularly Sam Burrell, and the Alfred Wegener Institute and the crew of R.V. Polarstern for invaluable assistance with the recovery of the data and payload after the 2015 flight. Brendan Crill and Tom Montroy made significant contributions to Spider's development. This project, like so many others that he founded and supported, owes much to the vision and leadership of the late Professor Andrew E. Lange.\n\nPublished - Gambrel_2021_ApJ_922_132.pdf
Submitted - 2104.01172.pdf
", "abstract": "We present the XFaster analysis package, a fast, iterative angular power spectrum estimator based on a diagonal approximation to the quadratic Fisher matrix estimator. It uses Monte Carlo simulations to compute noise biases and filter transfer functions and is thus a hybrid of both Monte Carlo and quadratic estimator methods. In contrast to conventional pseudo-C\u2113\u2013based methods, the algorithm described here requires a minimal number of simulations and does not require them to be precisely representative of the data to estimate accurate covariance matrices for the bandpowers. The formalism works with polarization-sensitive observations and also data sets with identical, partially overlapping, or independent survey regions. The method was first implemented for the analysis of BOOMERanG data and also used as part of the Planck analysis. Here we describe the full, publicly available analysis package, written in Python, as developed for the analysis of data from the 2015 flight of the Spider instrument. The package includes extensions for self-consistently estimating null spectra and estimating fits for Galactic foreground contributions. We show results from the extensive validation of XFaster using simulations and its application to the Spider data set.", "date": "2021-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "922", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 132", "id_number": "CaltechAUTHORS:20210409-140459958", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210409-140459958", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NASA", "grant_number": "NNX17AC55G" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Research Council of Norway" }, { "agency": "Swedish Research Council", "grant_number": "638-2013-8993" }, { "agency": "Swedish Research Council", "grant_number": "2019-93959" }, { "agency": "Swedish Research Council", "grant_number": "139/17" }, { "agency": "David Dunlap Family" }, { "agency": "University of Toronto" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "British Columbia Knowledge Development Fund" }, { "agency": "Kavli Institute for Cosmological Physics" }, { "agency": "Kavli Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/P000762/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000838/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/T000791/1" }, { "agency": "University of Texas at Austin" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Compute Canada" }, { "agency": "Ontario Research Fund-Research Excellence" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac230b", "primary_object": { "basename": "2104.01172.pdf", "url": "https://authors.library.caltech.edu/records/kannx-arh81/files/2104.01172.pdf" }, "related_objects": [ { "basename": "Gambrel_2021_ApJ_922_132.pdf", "url": "https://authors.library.caltech.edu/records/kannx-arh81/files/Gambrel_2021_ApJ_922_132.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Gambrel, A. E.; Rahlin, A. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/kvyjg-xy991", "eprint_id": 111176, "eprint_status": "archive", "datestamp": "2023-08-20 05:32:59", "lastmod": "2023-10-23 15:38:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P.\u2009A.\u2009R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-Ritoban", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C.\u2009A." } }, { "name": { "family": "Beck", "given": "D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Cheshire", "given": "J.\u2009R." } }, { "name": { "family": "Connors", "given": "J." } }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." } }, { "name": { "family": "Denison", "given": "E.\u2009V." } }, { "name": { "family": "Dierickx", "given": "M." } }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Eiben", "given": "M." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "name": { "family": "Filippini", "given": "J.\u2009P." } }, { "name": { "family": "Fliescher", "given": "S." } }, { "name": { "family": "Goeckner-Wald", "given": "N." } }, { "name": { "family": "Goldfinger", "given": "D.\u2009C." } }, { "name": { "family": "Grayson", "given": "J." } }, { "name": { "family": "Grimes", "given": "P." } }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halal", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." } }, { "name": { "family": "Hand", "given": "E." } }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G.\u2009C." } }, { "name": { "family": "Hubmayr", "given": "J." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "name": { "family": "Irwin", "given": "K.\u2009D." } }, { "id": "Kang-Jae-Hwan", "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K.\u2009S." } }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kernasovskiy", "given": "S.\u2009A." } }, { "name": { "family": "Kovac", "given": "J.\u2009M." } }, { "name": { "family": "Kuo", "given": "C.\u2009L." } }, { "name": { "family": "Lau", "given": "K." } }, { "name": { "family": "Leitch", "given": "E.\u2009M." } }, { "name": { "family": "Lennox", "given": "A." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Minutolo-Lorenzo", "name": { "family": "Minutolo", "given": "L." }, "orcid": "0000-0002-4876-112X" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Nakato", "given": "Y." } }, { "name": { "family": "Namikawa", "given": "T." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Ogburn", "given": "R.\u2009W." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Prouve", "given": "T." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C.\u2009D." } }, { "name": { "family": "Richter", "given": "S." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Schmitt", "given": "B.\u2009L." } }, { "name": { "family": "Sheehy", "given": "C.\u2009D." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "Germaine", "given": "T.\u2009St." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "name": { "family": "Sudiwala", "given": "R.\u2009V." } }, { "id": "Teply-Grant-P", "name": { "family": "Teply", "given": "G. P." } }, { "name": { "family": "Thompson", "given": "K.\u2009L." } }, { "name": { "family": "Tolan", "given": "J.\u2009E." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Verg\u00e8s", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A.\u2009G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D.\u2009V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wong", "given": "C.\u2009L." } }, { "name": { "family": "Wu", "given": "W.\u2009L.\u2009K." } }, { "name": { "family": "Yang", "given": "H." } }, { "name": { "family": "Yoon", "given": "K.\u2009W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "name": { "family": "Zeng", "given": "L." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" }, { "id": "Zhang-Silvia", "name": { "family": "Zhang", "given": "S." } } ] }, "title": "Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\nReceived 21 June 2021; accepted 12 August 2021; published 4 October 2021. \n\nThe BICEP/Keck projects have been made possible through a series of grants from the National Science Foundation including Grants No. 0742818, No. 0742592, No. 1044978, No. 1110087, No. 1145172, No. 1145143, No. 1145248, No. 1639040, No. 1638957, No. 1638978, and No. 1638970, and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund, and by NASA Grants No. 06-ARPA206-0040, No. 10-SAT10-0017, No. 12-SAT12-0031, No. 14-SAT14-0009, and No. 16-SAT-16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Support for quasioptical filtering was provided by UK STFC Grant No. ST/N000706/1. The computations in this Letter were run on the Odyssey/Cannon cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and S.\u2009L.\u2009A.\u2009C. is partially supported by the U.S. DOE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz, Steffen Richter, Sam Harrison, Grantland Hall, and Hans Boenish. We thank all those who have contributed past efforts to the BICEP/Keck series of experiments, including the BICEP1 team. We also thank the Planck and WMAP teams for the use of their data, and are grateful to the Planck team for helpful discussions.\n\nPublished - PhysRevLett.127.151301.pdf
Submitted - 2110.00483.pdf
Supplemental Material - prl_supp.pdf
", "abstract": "We present results from an analysis of all data taken by the BICEP2, Keck Array, and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220\u2009\u2009GHz dataset. The Q/U maps now reach depths of 2.8, 2.8, and 8.8\u2009\u2009\u03bcK_(CMB)\u2009arcmin at 95, 150, and 220 GHz, respectively, over an effective area of \u2248600 square degrees at 95 GHz and \u2248400 square degrees at 150 and 220 GHz. The 220 GHz maps now achieve a signal-to-noise ratio on polarized dust emission exceeding that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz and evaluate the joint likelihood of the spectra versus a multicomponent model of lensed \u039bCDM + r + dust + synchrotron + noise. The foreground model has seven parameters, and no longer requires a prior on the frequency spectral index of the dust emission taken from measurements on other regions of the sky. This model is an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r_(0.05) < 0.036 at 95% confidence. Running maximum likelihood search on simulations we obtain unbiased results and find that \u03c3(r) = 0.009. These are the strongest constraints to date on primordial gravitational waves.", "date": "2021-10-08", "date_type": "published", "publication": "Physical Review Letters", "volume": "127", "number": "15", "publisher": "American Physical Society", "pagerange": "Art. No. 151301", "id_number": "CaltechAUTHORS:20211004-183512532", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20211004-183512532", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT-16-0002" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000706/1" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "BICEP Collaboration", "Keck Collaboration" ] }, "doi": "10.1103/physrevlett.127.151301", "primary_object": { "basename": "PhysRevLett.127.151301.pdf", "url": "https://authors.library.caltech.edu/records/kvyjg-xy991/files/PhysRevLett.127.151301.pdf" }, "related_objects": [ { "basename": "prl_supp.pdf", "url": "https://authors.library.caltech.edu/records/kvyjg-xy991/files/prl_supp.pdf" }, { "basename": "2110.00483.pdf", "url": "https://authors.library.caltech.edu/records/kvyjg-xy991/files/2110.00483.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Ade, P.\u2009A.\u2009R.; Ahmed, Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/0h4zv-97y29", "eprint_id": 109082, "eprint_status": "archive", "datestamp": "2023-08-22 11:28:32", "lastmod": "2023-10-23 17:38:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Yun-Ting" }, "orcid": "0000-0002-5437-0504" }, { "id": "Arai-Toshiaki", "name": { "family": "Arai", "given": "Toshiaki" } }, { "id": "Bangale-Priyadarshini", "name": { "family": "Bangale", "given": "Priyadarshini" }, "orcid": "0000-0002-3886-3739" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "Tzu-Ching" }, "orcid": "0000-0001-5929-4187" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Feder-Richard-M", "name": { "family": "Feder", "given": "Richard M." }, "orcid": "0000-0002-9330-8738" }, { "id": "Korngut-Phillip-M", "name": { "family": "Korngut", "given": "Phillip M." } }, { "id": "Lee-Dae-Hee", "name": { "family": "Lee", "given": "Dae Hee" } }, { "id": "Liu-Lunjun", "name": { "family": "Liu", "given": "Lunjun" } }, { "id": "Matsumoto-Toshio", "name": { "family": "Matsumoto", "given": "Toshio" }, "orcid": "0000-0001-6066-5221" }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "Shuji" }, "orcid": "0000-0002-5698-9634" }, { "id": "Nguyen-Chi-H", "name": { "family": "Nguyen", "given": "Chi H." }, "orcid": "0000-0001-9368-3186" }, { "id": "Sano-Kei", "name": { "family": "Sano", "given": "Kei" }, "orcid": "0000-0002-6468-8532" }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "Kohji" }, "orcid": "0000-0001-7143-6520" }, { "id": "Zemcov-Michael", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Probing Intra-Halo Light with Galaxy Stacking in CIBER Images", "ispublished": "pub", "full_text_status": "public", "keywords": "Diffuse radiation; Near infrared astronomy; Large-scale structure of the universe; Galaxy evolution; Cosmic background radiation", "note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2021 March 5; revised 2021 June 21; accepted 2021 June 24; published 2021 September 28. \n\nWe would like to thank the anonymous referee for valuable comments that improved the manuscript. We thank the dedicated efforts of the sounding rocket staff at NASA Wallops Flight Facility and White Sands Missile Range. This work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, NNX10AE12G, and 80NSSC20K0595. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. Japanese participation in CIBER was supported by KAKENHI (20.34, 18204018, 19540250, 21340047, 21111004, 24111717, 26800112, and 15H05744) from Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports, Science and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from Korea Astronomy and Space Science Institute (KASI). Y.-T.C. acknowledges support by the Ministry of Education, Taiwan through the Taiwan-Caltech Scholarship. C.H.N. acknowledges support by NASA Headquarters under the NASA Earth and Space Science Fellowship Program\u2014Grant 80NSSCK0706. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). \n\nThis publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. \n\nThe Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. \n\nFunding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrof\u00edsica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut f\u00fcr Astrophysik Potsdam (AIP), Max-Planck-Institut f\u00fcr Astronomie (MPIA Heidelberg), Max-Planck-Institut f\u00fcr Astrophysik (MPA Garching), Max-Planck-Institut f\u00fcr Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observat\u00e1rio Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Aut\u00f3noma de M\u00e9xico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. \n\nThis work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. \n\nThis work has made use of CosmoHub. CosmoHub has been developed by the Port d'Informaci\u00f3 Cient\u00edfica (PIC), maintained through a collaboration of the Institut de F\u00edsica d'Altes Energies (IFAE) and the Centro de Investigaciones Energ\u00e9ticas, Medioambientales y Tecnol\u00f3gicas (CIEMAT) and the Institute of Space Sciences (CSIC & IEEC), and was partially funded by the \"Plan Estatal de Investigaci\u00f3n Cient\u00edfica y T\u00e9cnica y de Innovaci\u00f3n\" program of the Spanish government. \n\nSoftware: astropy (Astropy Collaboration et al. 2013), emcee (Foreman-Mackey et al. 2013), corner (Foreman-Mackey 2016), astrometry.net (Lang et al. 2010), LePHARE (Arnouts et al. 1999; Ilbert et al. 2006).\n\nPublished - Cheng_2021_ApJ_919_69.pdf
Submitted - 2103.03882.pdf
", "abstract": "We study the stellar halos of 0.2 \u2272 z \u2272 0.5 galaxies with stellar masses spanning M* \u223c 10^(10.5) to 10\u00b9\u00b2 M_\u2299 (approximately L* galaxies at this redshift) using imaging data from the Cosmic Infrared Background Experiment (CIBER). A previous CIBER fluctuation analysis suggested that intra-halo light (IHL) contributes a significant portion of the near-infrared extragalactic background light (EBL), the integrated emission from all sources throughout cosmic history. In this work, we carry out a stacking analysis with a sample of \u223c30,000 Sloan Digital Sky Survey (SDSS) photometric galaxies from CIBER images in two near-infrared bands (1.1 and 1.8 \u03bcm) to directly probe the IHL associated with these galaxies. We stack galaxies in five sub-samples split by brightness and detect an extended galaxy profile beyond the instrument point-spread function (PSF) derived by stacking stars. We jointly fit a model for the inherent galaxy light profile plus large-scale one- and two-halo clustering to measure the extended galaxy IHL. We detect nonlinear one-halo clustering in the 1.8 \u03bcm band at a level consistent with numerical simulations. By extrapolating the fraction of extended galaxy light we measure to all galaxy mass scales, we find \u223c30%/15% of the total galaxy light budget from galaxies is at radius r > 10/20 kpc, respectively. These results are new at near-infrared wavelengths at the L* mass scale and suggest that the IHL emission and one-halo clustering could have appreciable contributions to the amplitude of large-scale EBL background fluctuations.", "date": "2021-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "919", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 69", "id_number": "CaltechAUTHORS:20210511-124440585", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210511-124440585", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "NASA", "grant_number": "80NSSC20K0595" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "24111717" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26800112" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H05744" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "Ministry of Education (Taipei)" }, { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "80NSSCK0706" }, { "agency": "NASA", "grant_number": "80NM0018D0004" }, { "agency": "NASA", "grant_number": "NNX08AR22G" }, { "agency": "NSF", "grant_number": "AST-1238877" }, { "agency": "University of Maryland" }, { "agency": "Eotvos Lorand University (ELTE)" }, { "agency": "Los Alamos National Laboratory" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Participating Institutions" }, { "agency": "Gaia Multilateral Agreement" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ac0f5b", "primary_object": { "basename": "Cheng_2021_ApJ_919_69.pdf", "url": "https://authors.library.caltech.edu/records/0h4zv-97y29/files/Cheng_2021_ApJ_919_69.pdf" }, "related_objects": [ { "basename": "2103.03882.pdf", "url": "https://authors.library.caltech.edu/records/0h4zv-97y29/files/2103.03882.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Cheng, Yun-Ting; Arai, Toshiaki; et el." }, { "id": "https://authors.library.caltech.edu/records/s4v3n-aac26", "eprint_id": 110659, "eprint_status": "archive", "datestamp": "2023-10-04 21:58:17", "lastmod": "2023-10-24 15:33:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Agrawal-Shubh", "name": { "family": "Agrawal", "given": "Shubh" }, "orcid": "0000-0003-2429-5811" }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "Bryan" }, "orcid": "0000-0001-6544-7469" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Frez-Clifford-F", "name": { "family": "Frez", "given": "Clifford" } }, { "id": "Minutolo-Lorenzo", "name": { "family": "Minutolo", "given": "Lorenzo" }, "orcid": "0000-0002-4876-112X" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "Hien" } }, { "id": "O'Brient-Roger-C", "name": { "family": "O'Brient", "given": "Roger" }, "orcid": "0000-0002-4987-6375" }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "Anthony" } }, { "id": "Wandui-Albert-K", "name": { "family": "Wandui", "given": "Albert" }, "orcid": "0000-0002-8232-7343" } ] }, "title": "Strong negative electrothermal feedback in thermal kinetic inductance detectors", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 Author(s). Published under an exclusive license by AIP Publishing. \n\nSubmitted: 26 July 2021; Accepted: 14 September 2021; Published Online: 28 September 2021. \n\nOur work was carried out at the Jet Propulsion Laboratory, Caltech, under contract from the National Aeronautics and Space Administration. We thank Mark Lindeman and Jonas Zmuidzinas for insightful discussion. Shubh Agrawal's work was supported by the Dr. Gary Stupian SURF Fellowship. \n\nData Availability: The data that support the findings of this study are available from the corresponding author upon reasonable request.\n\nPublished - 124503_1_online.pdf
Submitted - 2107-12493.pdf
", "abstract": "We demonstrate strong negative electrothermal feedback accelerating and linearizing the response of a thermal kinetic inductance detector (TKID). TKIDs are a proposed highly multiplexable replacement to transition-edge sensors and measure power through the temperature-dependent resonant frequency of a superconducting microresonator bolometer. At high readout probe power and probe frequency detuned from the TKID resonant frequency, we observe electrothermal feedback loop gain up to \u2112\u224816 through measuring the reduction of settling time. We also show that the detector response has no detectable non-linearity over a 38% range of incident power and that the noise-equivalent power is below the design photon noise.", "date": "2021-09-28", "date_type": "published", "publication": "Journal of Applied Physics", "volume": "130", "number": "12", "publisher": "American Institute of Physics", "pagerange": "Art. No. 124503", "id_number": "CaltechAUTHORS:20210831-203945767", "issn": "0021-8979", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210831-203945767", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Caltech Summer Undergraduate Research Fellowship (SURF)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1063/5.0064723", "primary_object": { "basename": "2107-12493.pdf", "url": "https://authors.library.caltech.edu/records/s4v3n-aac26/files/2107-12493.pdf" }, "related_objects": [ { "basename": "124503_1_online.pdf", "url": "https://authors.library.caltech.edu/records/s4v3n-aac26/files/124503_1_online.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Agrawal, Shubh; Steinbach, Bryan; et el." }, { "id": "https://authors.library.caltech.edu/records/mprae-asv49", "eprint_id": 108770, "eprint_status": "archive", "datestamp": "2023-08-20 04:25:21", "lastmod": "2023-10-23 17:18:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Minutolo-Lorenzo", "name": { "family": "Minutolo", "given": "Lorenzo" }, "orcid": "0000-0002-4876-112X" }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "Albert" }, "orcid": "0000-0002-8232-7343" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Frez-Clifford-F", "name": { "family": "Frez", "given": "Clifford F." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "Bryan" } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "Anthony" } }, { "id": "O'Brient-Roger-C", "name": { "family": "O'Brient", "given": "Roger" }, "orcid": "0000-0002-4987-6375" } ] }, "title": "Thermal Kinetic Inductance Detectors Camera: System Level Design, Strategy and Performance Forecast", "ispublished": "pub", "full_text_status": "restricted", "keywords": "KIDs, MKIDs, observational cosmology, RF, readout, TKIDs", "note": "\u00a9 2021 IEEE. \n\nManuscript receivedDecember 1, 2020; revised February 15, 2021 and March 18, 2021; accepted March 20, 2021. Date of publication March 30, 2021; date of current version May 17, 2021. \n\nThis work was supported by JPL RTD program (2016\u201319) Strategic support for TKIDs, and readout; President Director Funds, 2018\u20132020; NASA SAT: started 2020 (JPL); Moore Foundation: started 2019 (Caltech).", "abstract": "The next-generation instruments for millimeter-wave astronomy will require large arrays of detectors to surpass current performance [see (Hui, 2016) and (Ade, 2018)]. On account of integration challenges, focal planes relying on transition edge sensor (TES) bolometers will not scale gracefully. Thermal Kinetic Inductance Detectors (TKIDs) are highly scalable and have the design flexibility to solve this problem. We present an update on our detector development and systems engineering in preparation for a 2022 TKIDs camera deployment that includes noise performance, optical characterization, and a calibration strategy.", "date": "2021-08", "date_type": "published", "publication": "IEEE Transactions on Applied Superconductivity", "volume": "31", "number": "5", "publisher": "IEEE", "pagerange": "Art. No. 1501104", "id_number": "CaltechAUTHORS:20210420-091658021", "issn": "1051-8223", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210420-091658021", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL Research and Technology Development Fund" }, { "agency": "JPL President and Director's Fund" }, { "agency": "NASA" }, { "agency": "Gordon and Betty Moore Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1109/tasc.2021.3069732", "resource_type": "article", "pub_year": "2021", "author_list": "Minutolo, Lorenzo; Wandui, Albert; et el." }, { "id": "https://authors.library.caltech.edu/records/de7n2-r6v91", "eprint_id": 108164, "eprint_status": "archive", "datestamp": "2023-08-22 10:26:13", "lastmod": "2023-10-23 16:30:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sun-Guochao", "name": { "family": "Sun", "given": "G." }, "orcid": "0000-0003-4070-497X" }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "T.-C." }, "orcid": "0000-0001-5929-4187" }, { "id": "Uzgil-Bade-D", "name": { "family": "Uzgil", "given": "B. D." }, "orcid": "0000-0001-8526-3464" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-Charles-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Butler-Victoria", "name": { "family": "Butler", "given": "V." } }, { "id": "Caze-Cortes-Tessalie", "name": { "family": "Caze-Cortes", "given": "T." } }, { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Y.-T." }, "orcid": "0000-0002-5437-0504" }, { "id": "Cooray-Asantha", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Crites-Abigail-T", "name": { "family": "Crites", "given": "A. T." } }, { "id": "Hailey-Dunsheath-Steven", "name": { "family": "Hailey-Dunsheath", "given": "S." }, "orcid": "0000-0002-8504-7988" }, { "id": "Emerson-Nick", "name": { "family": "Emerson", "given": "N." } }, { "id": "Frez-Clifford", "name": { "family": "Frez", "given": "C." } }, { "id": "Hoscheit-Benjamin-L", "name": { "family": "Hoscheit", "given": "B. L." } }, { "id": "Hunacek-Jonathon-R", "name": { "family": "Hunacek", "given": "J." } }, { "id": "Keenan-Ryan-P", "name": { "family": "Keenan", "given": "R. P." } }, { "id": "Li-Chao-Te", "name": { "family": "Li", "given": "C. T." } }, { "id": "Madonia-Paolo", "name": { "family": "Madonia", "given": "P." } }, { "id": "Marrone-Daniel-P", "name": { "family": "Marrone", "given": "D. P." }, "orcid": "0000-0002-2367-1080" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Shiu-Corwin", "name": { "family": "Shiu", "given": "C." } }, { "id": "Trumper-Isaac", "name": { "family": "Trumper", "given": "I." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A." } }, { "id": "Weber-Alexis", "name": { "family": "Weber", "given": "A." } }, { "id": "Wei-Ta-Shun", "name": { "family": "Wei", "given": "T. S." } }, { "id": "Zemcov-Michael", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Probing Cosmic Reionization and Molecular Gas Growth with TIME", "ispublished": "pub", "full_text_status": "public", "keywords": "Reionization; Interstellar medium; Molecular gas; Large-scale structure of the universe; Observational cosmology; High-redshift galaxies", "note": "\u00a9 2021. The American Astronomical Society. \n\nReceived 2020 December 16; revised 2021 May 4; accepted 2021 May 4; published 2021 July 1. \n\nWe would like to thank the anonymous referees for their comments that improved the manuscript. We are indebted to Lluis Mas-Ribas for helpful comments on an early version of the paper and to Lin Yan for discussion on the [C ii] luminosity function measured from the ALPINE survey. We are also grateful to Garrett (Karto) Keating for compiling the observational constraints on molecular gas density. T.C.C. and G.S. acknowledge support from the JPL Strategic R&TD awards. A.C. acknowledges support from NSF AST-1313319 and 2015\u20132016 UCI Office of Research Seed Funding Award. D.P.M. and R.P.K. were supported by the National Science Foundation through CAREER grant AST-1653228. R.P.K. was supported by the National Science Foundation through Graduate Research Fellowship grant DGE-1746060. A.T.C. was supported by a KISS postdoctoral fellowship and a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under grant No. 1602677. This work is supported by National Science Foundation award number 1910598. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \n\nSoftware: ares (Mirocha et al. 2017), corner (Foreman-Mackey 2016), emcee (Foreman-Mackey et al. 2013), matplotlib (Hunter 2007), numpy (Walt et al. 2011), pygtc (Bocquet & Carter 2016), and scipy (Jones et al. 2001).\n\nPublished - Sun_2021_ApJ_915_33.pdf
Submitted - 2012.09160.pdf
", "abstract": "Line intensity mapping (LIM) provides a unique and powerful means to probe cosmic structures by measuring the aggregate line emission from all galaxies across redshift. The method is complementary to conventional galaxy redshift surveys that are object based and demand exquisite point-source sensitivity. The Tomographic Ionized-carbon Mapping Experiment (TIME) will measure the star formation rate during cosmic reionization by observing the redshifted [C II] 158 \u03bcm line (6 \u227e z \u227e 9) in the LIM regime. TIME will simultaneously study the abundance of molecular gas during the era of peak star formation by observing the rotational CO lines emitted by galaxies at 0.5 \u227e z \u227e 2. We present the modeling framework that predicts the constraining power of TIME on a number of observables, including the line luminosity function and the auto- and cross-correlation power spectra, including synergies with external galaxy tracers. Based on an optimized survey strategy and fiducial model parameters informed by existing observations, we forecast constraints on physical quantities relevant to reionization and galaxy evolution, such as the escape fraction of ionizing photons during reionization, the faint-end slope of the galaxy luminosity function at high redshift, and the cosmic molecular gas density at cosmic noon. We discuss how these constraints can advance our understanding of cosmological galaxy evolution at the two distinct cosmic epochs for TIME, starting in 2021, and how they could be improved in future phases of the experiment.", "date": "2021-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "915", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 33", "id_number": "CaltechAUTHORS:20210224-085555089", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210224-085555089", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "University of California, Irvine" }, { "agency": "NSF", "grant_number": "AST-1653228" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1746060" }, { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1602677" }, { "agency": "NSF", "grant_number": "AST-1910598" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" }, { "id": "Keck-Institute-for-Space-Studies" } ] }, "doi": "10.3847/1538-4357/abfe62", "primary_object": { "basename": "2012.09160.pdf", "url": "https://authors.library.caltech.edu/records/de7n2-r6v91/files/2012.09160.pdf" }, "related_objects": [ { "basename": "Sun_2021_ApJ_915_33.pdf", "url": "https://authors.library.caltech.edu/records/de7n2-r6v91/files/Sun_2021_ApJ_915_33.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Sun, G.; Chang, T.-C.; et el." }, { "id": "https://authors.library.caltech.edu/records/qfs5g-y4g48", "eprint_id": 108038, "eprint_status": "archive", "datestamp": "2023-08-20 01:52:20", "lastmod": "2023-10-23 16:25:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P.\u2009A.\u2009R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-Ritoban", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C.\u2009A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Cheshire", "given": "J.\u2009R." } }, { "name": { "family": "Connors", "given": "J." }, "orcid": "0000-0002-6094-2943" }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "id": "Filippini-Jeffrey-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fliescher", "given": "S." } }, { "name": { "family": "Goeckner-Wald", "given": "N." } }, { "name": { "family": "Grayson", "given": "J." } }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G.\u2009C." } }, { "name": { "family": "Hubmayr", "given": "J." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "name": { "family": "Irwin", "given": "K.\u2009D." } }, { "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K.\u2009S." } }, { "name": { "family": "Karpel", "given": "E." } }, { "name": { "family": "Keating", "given": "B.\u2009G." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kernasovskiy", "given": "S.\u2009A." } }, { "name": { "family": "Kovac", "given": "J.\u2009M." } }, { "name": { "family": "Kuo", "given": "C.\u2009L." } }, { "name": { "family": "Lau", "given": "K." } }, { "name": { "family": "Leitch", "given": "E.\u2009M." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Namikawa", "given": "T." } }, { "name": { "family": "Netterfield", "given": "C.\u2009B." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Ogburn", "given": "R.\u2009W." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Prouve", "given": "T." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C.\u2009D." } }, { "name": { "family": "Richter", "given": "S." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schmitt", "given": "B.\u2009L." } }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Sheehy", "given": "C.\u2009D." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "St. Germaine", "given": "T." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "name": { "family": "Sudiwala", "given": "R.\u2009V." } }, { "id": "Teply-Grant-P", "name": { "family": "Teply", "given": "G." } }, { "name": { "family": "Thompson", "given": "K.\u2009L." } }, { "name": { "family": "Tolan", "given": "J.\u2009E." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilta", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A.\u2009G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D.\u2009V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wong", "given": "C.\u2009L." } }, { "name": { "family": "Wu", "given": "W.\u2009L.\u2009K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "H." } }, { "name": { "family": "Yoon", "given": "K.\u2009W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "name": { "family": "Zeng", "given": "L." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "BICEP/Keck XII: Constraints on axionlike polarization oscillations in the cosmic microwave background", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\nReceived 17 November 2020; accepted 7 January 2021; published 12 February 2021. \n\nWe thank Adam J. Anderson, Aviv R. Cukierman, Michael A. Fedderke, and Ethan O. Nadler for useful conversations. The BICEP/Keck projects have been made possible through a series of grants from the National Science Foundation including Grants No. 0742818, No. 0742592, No. 1044978, No. 1110087, No. 1145172, No. 1145143, No. 1145248, No. 1639040, No. 1638957, No. 1638978, No. 1638970, and No. 1836010, and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the Jet Propulsion Laboratory (JPL) Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA Astrophysics Research and Analysis program (APRA) and Strategic Astrophysics Technology (SAT) programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and S.\u2009L.\u2009A.\u2009C. was partially supported by the Department of Energy, Contract No. DE-AC02-76SF00515. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP/Keck series of experiments, including the BICEP1 team.\n\nPublished - PhysRevD.103.042002.pdf
Submitted - 2011.03483.pdf
", "abstract": "We present a search for axionlike polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. A local axion field induces an all-sky, temporally sinusoidal rotation of CMB polarization. A CMB polarimeter can thus function as a direct-detection experiment for axionlike dark matter. We develop techniques to extract an oscillation signal. Many elements of the method are generic to CMB polarimetry experiments and can be adapted for other datasets. As a first demonstration, we process data from the 2012 observing season to set upper limits on the axion-photon coupling constant in the mass range 10\u207b\u00b2\u00b9\u201310\u207b\u00b9\u2078\u2009eV, which corresponds to oscillation periods on the order of hours to months. We find no statistically significant deviations from the background model. For periods larger than 24 hr (mass m < 4 .8\u00d710\u207b\u00b2\u2070\u2009\u2009eV), the median 95% confidence upper limit is equivalent to a rotation amplitude of 0.68\u00b0, which constrains the axion-photon coupling constant to g_(\u03d5\u03b3) < (1.1\u00d710\u207b\u00b9\u00b9\u2009GeV\u207b\u00b9)m/(10\u207b\u00b2\u00b9\u2009eV), if axionlike particles constitute all of the dark matter. The constraints can be improved substantially with data already collected by the BICEP series of experiments. Current and future CMB polarimetry experiments are expected to achieve sufficient sensitivity to rule out unexplored regions of the axion parameter space.", "date": "2021-02-15", "date_type": "published", "publication": "Physical Review D", "volume": "103", "number": "4", "publisher": "American Physical Society", "pagerange": "Art. No. 042002", "id_number": "CaltechAUTHORS:20210212-124140264", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210212-124140264", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "NSF", "grant_number": "AST-1836010" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "BICEP Collaboration", "Keck Collaboration" ] }, "doi": "10.1103/physrevd.103.042002", "primary_object": { "basename": "2011.03483.pdf", "url": "https://authors.library.caltech.edu/records/qfs5g-y4g48/files/2011.03483.pdf" }, "related_objects": [ { "basename": "PhysRevD.103.042002.pdf", "url": "https://authors.library.caltech.edu/records/qfs5g-y4g48/files/PhysRevD.103.042002.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Ade, P.\u2009A.\u2009R.; Ahmed, Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/h51f3-5es64", "eprint_id": 107874, "eprint_status": "archive", "datestamp": "2023-08-22 08:44:52", "lastmod": "2023-10-23 16:18:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Symons-Teresa", "name": { "family": "Symons", "given": "Teresa" }, "orcid": "0000-0002-9554-1082" }, { "id": "Zemcov-Michael", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Yun-Ting" }, "orcid": "0000-0002-5437-0504" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "Brendan" }, "orcid": "0000-0002-4650-8518" }, { "id": "Hirata-C-M", "name": { "family": "Hirata", "given": "Christopher" }, "orcid": "0000-0002-2951-4932" }, { "id": "Venuto-Stephanie", "name": { "family": "Venuto", "given": "Stephanie" } } ] }, "title": "Superresolution Reconstruction of Severely Undersampled Point-spread Functions Using Point-source Stacking and Deconvolution", "ispublished": "pub", "full_text_status": "public", "keywords": "Astrostatistics techniques; Deconvolution; Astronomy data analysis; Computational methods", "note": "\u00a9 2021 The American Astronomical Society. \n\nReceived 2020 July 16; revised 2020 November 3; accepted 2020 November 13; published 2021 February 1. \n\nThanks to Chi Nguyen for helpful comments and suggestions. This work was supported by NASA awards 80GSFC18C0011/S442557, NNN12AA01C/1594971, and 80NSSC18K1557. The research was partly carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA (80NM0018D0004). \n\nThis publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. \n\nThe authors acknowledge Research Computing at the Rochester Institute of Technology for providing computational resources and support that have contributed to the research results reported in this publication. \n\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018), Matplotlib (Hunter 2007), NumPy (Van Der Walt et al. 2011), SciPy (Virtanen et al. 2020).\n\nPublished - Symons_2021_ApJS_252_24.pdf
", "abstract": "Point-spread function (PSF) estimation in spatially undersampled images is challenging because large pixels average fine-scale spatial information. This is problematic when fine-resolution details are necessary, as in optimal photometry where knowledge of the illumination pattern beyond the native spatial resolution of the image may be required. Here, we introduce a method of PSF reconstruction where point sources are artificially sampled beyond the native resolution of an image and combined together via stacking to return a finely sampled estimate of the PSF. This estimate is then deconvolved from the pixel-gridding function to return a superresolution kernel that can be used for optimally weighted photometry. We benchmark against the <1% photometric error requirement of the upcoming SPHEREx mission to assess performance in a concrete example. We find that standard methods like Richardson\u2013Lucy deconvolution are not sufficient to achieve this stringent requirement. We investigate a more advanced method with significant heritage in image analysis called iterative back-projection (IBP) and demonstrate it using idealized Gaussian cases and simulated SPHEREx images. In testing this method on real images recorded by the LORRI instrument on New Horizons, we are able to identify systematic pointing drift. Our IBP-derived PSF kernels allow photometric accuracy significantly better than the requirement in individual SPHEREx exposures. This PSF reconstruction method is broadly applicable to a variety of problems and combines computationally simple techniques in a way that is robust to complicating factors such as severe undersampling, spatially complex PSFs, noise, crowded fields, or limited source numbers.", "date": "2021-02", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "252", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 24", "id_number": "CaltechAUTHORS:20210202-122853538", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210202-122853538", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "80GSFC18C0011/S442557" }, { "agency": "NASA", "grant_number": "NNN12AA01C/1594971" }, { "agency": "NASA", "grant_number": "80NSSC18K1557" }, { "agency": "NASA", "grant_number": "80NM0018D0004" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Gaia Multilateral Agreement" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4365/abcaa5", "primary_object": { "basename": "Symons_2021_ApJS_252_24.pdf", "url": "https://authors.library.caltech.edu/records/h51f3-5es64/files/Symons_2021_ApJS_252_24.pdf" }, "resource_type": "article", "pub_year": "2021", "author_list": "Symons, Teresa; Zemcov, Michael; et el." }, { "id": "https://authors.library.caltech.edu/records/pc0kb-6f774", "eprint_id": 107771, "eprint_status": "archive", "datestamp": "2023-08-20 01:25:54", "lastmod": "2023-10-23 16:14:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Anderson", "given": "A.\u2009J." } }, { "name": { "family": "Austermann", "given": "J.\u2009E." } }, { "name": { "family": "Avva", "given": "J.\u2009S." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-Ritoban", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Beall", "given": "J.\u2009A." } }, { "name": { "family": "Bender", "given": "A.\u2009N." } }, { "name": { "family": "Benson", "given": "B.\u2009A." } }, { "name": { "family": "Bianchini", "given": "F." }, "orcid": "0000-0003-4847-3483" }, { "name": { "family": "Bischoff", "given": "C.\u2009A." } }, { "name": { "family": "Bleem", "given": "L.\u2009E." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Carlstrom", "given": "J.\u2009E." } }, { "name": { "family": "Chang", "given": "C.\u2009L." } }, { "name": { "family": "Cheshire", "given": "J.\u2009R." } }, { "name": { "family": "Chiang", "given": "H.\u2009C." } }, { "name": { "family": "Chou", "given": "T-L." } }, { "name": { "family": "Citron", "given": "R." } }, { "name": { "family": "Connors", "given": "J." }, "orcid": "0000-0002-6094-2943" }, { "id": "Moran-C-Corbett", "name": { "family": "Moran", "given": "C. Corbett" }, "orcid": "0000-0003-2088-7465" }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crawford", "given": "T.\u2009M." } }, { "name": { "family": "Crites", "given": "A.\u2009T." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "de Haan", "given": "T." }, "orcid": "0000-0001-5105-9473" }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Dobbs", "given": "M.\u2009A." } }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Everett", "given": "W." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "id": "Filippini-Jeffrey-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fliescher", "given": "S." } }, { "name": { "family": "Gallicchio", "given": "J." } }, { "name": { "family": "George", "given": "E.\u2009M." } }, { "name": { "family": "St. Germaine", "given": "T." } }, { "name": { "family": "Goeckner-Wald", "given": "N." } }, { "name": { "family": "Goldfinger", "given": "D.\u2009C." } }, { "name": { "family": "Grayson", "given": "J." } }, { "name": { "family": "Gupta", "given": "N." } }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Halverson", "given": "N.\u2009W." } }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "name": { "family": "Henning", "given": "J.\u2009W." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G. C." }, "orcid": "0000-0003-4247-467X" }, { "name": { "family": "Holder", "given": "G.\u2009P." } }, { "name": { "family": "Holzapfel", "given": "W.\u2009L." } }, { "name": { "family": "Hrubes", "given": "J.\u2009D." } }, { "name": { "family": "Huang", "given": "N." } }, { "name": { "family": "Hubmayr", "given": "J." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "name": { "family": "Irwin", "given": "K.\u2009D." } }, { "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K. S." }, "orcid": "0000-0002-5215-6993" }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kernasovskiy", "given": "S.\u2009A." } }, { "name": { "family": "Knox", "given": "L." } }, { "name": { "family": "Kovac", "given": "J.\u2009M." } }, { "name": { "family": "Kuo", "given": "C.\u2009L." } }, { "name": { "family": "Lau", "given": "K." } }, { "name": { "family": "Lee", "given": "A.\u2009T." } }, { "name": { "family": "Leitch", "given": "E.\u2009M." } }, { "name": { "family": "Li", "given": "D." } }, { "name": { "family": "Lowitz", "given": "A." } }, { "name": { "family": "Manzotti", "given": "A." }, "orcid": "0000-0003-0057-877X" }, { "name": { "family": "McMahon", "given": "J.\u2009J." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K." } }, { "name": { "family": "Meyer", "given": "S.\u2009S." } }, { "name": { "family": "Millea", "given": "M." } }, { "name": { "family": "Mocanu", "given": "L.\u2009M." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Montgomery", "given": "J." } }, { "name": { "family": "Nadolski", "given": "A." } }, { "name": { "family": "Namikawa", "given": "T." } }, { "name": { "family": "Natoli", "given": "T." } }, { "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "name": { "family": "Nibarger", "given": "J.\u2009P." } }, { "name": { "family": "Noble", "given": "G." } }, { "name": { "family": "Novosad", "given": "V." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Ogburn", "given": "R.\u2009W." } }, { "name": { "family": "Omori", "given": "Y." }, "orcid": "0000-0002-0963-7310" }, { "id": "Padin-S", "name": { "family": "Padin", "given": "S." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Patil", "given": "S." } }, { "name": { "family": "Prouve", "given": "T." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reichardt", "given": "C.\u2009L." } }, { "name": { "family": "Reintsema", "given": "C.\u2009D." } }, { "name": { "family": "Richter", "given": "S." } }, { "name": { "family": "Ruhl", "given": "J.\u2009E." } }, { "name": { "family": "Saliwanchik", "given": "B.\u2009R." } }, { "name": { "family": "Schaffer", "given": "K.\u2009K." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schmitt", "given": "B.\u2009L." } }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Sheehy", "given": "C.\u2009D." } }, { "name": { "family": "Sievers", "given": "C." } }, { "name": { "family": "Smecher", "given": "G." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "Stark", "given": "A.\u2009A." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "name": { "family": "Sudiwala", "given": "R.\u2009V." } }, { "id": "Teply-Grant-P", "name": { "family": "Teply", "given": "G. P." } }, { "name": { "family": "Thompson", "given": "K.\u2009L." } }, { "name": { "family": "Tolan", "given": "J.\u2009E." } }, { "name": { "family": "Tucker", "given": "C." }, "orcid": "0000-0002-1851-3918" }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Veach", "given": "T." } }, { "name": { "family": "Vieira", "given": "J.\u2009D." } }, { "name": { "family": "Vieregg", "given": "A.\u2009G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "name": { "family": "Wang", "given": "G." } }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Whitehorn", "given": "N." }, "orcid": "0000-0002-3157-0407" }, { "name": { "family": "Wiebe", "given": "D.\u2009V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wong", "given": "C.\u2009L." } }, { "name": { "family": "Wu", "given": "W.\u2009L.\u2009K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "H." } }, { "name": { "family": "Yefremenko", "given": "V." } }, { "name": { "family": "Yoon", "given": "K.\u2009W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "name": { "family": "Zeng", "given": "L." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "A demonstration of improved constraints on primordial gravitational waves with delensing", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2021 American Physical Society. \n\nReceived 18 November 2020; accepted 23 December 2020; published 26 January 2021. \n\nThe authors thank Dominic Beck and Chang Feng for useful comments on an early version of the draft. The bicep2/Keck Array projects have been made possible through a series of grants from the National Science Foundation including Grants No. 0742818, No. 0742592, No. 1044978, No. 1110087, No. 1145172, No. 1145143, No. 1145248, No. 1639040, No. 1638957, No. 1638978, and No. 1638970, and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund, and by NASA Grants No. 06-ARPA206-0040, No. 10-SAT10-0017, No. 12-SAT12-0031, No. 14-SAT14-0009, and No. 16-SAT-16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Support for quasioptical filtering was provided by UK STFC Grant No. ST/N000706/1. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and S.\u2009L.\u2009A.\u2009C. is partially supported by the U.S. DOE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the bicep\u2013Keck Array series of experiments, including the bicep1 team. S.\u2009P.\u2009T. is supported by the National Science Foundation through Grants No. PLR-1248097 and No. OPP-1852617. Partial support is also provided by the NSF Physics Frontier Center Grant No. PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation Grant No. GBMF 947. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. The Melbourne group acknowledges support from the University of Melbourne and an Australian Research Council's Future Fellowship (FT150100074). Work at Argonne National Lab is supported by UChicago Argonne LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. Work at McGill is supported by the Natural Science and Engineering Research Council of Canada, the Canadian Institute for Advanced Research, and M.\u2009D. acknowledges a Killam research fellowship W.\u2009L.\u2009K.\u2009W. is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through Grant No. NSF PHY-1125897, an endowment from the Kavli Foundation and its founder Fred Kavli, and by the Department of Energy, Laboratory Directed Research and Development program and as part of the Panofsky Fellowship program at SLAC National Accelerator Laboratory, under Contract No. DE-AC02-76SF00515. B.\u2009B. is supported by the Fermi Research Alliance LLC under Contract No. De-AC02- 07CH11359 with the U.S. Department of Energy. We acknowledge the use of many python packages: ipython [69], matplotlib [70], scipy [71], and healpy [72,73]. We also thank the Planck and WMAP teams for the use of their data. Some of the sky simulations used in this paper were developed by the WebSky Extragalactic CMB Mocks team, with the continuous support of the Canadian Institute for Theoretical Astrophysics (CITA), the Canadian Institute for Advanced Research (CIFAR), and the Natural Sciences and Engineering Research Council of Canada (NSERC), and were generated on the Niagara supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund\u2014Research Excellence; and the University of Toronto.\n\nPublished - PhysRevD.103.022004.pdf
Submitted - 2011.08163.pdf
", "abstract": "We present a constraint on the tensor-to-scalar ratio, r, derived from measurements of cosmic microwave background (CMB) polarization B-modes with \"delensing,\" whereby the uncertainty on r contributed by the sample variance of the gravitational lensing B-modes is reduced by cross-correlating against a lensing B-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, BICEP/Keck, and Planck data. We expand the BICEP/Keck likelihood analysis framework to accept a lensing template and apply it to the BICEP/Keck dataset collected through 2014 using the same parametric foreground modeling as in the previous analysis. From simulations, we find that the uncertainty on r is reduced by \u223c10%, from \u03c3(r) = 0.024 to 0.022, which can be compared with a \u223c26% reduction obtained when using a perfect lensing template or if there were zero lensing B-modes. Applying the technique to the real data, the constraint on r is improved from r_(0.05) < 0.090 to r_(0.05) < 0.082 (95% C.L.). This is the first demonstration of improvement in an r constraint through delensing.", "date": "2021-01-15", "date_type": "published", "publication": "Physical Review D", "volume": "103", "number": "2", "publisher": "American Physical Society", "pagerange": "Art. No. 022004", "id_number": "CaltechAUTHORS:20210127-093358968", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210127-093358968", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT-16-0002" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF 947" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000706/1" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "NSF", "grant_number": "PLR-1248097" }, { "agency": "NSF", "grant_number": "OPP-1852617" }, { "agency": "NSF", "grant_number": "PHY-1125897" }, { "agency": "Kavli Foundation" }, { "agency": "University of Melbourne" }, { "agency": "Australian Research Council", "grant_number": "FT150100074" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-06CH11357" }, { "agency": "Argonne Center for Nanoscale Materials" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Killam Research Fellowship" }, { "agency": "Kavli Institute for Cosmological Physics" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-07CH11359" }, { "agency": "Canadian Institute for Theoretical Astrophysics (CITA)" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canada Foundation for Innovation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "BICEP Collaboration", "Keck Collaboration", "SPTpol Collaboration" ] }, "doi": "10.1103/physrevd.103.022004", "primary_object": { "basename": "2011.08163.pdf", "url": "https://authors.library.caltech.edu/records/pc0kb-6f774/files/2011.08163.pdf" }, "related_objects": [ { "basename": "PhysRevD.103.022004.pdf", "url": "https://authors.library.caltech.edu/records/pc0kb-6f774/files/PhysRevD.103.022004.pdf" } ], "resource_type": "article", "pub_year": "2021", "author_list": "Ade, P. A. R.; Ahmed, Z.; et el." }, { "id": "https://authors.library.caltech.edu/records/hprmd-0jb19", "eprint_id": 104440, "eprint_status": "archive", "datestamp": "2023-08-22 06:52:27", "lastmod": "2023-10-20 20:28:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Yun-Ting" }, "orcid": "0000-0002-5437-0504" }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "Tzu-Ching" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Phase-space Spectral Line Deconfusion in Intensity Mapping", "ispublished": "pub", "full_text_status": "public", "keywords": "Observational cosmology; Large-scale structure of the universe; Diffuse radiation", "note": "\u00a9 2020 The American Astronomical Society. \n\nReceived 2020 May 10; revised 2020 August 11; accepted 2020 August 16; published 2020 October 1. \n\nWe are grateful for the helpful discussions with Chun-Lin Liu, Patrick Breysse, Matthieu B\u00e9thermin, Emmanuel Schaan, Matt Orr, the TIME collaboration, the Caltech ObsCos group, and the participants of the conference \"Lines in the Large Scale Structure.\" We would like to thank the anonymous referee for valuable comments that improved the manuscript. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.\n\nPublished - Cheng_2020_ApJ_901_142.pdf
Submitted - 2005.05341.pdf
", "abstract": "Line intensity mapping (LIM) is a promising tool to efficiently probe the three-dimensional large-scale structure by mapping the aggregate emission of a spectral line from all sources that trace the matter density field. Spectral lines from different redshifts can fall in the same observed frequency and be confused, however, which is a major challenge in LIM. In this work, we develop a line deconfusion technique in map space capable of reconstructing the three-dimensional spatial distribution of line-emitting sources. If multiple spectral lines of a source population are observable in multiple frequencies, using the sparse approximation, our technique iteratively extracts sources along a given line of sight by fitting the LIM data to a set of spectral templates. We demonstrate that the technique successfully extracts sources with emission lines present at a few \u03c3 above the noise level, taking into account uncertainties in the source modeling and presence of continuum foreground contamination and noise fluctuations. As an example, we consider a Tomographic Ionized-carbon Mapping Experiment/CarbON C II line in post-rEionisation and ReionisaTiOn epoch (TIME/CONCERTO)-like survey targeting [C II] at the epoch of reionization, and reliably reconstruct the 3D spatial distribution of the CO interlopers and their luminosity functions at 0.5 \u227e z \u227e 1.5. We also demonstrate a successful deconfusion for the Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer (SPHEREx) mission in the near-infrared wavelengths. We discuss a formalism in which the reconstructed maps can be further cross-correlated with a (galaxy) tracer population to estimate the total interloper power. This technique is a general framework to extract the phase-space distribution of low-redshift interlopers, without the need of external information, for any line deconfusion problem.", "date": "2020-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "901", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 142", "id_number": "CaltechAUTHORS:20200720-082506342", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200720-082506342", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/abb023", "primary_object": { "basename": "2005.05341.pdf", "url": "https://authors.library.caltech.edu/records/hprmd-0jb19/files/2005.05341.pdf" }, "related_objects": [ { "basename": "Cheng_2020_ApJ_901_142.pdf", "url": "https://authors.library.caltech.edu/records/hprmd-0jb19/files/Cheng_2020_ApJ_901_142.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Cheng, Yun-Ting; Chang, Tzu-Ching; et el." }, { "id": "https://authors.library.caltech.edu/records/erkpg-pt466", "eprint_id": 96756, "eprint_status": "archive", "datestamp": "2023-08-19 23:05:11", "lastmod": "2023-10-20 21:29:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Akrami-Yashar", "name": { "family": "Akrami", "given": "Y." }, "orcid": "0000-0002-2407-7956" }, { "id": "Ghosh-T", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "G\u00f3rski-K-M", "name": { "family": "G\u00f3rski", "given": "K. M." } }, { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "id": "Roudier-G", "name": { "family": "Roudier", "given": "G." } }, { "id": "Wehus-I-K", "name": { "family": "Wehus", "given": "I. K." } } ] }, "title": "Planck 2018 results. I. Overview and the cosmological legacy of Planck", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmology: theory \u2013 cosmic background radiation \u2013 surveys", "note": "\u00a9 2020 ESO. Article published by EDP Sciences. \n\nReceived 16 July 2018; Accepted 27 September 2019; Published online 11 September 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states (in particular the lead countries France and Italy), with contributions from NASA (USA), and telescope reflectors provided by a collaboration between ESA and a scientific consortium led and funded by Denmark. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.cosmos.esa.int/web/planck/ planck-collaboration. In addition, we thank Sol\u00e8ne Chabanier and Nathalie Palanque-Delabrouille for computing the Ly\u2006\u03b1 forest constraints we have used in Fig. 19 and Inigo Zubeldia for preparing Fig. 32.\n\nPublished - aa33880-18.pdf
Submitted - 1807.06205.pdf
", "abstract": "The European Space Agency's Planck satellite, which was dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013, producing deep, high-resolution, all-sky maps in nine frequency bands from 30 to 857 GHz. This paper presents the cosmological legacy of Planck, which currently provides our strongest constraints on the parameters of the standard cosmological model and some of the tightest limits available on deviations from that model. The 6-parameter \u039bCDM model continues to provide an excellent fit to the cosmic microwave background data at high and low redshift, describing the cosmological information in over a billion map pixels with just six parameters. With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the six parameters to better than 1% (simultaneously), with the best-determined parameter (\u03b8*) now known to 0.03%. We describe the multi-component sky as seen by Planck, the success of the \u039bCDM model, and the connection to lower-redshift probes of structure formation. We also give a comprehensive summary of the major changes introduced in this 2018 release. The Planck data, alone and in combination with other probes, provide stringent constraints on our models of the early Universe and the large-scale structure within which all astrophysical objects form and evolve. We discuss some lessons learned from the Planck mission, and highlight areas ripe for further experimental advances.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "number": "Art. No. A1", "publisher": "EDP Sciences", "id_number": "CaltechAUTHORS:20190626-154014679", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190626-154014679", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministry of Science, Innovation and Universities (MICINN)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833880", "primary_object": { "basename": "1807.06205.pdf", "url": "https://authors.library.caltech.edu/records/erkpg-pt466/files/1807.06205.pdf" }, "related_objects": [ { "basename": "aa33880-18.pdf", "url": "https://authors.library.caltech.edu/records/erkpg-pt466/files/aa33880-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Akrami, Y.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/qfgj3-qkf16", "eprint_id": 98843, "eprint_status": "archive", "datestamp": "2023-08-19 23:05:47", "lastmod": "2023-10-18 17:40:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Ghosh-Tuhin", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "G\u00f3rski-Krzysztof-M", "name": { "family": "G\u00f3rski", "given": "K. M." }, "orcid": "0000-0003-2933-8630" }, { "id": "Lawrence-Charles-R", "name": { "family": "Lawrence", "given": "C. R." }, "orcid": "0000-0002-5983-6481" }, { "id": "Roudier-Gael-M", "name": { "family": "Roudier", "given": "G." }, "orcid": "0000-0002-7402-7797" } ] }, "title": "Planck 2018 results. V. CMB power spectra and likelihoods", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 cosmological parameters \u2013 methods: data analysis", "note": "\u00a9 2020 Planck Collaboration. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nReceived 25 July 2019; Accepted 25 May 2020; Published online 11 September 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research used resources of the IN2P3 Computer Center (http://cc.in2p3.fr) as well as of the Planck-HFI DPC infrastructure hosted at the Institut d'Astrophysique de Paris (France) and financially supported by CNES.\n\nPublished - aa36386-19.pdf
Submitted - 1907.12875.pdf
", "abstract": "We describe the legacy Planck cosmic microwave background (CMB) likelihoods derived from the 2018 data release. The overall approach is similar in spirit to the one retained for the 2013 and 2015 data release, with a hybrid method using different approximations at low (\u2113\u2004< \u200430) and high (\u2113\u2004\u2265\u200430) multipoles, implementing several methodological and data-analysis refinements compared to previous releases. With more realistic simulations, and better correction and modelling of systematic effects, we can now make full use of the CMB polarization observed in the High Frequency Instrument (HFI) channels. The low-multipole EE cross-spectra from the 100 GHz and 143 GHz data give a constraint on the \u039bCDM reionization optical-depth parameter \u03c4 to better than 15% (in combination with the TT low-\u2113 data and the high-\u2113 temperature and polarization data), tightening constraints on all parameters with posterior distributions correlated with \u03c4. We also update the weaker constraint on \u03c4 from the joint TEB likelihood using the Low Frequency Instrument (LFI) channels, which was used in 2015 as part of our baseline analysis. At higher multipoles, the CMB temperature spectrum and likelihood are very similar to previous releases. A better model of the temperature-to-polarization leakage and corrections for the effective calibrations of the polarization channels (i.e., the polarization efficiencies) allow us to make full use of polarization spectra, improving the \u039bCDM constraints on the parameters \u03b8MC, \u03c9c, \u03c9b, and H0 by more than 30%, and n_s by more than 20% compared to TT-only constraints. Extensive tests on the robustness of the modelling of the polarization data demonstrate good consistency, with some residual modelling uncertainties. At high multipoles, we are now limited mainly by the accuracy of the polarization efficiency modelling. Using our various tests, simulations, and comparison between different high-multipole likelihood implementations, we estimate the consistency of the results to be better than the 0.5\u2006\u03c3 level on the \u039bCDM parameters, as well as classical single-parameter extensions for the joint likelihood (to be compared to the 0.3\u2006\u03c3 levels we achieved in 2015 for the temperature data alone on \u039bCDM only). Minor curiosities already present in the previous releases remain, such as the differences between the best-fit \u039bCDM parameters for the \u2113\u2004< \u2004800 and \u2113\u2004> \u2004800 ranges of the power spectrum, or the preference for more smoothing of the power-spectrum peaks than predicted in \u039bCDM fits. These are shown to be driven by the temperature power spectrum and are not significantly modified by the inclusion of the polarization data. Overall, the legacy Planck CMB likelihoods provide a robust tool for constraining the cosmological model and represent a reference for future CMB observations.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A5", "id_number": "CaltechAUTHORS:20190925-091335835", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190925-091335835", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Red Espa\u00f1ola de Supercomputaci\u00f3n (RES)" }, { "agency": "Ministry of Employment and the Economy (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201936386", "primary_object": { "basename": "1907.12875.pdf", "url": "https://authors.library.caltech.edu/records/qfgj3-qkf16/files/1907.12875.pdf" }, "related_objects": [ { "basename": "aa36386-19.pdf", "url": "https://authors.library.caltech.edu/records/qfgj3-qkf16/files/aa36386-19.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Aghanim, N.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/74pef-jas67", "eprint_id": 99005, "eprint_status": "archive", "datestamp": "2023-08-19 23:06:31", "lastmod": "2023-10-20 22:52:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Ghosh-Tuhin", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "G\u00f3rski-Krzysztof-M", "name": { "family": "G\u00f3rski", "given": "K. M." }, "orcid": "0000-0003-2933-8630" }, { "id": "Lawrence-Charles-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "id": "Roudier-Gael-M", "name": { "family": "Roudier", "given": "G." }, "orcid": "0000-0002-7402-7797" } ] }, "title": "Planck 2018 results. VI. Cosmological parameters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmological parameters", "note": "\u00a9 2020 ESO. Article published by EDP Sciences. \n\nReceived 20 July 2018; Accepted 20 March 2020; Published online 11 September 2020. \n\nThe Planck Collaboration acknowledges the support of:\nESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF\n(Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO,\nJA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany);\nCSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN\n(Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A\ndescription of the Planck Collaboration and a list of its members, indicating\nwhich technical or scientific activities they have been involved in, can be found\nat https://www.cosmos.esa.int/web/planck/planck-collaboration.\nWe additionally acknowledge support from the European Research Council\nunder the European Union's Seventh Framework Programme (FP/2007-\n2013)/ERC Grant Agreement No. [616170]. This project has received funding\nfrom the European Research Council (ERC) under the European Union's Horizon\n2020 research and innovation programme (grant agreement No 725456,\nCMBSPEC). We thank Ofelia Pisanti for providing updated numerical BBN\nresults from the PArthENoPE code, Cyril Pitrou for producing some results from\nthe PRIMAT code, and the DES team for sharing their likelihoods. We also thank\nMarco Crisostomi, Ignacy Sawicky, Alessandra Silvestri, and Filippo Vernizzi\nfor discussions on the dark-energy and modified-gravity models. Some of the\nresults in this paper have been derived using the HEALPix package.\n\nPlanck 2018 results - VI. Cosmological parameters (Corrigendum).\nPlanck Collaboration, N. Aghanim, et. al.,\nA&A, 652 (2021) C4;\nDOI: https://doi.org/10.1051/0004-6361/201833910e\n\nPublished - aa33910-18.pdf
Submitted - 1807.06209.pdf
Erratum - aa33910e-18.pdf
", "abstract": "We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction. Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters. Improved modelling of the small-scale polarization leads to more robust constraints on many parameters, with residual modelling uncertainties estimated to affect them only at the 0.5\u03c3 level. We find good consistency with the standard spatially-flat 6-parameter \u039bCDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted \"base \u039bCDM\" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density \u03a9_ch\u00b2\u2004=\u20040.120 \u00b1 0.001, baryon density \u03a9_bh\u00b2\u2004=\u20040.0224 \u00b1 0.0001, scalar spectral index n_s\u2004=\u20040.965 \u00b1 0.004, and optical depth \u03c4\u2004=\u20040.054 \u00b1 0.007 (in this abstract we quote 68% confidence regions on measured parameters and 95% on upper limits). The angular acoustic scale is measured to 0.03% precision, with 100\u03b8*\u2004=\u20041.0411 \u00b1 0.0003. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-\u039bCDM cosmology, the inferred (model-dependent) late-Universe parameters are: Hubble constant H\u2080\u2004=\u2004(67.4 \u00b1 0.5)\u2006\u2006km\u2006s\u207b\u00b9\u2006Mpc\u207b\u00b9; matter density parameter \u03a9m\u2004=\u20040.315 \u00b1 0.007; and matter fluctuation amplitude \u03c3\u2088\u2004=\u20040.811 \u00b1 0.006. We find no compelling evidence for extensions to the base-\u039bCDM model. Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter extensions) we constrain the effective extra relativistic degrees of freedom to be N_(eff)\u2004=\u20042.99 \u00b1 0.17, in agreement with the Standard Model prediction N_(eff)\u2004=\u20043.046, and find that the neutrino mass is tightly constrained to \u2211m_\u03bd\u2004< \u20040.12\u2006\u2006eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base \u039bCDM at over 2\u03c3, which pulls some parameters that affect the lensing amplitude away from the \u039bCDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. The joint constraint with BAO measurements on spatial curvature is consistent with a flat universe, \u03a9_K\u2004=\u20040.001 \u00b1 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w\u2080\u2004=\u2004\u22121.03 \u00b1 0.03, consistent with a cosmological constant. We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r_(0.002)\u2004< \u20040.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-\u039bCDM cosmology are in excellent agreement with observations. The Planck base-\u039bCDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey's combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 3.6\u03c3, tension with local measurements of the Hubble constant (which prefer a higher value). Simple model extensions that can partially resolve these tensions are not favoured by the Planck data.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A6", "id_number": "CaltechAUTHORS:20191002-090602025", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191002-090602025", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Ministry of Employment and the Economy (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "616170" }, { "agency": "European Research Council (ERC)", "grant_number": "725456" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833910", "primary_object": { "basename": "1807.06209.pdf", "url": "https://authors.library.caltech.edu/records/74pef-jas67/files/1807.06209.pdf" }, "related_objects": [ { "basename": "aa33910-18.pdf", "url": "https://authors.library.caltech.edu/records/74pef-jas67/files/aa33910-18.pdf" }, { "basename": "aa33910e-18.pdf", "url": "https://authors.library.caltech.edu/records/74pef-jas67/files/aa33910e-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Aghanim, N.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/kr7ds-9xj61", "eprint_id": 98902, "eprint_status": "archive", "datestamp": "2023-08-19 23:06:05", "lastmod": "2023-10-18 17:43:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Akrami-Yashar", "name": { "family": "Akrami", "given": "Y." }, "orcid": "0000-0002-2407-7956" }, { "id": "Ghosh-T", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "G\u00f3rski-K-M", "name": { "family": "G\u00f3rski", "given": "K. M." } }, { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "id": "Roudier-G", "name": { "family": "Roudier", "given": "G." } } ] }, "title": "Planck 2018 results. VII. Isotropy and statistics of the CMB", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmic background radiation \u2013 polarization \u2013 methods: data analysis \u2013 methods: statistical", "note": "\u00a9 2020 Planck Collaboration. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nReceived 4 February 2019; Accepted 3 May 2019; Published online 11 September 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This work has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement numbers 687312, 776282, and 772253.\n\nPublished - aa35201-19.pdf
Submitted - 1906.02552.pdf
", "abstract": "Analysis of the Planck 2018 data set indicates that the statistical properties of the cosmic microwave background (CMB) temperature anisotropies are in excellent agreement with previous studies using the 2013 and 2015 data releases. In particular, they are consistent with the Gaussian predictions of the \u039bCDM cosmological model, yet also confirm the presence of several so-called \"anomalies\" on large angular scales. The novelty of the current study, however, lies in being a first attempt at a comprehensive analysis of the statistics of the polarization signal over all angular scales, using either maps of the Stokes parameters, Q and U, or the E-mode signal derived from these using a new methodology (which we describe in an appendix). Although remarkable progress has been made in reducing the systematic effects that contaminated the 2015 polarization maps on large angular scales, it is still the case that residual systematics (and our ability to simulate them) can limit some tests of non-Gaussianity and isotropy. However, a detailed set of null tests applied to the maps indicates that these issues do not dominate the analysis on intermediate and large angular scales (i.e., \u2113\u2004\u2272\u2004400). In this regime, no unambiguous detections of cosmological non-Gaussianity, or of anomalies corresponding to those seen in temperature, are claimed. Notably, the stacking of CMB polarization signals centred on the positions of temperature hot and cold spots exhibits excellent agreement with the \u039bCDM cosmological model, and also gives a clear indication of how Planck provides state-of-the-art measurements of CMB temperature and polarization on degree scales.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A7", "id_number": "CaltechAUTHORS:20190927-095417342", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190927-095417342", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Ministry of Employment and the Economy (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "687312" }, { "agency": "European Research Council (ERC)", "grant_number": "776282" }, { "agency": "European Research Council (ERC)", "grant_number": "772253" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201935201", "primary_object": { "basename": "1906.02552.pdf", "url": "https://authors.library.caltech.edu/records/kr7ds-9xj61/files/1906.02552.pdf" }, "related_objects": [ { "basename": "aa35201-19.pdf", "url": "https://authors.library.caltech.edu/records/kr7ds-9xj61/files/aa35201-19.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Akrami, Y.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/5rr5q-7zq48", "eprint_id": 98995, "eprint_status": "archive", "datestamp": "2023-08-19 23:06:21", "lastmod": "2023-10-18 17:46:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Ghosh-Tuhin", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "G\u00f3rski-Krzysztof-M", "name": { "family": "G\u00f3rski", "given": "K. M." }, "orcid": "0000-0003-2933-8630" }, { "id": "Lawrence-Charles-R", "name": { "family": "Lawrence", "given": "C. R." }, "orcid": "0000-0002-5983-6481" }, { "id": "Roudier-Gael-M", "name": { "family": "Roudier", "given": "G." }, "orcid": "0000-0002-7402-7797" } ] }, "title": "Planck 2018 results. VIII. Gravitational lensing", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak \u2013 cosmological parameters \u2013 cosmic background radiation \u2013 large-scale structure of Universe \u2013\ncosmology: observations", "note": "\u00a9 2020 ESO. Article published by EDP Sciences. \n\nReceived 17 July 2018; Accepted 18 July 2019; Published online 11 September 2020. \n\nWe thank Duncan Hanson for all his work on the previous Planck analyses without which the current work would not have been possible. We thank the DES collaboration for sharing their data. Some of the results in this paper have been derived using the HEALPix package. Support is acknowledged from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. [616170], and from the Science and Technology Facilities Council [grant numbers ST/L000652/1 and ST/N000927/1, respectively]. The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at https://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa33886-18.pdf
Submitted - 1807.06210.pdf
", "abstract": "We present measurements of the cosmic microwave background (CMB) lensing potential using the final Planck 2018 temperature and polarization data. Using polarization maps filtered to account for the noise anisotropy, we increase the significance of the detection of lensing in the polarization maps from 5\u03c3 to 9\u03c3. Combined with temperature, lensing is detected at 40\u03c3. We present an extensive set of tests of the robustness of the lensing-potential power spectrum, and construct a minimum-variance estimator likelihood over lensing multipoles 8\u2004\u2264\u2004L\u2004\u2264\u2004400 (extending the range to lower L compared to 2015), which we use to constrain cosmological parameters. We find good consistency between lensing constraints and the results from the Planck CMB power spectra within the \u039bCDM model. Combined with baryon density and other weak priors, the lensing analysis alone constrains \u03c3\u2088\u03a9_m^(0.25) = 0.589 \u00b1 0.020 (1\u03c3 errors). Also combining with baryon acoustic oscillation data, we find tight individual parameter constraints, \u03c3\u2088\u2004=\u20040.811 \u00b1 0.019, H\u2080 = 67.9_(\u22121.3)^(+1.2) km s\u207b\u00b9 Mpc\u207b\u00b9, and \u03a9_m = 0.303_(\u22120.018)^(+0.016). Combining with Planck CMB power spectrum data, we measure \u03c3\u2088 to better than 1% precision, finding \u03c3\u2088\u2004=\u20040.811 \u00b1 0.006. CMB lensing reconstruction data are complementary to galaxy lensing data at lower redshift, having a different degeneracy direction in \u03c3\u2088 \u2212 \u03a9_m space; we find consistency with the lensing results from the Dark Energy Survey, and give combined lensing-only parameter constraints that are tighter than joint results using galaxy clustering. Using the Planck cosmic infrared background (CIB) maps as an additional tracer of high-redshift matter, we make a combined Planck-only estimate of the lensing potential over 60% of the sky with considerably more small-scale signal. We additionally demonstrate delensing of the Planck power spectra using the joint and individual lensing potential estimates, detecting a maximum removal of 40% of the lensing-induced power in all spectra. The improvement in the sharpening of the acoustic peaks by including both CIB and the quadratic lensing reconstruction is detected at high significance.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A8", "id_number": "CaltechAUTHORS:20191001-135625979", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191001-135625979", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "616170" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000652/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000927/1" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Ministry of Employment and the Economy (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833886", "primary_object": { "basename": "1807.06210.pdf", "url": "https://authors.library.caltech.edu/records/5rr5q-7zq48/files/1807.06210.pdf" }, "related_objects": [ { "basename": "aa33886-18.pdf", "url": "https://authors.library.caltech.edu/records/5rr5q-7zq48/files/aa33886-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Aghanim, N.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/1w1xj-7d380", "eprint_id": 98858, "eprint_status": "archive", "datestamp": "2023-08-19 23:05:56", "lastmod": "2023-10-18 17:41:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Akrami-Yashar", "name": { "family": "Akrami", "given": "Y." }, "orcid": "0000-0002-2407-7956" }, { "id": "Ghosh-T", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G. M." }, "orcid": "0000-0002-4150-8076" }, { "id": "G\u00f3rski-K-M", "name": { "family": "G\u00f3rski", "given": "K. M." } }, { "id": "Lawrence-C-R", "name": { "family": "Lawrence", "given": "C. R." } }, { "id": "Mitra-S", "name": { "family": "Mitra", "given": "S." } }, { "id": "Roudier-G", "name": { "family": "Roudier", "given": "G." } }, { "id": "Wehus-I-K", "name": { "family": "Wehus", "given": "I. K." } } ] }, "title": "Planck 2018 results. X. Constraints on inflation", "ispublished": "pub", "full_text_status": "public", "keywords": "inflation \u2013 cosmic background radiation", "note": "\u00a9 2020 Planck Collaboration. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nReceived 17 July 2018; Accepted 19 August 2019; Published online 11 September 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). \n\nWe are grateful to Jan Hamann and Jim Zibin for extensive help with the final editing of this manuscript. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa33887-18.pdf
Submitted - 1807.06211.pdf
", "abstract": "We report on the implications for cosmic inflation of the 2018 release of the Planck cosmic microwave background (CMB) anisotropy measurements. The results are fully consistent with those reported using the data from the two previous Planck cosmological releases, but have smaller uncertainties thanks to improvements in the characterization of polarization at low and high multipoles. Planck temperature, polarization, and lensing data determine the spectral index of scalar perturbations to be n_s\u2004=\u20040.9649 \u00b1 0.0042 at 68% CL. We find no evidence for a scale dependence of n_s, either as a running or as a running of the running. The Universe is found to be consistent with spatial flatness with a precision of 0.4% at 95% CL by combining Planck with a compilation of baryon acoustic oscillation data. The Planck 95% CL upper limit on the tensor-to-scalar ratio, r_(0.002)\u2004< \u20040.10, is further tightened by combining with the BICEP2/Keck Array BK15 data to obtain r_(0.002)\u2004< \u20040.056. In the framework of standard single-field inflationary models with Einstein gravity, these results imply that: (a) the predictions of slow-roll models with a concave potential, V\u2033(\u03d5) < 0, are increasingly favoured by the data; and (b) based on two different methods for reconstructing the inflaton potential, we find no evidence for dynamics beyond slow roll. Three different methods for the non-parametric reconstruction of the primordial power spectrum consistently confirm a pure power law in the range of comoving scales 0.005\u2006Mpc\u207b\u00b9\u2004\u2272\u2004k\u2004\u2272\u20040.2\u2006Mpc\u207b\u00b9. A complementary analysis also finds no evidence for theoretically motivated parameterized features in the Planck power spectra. For the case of oscillatory features that are logarithmic or linear in k, this result is further strengthened by a new combined analysis including the Planck bispectrum data. The new Planck polarization data provide a stringent test of the adiabaticity of the initial conditions for the cosmological fluctuations. In correlated, mixed adiabatic and isocurvature models, the non-adiabatic contribution to the observed CMB temperature variance is constrained to 1.3%, 1.7%, and 1.7% at 95% CL for cold dark matter, neutrino density, and neutrino velocity, respectively. Planck power spectra plus lensing set constraints on the amplitude of compensated cold dark matter-baryon isocurvature perturbations that are consistent with current complementary measurements. The polarization data also provide improved constraints on inflationary models that predict a small statistically anisotropic quadupolar modulation of the primordial fluctuations. However, the polarization data do not support physical models for a scale-dependent dipolar modulation. All these findings support the key predictions of the standard single-field inflationary models, which will be further tested by future cosmological observations.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A10", "id_number": "CaltechAUTHORS:20190925-124312083", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190925-124312083", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Ministry of Employment and the Economy (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833887", "primary_object": { "basename": "1807.06211.pdf", "url": "https://authors.library.caltech.edu/records/1w1xj-7d380/files/1807.06211.pdf" }, "related_objects": [ { "basename": "aa33887-18.pdf", "url": "https://authors.library.caltech.edu/records/1w1xj-7d380/files/aa33887-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Akrami, Y.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/6kw2r-1q771", "eprint_id": 96767, "eprint_status": "archive", "datestamp": "2023-08-19 23:05:19", "lastmod": "2023-10-20 21:30:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Ghosh-Tuhin", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-Ranga-Ram", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "G\u00f3rski-Krzysztof-M", "name": { "family": "G\u00f3rski", "given": "K. M." }, "orcid": "0000-0003-2933-8630" }, { "id": "Lawrence-Charles-R", "name": { "family": "Lawrence", "given": "C. R." }, "orcid": "0000-0002-5983-6481" }, { "id": "Roudier-Gael-M", "name": { "family": "Roudier", "given": "G." }, "orcid": "0000-0002-7402-7797" } ] }, "title": "Planck 2018 results. XII. Galactic astrophysics using polarized dust emission", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 magnetic fields \u2013 turbulence \u2013 dust, extinction \u2013 local insterstellar matter \u2013 submillimeter: ISM", "note": "\u00a9 2020 Planck Collaboration. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nReceived 16 July 2018; Accepted 28 February 2019; Published online 11 September 2020. \n\nPlanck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states and led by Principal Investigators from France and Italy, telescope reflectors provided through a collaboration between ESA and a scientific consortium led and funded by Denmark, and additional contributions from NASA (USA). \n\nThe Planck Collaboration acknowledges the support of ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The research leading to these results has received funding from the European Research Council under the European Union's Horizon 2020 Research & Innovation Framework Programme/ERC grant agreement ERC-2016-ADG-742719. This research has received funding from the Agence Nationale de la Recherche (ANR-17-CE31-0022). We thank Pekka Teerikorpi and Andrei Berdyugin for kindly providing stellar polarization data and providing insights on stellar polarization references, Gina Panopoulou for discussions of the zero point calibration of the polarization angle, and Ralf Siebenmorgen and Nikolai Voshchinnikov for statistical discussions. We gratefully acknowledge the help of Rosine Lallement regarding the handling of the Gaia data.\n\nPublished - aa33885-18.pdf
Submitted - 1807.06212.pdf
", "abstract": "Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle \u03c8, and dispersion function of polarization angles S. The joint distribution (one-point statistics) of p and N_H confirms that the mean and maximum polarization fractions decrease with increasing N_H. The uncertainty on the maximum observed polarization fraction, p_(max) = 22.0_(\u22121.4)^(+3.5)% at 353 GHz and 80\u2032 resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and S found earlier is seen to be present at high latitudes. This follows the S\u2004\u221d\u2004p\u207b\u00b9 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, \u03c8, and S for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map S \u00d7 p, looking for residual trends. While the polarization fraction p decreases by a factor of 3\u22124 between N_H\u2004=\u200410\u00b2\u2070 cm\u207b\u00b2 and N_H\u2004=\u20042 \u00d7 1022\u2006cm\u207b\u00b2, out of the Galactic plane, this product S \u00d7 p only decreases by about 25%. Because S is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with N_H is determined mostly by the magnetic-field structure and not by a drop in grain alignment. This systematic trend is observed both in the diffuse interstellar medium (ISM) and in molecular clouds of the Gould Belt. Second, we look for a dependence of polarization properties on the dust temperature, as we would expect from the radiative alignment torque (RAT) theory. We find no systematic trend of S \u00d7 p with the dust temperature T_d, whether in the diffuse ISM or in the molecular clouds of the Gould Belt. In the diffuse ISM, lines of sight with high polarization fraction p and low polarization angle dispersion S tend, on the contrary, to have colder dust than lines of sight with low p and high S. We also compare the Planck thermal dust polarization with starlight polarization data in the visible at high Galactic latitudes. The agreement in polarization angles is remarkable, and is consistent with what we expect from the noise and the observed dispersion of polarization angles in the visible on the scale of the Planck beam. The two polarization emission-to-extinction ratios, R_(P/p) and R_(S/V), which primarily characterize dust optical properties, have only a weak dependence on the column density, and converge towards the values previously determined for translucent lines of sight. We also determine an upper limit for the polarization fraction in extinction, p_V/E(B \u2212 V), of 13% at high Galactic latitude, compatible with the polarization fraction p\u2004\u2248\u200420% observed at 353 GHz. Taken together, these results provide strong constraints for models of Galactic dust in diffuse gas.", "date": "2020-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "641", "publisher": "EDP Sciences", "pagerange": "Art. No. A12", "id_number": "CaltechAUTHORS:20190627-085435272", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190627-085435272", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)", "grant_number": "742719" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "Gaia Multilateral Agreement" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-17-CE31-0022" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201833885", "primary_object": { "basename": "1807.06212.pdf", "url": "https://authors.library.caltech.edu/records/6kw2r-1q771/files/1807.06212.pdf" }, "related_objects": [ { "basename": "aa33885-18.pdf", "url": "https://authors.library.caltech.edu/records/6kw2r-1q771/files/aa33885-18.pdf" } ], "resource_type": "article", "pub_year": "2020", "author_list": "Aghanim, N.; Ghosh, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/58ks1-2ac03", "eprint_id": 104643, "eprint_status": "archive", "datestamp": "2023-08-19 22:33:23", "lastmod": "2023-10-20 20:41:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "Albert" }, "orcid": "0000-0002-8232-7343" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Frez-Clifford", "name": { "family": "Frez", "given": "Clifford" } }, { "id": "Hollister-Matthew-I", "name": { "family": "Hollister", "given": "M." } }, { "id": "Minutolo-Lorenzo", "name": { "family": "Minutolo", "given": "Lorenzo" }, "orcid": "0000-0002-4876-112X" }, { "id": "Nguyen-Hien", "name": { "family": "Nguyen", "given": "Hien" } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "Bryan" } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "Anthony" } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "Jonas" } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "Roger" } } ] }, "title": "Thermal kinetic inductance detectors for millimeter-wave detection", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2020 Published under license by AIP Publishing. \n\nSubmitted: 24 January 2020; Accepted: 13 July 2020; Published Online: 29 July 2020. \n\nThe research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the JPL Research and Technology Development (RTD) program for supporting funds, as well as the Dominic Orr Graduate Fellowship in Physics at Caltech for supporting A. Wandui's graduate research. We are grateful to Warren Holmes for his early guidance in shaping this project. \n\nData Availability: The data that support the findings of this study are available from the corresponding author upon reasonable request.\n\nPublished - 5.0002413.pdf
", "abstract": "Thermal Kinetic-Inductance Detectors (TKIDs) combine the excellent noise performance of traditional bolometers with a radio frequency multiplexing architecture that enables the large detector counts needed for the next generation of millimeter-wave instruments. In this paper, we first discuss the expected noise sources in TKIDs and derive the limits where the phonon noise contribution dominates over the other detector noise terms: generation\u2013recombination, amplifier, and two-level system noise. Second, we characterize aluminum TKIDs in a dark environment. We present measurements of TKID resonators with quality factors of about 10\u2075 at 80\u2009mK. We also discuss the bolometer thermal conductance, heat capacity, and time constants. These were measured by the use of a resistor on the thermal island to excite the bolometers. These dark aluminum TKIDs demonstrate a noise equivalent power, NEP = 2\u00d710\u207b\u00b9\u2077 W/\u221aHz, with a 1/f knee at 0.1\u2009Hz, which provides background noise limited performance for ground-based telescopes observing at 150\u2009GHz.", "date": "2020-07-28", "date_type": "published", "publication": "Journal of Applied Physics", "volume": "128", "number": "4", "publisher": "American Institute of Physics", "pagerange": "Art. No. 044508", "id_number": "CaltechAUTHORS:20200729-143211488", "issn": "0021-8979", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200729-143211488", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Dominic Orr Graduate Fellowship" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1063/5.0002413", "primary_object": { "basename": "5.0002413.pdf", "url": "https://authors.library.caltech.edu/records/58ks1-2ac03/files/5.0002413.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "Wandui, Albert; Bock, James J.; et el." }, { "id": "https://authors.library.caltech.edu/records/mp2rp-1z284", "eprint_id": 101522, "eprint_status": "archive", "datestamp": "2023-08-22 04:50:31", "lastmod": "2023-10-19 22:49:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" }, { "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-R", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C. A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Cheshire", "given": "J." } }, { "name": { "family": "Connors", "given": "J." } }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S.R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G. C." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "name": { "family": "Irwin", "given": "K. D." } }, { "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K. S." }, "orcid": "0000-0002-5215-6993" }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kovac", "given": "J. M." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Lau", "given": "K." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Namikawa", "given": "T." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Precup", "given": "N." } }, { "name": { "family": "Prouv\u00e9", "given": "T." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C. D." } }, { "name": { "family": "Richter", "given": "S." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schmitt", "given": "B." } }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Sheehy", "given": "C. D." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "St. Germaine", "given": "T." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "name": { "family": "Sudiwala", "given": "R. V." } }, { "name": { "family": "Thompson", "given": "K. L." } }, { "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wu", "given": "W. L. K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "E." } }, { "name": { "family": "Yoon", "given": "K. W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } } ] }, "title": "Characterizing the Sensitivity of 40 GHz TES Bolometers for BICEP Array", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmology; B-Mode polarization; Inflation; CMB; TES", "note": "\u00a9 2020 Springer Nature Switzerland AG. \n\nReceived 01 September 2019; Accepted 10 February 2020; Published 24 February 2020. \n\nThe BICEP/Keck project have been made possible through a series of grants from the National Science Foundation including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, 1638970, and 1726917 and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and NASA Grants 06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031, 14-SAT14-0009 and 16-SAT16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. DoE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Tireless administrative support was provided by Kathy Deniston, Sheri Stoll, Irene Coyle, Donna Hernandez, and Dana Volponi.\n\nAccepted Version - 2002.05219.pdf
", "abstract": "The BICEP/Keck (BK) experiment aims to detect the imprint of primordial gravitational waves in the cosmic microwave background polarization, which would be direct evidence of the inflation theory. While the tensor-to-scalar ratio has been constrained to be r_(0.05) < 0.06 at 95% c.l., further improvements on this upper limit are hindered by polarized galactic foreground emissions and removal of gravitational lensing polarization. The 30/40 GHz receiver of the BICEP Array (BA) will deploy at the end of 2019 and will constrain the synchrotron foreground with unprecedented accuracy within the BK sky patch. We will show the design of the 30/40 GHz detectors and test results summarizing its performance. The low optical and atmospheric loading at these frequencies requires our TES detectors to have low saturation power in order to be photon noise dominated. To realize the low thermal conductivity required from a 250 mK base temperature, we developed new bolometer leg designs. We will present the relevant measured detector parameters: G, T_c, R_n, P_(sat), and spectral bands, and noise spectra. We achieved a per bolometer NEP including all noise components of 2.07\u00d710\u207b\u00b9\u2077 W/\u221aHz, including an anticipated photon noise level 1.54\u00d710\u207b\u00b9\u2077W/\u221aHz.", "date": "2020-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "199", "number": "3-4", "publisher": "Springer", "pagerange": "968-975", "id_number": "CaltechAUTHORS:20200225-082326440", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200225-082326440", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "NSF", "grant_number": "OPP-1726917" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT16-0002" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-020-02411-8", "primary_object": { "basename": "2002.05219.pdf", "url": "https://authors.library.caltech.edu/records/mp2rp-1z284/files/2002.05219.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "Zhang, C.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/eqnha-wb714", "eprint_id": 101535, "eprint_status": "archive", "datestamp": "2023-08-22 04:51:02", "lastmod": "2023-10-19 22:50:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-Ritoban", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C. A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Cheshire", "given": "J." } }, { "name": { "family": "Connors", "given": "J." }, "orcid": "0000-0002-6094-2943" }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G. C." }, "orcid": "0000-0003-4247-467X" }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "name": { "family": "Irwin", "given": "K. D." } }, { "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K. S." }, "orcid": "0000-0002-5215-6993" }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kovac", "given": "J. M." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Lau", "given": "K." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Namikawa", "given": "T." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Precup", "given": "N." } }, { "name": { "family": "Prouve", "given": "T." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C. D." } }, { "name": { "family": "Richter", "given": "S." } }, { "name": { "family": "Schmitt", "given": "B. L." } }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Sheehy", "given": "C. D." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "St. Germaine", "given": "T." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "name": { "family": "Sudiwala", "given": "R. V." } }, { "name": { "family": "Thompson", "given": "K. L." } }, { "name": { "family": "Tucker", "given": "C." }, "orcid": "0000-0002-1851-3918" }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wu", "given": "W. L. K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "E." } }, { "name": { "family": "Yoon", "given": "K. W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "Design and Performance of the First BICEP Array Receiver", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmology; B-mode polarization; Inflation; CMB; BICEP Array", "note": "\u00a9 2020 Springer Nature Switzerland AG. \n\nReceived 04 September 2019; Accepted 05 February 2020; Published 17 February 2020. \n\nThe BICEP/Keck project has been made possible through a series of Grants from the National Science Foundation including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, 1638970, and 1726917 and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and NASA Grants 06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031, 14-SAT14-0009 and 16-SAT16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the US DoE Office of Science. We thank the staff of the US Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Tireless administrative support was provided by Kathy Deniston, Sheri Stoll, Irene Coyle, Donna Hernandez, and Dana Volponi.\n\nAccepted Version - 2002.05228.pdf
", "abstract": "Branches of cosmic inflationary models, such as slow-roll inflation, predict a background of primordial gravitational waves that imprints a unique odd-parity \"B-mode\" pattern in the Cosmic Microwave Background (CMB) at amplitudes that are within experimental reach. The BICEP/Keck (BK) experiment targets this primordial signature, the amplitude of which is parameterized by the tensor-to-scalar ratio r, by observing the polarized microwave sky through the exceptionally clean and stable atmosphere at the South Pole. B-mode measurements require an instrument with exquisite sensitivity, tight control of systematics, and wide frequency coverage to disentangle the primordial signal from the Galactic foregrounds. BICEP Array represents the most recent stage of the BK program and comprises four BICEP3-class receivers observing at 30/40, 95, 150 and 220/270 GHz. The 30/40 GHz receiver will be deployed at the South Pole during the 2019/2020 austral summer. After 3 full years of observations with 30,000+ detectors, BICEP Array will measure primordial gravitational waves to a precision \u03c3(r) between 0.002 and 0.004, depending on foreground complexity and the degree of lensing removal. In this paper, we give an overview of the instrument, highlighting the design features in terms of cryogenics, magnetic shielding, detectors and readout architecture as well as reporting on the integration and tests that are ongoing with the first receiver at 30/40 GHz.", "date": "2020-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "199", "number": "3-4", "publisher": "Springer", "pagerange": "976-984", "id_number": "CaltechAUTHORS:20200225-111516904", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200225-111516904", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "NSF", "grant_number": "OPP-1726917" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT16-0002" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-020-02394-6", "primary_object": { "basename": "2002.05228.pdf", "url": "https://authors.library.caltech.edu/records/eqnha-wb714/files/2002.05228.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "Schillaci, A.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/nxers-gw529", "eprint_id": 98964, "eprint_status": "archive", "datestamp": "2023-08-22 04:47:19", "lastmod": "2023-10-18 17:45:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cukierman-Ari", "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "id": "Basu-Thakur-R", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "Microwave multiplexing on the Keck Array", "ispublished": "pub", "full_text_status": "public", "keywords": "Microwave multiplexing; BICEP; Keck Array; SMuRF; Tone tracking; CMB", "note": "\u00a9 2019 Springer Verlag. \n\nReceived 30 August 2019; Accepted 02 December 2019; Published 17 December 2019. \n\nThis work was supported by the US Department of Energy, Office of Science, Contract DE-AC02-76SF00515. CY was supported by the NSF GRFP.\n\nSubmitted - 1909.01305.pdf
", "abstract": "We describe an on-sky demonstration of a microwave-multiplexing readout system in one of the receivers of the Keck Array, a polarimetry experiment observing the cosmic microwave background at the South Pole. During the austral summer of 2018\u20132019, we replaced the time-division multiplexing readout system with microwave-multiplexing components including superconducting microwave resonators coupled to radio frequency superconducting quantum interference devices at the sub-Kelvin focal plane, coaxial-cable plumbing and amplification between room temperature and the cold stages, and a SLAC Microresonator Radio Frequency system for the warm electronics. In the range 5\u20136 GHz, a single coaxial cable reads out 528 channels. The readout system is coupled to transition-edge sensors, which are in turn coupled to 150-GHz slot-dipole phased-array antennas. Observations began in April 2019, and we report here on an initial characterization of the system performance.", "date": "2020-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "199", "number": "3-4", "publisher": "Springer", "pagerange": "858-866", "id_number": "CaltechAUTHORS:20190930-144824603", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190930-144824603", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-019-02296-2", "primary_object": { "basename": "1909.01305.pdf", "url": "https://authors.library.caltech.edu/records/nxers-gw529/files/1909.01305.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "Cukierman, A.; Basu Thakur, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/zjabv-pzs58", "eprint_id": 101528, "eprint_status": "archive", "datestamp": "2023-08-22 04:50:51", "lastmod": "2023-10-19 22:49:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "St-Germaine-Tyler", "name": { "family": "St. Germaine", "given": "T." } }, { "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-Ritoban", "name": { "family": "Basu Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C. A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Cheshire", "given": "J." } }, { "name": { "family": "Connors", "given": "J." }, "orcid": "0000-0002-6094-2943" }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fliescher", "given": "S." } }, { "name": { "family": "Grayson", "given": "J. A." } }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Harrison", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G. C." }, "orcid": "0000-0003-4247-467X" }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "name": { "family": "Irwin", "given": "K. D." } }, { "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K. S." }, "orcid": "0000-0002-5215-6993" }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kernasovskiy", "given": "S. A." } }, { "name": { "family": "Kovac", "given": "J. M." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Lau", "given": "K." } }, { "name": { "family": "Leitch", "given": "E. M." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Namikawa", "given": "T." } }, { "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Ogburn", "given": "R. W." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C. D." } }, { "name": { "family": "Richter", "given": "S." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Sheehy", "given": "C. D." } }, { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "name": { "family": "Sudiwala", "given": "R. V." } }, { "name": { "family": "Thompson", "given": "K. L." } }, { "name": { "family": "Tolan", "given": "J. E." } }, { "name": { "family": "Tucker", "given": "C." }, "orcid": "0000-0002-1851-3918" }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wong", "given": "C. L." } }, { "name": { "family": "Wu", "given": "W. L. K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "E." } }, { "name": { "family": "Yoon", "given": "K. W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "Optical Characterization of the Keck Array and BICEP3 CMB Polarimeters from 2016 to 2019", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmic microwave background; Inflation; Polarization; Transition-edge sensor; Keck Array; BICEP3", "note": "\u00a9 2020 Springer Nature Switzerland AG. \n\nReceived 31 August 2019; Accepted 05 February 2020; Published 24 February 2020. \n\nThe BICEP/Keck projects have been made possible through a series of Grants from the National Science Foundation including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, 1638970, and 1726917, by the Gordon and Betty Moore Foundation, by the Keck Foundation, and by the Grant 55802 from John Templeton Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and NASA Grants 06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031, 14-SAT14-0009 and 16-SAT16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. DoE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed past efforts to the BICEP/Keck series of experiments, including the Bicep1 team. Tireless administrative support was provided by Kathy Deniston, Sheri Stoll, Irene Coyle, Donna Hernandez, Dana Volponi, and Julie Shih.\n\nAccepted Version - 2002.05197.pdf
", "abstract": "The BICEP/Keck experiment (BK) is a series of small-aperture refracting telescopes observing degree-scale cosmic microwave background (CMB) polarization from the South Pole in search of a primordial B-mode signature. This B-mode signal arises from primordial gravitational waves interacting with the CMB and has amplitude parametrized by the tensor-to-scalar ratio r. Since 2016, BICEP3 and the Keck Array have been observing with 4800 total antenna-coupled transition-edge sensor detectors, with frequency bands spanning 95, 150, 220, and 270 GHz. Here we present the optical performance of these receivers from 2016 to 2019, including far-field beams measured in situ with an improved chopped thermal source and instrument spectral response measured with a field-deployable Fourier transform spectrometer. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We generate per-detector far-field beam maps and the corresponding differential beam mismatch that is used to estimate the temperature-to-polarization leakage in our CMB maps and to give feedback on detector and optics fabrication. The differential beam parameters presented here were estimated using improved low-level beam map analysis techniques, including efficient removal of non-Gaussian noise as well as improved spatial masking. These techniques help minimize systematic uncertainty in the beam analysis, with the goal of constraining the bias on r induced by temperature-to-polarization leakage to be subdominant to the statistical uncertainty. This is essential as we progress to higher detector counts in the next generation of CMB experiments.", "date": "2020-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "199", "number": "3-4", "publisher": "Springer", "pagerange": "824-832", "id_number": "CaltechAUTHORS:20200225-100023216", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200225-100023216", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "NSF", "grant_number": "OPP-1726917" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "W. M. Keck Foundation" }, { "agency": "John Templeton Foundation", "grant_number": "55802" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT16-0002" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-020-02392-8", "primary_object": { "basename": "2002.05197.pdf", "url": "https://authors.library.caltech.edu/records/zjabv-pzs58/files/2002.05197.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "St. Germaine, T.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/yaazn-pta76", "eprint_id": 101517, "eprint_status": "archive", "datestamp": "2023-08-22 04:50:20", "lastmod": "2023-10-19 22:49:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Soliman-Ahmed", "name": { "family": "Soliman", "given": "A." } }, { "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Ahmed", "given": "Z." } }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Barkats", "given": "D." } }, { "id": "Basu-Thakur-R", "name": { "family": "Basu-Thakur", "given": "R." }, "orcid": "0000-0002-3351-3078" }, { "name": { "family": "Bischoff", "given": "C. A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Boenish", "given": "H." } }, { "name": { "family": "Bullock", "given": "E." } }, { "name": { "family": "Buza", "given": "V." } }, { "name": { "family": "Cheshire", "given": "J." } }, { "name": { "family": "Connors", "given": "J." }, "orcid": "0000-0002-6094-2943" }, { "name": { "family": "Cornelison", "given": "J." } }, { "name": { "family": "Crumrine", "given": "M." } }, { "name": { "family": "Cukierman", "given": "A." }, "orcid": "0000-0002-7471-719X" }, { "name": { "family": "Dierickx", "given": "M." }, "orcid": "0000-0002-3519-8593" }, { "name": { "family": "Duband", "given": "L." } }, { "name": { "family": "Fatigoni", "given": "S." } }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Hall", "given": "G." } }, { "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "name": { "family": "Harrison", "given": "S." } }, { "name": { "family": "Henderson", "given": "S." } }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "name": { "family": "Hilton", "given": "G. C." }, "orcid": "0000-0003-4247-467X" }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "name": { "family": "Irwin", "given": "K. D." } }, { "name": { "family": "Kang", "given": "J." } }, { "name": { "family": "Karkare", "given": "K. S." }, "orcid": "0000-0002-5215-6993" }, { "name": { "family": "Karpel", "given": "E." } }, { "id": "Kefeli-Sinan", "name": { "family": "Kefeli", "given": "S." } }, { "name": { "family": "Kovac", "given": "J. M." } }, { "name": { "family": "Kuo", "given": "C. L." } }, { "name": { "family": "Lau", "given": "K." } }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K. G." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "name": { "family": "Namikawa", "given": "T." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger", "name": { "family": "O'Brient", "given": "R." } }, { "name": { "family": "Palladino", "given": "S." } }, { "name": { "family": "Prouve", "given": "T." } }, { "name": { "family": "Precup", "given": "N." } }, { "name": { "family": "Pryke", "given": "C." } }, { "name": { "family": "Racine", "given": "B." } }, { "name": { "family": "Reintsema", "given": "C. D." } }, { "name": { "family": "Richter", "given": "S." } }, { "name": { "family": "Schmitt", "given": "B." } }, { "name": { "family": "Schwarz", "given": "R." } }, { "name": { "family": "Sheehy", "given": "C. D." } }, { "id": "Schillaci-Alessandro", "name": { "family": "Schillaci", "given": "A." }, "orcid": "0000-0002-0512-1042" }, { "name": { "family": "St. Germaine", "given": "T." } }, { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B." } }, { "name": { "family": "Sudiwala", "given": "R. V." } }, { "name": { "family": "Thompson", "given": "K. L." } }, { "name": { "family": "Tucker", "given": "C." }, "orcid": "0000-0002-1851-3918" }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "name": { "family": "Umilt\u00e0", "given": "C." } }, { "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Wandui-Albert", "name": { "family": "Wandui", "given": "A." }, "orcid": "0000-0002-8232-7343" }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Willmert", "given": "J." } }, { "name": { "family": "Wu", "given": "W. L. K." }, "orcid": "0000-0001-5411-6920" }, { "name": { "family": "Yang", "given": "E." } }, { "name": { "family": "Yoon", "given": "K. W." } }, { "name": { "family": "Young", "given": "E." } }, { "name": { "family": "Yu", "given": "C." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "Optical Design and Characterization of 40-GHz Detector and Module for the BICEP Array", "ispublished": "pub", "full_text_status": "public", "keywords": "BICEP array; Cosmology; Inflation; CMB; Antennas; Detectors; Polarization", "note": "\u00a9 2020 Springer Nature Switzerland AG. \n\nReceived 05 September 2019; Accepted 03 December 2019; Published 24 February 2020. \n\nThe BICEP/Keck project has been made possible through a series of grants from the National Science Foundation including 0742818, 0742592, 1044978, 1110087, 1145172, 1145143, 1145248, 1639040, 1638957, 1638978, 1638970, & 1726917 and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and NASA Grants 06-ARPA206-0040, 10-SAT10-0017, 12-SAT12-0031, 14-SAT14-0009 & 16-SAT16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the US DoE Office of Science. We thank the staff of the US Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Tireless administrative support was provided by Kathy Deniston, Sheri Stoll, Irene Coyle, Donna Hernandez, and Dana Volponi.\n\nAccepted Version - 2002.05254.pdf
", "abstract": "Families of cosmic inflation models predict a primordial gravitational-wave background that imprints B-mode polarization pattern in the cosmic microwave background (CMB). High-sensitivity instruments with wide frequency coverage and well-controlled systematic errors are needed to constrain the faint B-mode amplitude. We have developed antenna-coupled transition edge sensor arrays for high-sensitivity polarized CMB observations over a wide range of millimeter-wave bands. BICEP array, the latest phase of the BICEP/Keck experiment series, is a multi-receiver experiment designed to search for inflationary B-mode polarization to a precision \u03c3(r) between 0.002 and 0.004 after 3 full years of observations, depending on foreground complexity and the degree of lensing removal. We describe the electromagnetic design and measured performance of BICEP array's low-frequency 40-GHz detector, their packaging in focal plane modules, and optical characterization including efficiency and beam matching between polarization pairs. We summarize the design and simulated optical performance, including an approach to improve the optical efficiency due to mismatch losses. We report the measured beam maps for a new broadband corrugation design to minimize beam differential ellipticity between polarization pairs caused by interactions with the module housing frame, which helps minimize polarized beam mismatch that converts CMB temperature to polarization (T\u2192P) anisotropy in CMB maps.", "date": "2020-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "199", "number": "3-4", "publisher": "Springer", "pagerange": "1118-1126", "id_number": "CaltechAUTHORS:20200225-072133380", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200225-072133380", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "NSF", "grant_number": "OPP-1726917" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT16-0002" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-019-02299-z", "primary_object": { "basename": "2002.05254.pdf", "url": "https://authors.library.caltech.edu/records/yaazn-pta76/files/2002.05254.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "Soliman, A.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/0v7jd-my358", "eprint_id": 101905, "eprint_status": "archive", "datestamp": "2023-08-19 21:10:22", "lastmod": "2023-10-19 23:37:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Osherson-Benjamin", "name": { "family": "Osherson", "given": "B." }, "orcid": "0000-0001-7596-2536" }, { "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "name": { "family": "Fu", "given": "J." } }, { "name": { "family": "Gramillano", "given": "R. V." } }, { "name": { "family": "Gualtieri", "given": "R" } }, { "id": "Shaw-E-C", "name": { "family": "Shaw", "given": "E. C." } }, { "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "name": { "family": "Amiri", "given": "M." } }, { "name": { "family": "Benton", "given": "S. J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "name": { "family": "Bryan", "given": "S. A." } }, { "name": { "family": "Chiang", "given": "H. C." } }, { "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "name": { "family": "Fraisse", "given": "A. A." } }, { "name": { "family": "Gambrel", "given": "A. E." } }, { "name": { "family": "Gandilo", "given": "N. N." } }, { "name": { "family": "Gudmundsson", "given": "J. E." } }, { "name": { "family": "Halpern", "given": "M." } }, { "name": { "family": "Hartley", "given": "J. W." } }, { "name": { "family": "Hasselfield", "given": "M." } }, { "name": { "family": "Hilton", "given": "G. C." }, "orcid": "0000-0003-4247-467X" }, { "id": "Holmes-W-A", "name": { "family": "Holmes", "given": "W. A." } }, { "id": "Hristov-Viktor-V", "name": { "family": "Hristov", "given": "V. V." } }, { "name": { "family": "Irwin", "given": "K. D." } }, { "name": { "family": "Jones", "given": "W. C." } }, { "name": { "family": "Kermish", "given": "Z. D." } }, { "id": "Mason-Peter-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Megerian-Krikor-G", "name": { "family": "Megerian", "given": "K." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-Tracy-A", "name": { "family": "Morford", "given": "T. A." } }, { "name": { "family": "Nagy", "given": "J. M." }, "orcid": "0000-0002-2036-7008" }, { "name": { "family": "Netterfield", "given": "C. B." } }, { "name": { "family": "Padilla", "given": "I.L." } }, { "name": { "family": "Rahlin", "given": "A. S." } }, { "name": { "family": "Reintsema", "given": "C." } }, { "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Runyan-Marcus-C", "name": { "family": "Runyan", "given": "M. C." } }, { "name": { "family": "Shariff", "given": "J. A." } }, { "name": { "family": "Soler", "given": "J. D." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "name": { "family": "Tucker", "given": "C." }, "orcid": "0000-0002-1851-3918" }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } }, { "id": "Weber-Alexis-C", "name": { "family": "Weber", "given": "A. C." } }, { "name": { "family": "Wiebe", "given": "D. V." } }, { "name": { "family": "Young", "given": "E. Y." } } ] }, "title": "Particle Response of Antenna-Coupled TES Arrays: Results from SPIDER\u00a0and the Laboratory", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2020 Springer Nature. \n\nReceived 31 August 2019. Accepted 15 February 2020. Published 13 March 2020. \n\nThis work is supported by NASA's Strategic Astrophysics Technology program (14-SAT14-0009, 16-SAT16-0002). SPIDER is supported by in the USA by NASA (NNX07AL64G, NNX12AE95G, NNX17AC55G) and NSF (PLR-1043515); in Canada by NSERC and CSA; as well as by the Research Council of Norway, the Swedish Research Council, and the Packard Foundation. Logistical support in Antarctica is supported by the NSF through the US Antarctic Program. The collaboration is grateful to the British Antarctic Survey, particularly Sam Burrell, for invaluable assistance with data and payload recovery after the 2015 flight.\n\nAccepted Version - 2002.05771.pdf
", "abstract": "Future mm-wave and sub-mm space missions will employ large arrays of multiplexed transition-edge-sensor (TES) bolometers. Such instruments must contend with the high flux of cosmic rays beyond our atmosphere that induce 'glitches' in bolometer data, which posed a challenge to data analysis from the Planck bolometers. Future instruments will face the additional challenges of shared substrate wafers and multiplexed readout wiring. In this work, we explore the susceptibility of modern TES arrays to the cosmic ray environment of space using two data sets: the 2015 long-duration balloon flight of the SPIDER cosmic microwave background polarimeter, and a laboratory exposure of SPIDER flight hardware to radioactive sources. We find manageable glitch rates and short glitch durations, leading to minimal effect on SPIDER analysis. We constrain energy propagation within the substrate through a study of multi-detector coincidences and give a preliminary look at pulse shapes in laboratory data.", "date": "2020-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "199", "number": "3-4", "publisher": "Springer", "pagerange": "1127-1136", "id_number": "CaltechAUTHORS:20200313-132837205", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200313-132837205", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT16-0002" }, { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NASA", "grant_number": "NNX17AC55G" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Research Council of Norway" }, { "agency": "Swedish Research Council" }, { "agency": "David and Lucile Packard Foundation" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-020-02415-4", "primary_object": { "basename": "2002.05771.pdf", "url": "https://authors.library.caltech.edu/records/0v7jd-my358/files/2002.05771.pdf" }, "resource_type": "article", "pub_year": "2020", "author_list": "Osherson, B.; Filippini, J. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/kvxxw-f0860", "eprint_id": 98848, "eprint_status": "archive", "datestamp": "2023-08-22 03:20:25", "lastmod": "2023-10-18 17:41:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hensley-B-S", "name": { "family": "Hensley", "given": "Brandon S." }, "orcid": "0000-0001-7449-4638" }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "Cheng" }, "orcid": "0000-0001-8288-5823" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "An Imprint of the Galactic Magnetic Field in the Diffuse Unpolarized Dust Emission", "ispublished": "pub", "full_text_status": "public", "keywords": "Interstellar dust; Interstellar magnetic fields; Dust continuum\nemission; H I line emission", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 September 14; revised 2019 October 23; accepted 2019 October 24; published 2019 December 17. \n\nIt is a pleasure to thank Fran\u00e7ois Boulanger, Susan Clark, Bruce Draine, Laura Fissel, and Vincent Guillet for stimulating discussions and helpful suggestions. This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \n\nFacilities: Effelsberg - Effelsberg Radio Telescope, Parkes - Parkes Radio Telescope, Planck - European Space Agency's Planck space observatory. \n\nSoftware: Astropy (Astropy Collaboration et al. 2013, 2018), corner (Foreman-Mackey 2016), emcee (Foreman-Mackey et al. 2013), HEALPix (G\u00f3rski et al. 2005), healpy (Zonca et al. 2019), Matplotlib (Hunter 2007), NumPy (van der Walt et al. 2011).\n\nPublished - Hensley_2019_ApJ_887_159.pdf
Submitted - 1909.07394.pdf
", "abstract": "It is well known that aligned, aspherical dust grains emit polarized radiation and that the degree of polarization depends on the angle \u03c8 between the interstellar magnetic field and the line of sight (LOS). However, anisotropy of the dust absorption cross sections also modulates the total intensity of the radiation as the viewing geometry changes. We report a detection of this effect in the high Galactic latitude Planck data, finding that the 353 GHz dust intensity per N_(H I) is smaller when the Galactic magnetic field is mostly in the plane of the sky and larger when the field is mostly along the LOS. These variations are of opposite sign and roughly equal magnitude as the changes in polarized intensity per N_(H I) with \u03c8, as predicted. In principle, the variation in intensity can be used in conjunction with the dust polarization angle to constrain the full 3D orientation of the Galactic magnetic field.", "date": "2019-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "887", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 159", "id_number": "CaltechAUTHORS:20190925-100235448", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190925-100235448", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab5183", "primary_object": { "basename": "Hensley_2019_ApJ_887_159.pdf", "url": "https://authors.library.caltech.edu/records/kvxxw-f0860/files/Hensley_2019_ApJ_887_159.pdf" }, "related_objects": [ { "basename": "1909.07394.pdf", "url": "https://authors.library.caltech.edu/records/kvxxw-f0860/files/1909.07394.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Hensley, Brandon S.; Zhang, Cheng; et el." }, { "id": "https://authors.library.caltech.edu/records/fqq8d-zrk68", "eprint_id": 99901, "eprint_status": "archive", "datestamp": "2023-08-19 18:20:37", "lastmod": "2023-10-18 18:54:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "O'Brient-R-C", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Schillaci-A", "name": { "family": "Schillaci", "given": "A." } }, { "id": "Soliman-A", "name": { "family": "Soliman", "given": "A." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B-A", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } }, { "id": "Wandui-A", "name": { "family": "Wandui", "given": "A." } }, { "id": "Zhang-C", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "BICEP2/Keck Array XI: Beam Characterization and Temperature-to-Polarization Leakage in the BK15 Data Set", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 gravitational waves \u2013 inflation \u2013 polarization", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 April 9; revised 2019 July 23; accepted 2019 August 5; published 2019 October 16. \n\nThe Keck Array project has been made possible through support from the National Science Foundation under grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota), and ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grant Nos. 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. DoE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP\u2013Keck Array series of experiments, including the BICEP1 team. We also thank the Planck and WMAP teams for the use of their data.\n\nPublished - Ade_2019_ApJ_884_114.pdf
", "abstract": "Precision measurements of cosmic microwave background (CMB) polarization require extreme control of instrumental systematics. In a companion paper we have presented cosmological constraints from observations with the BICEP2 and Keck Array experiments up to and including the 2015 observing season (BK15), resulting in the deepest CMB polarization maps to date and a statistical sensitivity to the tensor-to-scalar ratio of \u03c3(r) = 0.020. In this work we characterize the beams and constrain potential systematic contamination from main beam shape mismatch at the three BK15 frequencies (95, 150, and 220 GHz). Far-field maps of 7360 distinct beam patterns taken from 2010\u20132015 are used to measure differential beam parameters and predict the contribution of temperature-to-polarization leakage to the BK15 B-mode maps. In the multifrequency, multicomponent likelihood analysis that uses BK15, Planck, and Wilkinson Microwave Anisotropy Probe maps to separate sky components, we find that adding this predicted leakage to simulations induces a bias of \u0394r = 0.0027 \u00b1 0.0019. Future results using higher-quality beam maps and improved techniques to detect such leakage in CMB data will substantially reduce this uncertainty, enabling the levels of systematics control needed for BICEP Array and other experiments that plan to definitively probe large-field inflation.", "date": "2019-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "884", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 114", "id_number": "CaltechAUTHORS:20191118-122250509", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191118-122250509", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "KECK ARRAY Collaboration", "BICEP2 Collaboration" ] }, "doi": "10.3847/1538-4357/ab391d", "primary_object": { "basename": "Ade_2019_ApJ_884_114.pdf", "url": "https://authors.library.caltech.edu/records/fqq8d-zrk68/files/Ade_2019_ApJ_884_114.pdf" }, "resource_type": "article", "pub_year": "2019", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/prgk7-a7w84", "eprint_id": 98997, "eprint_status": "archive", "datestamp": "2023-08-19 18:20:05", "lastmod": "2023-10-18 17:46:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "O'Brient-R", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Schillaci-A", "name": { "family": "Schillaci", "given": "A." } }, { "id": "Soliman-A", "name": { "family": "Soliman", "given": "A." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } }, { "id": "Wandui-A", "name": { "family": "Wandui", "given": "A." } }, { "id": "Zhang-Cheng", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "BICEP2/Keck Array XI: Beam Characterization and Temperature-to-Polarization Leakage in the BK15 Dataset", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 gravitational waves \u2013 inflation \u2013 polarization", "note": "\u00a9 2019 The American Astronomical Society. \n\nReceived 2019 April 9; revised 2019 July 23; accepted 2019 August 5; published 2019 October 16. \n\nThe Keck Array project has been made possible through support from the National Science Foundation under grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota), and ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grant Nos. 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. DoE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP\u2013Keck Array series of experiments, including the BICEP1 team. We also thank the Planck and WMAP teams for the use of their data.\n\nPublished - Ade_2019_ApJ_884_114.pdf
Submitted - 1904.01640.pdf
", "abstract": "Precision measurements of cosmic microwave background (CMB) polarization require extreme control of instrumental systematics. In a companion paper we have presented cosmological constraints from observations with the BICEP2 and Keck Array experiments up to and including the 2015 observing season (BK15), resulting in the deepest CMB polarization maps to date and a statistical sensitivity to the tensor-to-scalar ratio of \u03c3(r) = 0.020. In this work we characterize the beams and constrain potential systematic contamination from main beam shape mismatch at the three BK15 frequencies (95, 150, and 220 GHz). Far-field maps of 7360 distinct beam patterns taken from 2010\u20132015 are used to measure differential beam parameters and predict the contribution of temperature-to-polarization leakage to the BK15 B-mode maps. In the multifrequency, multicomponent likelihood analysis that uses BK15, Planck, and Wilkinson Microwave Anisotropy Probe maps to separate sky components, we find that adding this predicted leakage to simulations induces a bias of \u0394r = 0.0027 \u00b1 0.0019. Future results using higher-quality beam maps and improved techniques to detect such leakage in CMB data will substantially reduce this uncertainty, enabling the levels of systematics control needed for BICEP Array and other experiments that plan to definitively probe large-field inflation.", "date": "2019-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "884", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 114", "id_number": "CaltechAUTHORS:20191001-142148594", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191001-142148594", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "KECK ARRAY Collaboration", "BICEP2 Collaboration" ] }, "doi": "10.3847/1538-4357/ab391d", "primary_object": { "basename": "1904.01640.pdf", "url": "https://authors.library.caltech.edu/records/prgk7-a7w84/files/1904.01640.pdf" }, "related_objects": [ { "basename": "Ade_2019_ApJ_884_114.pdf", "url": "https://authors.library.caltech.edu/records/prgk7-a7w84/files/Ade_2019_ApJ_884_114.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/rfjpm-4wd23", "eprint_id": 94834, "eprint_status": "archive", "datestamp": "2023-08-22 01:25:51", "lastmod": "2023-10-20 18:19:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Feng-Chang", "name": { "family": "Feng", "given": "Chang" } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "Jamie" }, "orcid": "0000-0002-5710-5212" }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "Tzu-Ching" } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "Olivier" }, "orcid": "0000-0001-7432-2932" }, { "id": "Santos-M-G", "name": { "family": "Santos", "given": "Mario G." }, "orcid": "0000-0003-3892-3073" }, { "id": "Silva-M-B", "name": { "family": "Silva", "given": "Marta B." }, "orcid": "0000-0003-0209-4816" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Multi-component Decomposition of Cosmic Infrared Background Fluctuations", "ispublished": "pub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars; Galaxy: formation; infrared: diffuse background; methods: data analysis; stars: Population II; stars: Population III", "note": "\u00a9 2019. The American Astronomical Society. \n\nReceived 2018 August 23; revised 2019 February 27; accepted 2019 March 5; published 2019 April 17. \n\nWe thank the SPHEREx team for insightful comments that improved the quality of the paper. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. C.F. acknowledges support from NASA grants NASA NNX16AJ69G, NASA NNX16AF39G, Ax Foundation for Cosmology at UC San Diego, and the Brand and Monica Fortner Chair. M.B.S. acknowledges the Netherlands Foundation for Scientific Research support through the VICI grant 639.043.006. M.G.S. acknowledges support from the South African Square Kilometre Array Project and National Research Foundation (grant No. 84156).\n\nPublished - Feng_2019_ApJ_875_86.pdf
Submitted - 1808.05964.pdf
", "abstract": "The near-infrared background between 0.5 and 2 \u03bcm contains a wealth of information related to radiative processes in the universe. Infrared background anisotropies encode the redshift-weighted total emission over cosmic history, including any spatially diffuse and extended contributions. The anisotropy power spectrum is dominated by undetected galaxies at small angular scales and a diffuse background of Galactic emission at large angular scales. In addition to these known sources, the infrared background also arises from intrahalo light (IHL) at z < 3 associated with tidally stripped stars during galaxy mergers. Moreover, it contains information on the very first galaxies from the epoch of reionization (EoR). The EoR signal has a spectral energy distribution (SED) that goes to zero near optical wavelengths due to Lyman absorption, while other signals have spectra that vary smoothly with frequency. Due to differences in SEDs and spatial clustering, these components may be separated in a multi-wavelength-fluctuation experiment. To study the extent to which EoR fluctuations can be separated in the presence of IHL, and extragalactic and Galactic foregrounds, we develop a maximum likelihood technique that incorporates a full covariance matrix among all the frequencies at different angular scales. We apply this technique to simulated deep imaging data over a 2 \u00d7 45 deg^2 sky area from 0.75 to 5 \u03bcm in 9 bands and find that such a \"frequency tomography\" can successfully reconstruct both the amplitude and spectral shape for representative EoR, IHL, and the foreground signals.", "date": "2019-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "875", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 86", "id_number": "CaltechAUTHORS:20190422-093047976", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190422-093047976", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NNX16AJ69G" }, { "agency": "NASA", "grant_number": "NNX16AF39G" }, { "agency": "Ax Foundation for Cosmology" }, { "agency": "Brand and Monica Fortner Chair" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.043.006" }, { "agency": "South African Square Kilometre Array Project" }, { "agency": "National Research Foundation (South Africa)", "grant_number": "84156" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/ab0d8e", "primary_object": { "basename": "1808.05964.pdf", "url": "https://authors.library.caltech.edu/records/rfjpm-4wd23/files/1808.05964.pdf" }, "related_objects": [ { "basename": "Feng_2019_ApJ_875_86.pdf", "url": "https://authors.library.caltech.edu/records/rfjpm-4wd23/files/Feng_2019_ApJ_875_86.pdf" } ], "resource_type": "article", "pub_year": "2019", "author_list": "Feng, Chang; Cooray, Asantha; et el." }, { "id": "https://authors.library.caltech.edu/records/06nhp-74449", "eprint_id": 98838, "eprint_status": "archive", "datestamp": "2023-08-19 13:06:31", "lastmod": "2023-10-18 17:40:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bergman-A-S", "name": { "family": "Bergman", "given": "A. S." }, "orcid": "0000-0002-4331-1357" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-T-A", "name": { "family": "Morford", "given": "T. A." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } } ] }, "title": "280 GHz Focal Plane Unit Design and Characterization for the Spider-2 Suborbital Polarimeter", "ispublished": "pub", "full_text_status": "public", "keywords": "Detector packaging \u00b7 Magnetic shielding \u00b7 Transition-edge sensors \u00b7 Scientific ballooning \u00b7 Cosmic microwave background", "note": "\u00a9 Springer Science+Business Media, LLC, part of Springer Nature 2018. \n\nReceived: 11 November 2017 / Accepted: 29 August 2018 / Published online: 12 September 2018. \n\nSpider is supported in the USA by the National Aeronautics and Space Administration under Grant Nos. NNX17AC55G and NNX12AE95G issued through the Science Mission Directorate and by the National Science Foundation through PLR-1043515. Additional support is provided by the Department of Energy Grant DE-SC007859. Corresponding author is supported by a National Science Foundation Graduate Research Fellowship. Logistical support for the Antarctic deployment and operations was provided by the NSF through the U.S. Antarctic Program. Support in Canada is provided by the National Sciences and Engineering Council and the Canadian Space Agency. Support in Norway is provided by the Research Council of Norway. Support in Sweden is provided by the Swedish Research Council through the Oskar Klein Centre (Contract No. 638-2013-8993). We also wish to acknowledge the generous support of the David and Lucile Packard Foundation, which has been crucial to the success of the project. The collaboration is grateful to the British Antarctic Survey, particularly Sam Burrell, for invaluable assistance with data and payload recovery after the 2015 flight.\n\nSubmitted - 1711.04169.pdf
", "abstract": "We describe the construction and characterization of the 280 GHz bolometric focal plane units (FPUs) to be deployed on the second flight of the balloon-borne Spider instrument. These FPUs are vital to Spider's primary science goal of detecting or placing an upper limit on the amplitude of the primordial gravitational wave signature in the cosmic microwave background (CMB) by constraining the B-mode contamination in the CMB from Galactic dust emission. Each 280 GHz focal plane contains a 16\u00d716 grid of corrugated silicon feedhorns coupled to an array of aluminum\u2013manganese transition-edge sensor (TES) bolometers fabricated on 150 mm diameter substrates. In total, the three 280 GHz FPUs contain 1530 polarization-sensitive bolometers (765 spatial pixels) optimized for the low loading environment in flight and read out by time-division SQUID multiplexing. In this paper, we describe the mechanical, thermal, and magnetic shielding architecture of the focal planes and present cryogenic measurements which characterize yield and the uniformity of several bolometer parameters. The assembled FPUs have high yields, with one array as high as 95% including defects from wiring and readout. We demonstrate high uniformity in device parameters, finding the median saturation power for each TES array to be \u223c 3 pW at 300 mK with a less than 6% variation across each array at 1", "date": "2018-12", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "193", "number": "5-6", "publisher": "Springer", "pagerange": "1075-1084", "id_number": "CaltechAUTHORS:20190924-143110039", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190924-143110039", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX17AC55G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC007859" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Research Council of Norway" }, { "agency": "Swedish Research Council", "grant_number": "638-2013-8993" }, { "agency": "David and Lucile Packard Foundation" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-018-2065-2", "primary_object": { "basename": "1711.04169.pdf", "url": "https://authors.library.caltech.edu/records/06nhp-74449/files/1711.04169.pdf" }, "resource_type": "article", "pub_year": "2018", "author_list": "Bergman, A. S.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/kqakc-fps17", "eprint_id": 85871, "eprint_status": "archive", "datestamp": "2023-08-22 00:21:53", "lastmod": "2023-10-18 18:53:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunacek-J-R", "name": { "family": "Hunacek", "given": "J." }, "orcid": "0000-0001-7066-226X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Butler-V", "name": { "family": "Butler", "given": "V." } }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "T.-C." } }, { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Y.-T." }, "orcid": "0000-0002-5437-0504" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Crites-A-T", "name": { "family": "Crites", "given": "A." } }, { "id": "Frez-C", "name": { "family": "Frez", "given": "C." } }, { "id": "Hailey-Dunsheath-S", "name": { "family": "Hailey-Dunsheath", "given": "S." }, "orcid": "0000-0002-8504-7988" }, { "id": "Hoscheit-B", "name": { "family": "Hoscheit", "given": "B." } }, { "id": "Kim-Dae-Wook", "name": { "family": "Kim", "given": "D. W." } }, { "id": "Li-Cheuk-Ting", "name": { "family": "Li", "given": "C.-T." } }, { "id": "Marrone-D-P", "name": { "family": "Marrone", "given": "D." }, "orcid": "0000-0002-2367-1080" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Shirokoff-E", "name": { "family": "Shirokoff", "given": "E." } }, { "id": "Steinbach-B-A", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Sun-Guochao", "name": { "family": "Sun", "given": "G." }, "orcid": "0000-0003-4070-497X" }, { "id": "Trumper-I", "name": { "family": "Trumper", "given": "I." } }, { "id": "Turner-A", "name": { "family": "Turner", "given": "A." } }, { "id": "Uzgil-B-D", "name": { "family": "Uzgil", "given": "B." }, "orcid": "0000-0001-8526-3464" }, { "id": "Weber-A", "name": { "family": "Weber", "given": "A." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Hafnium Films and Magnetic Shielding for TIME, A mm-Wavelength Spectrometer Array", "ispublished": "pub", "full_text_status": "restricted", "keywords": "Spectrometers; Bolometers; Transition-edge sensors; Hafnium; Magnetic shielding", "note": "\u00a9 2018 Springer Science+Business Media, LLC, part of Springer Nature. \n\nReceived: 30 October 2017; Accepted: 29 March 2018; First Online: 06 April 2018. \n\nJH is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. AC is supported by the National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under Grant No. 1602677.", "abstract": "TIME is a mm-wavelength grating spectrometer array that will map fluctuations of the 157.7-\u03bcm emission line of singly ionized carbon ([CII]) during the epoch of reionization (redshift z \u223c5\u20139). Sixty transition-edge sensor (TES) bolometers populate the output arc of each of the 32 spectrometers, for a total of 1920 detectors. Each bolometer consists of gold absorber on a \u223c 3 \u00d7 3 mm silicon nitride micro-mesh suspended near the corners by 1 \u00d7 1 \u00d7 500 \u03bcm silicon nitride legs targeting a photon-noise-dominated NEP \u223c1\u00d710^(-17)W/\u221aHz. Hafnium films are explored as a lower-T_c alternative to Ti (500 mK) for TIME TESs, allowing thicker support legs for improved yield. Hf T_c is shown to vary between 250 and 450 mK when varying the resident Ar pressure during deposition. Magnetic shielding designs and simulations are presented for the TIME first-stage SQUIDs. Total axial field suppression is predicted to be 5\u00d710^7.", "date": "2018-12", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "193", "number": "5-6", "publisher": "Springer", "pagerange": "893-900", "id_number": "CaltechAUTHORS:20180416-085137740", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180416-085137740", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1602677" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-018-1906-3", "resource_type": "article", "pub_year": "2018", "author_list": "Hunacek, J.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/z72y2-zxv75", "eprint_id": 98837, "eprint_status": "archive", "datestamp": "2023-08-19 13:06:21", "lastmod": "2023-10-18 17:40:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gualtieri-R", "name": { "family": "Gualtieri", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-T-A", "name": { "family": "Morford", "given": "T. A." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } } ] }, "title": "SPIDER: CMB Polarimetry from the Edge of Space", "ispublished": "pub", "full_text_status": "public", "keywords": "Cosmic microwave background \u00b7 Inflation \u00b7 Bolometers \u00b7 Transition-edge sensors \u00b7 Polarimetry", "note": "\u00a9 Springer Science+Business Media, LLC, part of Springer Nature 2018. \n\nReceived: 28 November 2017 / Accepted: 3 October 2018 / Published online: 11 October 2018. \n\nSpider is supported in the USA by the National Aeronautics and Space Administration under Grants NNX07AL64G, NNX12AE95G, and NNX17AC55G issued through the Science Mission Directorate and by the National Science Foundation through PLR-1043515. Logistical support for the Antarctic deployment and operations was provided by the NSF through the US Antarctic Program. Cosmic ray response studies are supported by NASA under Grant 14-SAT14-0009. Support in Canada is provided by the National Sciences and Engineering Council and the Canadian Space Agency. Support in Norway is provided by the Research Council of Norway. Support in Sweden is provided by the Swedish Research Council through the Oskar Klein Centre (Contract no. 638-2013-8993). KF acknowledges support from DoE Grant DE-SC0007859 at the University of Michigan. The collaboration is grateful to the British Antarctic Survey, particularly Sam Burrell, for invaluable assistance with data and payload recovery after the 2015 flight. We also wish to acknowledge the generous support of the David and Lucile Packard Foundation, which has been crucial to the success of the project.\n\nSubmitted - 1711.10596.pdf
", "abstract": "Spider is a balloon-borne instrument designed to map the polarization of the millimeter-wave sky at large angular scales. Spider targets the B-mode signature of primordial gravitational waves in the cosmic microwave background (CMB), with a focus on mapping a large sky area with high fidelity at multiple frequencies. Spider 's first long-duration balloon (LDB) flight in January 2015 deployed a total of 2400 antenna-coupled transition-edge sensors (TESs) at 90 GHz and 150 GHz. In this work we review the design and in-flight performance of the Spider instrument, with a particular focus on the measured performance of the detectors and instrument in a space-like loading and radiation environment. Spider 's second flight in December 2018 will incorporate payload upgrades and new receivers to map the sky at 285 GHz, providing valuable information for cleaning polarized dust emission from CMB maps.", "date": "2018-12", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "193", "number": "5-6", "publisher": "Springer", "pagerange": "1112-1121", "id_number": "CaltechAUTHORS:20190924-143109607", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190924-143109607", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NASA", "grant_number": "NNX17AC55G" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Research Council of Norway" }, { "agency": "Swedish Research Council", "grant_number": "638-2013-8993" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-SC0007859" }, { "agency": "David and Lucile Packard Foundation" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-018-2078-x", "primary_object": { "basename": "1711.10596.pdf", "url": "https://authors.library.caltech.edu/records/z72y2-zxv75/files/1711.10596.pdf" }, "resource_type": "article", "pub_year": "2018", "author_list": "Gualtieri, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/n9n6g-2rf49", "eprint_id": 91312, "eprint_status": "archive", "datestamp": "2023-08-19 12:52:16", "lastmod": "2023-10-19 22:23:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "O'Brient-R", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Schillaci-A", "name": { "family": "Schillaci", "given": "A." } }, { "id": "Soliman-A", "name": { "family": "Soliman", "given": "A." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } }, { "id": "Wandui-A", "name": { "family": "Wandui", "given": "A." } }, { "id": "Zhang-C", "name": { "family": "Zhang", "given": "C." }, "orcid": "0000-0001-8288-5823" } ] }, "title": "Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2018 American Physical Society. \n\nReceived 2 July 2018; revised manuscript received 28 August 2018; published 27 November 2018. \n\nThe bicep2/Keck Array projects have been made possible through a series of grants from the National Science Foundation including No. 0742818, No. 0742592, No. 1044978, No. 1110087, No. 1145172, No. 1145143, No. 1145248, No. 1639040, No. 1638957, No. 1638978, and No. 1638970, and by the Keck Foundation. The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund, and by NASA Grants No. 06-ARPA206-0040, No. 10-SAT10-0017, No. 12-SAT12-0031, No. 14-SAT14-0009, No. 16-SAT-16-0002. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Support for quasi-optical filtering was provided by UK STFC Grant No. ST/N000706/1. The computations in this Letter were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and S.\u2009L.\u2009A.\u2009C. is partially supported by the U.S. DOE Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP-Keck Array series of experiments, including the bicep1 team. We also thank the Planck and WMAP teams for the use of their data, and are grateful to the Planck team for helpful discussions including on the use of the \u03c4 prior in Fig. 5.\n\nPublished - PhysRevLett.121.221301.pdf
Accepted Version - 1810.05216.pdf
Supplemental Material - prl_supp.pdf
", "abstract": "We present results from an analysis of all data taken by the BICEP2/Keck CMB polarization experiments up to and including the 2015 observing season. This includes the first Keck Array observations at 220 GHz and additional observations at 95 and 150 GHz. The Q and U maps reach depths of 5.2, 2.9, and 26\u2009\u2009\u03bcK_(CMB)\u2009arcmin at 95, 150, and 220 GHz, respectively, over an effective area of \u2248400 square degrees. The 220 GHz maps achieve a signal to noise on polarized dust emission approximately equal to that of Planck at 353 GHz. We take auto and cross spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz. We evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-\u039bCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and we impose priors on some of these using external information from Planck and WMAP derived from larger regions of sky. The model is shown to be an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r_(0.05)<0.07 at 95% confidence, which tightens to r_(0.05)<0.06 in conjunction with Planck temperature measurements and other data. The lensing signal is detected at 8.8\u03c3 significance. Running a maximum likelihood search on simulations we obtain unbiased results and find that \u03c3(r)=0.020. These are the strongest constraints to date on primordial gravitational waves.", "date": "2018-11-30", "date_type": "published", "publication": "Physical Review Letters", "volume": "121", "number": "22", "publisher": "American Physical Society", "pagerange": "Art. No. 221301", "id_number": "CaltechAUTHORS:20181128-142206874", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181128-142206874", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0742818" }, { "agency": "NSF", "grant_number": "OPP-0742592" }, { "agency": "NSF", "grant_number": "OPP-1044978" }, { "agency": "NSF", "grant_number": "PLR-1110087" }, { "agency": "NSF", "grant_number": "OPP-1145172" }, { "agency": "NSF", "grant_number": "OPP-1145143" }, { "agency": "NSF", "grant_number": "OPP-1145248" }, { "agency": "NSF", "grant_number": "OPP-1639040" }, { "agency": "NSF", "grant_number": "OPP-1638957" }, { "agency": "NSF", "grant_number": "OPP-1638978" }, { "agency": "NSF", "grant_number": "OPP-1638970" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "NASA", "grant_number": "14-SAT14-0009" }, { "agency": "NASA", "grant_number": "16-SAT-16-0002" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/N000706/1" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "KECK ARRAY Collaboration", "BICEP2 Collaboration" ] }, "doi": "10.1103/PhysRevLett.121.221301", "primary_object": { "basename": "PhysRevLett.121.221301.pdf", "url": "https://authors.library.caltech.edu/records/n9n6g-2rf49/files/PhysRevLett.121.221301.pdf" }, "related_objects": [ { "basename": "prl_supp.pdf", "url": "https://authors.library.caltech.edu/records/n9n6g-2rf49/files/prl_supp.pdf" }, { "basename": "1810.05216.pdf", "url": "https://authors.library.caltech.edu/records/n9n6g-2rf49/files/1810.05216.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/3bwep-w7h94", "eprint_id": 87555, "eprint_status": "archive", "datestamp": "2023-09-22 22:46:13", "lastmod": "2023-10-23 23:28:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Steinbach-Bryan-A", "name": { "family": "Steinbach", "given": "B. A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-Roger-C", "name": { "family": "O'Brient", "given": "R. C." } }, { "id": "Turner-Anthony-D", "name": { "family": "Turner", "given": "A. D." } } ] }, "title": "Thermal Kinetic Inductance Detectors for Ground-Based Millimeter-Wave Cosmology", "ispublished": "pub", "full_text_status": "public", "keywords": "TKID \u00b7 Thermal kinetic inductance detector \u00b7 Resonator bolometer \u00b7 CMB \u00b7 Cosmic microwave background \u00b7 TLS \u00b7 Two-level systems", "note": "\u00a9 Springer Science+Business Media, LLC, part of Springer Nature 2018. \n\nReceived: 6 November 2017 / Accepted: 25 June 2018. \n\nThis work was supported by JPL's Research and Technology Development Fund for Projects R.17.223.057 and R.17.223.058.\n\nSubmitted - 1803.06413
", "abstract": "We show measurements of thermal kinetic inductance detectors (TKIDs) intended for millimeter-wave cosmology in the 200\u2013300 GHz atmospheric window. The TKID is a type of bolometer which uses the kinetic inductance of a superconducting resonator to measure the temperature of the thermally isolated bolometer island. We measure bolometer thermal conductance, time constant, and noise equivalent power. We also measure the quality factor of our resonators as the bath temperature varies to show they are limited by effects consistent with coupling to two-level systems.", "date": "2018-11", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "193", "number": "3-4", "publisher": "Springer", "pagerange": "88-95", "id_number": "CaltechAUTHORS:20180705-132400200", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180705-132400200", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL Research and Technology Development Fund", "grant_number": "R.17.223.057" }, { "agency": "JPL Research and Technology Development Fund", "grant_number": "R.17.223.058" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1007/s10909-018-2016-y", "primary_object": { "basename": "1803.06413", "url": "https://authors.library.caltech.edu/records/3bwep-w7h94/files/1803.06413" }, "resource_type": "article", "pub_year": "2018", "author_list": "Steinbach, B. A.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/f9ym3-xvk97", "eprint_id": 77863, "eprint_status": "archive", "datestamp": "2023-08-19 08:38:35", "lastmod": "2023-10-25 23:31:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sun-Guochao", "name": { "family": "Sun", "given": "G." }, "orcid": "0000-0003-4070-497X" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Silva-M-B", "name": { "family": "Silva", "given": "M. B." }, "orcid": "0000-0003-0209-4816" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "T.-C." } }, { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Y.-T." }, "orcid": "0000-0002-5437-0504" }, { "id": "Cooray-A-R", "name": { "family": "Cooray", "given": "A. R." }, "orcid": "0000-0002-3892-0190" }, { "id": "Crites-A-T", "name": { "family": "Crites", "given": "A." } }, { "id": "Hailey-Dunsheath-S", "name": { "family": "Hailey-Dunsheath", "given": "S." }, "orcid": "0000-0002-8504-7988" }, { "id": "Uzgil-B-D", "name": { "family": "Uzgil", "given": "B." }, "orcid": "0000-0001-8526-3464" }, { "id": "Hunacek-J-R", "name": { "family": "Hunacek", "given": "J. R." }, "orcid": "0000-0001-7066-226X" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "A Foreground Masking Strategy for [C II] Intensity Mapping Experiments Using Galaxies Selected by Stellar Mass and Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 dark ages, reionization, first stars \u2013 diffuse radiation \u2013 intergalactic medium\n\u2013 large-scale structure of universe", "note": "\u00a9 2018 The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. \n\nReceived 2017 October 27; revised 2018 February 19; accepted 2018 March 2; published 2018 March 29. \n\nThe authors would like to thank the anonymous referee for valuable suggestions. The authors also acknowledge Ryan Quadri and Adam Muzzin for the continued support of our stacking program and the valuable insights from the near-infrared community. T.-C.C. acknowledges MoST grant 103-2112-M-001-002-MY3 and JPL R&TD Award 01STCR\u2014R.17.226.063. J.H. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. A.C. was supported by a KISS postdoctoral fellowship and is now supported by the National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under Grant No. 1602677. M.B.S. acknowledges the Netherlands Foundation for Scientific Research support through the VICI grant 639.043.006. M.P.V. acknowledges support by the US Department of Energy through a KIPAC Fellowship at Stanford University.\n\nPublished - Sun_2018_ApJ_856_107.pdf
Submitted - 1610.10095.pdf
", "abstract": "Intensity mapping provides a unique means to probe the epoch of reionization (EoR), when the neutral intergalactic medium was ionized by energetic photons emitted from the first galaxies. The [C II] 158 \u03bcm fine-structure line is typically one of the brightest emission lines of star-forming galaxies and thus a promising tracer of the global EoR star formation activity. However, [C II] intensity maps at 6 \u227e z \u227e 8 are contaminated by interloping CO rotational line emission (3 \u2a7d J_(upp) \u2a7d 6) from lower-redshift galaxies. Here we present a strategy to remove the foreground contamination in upcoming [C II] intensity mapping experiments, guided by a model of CO emission from foreground galaxies. The model is based on empirical measurements of the mean and scatter of the total infrared luminosities of galaxies at z < 3 and with stellar masses M* > 10^8 M\u2299 selected in the K-band from the COSMOS/UltraVISTA survey, which can be converted to CO line strengths. For a mock field of the Tomographic Ionized-carbon Mapping Experiment, we find that masking out the \"voxels\" (spectral\u2013spatial elements) containing foreground galaxies identified using an optimized CO flux threshold results in a z-dependent criterion m^(AB)_K \u227e 22 (or M* \u2273 10^9 M\u2299)) at z < 1 and makes a [C II]/CO_(tot) power ratio of \u227310 at k = 0.1 h/Mpc achievable, at the cost of a moderate \u227e 8% loss of total survey volume.", "date": "2018-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "856", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 107", "id_number": "CaltechAUTHORS:20170531-140121068", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170531-140121068", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "103-2112-M-001-002-MY3" }, { "agency": "JPL", "grant_number": "01STCR-R.17.226.063" }, { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" }, { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NSF Astronomy and Astrophysics Fellowship", "grant_number": "AST-1602677" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.043.006" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aab3e3", "primary_object": { "basename": "1610.10095.pdf", "url": "https://authors.library.caltech.edu/records/f9ym3-xvk97/files/1610.10095.pdf" }, "related_objects": [ { "basename": "Sun_2018_ApJ_856_107.pdf", "url": "https://authors.library.caltech.edu/records/f9ym3-xvk97/files/Sun_2018_ApJ_856_107.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Sun, G.; Moncelsi, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/vv3ks-vk613", "eprint_id": 84775, "eprint_status": "archive", "datestamp": "2023-08-21 22:41:48", "lastmod": "2023-10-18 16:41:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nayyeri-H", "name": { "family": "Nayyeri", "given": "H." }, "orcid": "0000-0001-8242-9983" }, { "id": "Ghotbi-N", "name": { "family": "Ghotbi", "given": "N." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "D. L." }, "orcid": "0000-0002-9548-5033" }, { "id": "Im-Myungshin", "name": { "family": "Im", "given": "M." }, "orcid": "0000-0002-8537-6714" }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Korngut-P-M", "name": { "family": "Korngut", "given": "P." } }, { "id": "Lanz-A", "name": { "family": "Lanz", "given": "A." } }, { "id": "Lee-Hyung-Mok", "name": { "family": "Lee", "given": "H. M." }, "orcid": "0000-0003-4412-7161" }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Malkan-M", "name": { "family": "Malkan", "given": "M." }, "orcid": "0000-0001-6919-1237" }, { "id": "Matsuhara-Hideo", "name": { "family": "Matsuhara", "given": "H." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "U. W." } }, { "id": "Pearson-C-P", "name": { "family": "Pearson", "given": "C." }, "orcid": "0000-0001-6139-649X" }, { "id": "Serjeant-S", "name": { "family": "Serjeant", "given": "S." }, "orcid": "0000-0002-0517-7943" }, { "id": "Smidt-J", "name": { "family": "Smidt", "given": "J." } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "T." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Spitzer Observations of the North Ecliptic Pole", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies; infrared: stars; surveys", "note": "\u00a9 2018 American Astronomical Society. \n\nReceived 2017 September 3. Accepted 2017 November 19. Published 2018 February 8. \n\nWe wish to thank the referee for reading the original manuscript and providing useful suggestions. Financial support for this work was provided by NSF through AST-1313319 for H.N. and A.C. The UCI group also acknowledges support from HST-GO-14083.002-A, HST-GO-13718.002-A, and NASA NNX16AF38G grants. M.I. acknowledge the support from the NRFK grant, No. 2017R1A3A3001362. This work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.\n\nPublished - Nayyeri_2018_ApJS_234_38.pdf
Submitted - 1712.01290.pdf
", "abstract": "We present a photometric catalog for Spitzer Space Telescope warm mission observations of the North Ecliptic Pole (NEP; centered at R.A. = 18^h00^m00^s, decl. = 66^d33^m38^s.552). The observations are conducted with IRAC in the 3.6 and 4.5 \u03bcm bands over an area of 7.04 deg^2, reaching 1\u03c3 depths of 1.29 \u03bcJy and 0.79 \u03bcJy in the 3.6 \u03bcm and 4.5 \u03bcm bands, respectively. The photometric catalog contains 380,858 sources with 3.6 and 4.5 \u03bcm band photometry over the full-depth NEP mosaic. Point-source completeness simulations show that the catalog is 80% complete down to 19.7 AB. The accompanying catalog can be used for constraining the physical properties of extragalactic objects, studying the AGN population, measuring the infrared colors of stellar objects, and studying the extragalactic infrared background light.", "date": "2018-02", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "234", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 38", "id_number": "CaltechAUTHORS:20180212-073736632", "issn": "1538-4365", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180212-073736632", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "NASA", "grant_number": "HST-GO-14083.002-A" }, { "agency": "NASA", "grant_number": "HST-GO-13718.002-A" }, { "agency": "NASA", "grant_number": "NNX16AF38G" }, { "agency": "National Research Foundation of Korea", "grant_number": "2017R1A3A3001362" }, { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4365/aaa07e", "primary_object": { "basename": "1712.01290.pdf", "url": "https://authors.library.caltech.edu/records/vv3ks-vk613/files/1712.01290.pdf" }, "related_objects": [ { "basename": "Nayyeri_2018_ApJS_234_38.pdf", "url": "https://authors.library.caltech.edu/records/vv3ks-vk613/files/Nayyeri_2018_ApJS_234_38.pdf" } ], "resource_type": "article", "pub_year": "2018", "author_list": "Nayyeri, H.; Ghotbi, N.; et el." }, { "id": "https://authors.library.caltech.edu/records/h6ss3-3ax43", "eprint_id": 83159, "eprint_status": "archive", "datestamp": "2023-08-19 06:03:33", "lastmod": "2023-10-17 22:56:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Ghosh-T", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "O'Brient-R", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Schillaci-A", "name": { "family": "Schillaci", "given": "A." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B", "name": { "family": "Steinbach", "given": "B." } } ] }, "title": "BICEP2 / Keck Array IX: New bounds on anisotropies of CMB polarization rotation and implications for axionlike particles and primordial magnetic fields", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2017 American Physical Society. \n\nReceived 13 May 2017; revised manuscript received 28 June 2017; published 9 November 2017. \n\nThe Keck Array project has been made possible through support from the National Science Foundation under Grants No. ANT-1145172 (Harvard), No. ANT-1145143 (Minnesota), and No. ANT-1145248 (Stanford) and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station, without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP/Keck Array series of experiments, including the BICEP1 team. We thank Chang Feng for providing the histogram data shown in Ref. [31].\n\nPublished - PhysRevD.96.102003.pdf
Submitted - 1705.02523.pdf
", "abstract": "We present the strongest constraints to date on anisotropies of cosmic microwave background (CMB) polarization rotation derived from 150 GHz data taken by the BICEP2 & Keck Array CMB experiments up to and including the 2014 observing season (BK14). The definition of the polarization angle in BK14 maps has gone through self-calibration in which the overall angle is adjusted to minimize the observed TB and EB power spectra. After this procedure, the QU maps lose sensitivity to a uniform polarization rotation but are still sensitive to anisotropies of polarization rotation. This analysis places constraints on the anisotropies of polarization rotation, which could be generated by CMB photons interacting with axionlike pseudoscalar fields or Faraday rotation induced by primordial magnetic fields. The sensitivity of BK14 maps (\u223c3\u2009\u2009\u03bcK\u2212arc\u2009min) makes it possible to reconstruct anisotropies of the polarization rotation angle and measure their angular power spectrum much more precisely than previous attempts. Our data are found to be consistent with no polarization rotation anisotropies, improving the upper bound on the amplitude of the rotation angle spectrum by roughly an order of magnitude compared to the previous best constraints. Our results lead to an order of magnitude better constraint on the coupling constant of the Chern-Simons electromagnetic term g_(a\u03b3) \u2264 7.2\u00d710^(\u22122)/H_I (95% confidence) than the constraint derived from the B-mode spectrum, where H_I is the inflationary Hubble scale. This constraint leads to a limit on the decay constant of 10^(\u22126) \u2272 f_a/M_(pl) at mass range of 10^(\u221233) \u2264 ma \u2264 10^(\u221228)\u2009\u2009eV for r=0.01, assuming g_(a\u03b3) \u223c \u03b1/(2\u03c0f_a) with \u03b1 denoting the fine structure constant. The upper bound on the amplitude of the primordial magnetic fields is 30 nG (95% confidence) from the polarization rotation anisotropies.", "date": "2017-11-15", "date_type": "published", "publication": "Physical Review D", "volume": "96", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 102003", "id_number": "CaltechAUTHORS:20171113-140702052", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171113-140702052", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "corp_creators": { "items": [ "KECK ARRAY Collaboration", "BICEP2 Collaboration" ] }, "doi": "10.1103/PhysRevD.96.102003", "primary_object": { "basename": "1705.02523.pdf", "url": "https://authors.library.caltech.edu/records/h6ss3-3ax43/files/1705.02523.pdf" }, "related_objects": [ { "basename": "PhysRevD.96.102003.pdf", "url": "https://authors.library.caltech.edu/records/h6ss3-3ax43/files/PhysRevD.96.102003.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/gz8qj-sez48", "eprint_id": 80951, "eprint_status": "archive", "datestamp": "2023-08-21 21:42:52", "lastmod": "2023-10-17 19:17:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Manzotti-A", "name": { "family": "Manzotti", "given": "A." }, "orcid": "0000-0003-0057-877X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crites-A-T", "name": { "family": "Crites", "given": "A. T." } }, { "id": "Padin-S", "name": { "family": "Padin", "given": "S." } } ] }, "title": "CMB Polarization B-mode Delensing with SPTpol and Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; early universe; inflation", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 January 21; revised 2017 June 30; accepted 2017 July 25; published 2017 August 30. \n\nThe South Pole Telescope program is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago. Work at Argonne National Lab is supported by UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. This work is also supported by the U.S. Department of Energy. The CU Boulder group acknowledges support from NSF AST-0956135. BB is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the U.S. Department of Energy. C.R. acknowledges support from a Australian Research Councils Future Fellowship (FT150100074). W.L.K.W. is grateful for support from the Croucher Foundation and hospitality of Stanford University. J.W.H. is supported by the National Science Foundation under Award No. AST-1402161. The data analysis pipeline uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). The authors acknowledge useful discussions with Blake Sherwin and Toshiya Namikawa and use of code first written by Duncan Hanson.\n\nPublished - Manzotti_2017_ApJ_846_45.pdf
Submitted - 1701.04396.pdf
", "abstract": "We present a demonstration of delensing the observed cosmic microwave background (CMB) B-mode polarization anisotropy. This process of reducing the gravitational-lensing-generated B-mode component will become increasingly important for improving searches for the B modes produced by primordial gravitational waves. In this work, we delens B-mode maps constructed from multi-frequency SPTpol observations of a 90 deg^2 patch of sky by subtracting a B-mode template constructed from two inputs: SPTpol E-mode maps and a lensing potential map estimated from the Herschel 500 \u03bcm map of the cosmic infrared background. We find that our delensing procedure reduces the measured B-mode power spectrum by 28% in the multipole range 300 < \u2113 < 2300; this is shown to be consistent with expectations from simulations and to be robust against systematics. The null hypothesis of no delensing is rejected at 6.9\u03c3. Furthermore, we build and use a suite of realistic simulations to study the general properties of the delensing process and find that the delensing efficiency achieved in this work is limited primarily by the noise in the lensing potential map. We demonstrate the importance of including realistic experimental non-idealities in the delensing forecasts used to inform instrument and survey-strategy planning of upcoming lower-noise experiments, such as CMB-S4.", "date": "2017-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "846", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 45", "id_number": "CaltechAUTHORS:20170830-101242847", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170830-101242847", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PLR-1248097" }, { "agency": "NSF", "grant_number": "PHY-0114422" }, { "agency": "Kavli Foundation" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "947" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-06CH11357" }, { "agency": "Argonne Center for Nanoscale Materials" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canada Research Chairs Program" }, { "agency": "NSF", "grant_number": "AST-0956135" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-07CH11359" }, { "agency": "Australian Research Council", "grant_number": "FT150100074" }, { "agency": "Croucher Foundation" }, { "agency": "NSF", "grant_number": "AST-1402161" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa82bb", "primary_object": { "basename": "1701.04396.pdf", "url": "https://authors.library.caltech.edu/records/gz8qj-sez48/files/1701.04396.pdf" }, "related_objects": [ { "basename": "Manzotti_2017_ApJ_846_45.pdf", "url": "https://authors.library.caltech.edu/records/gz8qj-sez48/files/Manzotti_2017_ApJ_846_45.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Manzotti, A.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/wh6ga-m5h27", "eprint_id": 79749, "eprint_status": "archive", "datestamp": "2023-08-19 04:33:39", "lastmod": "2023-10-26 17:05:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nagy-J-M", "name": { "family": "Nagy", "given": "J. M." }, "orcid": "0000-0002-2036-7008" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-T-A", "name": { "family": "Morford", "given": "T. A." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } } ] }, "title": "A New Limit on CMB Circular Polarization from SPIDER", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2017 April 5; revised 2017 June 21; accepted 2017 June 28; published 2017 August 2. \n\nSpider is supported in the U.S. by the National Aeronautics and Space Administration under grants NNX07AL64G, NNX12AE95G, and NNX17AC55G issued through the Science Mission Directorate and by the National Science Foundation through PLR-1043515. Logistical support for the Antarctic deployment and operations was provided by the NSF through the U.S. Antarctic Program. Support in Canada is provided by the Natural Sciences and Engineering Research Council and the Canadian Space Agency. Support in Norway is provided by the Research Council of Norway. Support in Sweden is provided by the Swedish Research Council through the Oskar Klein Centre (contract no. 638-2013-8993). We also wish to acknowledge the generous support of the David and Lucile Packard Foundation, which has been crucial to the success of the project.\n\nThe collaboration is grateful to the British Antarctic Survey, particularly Sam Burrell, for invaluable assistance with data and payload recovery after the 2015 flight. We thank Brendan Crill and Tom Montroy for significant contributions to Spider's development. J.M.N. wishes to thank Glenn Starkman for useful discussions about methods of generating CMB circular polarization. The computations described in this paper were performed on the GPC supercomputer at the SciNet HPC Consortium (Loken et al. 2010). SciNet is funded by, the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund\u2014Research Excellence; and the University of Toronto.\n\nPublished - Nagy_2017_ApJ_844_151.pdf
Submitted - 1704.00215.pdf
", "abstract": "We present a new upper limit on cosmic microwave background (CMB) circular polarization from the 2015 flight of SPIDER, a balloon-borne telescope designed to search for B-mode linear polarization from cosmic inflation. Although the level of circular polarization in the CMB is predicted to be very small, experimental limits provide a valuable test of the underlying models. By exploiting the nonzero circular-to-linear polarization coupling of the half-wave plate polarization modulators, data from SPIDER's 2015 Antarctic flight provide a constraint on Stokes V at 95 and 150 GHz in the range 33 < \u2113 < 307. No other limits exist over this full range of angular scales, and SPIDER improves on the previous limit by several orders of magnitude, providing 95% C.L. constraints on \u2113(\u2113 + 1)C^(VV)_ \u2113/(2\u03c0) ranging from 141 to 255 \u03bcK^2 at 150 GHz for a thermal CMB spectrum. As linear CMB polarization experiments become increasingly sensitive, the techniques described in this paper can be applied to obtain even stronger constraints on circular polarization.", "date": "2017-08-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "844", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 151", "id_number": "CaltechAUTHORS:20170802-102243947", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170802-102243947", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NASA", "grant_number": "NNX17AC55G" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Research Council of Norway" }, { "agency": "Swedish Research Council", "grant_number": "638-2013-8993" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa7cfd", "primary_object": { "basename": "1704.00215.pdf", "url": "https://authors.library.caltech.edu/records/wh6ga-m5h27/files/1704.00215.pdf" }, "related_objects": [ { "basename": "Nagy_2017_ApJ_844_151.pdf", "url": "https://authors.library.caltech.edu/records/wh6ga-m5h27/files/Nagy_2017_ApJ_844_151.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Nagy, J. M.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/z26yz-58a97", "eprint_id": 88117, "eprint_status": "archive", "datestamp": "2023-08-19 03:00:32", "lastmod": "2023-10-18 21:48:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ghosh-T", "name": { "family": "Ghosh", "given": "T." } }, { "id": "Boulanger-F", "name": { "family": "Boulanger", "given": "F." } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "P. G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Bracco-A", "name": { "family": "Bracco", "given": "A." } }, { "id": "Vansyngel-F", "name": { "family": "Vansyngel", "given": "F." } }, { "id": "Aumont-J", "name": { "family": "Aumont", "given": "J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Haud-U", "name": { "family": "Haud", "given": "U." } }, { "id": "Kalberla-P-M-W", "name": { "family": "Kalberla", "given": "P. M. W." } }, { "id": "Serra-P", "name": { "family": "Serra", "given": "P." } } ] }, "title": "Modelling and simulation of large-scale polarized dust emission over the southern Galactic cap using the GASS HI data", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction \u2013 ISM: magnetic fields \u2013 ISM: structure \u2013 polarization \u2013 Galaxy: general \u2013 submillimeter: ISM", "note": "\u00a9 2017 ESO. Article published by EDP Sciences. \n\nReceived 2 October 2016; Accepted 24 January 2017; Published online 04 May 2017. \n\nThe research leading to these results has received funding from the European Research Council grant MISTIC (ERC-267934). Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. U.H. acknowledges the support by the Estonian Research Council grant IUT26-2, and by the European Regional Development Fund (TK133). The Parkes Radio Telescope is part of the Australia Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Some of the results in this paper have been derived using the HEALPix package. Finally, we acknowledge the use of Planck data available from Planck Legacy Archive (http://www.cosmos.esa.int/web/planck/pla).\n\nPublished - aa29829-16.pdf
Accepted Version - 1611.02418.pdf
", "abstract": "The Planck survey has quantified polarized Galactic foregrounds and established that they are a main limiting factor in the quest for the cosmic microwave background B-mode signal induced by primordial gravitational waves during cosmic inflation. Accurate separation of the Galactic foregrounds therefore binds this quest to our understanding of the magnetized interstellar medium. The two most relevant empirical results from analysis of Planck data are line of sight depolarization arising from fluctuations of the Galactic magnetic field orientation and alignment of filamentary dust structures with the magnetic field at high Galactic latitude. Furthermore, Planck and H I emission data in combination indicate that most of the filamentary dust structures are in the cold neutral medium. The goal of this paper is to test whether these salient observational results, taken together, can account fully for the statistical properties of the dust polarization over a selected low column density region comprising 34% of the southern Galactic cap (b \u2264 \u221230\u00b0). To do this, we construct a dust model that incorporates H I column density maps as tracers of the dust intensity structures and a phenomenological description of the Galactic magnetic field. By adjusting the parameters of the dust model, we were able to reproduce the Planck dust observations at 353GHz in the selected region. Realistic simulations of the polarized dust emission enabled by such a dust model are useful for testing the accuracy of component separation methods, studying non-Gaussianity, and constraining the amount of decorrelation with frequency.", "date": "2017-05", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "601", "publisher": "EDP Sciences", "pagerange": "Art. No. A71", "id_number": "CaltechAUTHORS:20180723-091906911", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180723-091906911", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Estonian Research Council", "grant_number": "IUT26-2" }, { "agency": "European Regional Development Fund", "grant_number": "TK133" }, { "agency": "Commonwealth of Australia" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.1051/0004-6361/201629829", "primary_object": { "basename": "1611.02418.pdf", "url": "https://authors.library.caltech.edu/records/z26yz-58a97/files/1611.02418.pdf" }, "related_objects": [ { "basename": "aa29829-16.pdf", "url": "https://authors.library.caltech.edu/records/z26yz-58a97/files/aa29829-16.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Ghosh, T.; Boulanger, F.; et el." }, { "id": "https://authors.library.caltech.edu/records/3kvdz-yns48", "eprint_id": 76481, "eprint_status": "archive", "datestamp": "2023-08-19 02:34:57", "lastmod": "2023-10-25 16:02:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "Shuji" }, "orcid": "0000-0002-5698-9634" }, { "id": "Arai-Toshiaki", "name": { "family": "Arai", "given": "Toshiaki" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Korngut-P-M", "name": { "family": "Korngut", "given": "Phillip M." } }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "Min Gyu" } }, { "id": "Lee-Hyung-Mok", "name": { "family": "Lee", "given": "Hyung Mok" }, "orcid": "0000-0003-4412-7161" }, { "id": "Lee-Dae-Hee", "name": { "family": "Lee", "given": "Dae Hee" } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "Louis R." } }, { "id": "Matsumoto-Toshio", "name": { "family": "Matsumoto", "given": "Toshio" }, "orcid": "0000-0001-6066-5221" }, { "id": "Onishi-Yosuke", "name": { "family": "Onishi", "given": "Yosuke" } }, { "id": "Shirahata-Mai", "name": { "family": "Shirahata", "given": "Mai" } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "Kohji" } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "Takehiko" } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "New Spectral Evidence of an Unaccounted Component of the Near-infrared Extragalactic Background Light from the CIBER", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 dark ages, reionization, first stars \u2013 diffuse radiation \u2013 infrared: diffuse background \u2013 infrared: general \u2013 zodiacal dust", "note": "\u00a9 2017 The American Astronomical Society. \n\nReceived 2016 November 14; revised 2017 March 15; accepted 2017 March 19; published 2017 April 7. \n\nWe acknowledge the support of Grants-in-Aid from the Japan Society for the Promotion of Science (KAKENHI 20.34, 18204018, 19540250, 21340047, 21111004, 24111717, 26800112, and 15H05744) and NASA APRA research grants, which funded US contributions to the CIBER instrument (NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G). Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. We thank the dedicated efforts of the sounding rocket staff at NASA Wallops Flight Facility and White Sands Missile Range, and also thank Dr. Allan Smith, Dr. Keith Lykke, and Dr. Steven Brown (NIST) for the laboratory calibration of LRS. A.C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319. H.M.L. was supported by NRF grant No.2012R1A4A1028713. S.M. thanks to Dr. Fumihiko Usui (Kobe University, CPS) and Dr. Takafumi Ootsubo (The University of Tokyo) for their help in coordinate calculations and for our discussions on the ZL models. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.\n\nPublished - Matsuura_2017_ApJ_839_7.pdf
Submitted - 1704.07166.pdf
", "abstract": "The extragalactic background light (EBL) captures the total integrated emission from stars and galaxies throughout the cosmic history. The amplitude of the near-infrared EBL from space absolute photometry observations has been controversial and depends strongly on the modeling and subtraction of the zodiacal light (ZL) foreground. We report the first measurement of the diffuse background spectrum at 0.8\u20131.7 \u03bcm from the CIBER experiment. The observations were obtained with an absolute spectrometer over two flights in multiple sky fields to enable the subtraction of ZL, stars, terrestrial emission, and diffuse Galactic light. After subtracting foregrounds and accounting for systematic errors, we find the nominal EBL brightness, assuming the Kelsall ZL model, is 42.7^(+11.9)_(-10.6) nW m^(\u22122) sr^(\u22121) at 1.4 \u03bcm. We also analyzed the data using the Wright ZL model, which results in a worse statistical fit to the data and an unphysical EBL, falling below the known background light from galaxies at \u03bb < 1.3 \u03bcm. Using a model-independent analysis based on the minimum EBL brightness, we find an EBL brightness of 28.7^(+5.1)_(-3.3) nWm^(\u22122) sr^(\u22121) at 1.4 \u03bcm. While the derived EBL amplitude strongly depends on the ZL model, we find that we cannot fit the spectral data to ZL, Galactic emission, and EBL from solely integrated galactic light from galaxy counts. The results require a new diffuse component, such as an additional foreground or an excess EBL with a redder spectrum than that of ZL.", "date": "2017-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "839", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 7", "id_number": "CaltechAUTHORS:20170410-140333599", "issn": "1538-4357", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170410-140333599", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20.34" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "24111717" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26800112" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "15H05744" }, { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "JPL Director's Research and Development Fund" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "National Research Foundation of Korea", "grant_number": "2012R1A4A1028713" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-4357/aa6843", "primary_object": { "basename": "1704.07166.pdf", "url": "https://authors.library.caltech.edu/records/3kvdz-yns48/files/1704.07166.pdf" }, "related_objects": [ { "basename": "Matsuura_2017_ApJ_839_7.pdf", "url": "https://authors.library.caltech.edu/records/3kvdz-yns48/files/Matsuura_2017_ApJ_839_7.pdf" } ], "resource_type": "article", "pub_year": "2017", "author_list": "Matsuura, Shuji; Arai, Toshiaki; et el." }, { "id": "https://authors.library.caltech.edu/records/fe7h9-fcr43", "eprint_id": 73766, "eprint_status": "archive", "datestamp": "2023-08-22 19:37:46", "lastmod": "2023-10-24 16:25:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "Min Gyu" } }, { "id": "Lee-Hyung-Mok", "name": { "family": "Lee", "given": "Hyung Mok" }, "orcid": "0000-0003-4412-7161" }, { "id": "Arai-Toshiaki", "name": { "family": "Arai", "given": "Toshiaki" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Jeong-Woong-Seob", "name": { "family": "Jeong", "given": "Woong-Seob" } }, { "id": "Kim-Seong-Jin", "name": { "family": "Kim", "given": "Seong Jin" } }, { "id": "Korngut-P-M", "name": { "family": "Korngut", "given": "Phillip" } }, { "id": "Lanz-A", "name": { "family": "Lanz", "given": "Alicia" } }, { "id": "Lee-Dae-Hee", "name": { "family": "Lee", "given": "Dae Hee" } }, { "id": "Lee-Myung-Gyoon", "name": { "family": "Lee", "given": "Myung Gyoon" } }, { "id": "Matsumoto-Toshio", "name": { "family": "Matsumoto", "given": "Toshio" }, "orcid": "0000-0001-6066-5221" }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "Shuji" }, "orcid": "0000-0002-5698-9634" }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "Uk Won" } }, { "id": "Onishi-Yosuke", "name": { "family": "Onishi", "given": "Yosuke" } }, { "id": "Shirahata-Mai", "name": { "family": "Shirahata", "given": "Mai" } }, { "id": "Smidt-J", "name": { "family": "Smidt", "given": "Joseph" } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "Kohji" } }, { "id": "Yamamura-Issei", "name": { "family": "Yamamura", "given": "Issei" } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Low-Resolution Near-infrared Stellar Spectra Observed by the Cosmic Infrared Background Experiment (CIBER)", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs; infrared: stars; stars: general; techniques: spectroscopic", "note": "\u00a9 2017. The American Astronomical Society. \n\nReceived 2016 August 22; revised 2016 November 29; accepted 2016 December 10; published 2017 January 25. \n\nThis work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. Japanese participation in CIBER was supported by KAKENHI (2034, 18204018, 19540250, 21340047, 21111004, and 26800112) from the Japan Society for the Promotion of Science and the Ministry of Education, Culture, Sports, Science, and Technology. Korean participation in CIBER was supported by the Pioneer Project from the Korea Astronomy and Space Science Institute. M.G.K. acknowledges support from the Global PhD Fellowship Program through the NRF, funded by the Ministry of Education (2011-0007760). H.M.L. and M.G.L. were supported by NRF grant 2012R1A4A1028713. M.Z. and P.K. acknowledge support from NASA postdoctoral program fellowships, and A.C. acknowledges support from NSF CAREER awards AST-0645427 and NSF AST-1313319. We acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and White Sands Missile Range and also thank Dr. Allan Smith, Dr. Keith Lykke, and Dr. Steven Brown (NIST) for the laboratory calibration of the LRS. This publication makes use of data products from 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the SpeX library.\n\nPublished - Kim_2017_AJ_153_84.pdf
", "abstract": "We present near-infrared (0.8\u20131.8 \u03bcm) spectra of 105 bright (m_J < 10) stars observed with the low-resolution spectrometer on the rocket-borne Cosmic Infrared Background Experiment. As our observations are performed above the Earth's atmosphere, our spectra are free from telluric contamination, which makes them a unique resource for near-infrared spectral calibration. Two-Micron All-Sky Survey photometry information is used to identify cross-matched stars after reduction and extraction of the spectra. We identify the spectral types of the observed stars by comparing them with spectral templates from the Infrared Telescope Facility library. All the observed spectra are consistent with late F to M stellar spectral types, and we identify various infrared absorption lines.", "date": "2017-02", "date_type": "published", "publication": "Astronomical Journal", "volume": "153", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 84", "id_number": "CaltechAUTHORS:20170126-164400934", "issn": "1538-3881", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170126-164400934", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "2034" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26800112" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "National Research Foundation of Korea", "grant_number": "2012R1A4A1028713" }, { "agency": "Ministry of Education (Korea)", "grant_number": "2011-0007760" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" } ] }, "local_group": { "items": [ { "id": "Astronomy-Department" } ] }, "doi": "10.3847/1538-3881/153/2/84", "primary_object": { "basename": "Kim_2017_AJ_153_84.pdf", "url": "https://authors.library.caltech.edu/records/fe7h9-fcr43/files/Kim_2017_AJ_153_84.pdf" }, "resource_type": "article", "pub_year": "2017", "author_list": "Kim, Min Gyu; Lee, Hyung Mok; et el." }, { "id": "https://authors.library.caltech.edu/records/1kgdt-d7j79", "eprint_id": 73999, "eprint_status": "archive", "datestamp": "2023-08-22 19:19:31", "lastmod": "2023-10-24 21:59:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "O'Brient-R", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "BICEP2 / Keck Array VIII: Measurement of gravitational lensing from large-scale B-mode polarization", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational lensing: weak; polarization", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 June 3. Accepted 2016 August 22. Published 2016 December 19. \n\nThe Keck Array project has been made possible through support from the National Science Foundation under Grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota), and ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grant Nos. 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP-Keck Array series of experiments, including the BICEP1 team. T.N. acknowledges support from Japan Society for the Promotion of Science Postdoctoral Fellowships for Research Abroad.\n\nPublished - Ade_2016_ApJ_833_228.pdf
Submitted - 1606.01968v2.pdf
", "abstract": "We present measurements of polarization lensing using the 150 GHz maps, which include all data taken by the BICEP2 and Keck Array Cosmic Microwave Background polarization experiments up to and including the 2014 observing season (BK14). Despite their modest angular resolution (~0\u00ba.5), the excellent sensitivity (~3\u03bcK-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales (\u2113 \u2a7e 700). From the auto-spectrum of the reconstructed potential, we measure an amplitude of the spectrum to be A_L^(\u00f8\u00f8) = 1.15 \u00b1 0.36 (Planck \u039bCDM prediction corresponds to A_L^(\u00f8\u00f8) = 1) and reject the no-lensing hypothesis at 5.8\u03c3, which is the highest significance achieved to date using an EB lensing estimator. Taking the cross-spectrum of the reconstructed potential with the Planck 2015 lensing map yields A_L^(\u00f8\u00f8) = 1.13 \u00b1 0.20. These direct measurements of A_L^(\u00f8\u00f8) are consistent with the \u039bCDM cosmology and with that derived from the previously reported BK14 B-mode auto-spectrum (A_L^(BB) = 1.20 \u00b1 0.17). We perform a series of null tests and consistency checks to show that these results are robust against systematics and are insensitive to analysis choices. These results unambiguously demonstrate that the B modes previously reported by BICEP/Keck at intermediate angular scales (150 \u227e \u2113 \u227e 350) are dominated by gravitational lensing. The good agreement between the lensing amplitudes obtained from the lensing reconstruction and B-mode spectrum starts to place constraints on any alternative cosmological sources of B modes at these angular scales.", "date": "2016-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "833", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 288", "id_number": "CaltechAUTHORS:20170203-073431857", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170203-073431857", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund", "grant_number": "06-ARPA206-0040" }, { "agency": "JPL Research and Technology Development Fund", "grant_number": "10-SAT10-0017" }, { "agency": "NASA" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" } ] }, "corp_creators": { "items": [ "KECK ARRAY Collaborations", "BICEP2 Collaboration" ] }, "doi": "10.3847/1538-4357/833/2/228", "primary_object": { "basename": "1606.01968v2.pdf", "url": "https://authors.library.caltech.edu/records/1kgdt-d7j79/files/1606.01968v2.pdf" }, "related_objects": [ { "basename": "Ade_2016_ApJ_833_228.pdf", "url": "https://authors.library.caltech.edu/records/1kgdt-d7j79/files/Ade_2016_ApJ_833_228.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/v31k7-47287", "eprint_id": 71188, "eprint_status": "archive", "datestamp": "2023-08-19 00:25:18", "lastmod": "2023-10-23 15:27:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Yun-Ting" }, "orcid": "0000-0002-5437-0504" }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "Tzu-Ching" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. Matt" }, "orcid": "0000-0001-5261-7094" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" } ] }, "title": "Spectral Line De-confusion in an Intensity Mapping Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: theory \u2013 observations \u2013 dark ages, reionization, first stars \u2013 large-scale structure of universe", "note": "\u00a9 2016. The American Astronomical Society. \n\nReceived 2016 April 26; revised 2016 September 19; accepted 2016 September 26; published 2016 November 30. \n\nWe are grateful to the Time-Pilot collaboration for providing useful inputs throughout this work. We thank Phil Bull, Olivier Dor\u00e9 Tony Li, Adam Lidz, Roland de Putter, Paolo Serra, Chun-Hao To, and Heidi Hao-Yi Wu for helpful discussions and valuable comments on the manuscript. Y.-T.C. and T.-C.C. were supported in part by MoST grant 103-2112-M-001-002-MY3. T.-C.C. gratefully acknowledges the hospitality of the Caltech OBSCOS group and the Jet Propulsion Laboratory, where part of this work was carried out.\n\nPublished - Cheng_2016_ApJ_832_165.pdf
Submitted - 1604.07833v2.pdf
", "abstract": "Spectral line intensity mapping (LIM) has been proposed as a promising tool to efficiently probe the cosmic reionization and the large-scale structure. Without detecting individual sources, LIM makes use of all available photons and measures the integrated light in the source confusion limit to efficiently map the three-dimensional matter distribution on large scales as traced by a given emission line. One particular challenge is the separation of desired signals from astrophysical continuum foregrounds and line interlopers. Here we present a technique to extract large-scale structure information traced by emission lines from different redshifts, embedded in a three-dimensional intensity mapping data cube. The line redshifts are distinguished by the anisotropic shape of the power spectra when projected onto a common coordinate frame. We consider the case where high-redshift [C ii] lines are confused with multiple low-redshift CO rotational lines. We present a semi-analytic model for [C ii] and CO line estimates based on the cosmic infrared background measurements, and show that with a modest instrumental noise level and survey geometry, the large-scale [C ii] and CO power spectrum amplitudes can be successfully extracted from a confusion-limited data set, without external information. We discuss the implications and limits of this technique for possible LIM experiments.", "date": "2016-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "832", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 165", "id_number": "CaltechAUTHORS:20161017-144435669", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161017-144435669", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Science and Technology (Taipei)", "grant_number": "103-2112-M-001-002-MY3" } ] }, "doi": "10.3847/0004-637X/832/2/165", "primary_object": { "basename": "Cheng_2016_ApJ_832_165.pdf", "url": "https://authors.library.caltech.edu/records/v31k7-47287/files/Cheng_2016_ApJ_832_165.pdf" }, "related_objects": [ { "basename": "1604.07833v2.pdf", "url": "https://authors.library.caltech.edu/records/v31k7-47287/files/1604.07833v2.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Cheng, Yun-Ting; Chang, Tzu-Ching; et el." }, { "id": "https://authors.library.caltech.edu/records/qb5z6-qkr53", "eprint_id": 73992, "eprint_status": "archive", "datestamp": "2023-08-19 00:17:21", "lastmod": "2023-10-24 21:59:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results XLVII. Planck constraints on reionization history", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / dark ages, reionization, first stars / polarization", "note": "\u00a9 ESO, 2016. \n\nReceived 11 May 2016. Accepted 23 July 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa28897-16.pdf
Submitted - 1605.03507v3.pdf
", "abstract": "We investigate constraints on cosmic reionization extracted from the Planck cosmic microwave background (CMB) data. We combine the Planck CMB anisotropy data in temperature with the low-multipole polarization data to fit \u039bCDM models with various parameterizations of the reionization history. We obtain a Thomson optical depth \u03c4 = 0.058 \u00b1 0.012 for the commonly adopted instantaneous reionization model. This confirms, with data solely from CMB anisotropies, the low value suggested by combining Planck 2015 results with other data sets, and also reduces the uncertainties. We reconstruct the history of the ionization fraction using either a symmetric or an asymmetric model for the transition between the neutral and ionized phases. To determine better constraints on the duration of the reionization process, we also make use of measurements of the amplitude of the kinetic Sunyaev-Zeldovich (kSZ) effect using additional information from the high-resolution Atacama Cosmology Telescope and South Pole Telescope experiments. The average redshift at which reionization occurs is found to lie between z = 7.8 and 8.8, depending on the model of reionization adopted. Using kSZ constraints and a redshift-symmetric reionization model, we find an upper limit to the width of the reionization period of \u0394z < 2.8. In all cases, we find that the Universe is ionized at less than the 10% level at redshifts above z \u2243 10. This suggests that an early onset of reionization is strongly disfavoured by the Planck data. We show that this result also reduces the tension between CMB-based analyses and constraints from other astrophysical sources.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A108", "id_number": "CaltechAUTHORS:20170202-143503710", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170202-143503710", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Centro Nazionale delle Ricerche (CNR)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Innovation" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "PRACE (EU)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Ministro da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201628897", "primary_object": { "basename": "1605.03507v3.pdf", "url": "https://authors.library.caltech.edu/records/qb5z6-qkr53/files/1605.03507v3.pdf" }, "related_objects": [ { "basename": "aa28897-16.pdf", "url": "https://authors.library.caltech.edu/records/qb5z6-qkr53/files/aa28897-16.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/n6t5r-6q222", "eprint_id": 73985, "eprint_status": "archive", "datestamp": "2023-08-19 00:17:00", "lastmod": "2023-10-24 21:58:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck intermediate results. XLI. A map of lensing-induced B-modes", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 ESO. \n\nReceived 9 December 2015; Accepted 7 September 2016; Published online 12 December 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck. This paper made use of the HEALPix software package. We thank the anonymous referee for their helpful comments and thoughtful suggestions that contributed to improve this paper.\n\nPublished - aa27932-15.pdf
Submitted - 1512.02882v2.pdf
", "abstract": "The secondary cosmic microwave background (CMB) B-modes stem from the post-decoupling distortion of the polarization E-modes due to the gravitational lensing effect of large-scale structures. These lensing-induced B-modes constitute both a valuable probe of the dark matter distribution and an important contaminant for the extraction of the primary CMB B-modes from inflation. Planck provides accurate nearly all-sky measurements of both the polarization E-modes and the integrated mass distribution via the reconstruction of the CMB lensing potential. By combining these two data products, we have produced an all-sky template map of the lensing-induced B-modes using a real-space algorithm that minimizes the impact of sky masks. The cross-correlation of this template with an observed (primordial and secondary) B-mode map can be used to measure the lensing B-mode power spectrum at multipoles up to 2000. In particular, when cross-correlating with the B-mode contribution directly derived from the Planck polarization maps, we obtain lensing-induced B-mode power spectrum measurement at a significance level of 12\u03c3, which agrees with the theoretical expectation derived from the Planck best-fit \u039b cold dark matter model. This unique nearly all-sky secondary B-mode template, which includes the lensing-induced information from intermediate to small (10 \u2272 \u2113 \u2272 1000) angular scales, is delivered as part of the Planck 2015 public data release. It will be particularly useful for experiments searching for primordial B-modes, such as BICEP2/Keck Array or LiteBIRD, since it will enable an estimate to be made of the lensing-induced contribution to the measured total CMB B-modes.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A102", "id_number": "CaltechAUTHORS:20170202-104324827", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170202-104324827", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00e9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministry of Economy, Industry and Competitiveness (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Institut for Rumforskning og Rumteknologi (DTU Space)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "collection": "CaltechAUTHORS", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)", "value": "Infrared Processing and Analysis Center (IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201527932", "primary_object": { "basename": "aa27932-15.pdf", "url": "https://authors.library.caltech.edu/records/n6t5r-6q222/files/aa27932-15.pdf" }, "related_objects": [ { "basename": "1512.02882v2.pdf", "url": "https://authors.library.caltech.edu/records/n6t5r-6q222/files/1512.02882v2.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/q9hh2-weh50", "eprint_id": 96871, "eprint_status": "archive", "datestamp": "2023-08-19 00:23:37", "lastmod": "2023-10-20 21:35:07", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. XLVI. Reduction of large-scale systematic effects in HFI polarization maps and estimation of the reionization optical depth", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 dark ages, reionization, first stars \u2013 cosmic background radiation \u2013 space vehicles: instruments \u2013\ninstrumentation: detectors", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 10 May 2016; Accepted 14 July 2016; Published online 12 December 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa28890-16.pdf
Submitted - 1605.02985.pdf
", "abstract": "This paper describes the identification, modelling, and removal of previously unexplained systematic effects in the polarization data of the Planck High Frequency Instrument (HFI) on large angular scales, including new mapmaking and calibration procedures, new and more complete end-to-end simulations, and a set of robust internal consistency checks on the resulting maps. These maps, at 100, 143, 217, and 353\u2009GHz, are early versions of those that will be released in final form later in 2016. The improvements allow us to determine the cosmic reionization optical depth \u03c4 using, for the first time, the low-multipole EE data from HFI, reducing significantly the central value and uncertainty, and hence the upper limit. Two different likelihood procedures are used to constrain \u03c4 from two estimators of the CMB E- and B-mode angular power spectra at 100 and 143\u2009GHz, after debiasing the spectra from a small remaining systematic contamination. These all give fully consistent results. A further consistency test is performed using cross-correlations derived from the Low Frequency Instrument maps of the Planck 2015 data release and the new HFI data. For this purpose, end-to-end analyses of systematic effects from the two instruments are used to demonstrate the near independence of their dominant systematic error residuals. The tightest result comes from the HFI-based \u03c4 posterior distribution using the maximum likelihood power spectrum estimator from EE data only, giving a value 0.055 \u00b1 0.009. In a companion paper these results are discussed in the context of the best-fit Planck\u039bCDM cosmological model and recent models of reionization.", "date": "2016-12", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "596", "publisher": "EDP Sciences", "pagerange": "Art. No. A107", "id_number": "CaltechAUTHORS:20190702-073429800", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190702-073429800", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201628890", "primary_object": { "basename": "aa28890-16.pdf", "url": "https://authors.library.caltech.edu/records/q9hh2-weh50/files/aa28890-16.pdf" }, "related_objects": [ { "basename": "1605.02985.pdf", "url": "https://authors.library.caltech.edu/records/q9hh2-weh50/files/1605.02985.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Aghanim, N.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/3depd-be733", "eprint_id": 60299, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:06", "lastmod": "2023-10-24 16:24:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "S." }, "orcid": "0000-0002-2849-559X" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Pelkonen-Veli-Matti", "name": { "family": "Pelkonen", "given": "V.-M." }, "orcid": "0000-0002-8898-1047" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. I. Overview of products and scientific results", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmic background radiation \u2013 surveys \u2013 space vehicles: instruments \u2013 instrumentation: detectors", "note": "\u00a9 2016 ESO.\n\nReceived 1 August 2015; Accepted 18 January 2016;\nPublished online 20 September 2016.\n\n\nPlanck is a project of the European Space Agency in cooperation with the scientific community, which started in 1993. ESA led the project, developed the satellite, integrated the payload into it, and launched and operated the satellite. Two Consortia, comprising around 100 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed and operated the scientific instruments LFI and HFI. The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA's US Planck Project, based at JPL and involving scientists at many US institutions, contributes significantly to the efforts of these two Consortia. A third Consortium, led by H.U. Norgaard-Nielsen and supported by the Danish Natural Research Council, contributed to the reflector programme. These three Consortia, together with ESA's Planck Science Office, form the Planck Collaboration. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). We thank Diego Falceta-Gon\u00e7alves for providing the technique for making the line-integral-convolution maps presented in Figs. 23 and 25.\n\nPublished - aa27101-15.pdf
Submitted - 1502.01582v2.pdf
", "abstract": "The European Space Agency's Planck satellite, which is dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013. In February 2015, ESA and the Planck Collaboration released the second set of cosmology products based ondata from the entire Planck mission, including both temperature and polarization, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the main characteristics of the data and the data products in the release, as well as the associated cosmological and astrophysical science results and papers. The data products include maps of the cosmic microwave background (CMB), the thermal Sunyaev-Zeldovich effect, diffuse foregrounds in temperature and polarization, catalogues of compact Galactic and extragalactic sources (including separate catalogues of Sunyaev-Zeldovich clusters and Galactic cold clumps), and extensive simulations of signals and noise used in assessing uncertainties and the performance of the analysis methods. The likelihood code used to assess cosmological models against the Planck data is described, along with a CMB lensing likelihood. Scientific results include cosmological parameters derived from CMB power spectra, gravitational lensing, and cluster counts, as well as constraints on inflation, non-Gaussianity, primordial magnetic fields, dark energy, and modified gravity, and new results on low-frequency Galactic foregrounds.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A1", "id_number": "CaltechAUTHORS:20150917-084452506", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-084452506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National D'\u00e9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Danish Natural Research Council" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Institut for Rumforskning og Rumteknologi (DTU Space)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway (RCN)" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Ministro da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201527101", "primary_object": { "basename": "1502.01582v2.pdf", "url": "https://authors.library.caltech.edu/records/3depd-be733/files/1502.01582v2.pdf" }, "related_objects": [ { "basename": "aa27101-15.pdf", "url": "https://authors.library.caltech.edu/records/3depd-be733/files/aa27101-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/9stj0-49896", "eprint_id": 74400, "eprint_status": "archive", "datestamp": "2023-08-20 14:05:27", "lastmod": "2023-10-24 22:36:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. II. Low Frequency Instrument data processings", "ispublished": "pub", "full_text_status": "public", "keywords": "space vehicles: instruments \u2013 methods: data analysis \u2013 cosmic background radiation", "note": "\u00a9 2016 ESO. \n\nReceived 5 February 2015; Accepted 4 February 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/. Finally, we thank Benjamin Walter for a careful reading of the manuscript.\n\nPublished - aa25818-15.pdf
Submitted - 1502.01583.pdf
", "abstract": "We present an updated description of the Planck Low Frequency Instrument (LFI) data processing pipeline, associated with the 2015 data release. We point out the places where our results and methods have remained unchanged since the 2013 paper and we highlight the changes made for the 2015 release, describing the products (especially timelines) and the ways in which they were obtained. We demonstrate that the pipeline is self-consistent (principally based on simulations) and report all null tests. For the first time, we present LFI maps in Stokes Q and U polarization. We refer to other related papers where more detailed descriptions of the LFI data processing pipeline may be found if needed.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A2", "id_number": "CaltechAUTHORS:20170217-094632152", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170217-094632152", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National D'\u00e9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Ministro da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525818", "primary_object": { "basename": "1502.01583.pdf", "url": "https://authors.library.caltech.edu/records/9stj0-49896/files/1502.01583.pdf" }, "related_objects": [ { "basename": "aa25818-15.pdf", "url": "https://authors.library.caltech.edu/records/9stj0-49896/files/aa25818-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/dbvx7-g5555", "eprint_id": 74520, "eprint_status": "archive", "datestamp": "2023-08-20 14:05:51", "lastmod": "2023-10-24 22:43:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. VIII. High Frequency Instrument data processing: Calibration and maps", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations / cosmic background radiation / surveys / methods: data analysis", "note": "\u00a9 2016 ESO. \n\nReceived: 5 February 2015; Accepted: 10 September 2015; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration\n\nPublished - aa25820-15.pdf
Submitted - 1502.01587.pdf
", "abstract": "This paper describes the processing applied to the cleaned, time-ordered information obtained from the Planck High Frequency Instrument (HFI) with the aim of producing photometrically calibrated maps in temperature and (for the first time) in polarization. The data from the entire 2.5-year HFI mission include almost five full-sky surveys. HFI observes the sky over a broad range of frequencies, from 100 to 857\u2009GHz. To obtain the best accuracy on the calibration over such a large range, two different photometric calibration schemes have been used. The 545 and 857\u2009GHz data are calibrated using models of planetary atmospheric emission. The lower frequencies (from 100 to 353\u2009GHz) are calibrated using the time-variable cosmological microwave background dipole, which we call the orbital dipole. This source of calibration only depends on the satellite velocity with respect to the solar system. Using a CMB temperature of T_(CMB) = 2.7255 \u00b1 0.0006 K, it permits an independent measurement of the amplitude of the CMB solar dipole (3364.3 \u00b1 1.5 \u03bcK), which is approximatively 1\u03c3 higher than the WMAP measurement with a direction that is consistent between the two experiments. We describe the pipeline used to produce the maps ofintensity and linear polarization from the HFI timelines, and the scheme used to set the zero level of the maps a posteriori. We also summarize the noise characteristics of the HFI maps in the 2015 Planck data release and present some null tests to assess their quality. Finally, we discuss the major systematic effects and in particular the leakage induced by flux mismatch between the detectors that leads to spurious polarization signal.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A8", "id_number": "CaltechAUTHORS:20170224-082939025", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170224-082939025", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525820", "primary_object": { "basename": "1502.01587.pdf", "url": "https://authors.library.caltech.edu/records/dbvx7-g5555/files/1502.01587.pdf" }, "related_objects": [ { "basename": "aa25820-15.pdf", "url": "https://authors.library.caltech.edu/records/dbvx7-g5555/files/aa25820-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/3pama-rd204", "eprint_id": 60302, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:22", "lastmod": "2023-10-24 16:24:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Adam-R", "name": { "family": "Adam", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. X. Diffuse component separation: Foreground maps", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general / cosmology: observations / polarization / cosmic background radiation / diffuse radiation / Galaxy: general", "note": "\u00a9 2016 ESO. \n\nReceived: 26 February 2015; Accepted: 22 February 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration\n\nPublished - aa25967-15.pdf
Submitted - 1502.01588v2.pdf
", "abstract": "Planck has mapped the microwave sky in temperature over nine frequency bands between 30 and 857\u2009GHz and in polarization over seven frequency bands between 30 and 353\u2009GHz in polarization. In this paper we consider the problem of diffuse astrophysical component separation, and process these maps within a Bayesian framework to derive an internally consistent set of full-sky astrophysical component maps. Component separation dedicated to cosmic microwave background (CMB) reconstruction is described in a companion paper. For the temperature analysis, we combine the Planck observations with the 9-yr Wilkinson Microwave Anisotropy Probe (WMAP) sky maps and the Haslam et al. 408\u2009MHz map, to derive a joint model of CMB, synchrotron, free-free, spinning dust, CO, line emission in the 94 and 100\u2009GHz channels, and thermal dust emission. Full-sky maps are provided for each component, with an angular resolution varying between 7.\u03015 and 1deg. Global parameters (monopoles, dipoles, relative calibration, and bandpass errors) are fitted jointly with the sky model, and best-fit values are tabulated. For polarization, the model includes CMB, synchrotron, and thermal dust emission. These models provide excellent fits to the observed data, with rms temperature residuals smaller than 4\u03bcK over 93% of the sky for all Planck frequencies up to 353\u2009GHz, and fractional errors smaller than 1% in the remaining 7% of the sky. The main limitations of the temperature model at the lower frequencies are internal degeneracies among the spinning dust, free-free, and synchrotron components; additional observations from external low-frequency experiments will be essential to break these degeneracies. The main limitations of the temperature model at the higher frequencies are uncertainties in the 545 and 857\u2009GHz calibration and zero-points. For polarization, the main outstanding issues are instrumental systematics in the 100\u2013353\u2009GHz bands on large angular scales in the form of temperature-to-polarization leakage, uncertainties in the analogue-to-digital conversion, and corrections for the very long time constant of the bolometer detectors, all of which are expected to improve in the near future.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A10", "id_number": "CaltechAUTHORS:20150917-134706855", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-134706855", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525967", "primary_object": { "basename": "1502.01588v2.pdf", "url": "https://authors.library.caltech.edu/records/3pama-rd204/files/1502.01588v2.pdf" }, "related_objects": [ { "basename": "aa25967-15.pdf", "url": "https://authors.library.caltech.edu/records/3pama-rd204/files/aa25967-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Adam, R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/gdt8x-q8b76", "eprint_id": 60321, "eprint_status": "archive", "datestamp": "2023-08-20 13:58:12", "lastmod": "2023-10-24 16:25:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "id": "Pearson-Timothy-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XI. CMB power spectra, likelihoods, and robustness of parameters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / cosmological parameters / cosmology: observations / methods: data analysis / methods: statistical", "note": "\u00a9 2016 ESO. \n\nReceived: 9 July 2015; Accepted: 18 May 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. \n\nWe further acknowledge the use of the CLASS Boltzmann code (Lesgourgues 2011) and the Monte Python package (Audren et al. 2013) in earlier stages of this work. The likelihood code and some of the validation work was built on the library pmclib from the CosmoPMC package (Kilbinger et al. 2011). \n\nThis research used resources of the IN2P3 Computer Center (http://cc.in2p3.fr) as well as of the Planck-HFI DPC infrastructure hosted at the Institut d'Astrophysique de Paris (France) and financially supported by CNES.\n\nPublished - aa26926-15.pdf
Submitted - 1507.02704v1.pdf
", "abstract": "This paper presents the Planck 2015 likelihoods, statistical descriptions of the 2-point correlationfunctions of the cosmic microwave background (CMB) temperature and polarization fluctuations that account for relevant uncertainties, both instrumental and astrophysical in nature. They are based on the same hybrid approach used for the previous release, i.e., a pixel-based likelihood at low multipoles (\u2113< 30) and a Gaussian approximation to the distribution of cross-power spectra at higher multipoles. The main improvements are the use of more and better processed data and of Planck polarization information, along with more detailed models of foregrounds and instrumental uncertainties. The increased redundancy brought by more than doubling the amount of data analysed enables further consistency checks and enhanced immunity to systematic effects. It also improves the constraining power of Planck, in particular with regard to small-scale foreground properties. Progress in the modelling of foreground emission enables the retention of a larger fraction of the sky to determine the properties of the CMB, which also contributes to the enhanced precision of the spectra. Improvements in data processing and instrumental modelling further reduce uncertainties. Extensive tests establish the robustness and accuracy of the likelihood results, from temperature alone, from polarization alone, and from their combination. For temperature, we also perform a full likelihood analysis of realistic end-to-end simulations of the instrumental response to the sky, which were fed into the actual data processing pipeline; this does not reveal biases from residual low-level instrumental systematics. Even with the increase in precision and robustness, the \u039bCDM cosmological model continues to offer a very good fit to the Planck data. The slope of the primordial scalar fluctuations, n_s, is confirmed smaller than unity at more than 5\u03c3 from Planck alone. We further validate the robustness of the likelihood results against specific extensions to the baseline cosmology, which are particularly sensitive to data at high multipoles. For instance, the effective number of neutrino species remains compatible with the canonical value of 3.046. For this first detailed analysis of Planck polarization spectra, we concentrate at high multipoles on the E modes, leaving the analysis of the weaker B modes to future work. At low multipoles we use temperature maps at all Planck frequencies along with a subset of polarization data. These data take advantage of Planck's wide frequency coverage to improve the separation of CMB and foreground emission. Within the baseline \u039bCDM cosmology this requires \u03c4 = 0.078 \u00b1 0.019 for the reionization optical depth, which is significantly lower than estimates without the use of high-frequency data for explicit monitoring of dust emission. At high multipoles we detect residual systematic errors in E polarization, typically at the \u03bcK^2 level; we therefore choose to retain temperature information alone for high multipoles as the recommended baseline, in particular for testing non-minimal models. Nevertheless, the high-multipole polarization spectra from Planck are already good enough to enable a separate high-precision determination of the parameters of the \u039bCDM model, showing consistency with those established independently from temperature information alone.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A11", "id_number": "CaltechAUTHORS:20150918-110504749", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-110504749", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526926", "primary_object": { "basename": "1507.02704v1.pdf", "url": "https://authors.library.caltech.edu/records/gdt8x-q8b76/files/1507.02704v1.pdf" }, "related_objects": [ { "basename": "aa26926-15.pdf", "url": "https://authors.library.caltech.edu/records/gdt8x-q8b76/files/aa26926-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Aghanim, N.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/x1rn2-33y63", "eprint_id": 60313, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:30", "lastmod": "2023-10-24 16:25:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIII. Cosmological parameters", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations / cosmology: theory / cosmic background radiation / cosmological parameters", "note": "\u00a9 2016 ESO. \n\nReceived: 6 February 2015; Accepted: 4 June 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007\u22122013)/ERC Grant Agreement No. [616170] and from the UK Science and Technology Facilities Council [grant number ST/L000652/1]. Part of this work was undertaken on the STFC DiRAC HPC Facilities at the University of Cambridge, funded by UK BIS National E-infrastructure capital grants, and on the Andromeda cluster of the University of Geneva. A large set of cosmological parameter constraints from different data combinations, and including many separate extensions to the 6-parameter base \u039bCDM model, are available at http://pla.esac.esa.int/pla/#cosmology.\n\nPublished - aa25830-15.pdf
Submitted - 1502.01589v2.pdf
", "abstract": "This paper presents cosmological results based on full-mission Planck observations of temperature and polarization anisotropies of the cosmic microwave background (CMB) radiation. Our results are in very good agreement with the 2013 analysis of the Planck nominal-mission temperature data, but with increased precision. The temperature and polarization power spectra are consistent with the standard spatially-flat 6-parameter \u039bCDM cosmology with a power-law spectrum of adiabatic scalar perturbations (denoted \"base \u039bCDM\" in this paper). From the Planck temperature data combined with Planck lensing, for this cosmology we find a Hubble constant, H_0 = (67.8 \u00b1 0.9) km s^(-1)Mpc^(-1), a matter density parameter \u03a9_m = 0.308 \u00b1 0.012, and a tilted scalar spectral index with n_s = 0.968 \u00b1 0.006, consistent with the 2013 analysis. Note that in this abstract we quote 68% confidence limits on measured parameters and 95% upper limits on other parameters. We present the first results of polarization measurements with the Low Frequency Instrument at large angular scales. Combined with the Planck temperature and lensing data, these measurements give a reionization optical depth of \u03c4 = 0.066 \u00b1 0.016, corresponding to a reionization redshift of Z_(re) = 8.8^(+1.7)_(-1.4). These results are consistent with those from WMAP polarization measurements cleaned for dust emission using 353-GHz polarization maps from the High Frequency Instrument. We find no evidence for any departure from base \u039bCDM in the neutrino sector of the theory; for example, combining Planck observations with other astrophysical data we find N_(eff) = 3.15 \u00b1 0.23 for the effective number of relativistic degrees of freedom, consistent with the value N_(eff) = 3.046 of the Standard Model of particle physics. The sum of neutrino masses is constrained to \u2211 m_\u03bd < 0.23 eV. The spatial curvature of our Universe is found to be very close to zero, with | \u03a9_K | < 0.005. Adding a tensor component as a single-parameter extension to base \u039bCDM we find an upper limit on the tensor-to-scalar ratio of r_(0.002)< 0.11, consistent with the Planck 2013 results and consistent with the B-mode polarization constraints from a joint analysis of BICEP2, Keck Array, and Planck (BKP) data. Adding the BKP B-mode data to our analysis leads to a tighter constraint of r_(0.002) < 0.09 and disfavours inflationarymodels with a V(\u03c6) \u221d \u03c6^2 potential. The addition of Planck polarization data leads to strong constraints on deviations from a purely adiabatic spectrum of fluctuations. We find no evidence for any contribution from isocurvature perturbations or from cosmic defects. Combining Planck data with other astrophysical data, including Type Ia supernovae, the equation of state of dark energy is constrained to w = \u22121.006 \u00b1 0.045, consistent with the expected value for a cosmological constant. The standard big bang nucleosynthesis predictions for the helium and deuterium abundances for the best-fit Planck base \u039bCDM cosmology are in excellent agreement with observations. We also constraints on annihilating dark matter and on possible deviations from the standard recombination history. In neither case do we find no evidence for new physics. The Planck results for base \u039bCDM are in good agreement with baryon acoustic oscillation data and with the JLA sample of Type Ia supernovae. However, as in the 2013 analysis, the amplitude of the fluctuation spectrum is found to be higher than inferred from some analyses of rich cluster counts and weak gravitational lensing. We show that these tensions cannot easily be resolved with simple modifications of the base \u039bCDM cosmology. Apart from these tensions, the base \u039bCDM cosmology provides an excellent description of the Planck CMB observations and many other astrophysical data sets.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A13", "id_number": "CaltechAUTHORS:20150918-070918069", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-070918069", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "616170" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000652/1" }, { "agency": "UK BIS National E-Infrastructure" }, { "agency": "University of Geneva" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525830", "primary_object": { "basename": "1502.01589v2.pdf", "url": "https://authors.library.caltech.edu/records/x1rn2-33y63/files/1502.01589v2.pdf" }, "related_objects": [ { "basename": "aa25830-15.pdf", "url": "https://authors.library.caltech.edu/records/x1rn2-33y63/files/aa25830-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/f8gw3-6cm87", "eprint_id": 60314, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:36", "lastmod": "2023-10-24 16:25:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIV. Dark energy and modified gravity", "ispublished": "pub", "full_text_status": "public", "keywords": "dark energy / cosmic background radiation / cosmology: theory / gravitation", "note": "\u00a9 2016 ESO. \n\nReceived 5 February 2015; Accepted 19 February 2016; Published online 20 September 2016. \n\nIt is a pleasure to thank Luca Amendola, Emilio Bellini, Diego Blas, Sarah Bridle, Noemi Frusciante, Catherine Heymans, Alireza Hojjati, Bin Hu, Thomas Kitching, Niall MacCrann, Marco Raveri, Ignacy Sawicki, Alessandra Silvestri, Fergus Simpson, Christof Wetterich and Gongbo Zhao for interesting discussions on theories, external data sets and numerical codes. Part of the analysis for this paper was run on the Andromeda and Perseus clusters of the University of Geneva and on WestGrid computers in Canada. We deeply thank Andreas Malaspinas for invaluable help with the Andromeda and Perseus Clusters. This research was partly funded by the DFG TransRegio TRR33 grant on \"The Dark Universe\" and by the Swiss NSF. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration.\n\nPublished - aa25814-15.pdf
Submitted - 1502.01590v1.pdf
", "abstract": "We study the implications of Planck data for models of dark energy (DE) and modified gravity (MG) beyond the standard cosmological constant scenario. We start with cases where the DE only directly affects the background evolution, considering Taylor expansions of the equation of state w(a), as well as principal component analysis and parameterizations related to the potential of a minimally coupled DE scalar field. When estimating the density of DE at early times, we significantly improve present constraints and find that it has to be below ~2% (at 95% confidence) of the critical density, even when forced to play a role for z < 50 only. We then move to general parameterizations of the DE or MG perturbations that encompass both effective field theories and the phenomenology of gravitational potentials in MG models. Lastly, we test a range of specific models, such as k-essence, f(R) theories, and coupled DE. In addition to the latest Planck data, for our main analyses, we use background constraints from baryonic acoustic oscillations, type-Ia supernovae, and local measurements of the Hubble constant. We further show the impact of measurements of the cosmological perturbations, such as redshift-space distortions and weak gravitational lensing. These additional probes are important tools for testing MG models and for breaking degeneracies that are still present in the combination of Planck and background data sets. All results that include only background parameterizations (expansion of the equation of state, early DE, general potentials in minimally-coupled scalar fields or principal component analysis) are in agreement with \u039bCDM. When testing models that also change perturbations (even when the background is fixed to \u039bCDM), some tensions appear in a few scenarios: the maximum one found is ~2\u03c3 for Planck TT+lowP when parameterizing observables related to the gravitational potentials with a chosen time dependence; the tension increases to, at most, 3\u03c3 when external data sets are included. It however disappears when including CMB lensing.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A14", "id_number": "CaltechAUTHORS:20150918-080156740", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-080156740", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "TRR33" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525814", "primary_object": { "basename": "1502.01590v1.pdf", "url": "https://authors.library.caltech.edu/records/f8gw3-6cm87/files/1502.01590v1.pdf" }, "related_objects": [ { "basename": "aa25814-15.pdf", "url": "https://authors.library.caltech.edu/records/f8gw3-6cm87/files/aa25814-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/sqgt0-nz529", "eprint_id": 60286, "eprint_status": "archive", "datestamp": "2023-08-20 13:56:58", "lastmod": "2023-10-24 16:23:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XIX. Constraints on primordial magnetic fields", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 ESO. \n\nReceived: 5 February 2015; Accepted: 19 February 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa25821-15.pdf
Submitted - 1502.01594v1.pdf
", "abstract": "We compute and investigate four types of imprint of a stochastic background of primordial magnetic fields (PMFs) on the cosmic microwave background (CMB) anisotropies: the impact of PMFs on the CMB temperature and polarization spectra, which is related to their contribution to cosmological perturbations; the effect on CMB polarization induced by Faraday rotation; the impact of PMFs on the ionization history; magnetically-induced non-Gaussianities and related non-zero bispectra; and the magnetically-induced breaking of statistical isotropy. We present constraints on the amplitude of PMFs that are derived from different Planck data products, depending on the specific effect that is being analysed. Overall, Planck data constrain the amplitude of PMFs to less than a few nanoGauss, with different bounds that depend on the considered model. In particular, individual limits coming from the analysis of the CMB angular power spectra, using the Planck likelihood, are B_(1 Mpc) < 4.4 nG (where B_(1 Mpc) is the comoving field amplitude at a scale of 1\u2009Mpc) at 95% confidence level, assuming zero helicity. By considering the Planck likelihood, based only on parity-even angular power spectra, we obtain B_(1 Mpc) < 5.6 nG for a maximally helical field. For nearly scale-invariant PMFs we obtain B_(1 Mpc) < 2.0\u2009nG and B_(1 Mpc) < 0.9\u2009nG if the impact of PMFs on the ionization history of the Universe is included in the analysis. From the analysis of magnetically-induced non-Gaussianity, we obtain three different values, corresponding to three applied methods, all below 5\u2009nG. The constraint from the magnetically-induced passive-tensor bispectrum is B_(1 Mpc) < 2.8\u2009nG. A search for preferred directions in the magnetically-induced passive bispectrum yields B_(1 Mpc) < 4.5\u2009nG, whereas the compensated-scalar bispectrum gives B_(1 Mpc) < 3\u2009nG. The analysis of the Faraday rotation of CMB polarization by PMFs uses the Planck power spectra in EE and BB at 70\u2009GHz and gives B_(1 Mpc) < 1380\u2009nG. In our final analysis, we consider the harmonic-space correlations produced by Alfv\u00e9n waves, finding no significant evidence for the presence of these waves. Together, these results comprise a comprehensive set of constraints on possible PMFs with Planck data.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A19", "id_number": "CaltechAUTHORS:20150916-145551601", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-145551601", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525821", "primary_object": { "basename": "1502.01594v1.pdf", "url": "https://authors.library.caltech.edu/records/sqgt0-nz529/files/1502.01594v1.pdf" }, "related_objects": [ { "basename": "aa25821-15.pdf", "url": "https://authors.library.caltech.edu/records/sqgt0-nz529/files/aa25821-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/eyhw3-dfk52", "eprint_id": 60315, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:44", "lastmod": "2023-10-24 16:25:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XVII. Constraints on primordial non-Gaussianity", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / cosmology: observations / cosmology: theory / early Universe / inflation / methods: data analysis", "note": "\u00a9 2016 ESO. \n\nReceived: 6 February 2015; Accepted: 27 January 2016;\nPublished online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. Part of this work was undertaken on the STFC COSMOS@DiRAC HPC Facility at the University of Cambridge, funded by UK BIS NEI grants. We gratefully acknowledge IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for the analysis with the binned bispectrum estimator. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We also acknowledge the IAP magique3 computer facilities. Some computations were performed on the GPC cluster at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada, the Government of Ontario, and the University of Toronto.\n\nPublished - aa25836-15.pdf
Submitted - 1502.01592v1.pdf
", "abstract": "The Planck full mission cosmic microwave background (CMB) temperature and E-mode polarization maps are analysed to obtain constraints on primordial non-Gaussianity (NG). Using three classes of optimal bispectrum estimators \u2013 separable template-fitting (KSW), binned, and modal \u2013 we obtain consistent values for the primordial local, equilateral, and orthogonal bispectrum amplitudes, quoting as our final result from temperature alone \u0192^(local)_(NL) = 2.5 \u00b1 5.7, \u0192^(equil)_(NL)= -16 \u00b1 70, , and \u0192^(ortho)_(NL) = -34 \u00b1 32 (68% CL, statistical). Combining temperature and polarization data we obtain \u0192^(local)_(NL) = 0.8 \u00b1 5.0, \u0192^(equil)_(NL)= -4 \u00b1 43, and \u0192^(ortho)_(NL) = -26 \u00b1 21 (68% CL, statistical). The results are based on comprehensive cross-validation of these estimators on Gaussian and non-Gaussian simulations, are stable across component separation techniques, pass an extensive suite of tests, and are consistent with estimators based on measuring the Minkowski functionals of the CMB. The effect of time-domain de-glitching systematics on the bispectrum is negligible. In spite of these test outcomes we conservatively label the results including polarization data as preliminary, owing to a known mismatch of the noise model in simulations and the data. Beyond estimates of individual shape amplitudes, we present model-independent, three-dimensional reconstructions of the Planck CMB bispectrum and derive constraints on early universe scenarios that generate primordial NG, including general single-field models of inflation, axion inflation, initial state modifications, models producing parity-violating tensor bispectra, and directionally dependent vector models. We present a wide survey of scale-dependent feature and resonance models, accounting for the \"look elsewhere\" effect in estimating the statistical significance of features. We also look for isocurvature NG, and find no signal, but we obtain constraints that improve significantly with the inclusion of polarization. The primordial trispectrum amplitude in the local model is constrained to be g^(local)_(NL) = (\u22129.0\u00b17.7)\u00d710^4 (68% CL statistical), and we perform an analysis of trispectrum shapes beyond the local case. The global picture that emerges is one of consistency with the premises of the \u039bCDM cosmology, namely that the structure we observe today was sourced by adiabatic, passive, Gaussian, and primordial seed perturbations.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A17", "id_number": "CaltechAUTHORS:20150918-082428843", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-082428843", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "UK BIS NEI Grants" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Compute Canada" }, { "agency": "Government of Ontario" }, { "agency": "University of Toronto" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525836", "primary_object": { "basename": "aa25836-15.pdf", "url": "https://authors.library.caltech.edu/records/eyhw3-dfk52/files/aa25836-15.pdf" }, "related_objects": [ { "basename": "1502.01592v1.pdf", "url": "https://authors.library.caltech.edu/records/eyhw3-dfk52/files/1502.01592v1.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/xrdg8-83809", "eprint_id": 74467, "eprint_status": "archive", "datestamp": "2023-08-20 14:05:35", "lastmod": "2023-10-24 22:40:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XX. Constraints on inflation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation / cosmology: theory / early Universe / inflation", "note": "\u00a9 2016 ESO. \n\nReceived: 14 February 2015; Accepted: 3 March 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. Part of this work was undertaken at the STFC DiRAC HPC Facilities at the University of Cambridge, funded by UK BIS National E-infrastructure capital grants. We gratefully acknowledge the IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for this work.\n\nPublished - aa25898-15.pdf
Submitted - 1502.02114.pdf
", "abstract": "We present the implications for cosmic inflation of the Planck measurements of the cosmic microwave background (CMB) anisotropies in both temperature and polarization based on the full Planck survey, which includes more than twice the integration time of the nominal survey used for the 2013 release papers. The Planck full mission temperature data and a first release of polarization data on large angular scales measure the spectral index of curvature perturbations to be ns = 0.968 \u00b1 0.006 and tightly constrain its scale dependence to dns/ dlnk = \u22120.003 \u00b1 0.007 when combined with the Planck lensing likelihood. When the Planck high-\u2113 polarization data are included, the results are consistent and uncertainties are further reduced. The upper bound on the tensor-to-scalar ratio is r_(0.002)< 0.11 (95% CL). This upper limit is consistent with the B-mode polarization constraint r< 0.12 (95% CL) obtained from a joint analysis of the BICEP2/Keck Array and Planck data. These results imply that V(\u03c6) \u221d \u03c6^2 and natural inflation are now disfavoured compared to models predicting a smaller tensor-to-scalar ratio, such as R^2 inflation. We search for several physically motivated deviations from a simple power-law spectrum of curvature perturbations, including those motivated by a reconstruction of the inflaton potential not relying on the slow-roll approximation. We find that such models are not preferred, either according to a Bayesian model comparison or according to a frequentist simulation-based analysis. Three independent methods reconstructing the primordial power spectrum consistently recover a featureless and smooth P_R(k) over the range of scales 0.008 Mpc^(-1) \u2272 k \u2272 0.1 Mpc^(-1). At large scales, each method finds deviations from a power law, connected to a deficit at multipoles \u2113 \u2248 20\u221240 in the temperature power spectrum, but at an uncompelling statistical significance owing to the large cosmic variance present at these multipoles. By combining power spectrum and non-Gaussianity bounds, we constrain models with generalized Lagrangians, including Galileon models and axion monodromy models. The Planck data are consistent with adiabatic primordial perturbations, and the estimated values for the parameters of the base \u039b cold dark matter (\u039bCDM) model are not significantly altered when more general initial conditions are admitted. In correlated mixed adiabatic and isocurvature models, the 95% CL upper bound for the non-adiabatic contribution to the observed CMB temperature variance is | \u03b1_(non \u2013 adi) | < 1.9%, 4.0%, and 2.9% for CDM, neutrino density, and neutrino velocity isocurvature modes, respectively. We have tested inflationary models producing an anisotropic modulation of the primordial curvature power spectrum findingthat the dipolar modulation in the CMB temperature field induced by a CDM isocurvature perturbation is not preferred at a statistically significant level. We also establish tight constraints on a possible quadrupolar modulation of the curvature perturbation. These results are consistent with the Planck 2013 analysis based on the nominal mission data and further constrain slow-roll single-field inflationary models, as expected from the increased precision of Planck data using the full set of observations.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A20", "id_number": "CaltechAUTHORS:20170222-105731785", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170222-105731785", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "UK BIS National E-Infrastructure" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525898", "primary_object": { "basename": "aa25898-15.pdf", "url": "https://authors.library.caltech.edu/records/xrdg8-83809/files/aa25898-15.pdf" }, "related_objects": [ { "basename": "1502.02114.pdf", "url": "https://authors.library.caltech.edu/records/xrdg8-83809/files/1502.02114.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/08mjd-84k07", "eprint_id": 96866, "eprint_status": "archive", "datestamp": "2023-08-20 14:07:24", "lastmod": "2023-10-20 21:34:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" } ] }, "title": "Planck 2015 results. XXIII. The thermal Sunyaev-Zeldovich effect-cosmic infrared background correlation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: general \u2013 infrared: galaxies \u2013 large-scale structure of Universe \u2013 methods: data analysis", "note": "\u00a9 2016 ESO. Article published by EDP Sciences.\n\nReceived 22 September 2015; Accepted 23 April 2016; Published online 20 September 2016.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. Some of the results in this paper have been derived using the HEALPix package. We also acknowledge the support of the French Agence Nationale de la Recherche under grant ANR-11-BD56-015.\n\nPublished - aa27418-15.pdf
Submitted - 1509.06555.pdf
", "abstract": "We use Planck data to detect the cross-correlation between the thermal Sunyaev-Zeldovich (tSZ) effect and the infrared emission from the galaxies that make up the the cosmic infrared background (CIB). We first perform a stacking analysis towards Planck-confirmed galaxy clusters. We detect infrared emission produced by dusty galaxies inside these clusters and demonstrate that the infrared emission is about 50% more extended than the tSZ effect. Modelling the emission with a Navarro-Frenk-White profile, we find that the radial profile concentration parameter is c_(500) = 1.00^(+0.18)_(-0.15). This indicates that infrared galaxies in the outskirts of clusters have higher infrared flux than cluster-core galaxies. We also study the cross-correlation between tSZ and CIB anisotropies, following three alternative approaches based on power spectrum analyses: (i) using a catalogue of confirmed clusters detected in Planck data; (ii) using an all-sky tSZ map built from Planck frequency maps; and (iii) using cross-spectra between Planckfrequency maps. With the three different methods, we detect the tSZ-CIB cross-power spectrum at significance levels of (i) 6\u03c3; (ii) 3\u03c3; and (iii) 4\u03c3. We model the tSZ-CIB cross-correlation signature and compare predictions with the measurements. The amplitude of the cross-correlation relative to the fiducial model is A_(tSZ\u2212CIB) = 1.2 \u00b1 0.3. This result is consistent with predictions for the tSZ-CIB cross-correlation assuming the best-fit cosmological model from Planck 2015 results along with the tSZ and CIB scaling relations.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A23", "id_number": "CaltechAUTHORS:20190701-132745145", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-132745145", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "Agence Nationale pour la Recherche (ANR)", "grant_number": "ANR-11-BD56-015" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201527418", "primary_object": { "basename": "1509.06555.pdf", "url": "https://authors.library.caltech.edu/records/08mjd-84k07/files/1509.06555.pdf" }, "related_objects": [ { "basename": "aa27418-15.pdf", "url": "https://authors.library.caltech.edu/records/08mjd-84k07/files/aa27418-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/2mwb8-crd22", "eprint_id": 60318, "eprint_status": "archive", "datestamp": "2023-08-20 13:57:55", "lastmod": "2023-10-24 16:25:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds", "ispublished": "pub", "full_text_status": "public", "keywords": "diffuse radiation / ISM: general / radiation mechanisms: general / radio continuum: ISM / polarization / local insterstellar matter", "note": "\u00a9 2016 ESO. \n\nReceived: 22 June 2015; Accepted: 20 April 2016; Published online 20 September 2016. \n\nThis paper is dedicated to the memory of the late Professor Rodney Deane Davies CBE FRS and Professor Richard John Davis OBE, both of whom contributed greatly to the Planck project. The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. This research was supported by an ERC Starting (Consolidator) Grant (no. 307209) and STFC Consolidated Grant (no. ST/L000768/1). We have made extensive use of the HEALPix package and the IDL astronomy library. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.\n\nPublished - aa26803-15.pdf
Submitted - 1506.06660v1.pdf
", "abstract": "We discuss the Galactic foreground emission between 20 and 100\u2009GHz based on observations by Planck and WMAP. The total intensity in this part of the spectrum is dominated by free-free and spinning dust emission, whereas the polarized intensity is dominated by synchrotron emission. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. Comparison with radio recombination line templates verifies the recovery of the free-free emission along the Galactic plane. Comparison of the high-latitude H\u03b1 emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (\u224830%) of H\u03b1 having been scattered by high-latitude dust. We highlight a number of diffuse spinning dust morphological features at high latitude. There is substantial spatial variation in the spinning dust spectrum, with the emission peak (in I_\u03bd) ranging from below 20\u2009GHz to more than 50\u2009GHz. There is a strong tendency for the spinning dust component near many prominent H\u2009II regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photo-dissociation regions around the nebulae. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. This can be explained by the difficulty in separating multiple broadband components with a limited number of frequency maps. Future surveys, particularly at 5\u201320\u2009GHz, will greatly improve the separation by constraining the synchrotron spectrum. We combine Planck and WMAP data to make the highest signal-to-noise ratio maps yet of the intensity of the all-sky polarized synchrotron emission at frequencies above a few GHz. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure. We argue that nearly all the emission at 40deg > l > \u221290deg is part of the Loop I structure, and show that the emission extends much further in to the southern Galactic hemisphere than previously recognised, giving Loop I an ovoid rather than circular outline. However, it does not continue as far as the \"Fermi bubble/microwave haze\", making it less probable that these are part of the same structure. We identify a number of new faint features in the polarized sky, including a dearth of polarized synchrotron emission directly correlated with a narrow, roughly 20deg long filament seen in H\u03b1 at high Galactic latitude. Finally, we look for evidence of polarized AME, however many AME regions are significantly contaminated by polarized synchrotron emission, and we find a 2\u03c3 upper limit of 1.6% in the Perseus region.", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A25", "id_number": "CaltechAUTHORS:20150918-100209126", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-100209126", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft (MPG)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "307209" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000768/1" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526803", "primary_object": { "basename": "1506.06660v1.pdf", "url": "https://authors.library.caltech.edu/records/2mwb8-crd22/files/1506.06660v1.pdf" }, "related_objects": [ { "basename": "aa26803-15.pdf", "url": "https://authors.library.caltech.edu/records/2mwb8-crd22/files/aa26803-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/f0qyk-mnn69", "eprint_id": 60320, "eprint_status": "archive", "datestamp": "2023-08-20 13:58:03", "lastmod": "2023-10-24 16:25:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C." }, "orcid": "0000-0002-5627-5471" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" } ] }, "title": "Planck 2015 results. XXVI. The Second Planck Catalogue of Compact Sources", "ispublished": "pub", "full_text_status": "public", "keywords": "catalogs / cosmology: observations / radio continuum: general / submillimeter: general", "note": "\u00a9 2016 ESO. \n\nReceived: 8 July 2015; Accepted: 28 January 2016; Published online 20 September 2016. \n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and, RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. We are grateful to the H-ATLAS Executive Committee and primarily to the PIs, S. Eales and L. Dunne, for permission to use the unpublished H-ATLAS catalogue for the validation of the present catalogue. This research has made use of the \"Aladin sky atlas\" (Bonnarel et al. 2000), developed at CDS, Strasbourg Observatory, France. Part of this work was performed using the Darwin Supercomputer of the University of Cambridge High Performance Computing Service (http://www.hpc.cam.ac.uk/), provided by Dell Inc. using Strategic Research Infrastructure Funding from the HEFCE and funding from the STFC. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - aa26914-15.pdf
Submitted - 1507.02058v1.pdf
", "abstract": "The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogues, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalogue. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow us to increase the number of objects in the catalogue, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC).", "date": "2016-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "594", "publisher": "EDP Sciences", "pagerange": "Art. No. A26", "id_number": "CaltechAUTHORS:20150918-104502219", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-104502219", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Finnish Funding Agency for Technology and Innovation (Tekes)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education, Research and Innovation (SER)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "European Research Council (ERC)" }, { "agency": "PRACE (EU)" }, { "agency": "Higher Education Funding Council for England (HEFCE)" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "COSMOS" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201526914", "primary_object": { "basename": "aa26914-15.pdf", "url": "https://authors.library.caltech.edu/records/f0qyk-mnn69/files/aa26914-15.pdf" }, "related_objects": [ { "basename": "1507.02058v1.pdf", "url": "https://authors.library.caltech.edu/records/f0qyk-mnn69/files/1507.02058v1.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Beichman, C.; et el." }, { "id": "https://authors.library.caltech.edu/records/7dfcc-20n50", "eprint_id": 62378, "eprint_status": "archive", "datestamp": "2023-08-20 13:02:42", "lastmod": "2023-10-25 17:06:37", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hunacek-J-R", "name": { "family": "Hunacek", "given": "J. R." }, "orcid": "0000-0001-7066-226X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Bumble-B", "name": { "family": "Bumble", "given": "B." } }, { "id": "Chang-Tzu-Ching", "name": { "family": "Chang", "given": "T.-C." } }, { "id": "Cheng-Yun-Ting", "name": { "family": "Cheng", "given": "Y.-T." }, "orcid": "0000-0002-5437-0504" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Crites-A-T", "name": { "family": "Crites", "given": "A." } }, { "id": "Hailey-Dunsheath-S", "name": { "family": "Hailey-Dunsheath", "given": "S." }, "orcid": "0000-0002-8504-7988" }, { "id": "Gong-Y", "name": { "family": "Gong", "given": "Y." } }, { "id": "Kenyon-M", "name": { "family": "Kenyon", "given": "M." } }, { "id": "Koch-P-M", "name": { "family": "Koch", "given": "P." }, "orcid": "0000-0003-2777-5861" }, { "id": "Li-Cheuk-Ting", "name": { "family": "Li", "given": "C.-T." } }, { "id": "O'Brient-R-C", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Shirokoff-E", "name": { "family": "Shirokoff", "given": "E." } }, { "id": "Shiu-Corwin", "name": { "family": "Shiu", "given": "C." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z." } }, { "id": "Uzgil-B-D", "name": { "family": "Uzgil", "given": "B." }, "orcid": "0000-0001-8526-3464" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Design and Fabrication of TES Detector Modules for the TIME-Pilot [CII] Intensity Mapping Experiment", "ispublished": "pub", "full_text_status": "restricted", "keywords": "Reionization, Intensity mapping, Bolometers, Transition edge sensors", "note": "\u00a9 2015 Springer. \n\nReceived: 13 September 2015 / Accepted: 30 October 2015. \n\nThis material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144469.", "abstract": "We are developing a series of close-packed modular detector arrays for TIME-Pilot, a new mm-wavelength grating spectrometer array that will map the intensity fluctuations of the redshifted 157.7 \u03bcm emission line of singly ionized carbon ([CII]) from redshift z\u223c5 to 9. TIME-Pilot's two banks of 16 parallel-plate waveguide spectrometers (one bank per polarization) will have a spectral range of 183\u2013326 GHz and a resolving power of R\u223c100. The spectrometers use a curved diffraction grating to disperse and focus the light on a series of output arcs, each sampled by 60 transition edge sensor (TES) bolometers with gold micro-mesh absorbers. These low-noise detectors will be operated from a 250 mK base temperature and are designed to have a background-limited NEP of \u223c10^(\u221217) W/Hz^(1/2). This proceeding presents an overview of the detector design in the context of the TIME-Pilot instrument. Additionally, a prototype detector module produced at the Microdevices Laboratory at JPL is shown.", "date": "2016-08", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "184", "number": "3", "publisher": "Springer", "pagerange": "733-738", "id_number": "CaltechAUTHORS:20151124-115155769", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151124-115155769", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF Graduate Research Fellowship", "grant_number": "DGE-1144469" } ] }, "doi": "10.1007/s10909-015-1359-x", "resource_type": "article", "pub_year": "2016", "author_list": "Hunacek, J. R.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/dfx00-xft81", "eprint_id": 69300, "eprint_status": "archive", "datestamp": "2023-08-20 13:05:15", "lastmod": "2023-10-20 16:46:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wu-W-L-K", "name": { "family": "Wu", "given": "W. L. K." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "O'Brient-R", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "Initial Performance of BICEP3: A Degree Angular Scale 95 GHz Band Polarimeter", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 The Author(s). This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made. \n\nReceived: 29 September 2015; Accepted: 30 November 2015; Published online: 29 December 2015. \n\nThis work is supported by the National Science Foundation (Grant Nos. 1313158, 1313010, 1313062, 1313287, 1056465, 0960243), the SLAC Laboratory Directed Research and Development Fund, the Canada Foundation for Innovation, Science and Technology Facilities Council Consolidated Grant (ST/K000926/1), and the British Columbia Development Fund. The development of detector technology was supported by the JPL Research and Technology Development Fund and Grants 06-ARPA206- 0040, 10-SAT10-0017, and 12-SAT12-0031 from the NASA APRA and SAT programs. The development and testing of detector modules were supported by the Gordon and Betty Moore Foundation.\n\nPublished - art_10.1007_s10909-015-1403-x.pdf
", "abstract": "BICEP3 is a 550-mm aperture telescope with cold, on-axis, refractive optics designed to observe at the 95-GHz band from the South Pole. It is the newest member of the BICEP/Keck family of inflationary probes specifically designed to measure the polarization of the cosmic microwave background (CMB) at degree angular scales. BICEP3 is designed to house 1280 dual-polarization pixels, which, when fully populated, totals to \u223c9\u00d7 the number of pixels in a single Keck 95-GHz receiver, thus further advancing the BICEP/Keck program's 95 GHz mapping speed. BICEP3 was deployed during the austral summer of 2014\u20132015 with nine detector tiles, to be increased to its full capacity of 20 in the second season. After instrument characterization, measurements were taken, and CMB observation commenced in April 2015. Together with multi-frequency observation data from Planck, BICEP2, and the Keck Array, BICEP3 is projected to set upper limits on the tensor-to-scalar ratio to r \u2272 0.03 at 95 % C.L.", "date": "2016-08", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "184", "number": "3", "publisher": "Springer", "pagerange": "765-771", "id_number": "CaltechAUTHORS:20160729-090031250", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160729-090031250", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PLR-1313158" }, { "agency": "NSF", "grant_number": "PLR-1313010" }, { "agency": "NSF", "grant_number": "PLR-1313062" }, { "agency": "NSF", "grant_number": "PLR-1313287" }, { "agency": "NSF", "grant_number": "AST-1056465" }, { "agency": "NSF", "grant_number": "PLR-0960243" }, { "agency": "Stanford Linear Accelerator Center (SLAC)" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K000926/1" }, { "agency": "British Columbia Development Fund" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NASA", "grant_number": "12-SAT12-0031" }, { "agency": "Gordon and Betty Moore Foundation" } ] }, "doi": "10.1007/s10909-015-1403-x", "primary_object": { "basename": "art_10.1007_s10909-015-1403-x.pdf", "url": "https://authors.library.caltech.edu/records/dfx00-xft81/files/art_10.1007_s10909-015-1403-x.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Wu, W. L. K.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/0r8zf-tze07", "eprint_id": 69357, "eprint_status": "archive", "datestamp": "2023-08-20 12:51:26", "lastmod": "2023-10-20 16:49:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "Hien T." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" }, { "id": "Battle-J", "name": { "family": "Battle", "given": "John" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "Viktor" } }, { "id": "Korngut-P-M", "name": { "family": "Korngut", "given": "Phillip" } }, { "id": "Meek-A", "name": { "family": "Meek", "given": "Andrew" } } ] }, "title": "Spatial and Temporal Stability of Airglow Measured in the Meinel Band Window at 1191.3 nm", "ispublished": "pub", "full_text_status": "public", "keywords": "atmospheric effects \u2013 site testing \u2013 techniques: imaging spectroscopy", "note": "\u00a9 2016 The Astronomical Society of the Pacific. \n\nReceived 2016 January 11; accepted 2016 January 31; published 2016 July 14. \n\nThe authors wish to thank Jaime Luna for his help designing the LAMP mechanical assembly, Heath Rhoades at JPL\u02bcs Table Mountain Observatory for his assistance setting up the instrument and guidance using the 24\u2033 telescope, and the Gemini Observatory for making their sky model tables public. The development of LAMP was supported by the JPL Research and Technology Development Fund. This publication makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.\n\nSubmitted - 1510.07567v1.pdf
", "abstract": "We report on the temporal and spatial fluctuations in the atmospheric brightness in the narrow band between Meinel emission lines at 1191.3 nm using a \u03bb/\u0394\u03bb = 320 near-infrared instrument. We present the instrument design and implementation, followed by a detailed analysis of data taken over the course of a night from Table Mountain Observatory. At low airmasses, the absolute sky brightness at this wavelength is found to be 5330 \u00b1 30 nW m^(\u22122) sr^(\u22121), consistent with previous measurements of the inter-band airglow at these wavelengths. This amplitude is larger than simple models of the continuum component of the airglow emission at these wavelengths, confirming that an extra emissive or scattering component is required to explain the observations. We perform a detailed investigation of the noise properties of the data and find no evidence for a noise component associated with temporal instability in the inter-line continuum. This result demonstrates that in several hours of ~100 s integrations the noise performance of the instrument does not appear to significantly degrade from expectations, giving a proof of concept that near-infrared line intensity mapping may be feasible from ground-based sites.", "date": "2016-07-14", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "128", "number": "967", "publisher": "Astronomical Society of the Pacific", "pagerange": "Art. No. 094504", "id_number": "CaltechAUTHORS:20160801-132118152", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160801-132118152", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/1538-3873/128/967/094504", "primary_object": { "basename": "1510.07567v1.pdf", "url": "https://authors.library.caltech.edu/records/0r8zf-tze07/files/1510.07567v1.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Nguyen, Hien T.; Zemcov, Michael; et el." }, { "id": "https://authors.library.caltech.edu/records/cwzpr-25b08", "eprint_id": 70779, "eprint_status": "archive", "datestamp": "2023-08-22 18:16:47", "lastmod": "2023-10-20 23:30:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "O'Brient-R-C", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B-A", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "BICEP2 / Keck Array VII: Matrix based E/B Separation applied to BICEP2 and the Keck Array", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization", "note": "\u00a9 2016 American Astronomical Society. \n\nReceived 2016 March 18; revised 2016 May 15; accepted 2016 May 17; published 2016 June 29. \n\n Bicep2 was supported by the US National Science Foundation under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford/SLAC is partially supported by the US Department of Energy Office of Science. Tireless administrative support was provided by Irene Coyle and Kathy Deniston.\n\nWe thank the staff of the US Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed efforts to the Bicep/Keck Array series of experiments, including the Bicep1 and Bicep3 teams.\n\nPublished - apj_825_1_66.pdf
Submitted - 1603.05976v2.pdf
", "abstract": "A linear polarization field on the sphere can be uniquely decomposed into an E-mode and a B-mode component. These two components are analytically defined in terms of spin-2 spherical harmonics. Maps that contain filtered modes on a partial sky can also be decomposed into E-mode and B-mode components. However, the lack of full sky information prevents orthogonally separating these components using spherical harmonics. In this paper, we present a technique for decomposing an incomplete map into E and B-mode components using E and B eigenmodes of the pixel covariance in the observed map. This method is found to orthogonally define E and B in the presence of both partial sky coverage and spatial filtering. This method has been applied to the Bicep2 and the Keck Array maps and results in reducing E to B leakage from \u039bCDM E-modes to a level corresponding to a tensor-to-scalar ratio of r < 1 x 10^(-4).", "date": "2016-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "825", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 66", "id_number": "CaltechAUTHORS:20161004-072520069", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161004-072520069", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT-1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Coyle and Kathy Deniston" } ] }, "corp_creators": { "items": [ "KECK ARRAY Collaborations", "BICEP2 Collaboration" ] }, "doi": "10.3847/0004-637X/825/1/66", "primary_object": { "basename": "1603.05976v2.pdf", "url": "https://authors.library.caltech.edu/records/cwzpr-25b08/files/1603.05976v2.pdf" }, "related_objects": [ { "basename": "apj_825_1_66.pdf", "url": "https://authors.library.caltech.edu/records/cwzpr-25b08/files/apj_825_1_66.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/8amm1-wnt25", "eprint_id": 66512, "eprint_status": "archive", "datestamp": "2023-08-20 10:26:05", "lastmod": "2023-10-18 18:09:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The HerMES submillimetre local and low-redshift luminosity functions", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution galaxies: luminosity function, mass function galaxies: statistics submillimetre: galaxies", "note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 November 17. Received 2015 November 16; in original form 2014 December 1. First published online December 30, 2015. \n\nLucia Marchetti (LM) acknowledges support from the Science and Technology Facilities Council (STFC) under grant ST/J001597/1. Lucia Marchetti, Mattia Vaccari and Alberto Franceschini acknowledge support from ASI 'Herschel Science' Contracts I/005/07/1 and I/005/11/0. Mattia Negrello produced additional predictions based on his models. Julie Wardlow acknowledges the Dark Cosmology Centre funded by the Danish National Research Foundation. Mattia Vaccari acknowledges support from the Square Kilometre Array South Africa project, the South African National Research Foundation and Department of Science and Technology (DST/CON 0134/2014), the European Commission Research Executive Agency (FP7-SPACE-2013-1 GA 607254) and the Italian Ministry for Foreign Affairs and International Cooperation (PGR GA ZA14GR02). Nicholas Seymour is the recipient of an ARC Future Fellowship. Anna Feltre acknowledges support from the ERC via an Advanced Grant under grant agreement no. 321323-NEOGAL. This work makes use of STILTS http://www.starlink.ac.uk/stilts/ and TOPCAT (Taylor 2005). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). The authors would like to thank the anonymous referee for helpful comments.\n\nPublished - MNRAS-2016-Marchetti-1999-2023.pdf
", "abstract": "We used wide-area surveys over 39 deg2 by the HerMES (Herschel Multi-tiered Extragalactic Survey) collaboration, performed with the Herschel Observatory SPIRE multiwavelength camera, to estimate the low-redshift, 0.02 < z < 0.5, monochromatic luminosity functions (LFs) of galaxies at 250, 350 and 500\u2009\u03bcm. Within this redshift interval, we detected 7087 sources in five independent sky areas, \u223c40 per cent of which have spectroscopic redshifts, while for the remaining objects photometric redshifts were used. The SPIRE LFs in different fields did not show any field-to-field variations beyond the small differences to be expected from cosmic variance. SPIRE flux densities were also combined with Spitzer photometry and multiwavelength archival data to perform a complete spectral energy distribution fitting analysis of SPIRE detected sources to calculate precise k-corrections, as well as the bolometric infrared (IR; 8\u20131000\u2009\u03bcm) LFs and their low-z evolution from a combination of statistical estimators. Integration of the latter prompted us to also compute the local luminosity density and the comoving star formation rate density (SFRD) for our sources, and to compare them with theoretical predictions of galaxy formation models. The LFs show significant and rapid luminosity evolution already at low redshifts, 0.02 < z < 0.2, with L^\u2217_(IR)\u221d(1+z)^(6.0\u00b10.4) and \u03a6^\u2217_(IR) \u221d(1+z)^(\u22122.1\u00b10.4), L^\u2217_(250)\u221d(1+z)5.3\u00b10.2 and \u03a6^\u2217_(250)\u221d(1+z)^(\u22120.6\u00b10.4) estimated using the IR bolometric and the 250\u2009\u03bcm LFs, respectively. Converting our IR LD estimate into an SFRD assuming a standard Salpeter initial mass function and including the unobscured contribution based on the UV dust-uncorrected emission from local galaxies, we estimate an SFRD scaling of SFRD_0 + 0.08z, where SFRD_0 \u2243 (1.9 \u00b1 0.03) \u00d7 10^(\u22122)\u2009[M_\u2299\u2009Mpc^(\u22123)] is our total SFRD estimate at z \u223c 0.02.", "date": "2016-02-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "456", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1999-2023", "id_number": "CaltechAUTHORS:20160427-105744845", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160427-105744845", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/J001597/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/11/0" }, { "agency": "Danish National Research Foundation" }, { "agency": "Department of Science and Technology (South Africa)", "grant_number": "DST/CON 0134/2014" }, { "agency": "European Research Council (ERC)", "grant_number": "FP7-SPACE-2013-1 GA 607254" }, { "agency": "Ministry for Foreign Affairs and International Cooperation (Italy)", "grant_number": "PGR GA ZA14GR02" }, { "agency": "Australian Research Council" }, { "agency": "European Research Council (ERC)", "grant_number": "321323-NEOGAL" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "doi": "10.1093/mnras/stv2717", "primary_object": { "basename": "MNRAS-2016-Marchetti-1999-2023.pdf", "url": "https://authors.library.caltech.edu/records/8amm1-wnt25/files/MNRAS-2016-Marchetti-1999-2023.pdf" }, "resource_type": "article", "pub_year": "2016", "author_list": "Marchetti, L.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/58472-cc358", "eprint_id": 60324, "eprint_status": "archive", "datestamp": "2023-08-20 10:03:24", "lastmod": "2023-10-24 16:26:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general \u2013 ISM: magnetic fields \u2013 ISM: clouds \u2013 dust, extinction \u2013 submillimeter: ISM \u2013 infrared: ISM", "note": "\u00a9 2016 ESO. Article published by EDP Sciences. \n\nReceived 13 February 2015; Accepted 25 May 2015. Published online 09 February 2016. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934.\n\nPublished - aa25896-15.pdf
Accepted Version - 1502.04123v3.pdf
", "abstract": "Within ten nearby (d < \u2009450\u2009pc) Gould belt molecular clouds we evaluate statistically the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353\u2009GHz, and the gas column density structures, quantified by the gradient of the column density, N_H. The selected regions, covering several degrees in size, are analysed at an effective angular resolution of 10\u2032 FWHM, thus sampling physical scales from 0.4 to 40\u2009pc in the nearest cloud. The column densities in the selected regions range from N_H\u2248 10^(21) to10^(23)\u2009cm^(-2), and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analysed in bins of column density using the novel statistical tool called \"histogram of relative orientations\". Throughout this study, we assume that the polarized emission observed by Planck at 353\u2009GHz is representative of the projected morphology of the magnetic field in each region, i.e., we assume a constant dust grain alignment efficiency, independent of the local environment. Within most clouds we find that the relative orientation changes progressively with increasing N_H, from mostly parallel or having no preferred orientation to mostly perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfv\u00e9nic or sub-Alfv\u00e9nic turbulence, implying that the magnetic field is significant for the gas dynamics at the scales probed by Planck. We compare the deduced magnetic field strength with estimates we obtain from other methods and discuss the implications of the Planck observations for the general picture of molecular cloud formation and evolution.", "date": "2016-02", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "586", "publisher": "EDP Sciences", "pagerange": "Art. No. A138", "id_number": "CaltechAUTHORS:20150918-114746985", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150918-114746985", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Institut national du patrimoine (INP)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "CSIC and RES (Spain)" }, { "agency": "Tekes and CSC (Finland)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "PRACE (EU)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Academy of Finland" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525896", "primary_object": { "basename": "1502.04123v3.pdf", "url": "https://authors.library.caltech.edu/records/58472-cc358/files/1502.04123v3.pdf" }, "related_objects": [ { "basename": "aa25896-15.pdf", "url": "https://authors.library.caltech.edu/records/58472-cc358/files/aa25896-15.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/yxbdd-s6d03", "eprint_id": 62154, "eprint_status": "archive", "datestamp": "2023-08-20 09:59:07", "lastmod": "2023-10-25 16:54:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "O'Brient-R-C", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Steinbach-B-A", "name": { "family": "Steinbach", "given": "B." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 American Physical Society. \n\nReceived 2 November 2015; published 20 January 2016. \n\nThe Keck Array project has been made possible through support from the National Science Foundation under Grants No. ANT-1145172 (Harvard), No. ANT-1145143 (Minnesota), and No. ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Read-out electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this Letter were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. DOE Office of Science. We thank the staff of the U.S. Antarctic Program and, in particular, the South Pole Station without whose help this research would not have been possible. Most special thanks go to Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP-Keck Array series of experiments, including the BICEP1 team. We also thank the Planck and WMAP teams for the use of their data.\n\nPublished - PhysRevLett.116.031302.pdf
Submitted - 1510.09217v1.pdf
", "abstract": "We present results from an analysis of all data taken by the BICEP2 and Keck Array cosmic microwave background (CMB) polarization experiments up to and including the 2014 observing season. This includes the first Keck Array observations at 95 GHz. The maps reach a depth of 50 nK\u2009deg in Stokes Q and U in the 150 GHz band and 127 nK\u2009deg in the 95 GHz band. We take auto- and cross-spectra between these maps and publicly available maps from WMAP and Planck at frequencies from 23 to 353 GHz. An excess over lensed \u039bCDM is detected at modest significance in the 95\u00d7150 BB spectrum, and is consistent with the dust contribution expected from our previous work. No significant evidence for synchrotron emission is found in spectra such as 23\u00d795, or for correlation between the dust and synchrotron sky patterns in spectra such as 23\u00d7353. We take the likelihood of all the spectra for a multicomponent model including lensed \u039bCDM, dust, synchrotron, and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r ) using priors on the frequency spectral behaviors of dust and synchrotron emission from previous analyses of WMAP and Planck data in other regions of the sky. This analysis yields an upper limit r_(0.05) <0.09 at 95% confidence, which is robust to variations explored in analysis and priors. Combining these B-mode results with the (more model-dependent) constraints from Planck analysis of CMB temperature plus baryon acoustic oscillations and other data yields a combined limit r_(0.05) <0.07 at 95% confidence. These are the strongest constraints to date on inflationary gravitational waves.", "date": "2016-01-22", "date_type": "published", "publication": "Physical Review Letters", "volume": "116", "number": "3", "publisher": "American Physical Society", "pagerange": "Art. No. 031302", "id_number": "CaltechAUTHORS:20151117-084910280", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151117-084910280", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "corp_creators": { "items": [ "KECK ARRAY Collaboration", "BICEP2 Collaboration" ] }, "doi": "10.1103/PhysRevLett.116.031302", "primary_object": { "basename": "1510.09217v1.pdf", "url": "https://authors.library.caltech.edu/records/yxbdd-s6d03/files/1510.09217v1.pdf" }, "related_objects": [ { "basename": "PhysRevLett.116.031302.pdf", "url": "https://authors.library.caltech.edu/records/yxbdd-s6d03/files/PhysRevLett.116.031302.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/890kt-7m777", "eprint_id": 64323, "eprint_status": "archive", "datestamp": "2023-08-20 09:43:06", "lastmod": "2023-10-17 20:50:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bryan-Sean", "name": { "family": "Bryan", "given": "Sean" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "Brendan" }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "Olivier" }, "orcid": "0000-0001-7432-2932" }, { "id": "Hristov-Viktor-V", "name": { "family": "Hristov", "given": "Viktor" } }, { "id": "Mason-Peter-V", "name": { "family": "Mason", "given": "Peter" }, "orcid": "0000-0002-7963-7420" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "Lorenzo" }, "orcid": "0000-0002-4242-3015" }, { "id": "Morford-Tracy-A", "name": { "family": "Morford", "given": "Tracy" } }, { "id": "Transgrud-Amy-R", "name": { "family": "Transgrud", "given": "Amy" } }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "Rebecca" } } ] }, "title": "A cryogenic rotation stage with a large clear aperture for the half-wave plates in the Spider instrument", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2016 AIP Publishing LLC. \n\nReceived 6 October 2015; accepted 18 December 2015; published online 8 January 2016. \n\nSPIDER is supported in the U.S. by National Aeronautics and Space Administration under Grant Nos. NNX07AL64G and NNX12AE95G issued through the Science Mission Directorate, with support for A.S.R. from NESSF NNX10AM55H, and by the National Science Foundation through No. PLR-1043515. Logistical support for the Antarctic deployment and operations was provided by the NSF through the U.S. Antarctic Program. The collaboration is grateful for the generous support of the David and Lucile Packard Foundation, which has been crucial to the success of the project. Support in Canada is provided by the National Sciences and Engineering Council and the Canadian Space Agency.\n\nPublished - 1.4939435.pdf
Submitted - 1510.01771v2.pdf
", "abstract": "We describe the cryogenic half-wave plate rotation mechanisms built for and used in Spider, a polarization-sensitive balloon-borne telescope array that observed the cosmic microwave background at 95 GHz and 150 GHz during a stratospheric balloon flight from Antarctica in January 2015. The mechanisms operate at liquid helium temperature in flight. A three-point contact design keeps the mechanical bearings relatively small but allows for a large (305 mm) diameter clear aperture. A worm gear driven by a cryogenic stepper motor allows for precise positioning and prevents undesired rotation when the motors are depowered. A custom-built optical encoder system monitors the bearing angle to an absolute accuracy of \u00b10.1\u2218. The system performed well in Spider during its successful 16 day flight.", "date": "2016-01", "date_type": "published", "publication": "Review of Scientific Instruments", "volume": "87", "number": "1", "publisher": "American Institute of Physics", "pagerange": "Art. No. 014501", "id_number": "CaltechAUTHORS:20160209-080319346", "issn": "0034-6748", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160209-080319346", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AL64G" }, { "agency": "NASA", "grant_number": "NNX12AE95G" }, { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX10AM55H" }, { "agency": "NSF", "grant_number": "PLR-1043515" }, { "agency": "David and Lucile Packard Foundation" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Space Agency (CSA)" } ] }, "doi": "10.1063/1.4939435", "primary_object": { "basename": "1.4939435.pdf", "url": "https://authors.library.caltech.edu/records/890kt-7m777/files/1.4939435.pdf" }, "related_objects": [ { "basename": "1510.01771v2.pdf", "url": "https://authors.library.caltech.edu/records/890kt-7m777/files/1510.01771v2.pdf" } ], "resource_type": "article", "pub_year": "2016", "author_list": "Bryan, Sean; Bock, James J.; et el." }, { "id": "https://authors.library.caltech.edu/records/gpttv-bz656", "eprint_id": 63146, "eprint_status": "archive", "datestamp": "2023-08-22 17:00:11", "lastmod": "2023-10-25 23:34:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "BICEP2. III. Instrumental Systematics", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; instrumentation: polarimeters; methods: data analysis", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 February 9; accepted 2015 October 21; published 2015 November 23. \n\nBicep2 was supported by the U.S. National Science Foundation under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W. M. Keck Foundation. Partial support for C. Sheehy was also provided by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. \n\nWe thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed past efforts to the Bicep/Keck Array series of experiments, including the Bicep1 and Keck Array teams, as well as our colleagues on the Spider team with whom we coordinated receiver and detector development efforts at Caltech. We dedicate this paper to the memory of Andrew Lange, whom we sorely miss.\n\nPublished - Ade_2015p110.pdf
Submitted - 1502.00608v2.pdf
", "abstract": "In a companion paper, we have reported a >5\u03c3 detection of degree scale B-mode polarization at 150 GHz by the Bicep2 experiment. Here we provide a detailed study of potential instrumental systematic contamination to that measurement. We focus extensively on spurious polarization that can potentially arise from beam imperfections. We present a heuristic classification of beam imperfections according to their symmetries and uniformities, and discuss how resulting contamination adds or cancels in maps that combine observations made at multiple orientations of the telescope about its boresight axis. We introduce a technique, which we call \"deprojection,\" for filtering the leading order beam-induced contamination from time-ordered data, and show that it reduces power in Bicep2's actual and null-test BB spectra consistent with predictions using high signal-to-noise beam shape measurements. We detail the simulation pipeline that we use to directly simulate instrumental systematics and the calibration data used as input to that pipeline. Finally, we present the constraints on BB contamination from individual sources of potential systematics. We find that systematics contribute BB power that is a factor of ~10\u00d7 below Bicep2's three-year statistical uncertainty, and negligible compared to the observed BB signal. The contribution to the best-fit tensor/scalar ratio is at a level equivalent to r = (3\u20136) \u00d7 10^(\u22123).", "date": "2015-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "814", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 110", "id_number": "CaltechAUTHORS:20151222-131922150", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151222-131922150", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT-1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "PHY-1125897" }, { "agency": "Kavli Foundation" }, { "agency": "Harvard University" }, { "agency": "Kavli Institute for Cosmological Physics" }, { "agency": "Fred Kavli" } ] }, "doi": "10.1088/0004-637X/814/2/110", "primary_object": { "basename": "Ade_2015p110.pdf", "url": "https://authors.library.caltech.edu/records/gpttv-bz656/files/Ade_2015p110.pdf" }, "related_objects": [ { "basename": "1502.00608v2.pdf", "url": "https://authors.library.caltech.edu/records/gpttv-bz656/files/1502.00608v2.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/4cz7n-mg310", "eprint_id": 63086, "eprint_status": "archive", "datestamp": "2023-08-22 16:41:41", "lastmod": "2023-10-25 23:30:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P." }, "orcid": "0000-0002-7963-7420" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "O'Brient-R-C", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Runyan-M-C", "name": { "family": "Runyan", "given": "M. C." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "id": "Tucker-Rebecca-S", "name": { "family": "Tucker", "given": "R. S." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Antenna-coupled TES Bolometers Used in BICEP2, Keck Array, and Spider", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; instrumentation: detectors; instrumentation: polarimeters; methods: laboratory: solid state; techniques: polarimetric", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 March 2; accepted 2015 July 28; published 2015 October 20. \n\nThe development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W. M. Keck Foundation. Bicep2 was supported by the US National Science Foundation under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). Some computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. We thank Warren Holmes and Matthew Kenyon for discussions on thermal conductivity. Tireless administrative support was provided by Irene Coyle and Kathy Deniston.\n\nPublished - Ade_2015p176.pdf
Submitted - 1502.00619v1.pdf
", "abstract": "We have developed antenna-coupled transition-edge sensor bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including Bicep2, Keck Array, and the balloon borne Spider. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%\u201330% bandwidth at 95, 150, or 230 GHz. The integrated antenna arrays synthesize symmetric co-aligned beams with controlled side-lobe levels. Cross-polarized response on boresight is typically ~ 0.5%, consistent with cross-talk in our multiplexed readout system. End-to-end optical efficiencies in our cameras are routinely 35% or higher, with per detector sensitivities of NET ~ 300 \u00b5K_(CMB\u221as). Thanks to the scalability of this design, we have deployed 2560 detectors as 1280 matched pairs in Keck Array with a combined instantaneous sensitivity of ~9 \u00b5K_CMB\u221as), as measured directly from CMB maps in the 2013 season. Similar arrays have recently flown in the Spider instrument, and development of this technology is ongoing.", "date": "2015-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "812", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 176", "id_number": "CaltechAUTHORS:20151221-071230729", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151221-071230729", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT-1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" } ] }, "corp_creators": { "items": [ "BICEP2 Collaboration", "KECK ARRAY Collaborations", "SPIDER Collaboration" ] }, "doi": "10.1088/0004-637X/812/2/176", "primary_object": { "basename": "1502.00619v1.pdf", "url": "https://authors.library.caltech.edu/records/4cz7n-mg310/files/1502.00619v1.pdf" }, "related_objects": [ { "basename": "Ade_2015p176.pdf", "url": "https://authors.library.caltech.edu/records/4cz7n-mg310/files/Ade_2015p176.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/k0wcs-vj290", "eprint_id": 57068, "eprint_status": "archive", "datestamp": "2023-08-20 08:36:59", "lastmod": "2023-10-23 15:28:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bussmann-Robert-S", "name": { "family": "Bussmann", "given": "R. S." } }, { "id": "Riechers-Dominik-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Filakov-Anastasia", "name": { "family": "Fialkov", "given": "A." } }, { "id": "Scudder-Jillian-M", "name": { "family": "Scudder", "given": "J." }, "orcid": "0000-0002-8798-3972" }, { "id": "Hayward-Christopher-C", "name": { "family": "Hayward", "given": "C. C." }, "orcid": "0000-0003-4073-3236" }, { "id": "Cowley-W-I", "name": { "family": "Cowley", "given": "W. I." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Calanog-J-A", "name": { "family": "Calanog", "given": "J." } }, { "id": "Chapman-Scott-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Cooray-Asantha", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "De-Bernardis-F", "name": { "family": "De Bernardis", "given": "F." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "Hai" }, "orcid": "0000-0001-9608-6395" }, { "id": "Gavazzo-R", "name": { "family": "Gavazzi", "given": "R." } }, { "id": "Hopwood-Rosalind", "name": { "family": "Hopwood", "given": "R." } }, { "id": "Ivison-Rob-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Jarvis-Matt-J", "name": { "family": "Jarvis", "given": "M." }, "orcid": "0000-0001-7039-9078" }, { "id": "Lacey-Cedric-G", "name": { "family": "Lacey", "given": "C." }, "orcid": "0000-0001-9016-5332" }, { "id": "Loeb-Abraham", "name": { "family": "Loeb", "given": "A." }, "orcid": "0000-0003-4330-287X" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "P\u00e9rez-Fournon-Ismael", "name": { "family": "P\u00e9rez-Fournon", "given": "I." }, "orcid": "0000-0002-2807-6459" }, { "id": "Rigopoulou-Dimitra", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Smith-A-J", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Vieira-Joaquin-D", "name": { "family": "Vieira", "given": "J. D." }, "orcid": "0000-0001-7192-3871" }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Wardlow-Julie-L", "name": { "family": "Wardlow", "given": "J." }, "orcid": "0000-0003-2376-8971" } ] }, "title": "HerMES: ALMA Imaging of Herschel-selected Dusty Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 submillimeter: galaxies \u2013 techniques: interferometric", "note": "\u00a9 2015 The American Astronomical Society. \n\nReceived 2015 April 20; accepted 2015 July 14; published 2015 October 7. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nWe thank the referee for useful comments that helped improve the clarity of the manuscript. This paper makes use of the following ALMA data: ADS/JAO.ALMA# 2011.0.00539.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. \n\nThe results described in this paper are based on observations obtained with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nThis research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists, and a mission scientist. HerMES is described in Oliver et al. (2012). The HerMES data presented in this paper will be released through the Herschel Database in Marseille (HeDaM). \n\nSPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). \n\nThe VIDEO imaging data are based on data products from observations made with ESO Telescopes at the La Silla or Paranal Observatories under ESO programme ID 179.A-2006. \n\nThis paper is partly based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil), and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u00f3n Productiva (Argentina). \n\nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Dark Cosmology Centre is funded by the Danish National Research Foundation. R. J. I. acknowledges support from European Research Council Advanced Investigator Grant, Cosmicism, 321302. C. C. H. is grateful to the Gordon and Betty Moore Foundation for financial support. \n\nFacilities: ALMA, Gemini-S.\n\nPublished - Bussmann_2015p43.pdf
Submitted - 1504.05256v1.pdf
Erratum - Bussmann_2015_erratum.pdf
", "abstract": "The Herschel Multi-tiered Extragalactic Survey (HerMES) has identified large numbers of dusty star-forming galaxies (DSFGs) over a wide range in redshift. A detailed understanding of these DSFGs is hampered by the limited spatial resolution of Herschel. We present 870 \u03bcm 0.\"45 resolution imaging obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) of a sample of 29 HerMES DSFGs that have far-infrared (FIR) flux densities that lie between the brightest of sources found by Herschel and fainter DSFGs found via ground-based surveys in the submillimeter region. The ALMA imaging reveals that these DSFGs comprise a total of 62 sources (down to the 5\u03c3 point-source sensitivity limit in our ALMA sample; \u03c3 \u2248 0.2 mJy). Optical or near-infrared imaging indicates that 36 of the ALMA sources experience a significant flux boost from gravitational lensing (\u00b5 > 1.1), but only six are strongly lensed and show multiple images. We introduce and make use of uvmcmcfit, a general-purpose and publicly available Markov chain Monte Carlo visibility-plane analysis tool to analyze the source properties. Combined with our previous work on brighter Herschel sources, the lens models presented here tentatively favor intrinsic number counts for DSFGs with a break near 8 mJy at 880 \u00b5m and a steep fall-off at higher flux densities. Nearly 70% of the Herschel sources break down into multiple ALMA counterparts, consistent with previous research indicating that the multiplicity rate is high in bright sources discovered in single-dish submillimeter or FIR surveys. The ALMA counterparts to our Herschel targets are located significantly closer to each other than ALMA counterparts to sources found in the LABOCA ECDFS Submillimeter Survey. Theoretical models underpredict the excess number of sources with small separations seen in our ALMA sample. The high multiplicity rate and small projected separations between sources seen in our sample argue in favor of interactions and mergers plausibly driving both the prodigious emission from the brightest DSFGs as well as the sharp downturn above S_(880) = 8 mJy.", "date": "2015-10-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "812", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 43", "id_number": "CaltechAUTHORS:20150428-152924348", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150428-152924348", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "321302" }, { "agency": "Gordon and Betty Moore Foundation" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/812/1/43", "primary_object": { "basename": "1504.05256v1.pdf", "url": "https://authors.library.caltech.edu/records/k0wcs-vj290/files/1504.05256v1.pdf" }, "related_objects": [ { "basename": "Bussmann_2015_erratum.pdf", "url": "https://authors.library.caltech.edu/records/k0wcs-vj290/files/Bussmann_2015_erratum.pdf" }, { "basename": "Bussmann_2015p43.pdf", "url": "https://authors.library.caltech.edu/records/k0wcs-vj290/files/Bussmann_2015p43.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Bussmann, R. S.; Riechers, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/e93zx-kky68", "eprint_id": 62246, "eprint_status": "archive", "datestamp": "2023-08-22 16:30:17", "lastmod": "2023-10-25 16:59:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "BICEP2/Keck Array V: Measurements of B-mode Polarization at Degree Angular Scales and 150 GHz by the Keck Array", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 February 3; accepted 2015 August 28; published 2015 September 29. \n\nThe Keck Array project has been made possible through support from the National Science Foundation under Grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota) & ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the Bicep\u2013Keck Array series of experiments, including the Bicep1 team.\n\nPublished - Ade_2015p126.pdf
Submitted - 1502.00643v2.pdf
", "abstract": "The Keck Array is a system of cosmic microwave background polarimeters, each similar to the Bicep2 experiment. In this paper we report results from the 2012 to 2013 observing seasons, during which the Keck Array consisted of five receivers all operating in the same (150 GHz) frequency band and observing field as Bicep2. We again find an excess of B-mode power over the lensed-\u039bCDM expectation of >5\u03c3 in the range 30 < \u2113 < 150 and confirm that this is not due to systematics using jackknife tests and simulations based on detailed calibration measurements. In map difference and spectral difference tests these new data are shown to be consistent with Bicep2. Finally, we combine the maps from the two experiments to produce final Q and U maps which have a depth of 57 nK deg (3.4 \u03bcK arcmin) over an effective area of 400 deg^2 for an equivalent survey weight of 250,000 \u03bcK^(\u22122). The final BB band powers have noise uncertainty a factor of 2.3 times better than the previous results, and a significance of detection of excess power of >6\u03c3.", "date": "2015-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "811", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 126", "id_number": "CaltechAUTHORS:20151119-132830511", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151119-132830511", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT- 1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "doi": "10.1088/0004-637X/811/2/126", "primary_object": { "basename": "1502.00643v2.pdf", "url": "https://authors.library.caltech.edu/records/e93zx-kky68/files/1502.00643v2.pdf" }, "related_objects": [ { "basename": "Ade_2015p126.pdf", "url": "https://authors.library.caltech.edu/records/e93zx-kky68/files/Ade_2015p126.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/s72a5-xrh69", "eprint_id": 60727, "eprint_status": "archive", "datestamp": "2023-08-22 16:29:52", "lastmod": "2023-10-24 21:08:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rawlings-J-I", "name": { "family": "Rawlings", "given": "J. I." } }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Guo-K", "name": { "family": "Guo", "given": "K." } }, { "id": "Hatziminaoglou-E", "name": { "family": "Hatziminaoglou", "given": "E." } }, { "id": "Ibar-E", "name": { "family": "Ibar", "given": "E." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Seymour-N", "name": { "family": "Seymour", "given": "N." }, "orcid": "0000-0003-3506-5536" }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "J. L." }, "orcid": "0000-0003-2376-8971" } ] }, "title": "HerMES: disentangling active galactic nuclei and star formation in the radio source population", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: ISM; galaxies: nuclei; infrared: galaxies; radio continuum: galaxies", "note": "\u00a9 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2015 July 11. Received 2015 June 28. In original form 2014 April 18. First published online August 10, 2015. \n\nWe thank the anonymous referee for their comments which improved the manuscript. We also thank Neal Miller for useful discussions and James Mullaney for help regarding DecompIR. JIR acknowledges the support of a Science and Technologies Facilities Council studentship. MJP acknowledges support from the Science and Technology Facilities Council (STFC) (grant number ST/K000977/1). SJO and MS acknowledge support from the STFC (grant number ST/I000976/1). NS is the recipient of an Australian Research Council Future Fellowship. MV acknowledges support from the South African Department of Science and Technology (DST/CON 0134/2014), the European Commission Research Executive Agency (FP7-SPACE-2013-1 GA 607254) and the Italian Ministry for Foreign Affairs and International Cooperation (PGR GA ZA14GR02). The Dark Cosmology Centre is funded by the Danish National Research Foundation. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). This work is also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology (Caltech) under contract with NASA. This work benefitted from the NASA/IPAC Extragalactic Database (NED), which is operated by the JPL, Caltech, under contract with NASA.\n\nPublished - MNRAS-2015-Rawlings-4111-27.pdf
Submitted - 1507.07044v1.pdf
", "abstract": "We separate the extragalactic radio source population above \u223c50 \u03bcJy into active galactic nuclei (AGN) and star-forming sources. The primary method of our approach is to fit the infrared spectral energy distributions (SEDs), constructed using Spitzer/IRAC (Infrared Array Camera) and Multiband Imaging Photometer for Spitzer (MIPS) and Herschel/SPIRE photometry, of 380 radio sources in the Extended Chandra Deep Field-South. From the fitted SEDs, we determine the relative AGN and star-forming contributions to their infrared emission. With the inclusion of other AGN diagnostics such as X-ray luminosity, Spitzer/IRAC colours, radio spectral index and the ratio of star-forming total infrared flux to k-corrected 1.4 GHz flux density, q_(IR), we determine whether the radio emission in these sources is powered by star formation or by an AGN. The majority of these radio sources (60 per cent) show the signature of an AGN at some wavelength. Of the sources with AGN signatures, 58 per cent are hybrid systems for which the radio emission is being powered by star formation. This implies that radio sources which have likely been selected on their star formation have a high AGN fraction. Below a 1.4 GHz flux density of 1 mJy, along with finding a strong contribution to the source counts from pure star-forming sources, we find that hybrid sources constitute 20\u201365 per cent of the sources. This result suggests that hybrid sources have a significant contribution, along with sources that do not host a detectable AGN, to the observed flattening of the source counts at \u223c1 mJy for the extragalactic radio source population.", "date": "2015-10-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "452", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "4111-4127", "id_number": "CaltechAUTHORS:20151002-141031378", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151002-141031378", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K000977/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Australian Research Council" }, { "agency": "Department of Science and Technology (South Africa)", "grant_number": "DST/CON 0134/2014" }, { "agency": "European Research Council (ERC)", "grant_number": "FP7-SPACE-2013-1 GA 607254" }, { "agency": "Ministero Affari Esteri e della Cooperazione internazionale (MAECI)", "grant_number": "PGR GA ZA14GR02" }, { "agency": "Danish National Research Foundation" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1093/mnras/stv1573", "primary_object": { "basename": "1507.07044v1.pdf", "url": "https://authors.library.caltech.edu/records/s72a5-xrh69/files/1507.07044v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Rawlings-4111-27.pdf", "url": "https://authors.library.caltech.edu/records/s72a5-xrh69/files/MNRAS-2015-Rawlings-4111-27.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Rawlings, J. I.; Page, M. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/83jg6-f6404", "eprint_id": 61467, "eprint_status": "archive", "datestamp": "2023-08-20 08:10:26", "lastmod": "2023-10-25 14:54:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Laporte-N", "name": { "family": "Laporte", "given": "N." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Environment of the submillimeter-bright massive starburst HFLS3 at z\u223c6.34", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation \u2013 galaxies: high-redshift \u2013 galaxies: luminosity function, mass function \u2013\ngalaxies: starburst", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 April 17; accepted 2015 July 24; published 2015 September 8.\n\nFinancial support for this work was provided by the Spanish\nMINECO under projects AYA2010-21697-C05-04 and FIS2012-\n39162-C06-02, by the Chilean Basal-CATA PFB-06/2007 and\nCONICYT-Chile under the grant Gemini-CONICYT #32120003,\nand by NASA through grant HST-GO-13045 from the Space\nTelescope Science Institute, which is operated by Associated\nUniversities for Research in Astronomy, Inc., under NASA\ncontract NAS 5-26555. Additional support for A.C., W.O., J.C., J.\nL.W., and C.M.C. was from NSF with AST-1313319. The Dark\nCosmology Centre is funded by the Danish National Research\nFoundation (J.L.W.). S.O. acknowledges support from the Science\nand Technology Facilities Council [grant number ST/I000976/1].\nD.R. acknowledges support from the Science and Technology\nFacilities Council (ST/K00106X/1). R.J.I. acknowledges support\nfrom the European Research Council in the form of Advanced Grant, COSMICISM, 321302. SPIRE has been developed by a\nconsortium of institutes led by Cardiff Univ. (UK) and\nincluding Univ. Lethbridge (Canada); NAOC (China); CEA,\nLAM (France); IFSI, Univ. Padua (Italy); Stockholm Observatory\n(Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado\n(USA). This development has been supported by national funding\nagencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS\n(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC,\nUKSA (UK); and NASA (USA).We thank Jos\u00e9 Acosta-Pulido for\nadvice on the LIRIS observations and help with the LIRIS data\nreduction package. This work is based on observations made with\nthe Gran Telescopio Canarias (GTC), installed in the Spanish\nObservatorio del Roque de los Muchachos of the Instituto de\nAstrof\u00edsica de Canarias, on the island of La Palma. The William\nHerschel Telescope is operated on the island of La Palma by the\nIsaac Newton Group in the Spanish Observatorio del Roque de los\nMuchachos of the Instituto de Astrofsica de Canarias. The data\npresented in this paper will be released through the Herschel\nDatabase in Marseille HeDaM (hedam.oamp.fr/HerMES)\nFacilities: GTC (OSIRIS), HST (ACS, WFC3), Spitzer\n(IRAC), WHT (LIRIS).\n\nPublished - Laporte_2015.pdf
Submitted - 1504.04534v2.pdf
", "abstract": "We describe the search for Lyman break galaxies (LBGs) near the submillimeter-bright starburst galaxy HFLS3 at z = 6.34 and a study on the environment of this massive galaxy during the end of reionization. We performed two independent selections of LBGs on images obtained with the Gran Telescopio Canarias (GTC) and the Hubble Space Telescope (HST) by combining nondetections in bands blueward of the Lyman break and color selection. A total of 10 objects fulfilling the LBG selection criteria at z > 5.5 were selected over the 4.54 and 55.5 arcmin^2 covered by our HST and GTC images, respectively. The photometric redshift, UV luminosity, and star formation rate of these sources were estimated with models of their spectral energy distribution. These z ~ 6 candidates have physical properties and number densities in agreement with previous results. The UV luminosity function at z ~ 6 and a Voronoi tessellation analysis of this field show no strong evidence for an overdensity of relatively bright objects (m_(F105W) < 25.9) associated with HFLS3. However, the overdensity parameter deduced from this field and the surface density of objects cannot exclude definitively the LBG overdensity hypothesis. Moreover, we identified three faint objects at less than 3'' from HFLS3 with color consistent with those expected for z ~ 6 galaxies. Deeper data are needed to confirm their redshifts and to study their association with HFLS3 and the galaxy merger that may be responsible for the massive starburst.", "date": "2015-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "810", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 130", "id_number": "CaltechAUTHORS:20151023-082526969", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151023-082526969", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "AYA2010-21697-C05-04" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MINECO)", "grant_number": "FIS2012-39162-C06-02" }, { "agency": "Basal-CATA", "grant_number": "PFB-06/2007" }, { "agency": "Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica (CONICYT)", "grant_number": "32120003" }, { "agency": "NASA", "grant_number": "HST-GO-13045" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "Danish National Research Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K00106X/1" }, { "agency": "European Research Council (ERC)", "grant_number": "321302" } ] }, "doi": "10.1088/0004-637X/810/2/130", "primary_object": { "basename": "Laporte_2015.pdf", "url": "https://authors.library.caltech.edu/records/83jg6-f6404/files/Laporte_2015.pdf" }, "related_objects": [ { "basename": "1504.04534v2.pdf", "url": "https://authors.library.caltech.edu/records/83jg6-f6404/files/1504.04534v2.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Laporte, N.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/73pad-r5x14", "eprint_id": 61792, "eprint_status": "archive", "datestamp": "2023-08-22 16:15:39", "lastmod": "2023-10-25 15:44:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O. P." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "S." }, "orcid": "0000-0002-2849-559X" }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XXXII. The updated Planck catalogue of Sunyaev-Zeldovich sources", "ispublished": "pub", "full_text_status": "public", "keywords": "errata, addenda; large-scale structure of Universe; galaxies: clusters: general; catalogs", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 2 February 2015; Accepted 18 February 2015; Published online 25 August 2015. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The authors thank N. Schartel, ESA XMM-Newton project scientist, for granting the DDT used for confirmation of SZ Planck candidates. The authors thank TUBITAK, IKI, KFU and AST for support in using RTT150; in particular we thank KFU and IKI for providing significant amounts of their observing time at RTT150. We also acknowledge the BTA 6 m telescope TAC for support of the optical follow-up project. The authors acknowledge the use of the INT and WHT telescopes operated on the island of La Palma by the Isaac Newton Group of Telescopes at the Spanish Observatorio del Roque de los Muchachos of the IAC; the NOT, operated on La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, at the Spanish Observatorio del Roque de los Muchachos; the TNG, operated on La Palma by the Fundacion Galileo Galilei of the INAF at the Spanish Observatorio del Roque de los Muchachos; the GTC telescope, operated on La Palma by the IAC at the Spanish Observatorio del Roque de los Muchachos; and the IAC80 telescope operated on the island of Tenerife by the IAC at the Spanish Observatorio del Teide. Part of this research has been carried out with telescope time awarded by the CCI International Time Programme. The authors thank the TAC of the MPG/ESO-2.2m telescope for support of optical follow-up with WFI under Max Planck time. Observations were also conducted with ESO NTT at the La Silla Paranal Observatory. This research has made use of SDSS-III data. Funding for SDSS-III (http://www.sdss3.org/) has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and DoE. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration. This research has made use of the following databases: the NED and IRSA databases, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA; SIMBAD, operated at CDS, Strasbourg, France; SZ cluster database (http://szcluster-db.ias.u-psud.fr) and SZ repository operated by IDOC operated by IAS under contract with CNES and CNRS.\n\nPublished - aa25787-15.pdf
", "abstract": "We update the all-sky Planck catalogue of 1227 clusters and cluster candidates (PSZ1) published in March 2013, derived from detections of the Sunyaev\u2013Zeldovich (SZ) effect using the first 15.5 months of Planck satellite observations. As an addendum, we deliver an updated version of the PSZ1 catalogue, reporting the further confirmation of 86 Planck-discovered clusters. In total, the PSZ1 now contains 947 confirmed clusters, of which 214 were confirmed as newly discovered clusters through follow-up observations undertaken by the Planck Collaboration. The updated PSZ1 contains redshifts for 913 systems, of which 736 (~ 80.6%) are spectroscopic, and associated mass estimates derived from the Y_z mass proxy. We also provide a new SZ quality flag for the remaining 280 candidates. This flag was derived from a novel artificial neural-network classification of the SZ signal. Based on this assessment, the purity of the updated PSZ1 catalogue is estimated to be 94%. In this release, we provide the full updated catalogue and an additional readme file with further information on the Planck SZ detections.", "date": "2015-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "581", "publisher": "EDP Sciences", "pagerange": "Art. No. A14", "id_number": "CaltechAUTHORS:20151103-100239624", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151103-100239624", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Ciencia e Innovacion (MICINN)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Red Espa\u00f1ola de Supercomputaci\u00f3n (RES)" }, { "agency": "Tekes (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "PRACE (EU)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national du patrimoine (INP)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201525787", "primary_object": { "basename": "aa25787-15.pdf", "url": "https://authors.library.caltech.edu/records/73pad-r5x14/files/aa25787-15.pdf" }, "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/e91z1-dhv08", "eprint_id": 61087, "eprint_status": "archive", "datestamp": "2023-08-20 07:49:56", "lastmod": "2023-10-24 23:23:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: Current Cosmic Infrared Background Estimates Can Be Explained by Known Galaxies and Their Faint Companions at z < 4", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 galaxies: evolution \u2013 infrared: galaxies \u2013 large-scale structure of universe \u2013 submillimeter: galaxies", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 May 22; accepted 2015 July 24; published 2015 August 17.\n\nM.P.V. warmly thanks Charlotte Clarke, Pete Hurley, Seb Oliver, and the University of Sussex for their hospitality during the development of this study, and Phil Hopkins for valuable discussions of the z > 4 universe. We also thank the anonymous referee, whose careful comments greatly improved this paper. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The SPIRE data for this paper were obtained as a part of proposal KPGT_soliver_1, with images made using the following OBSIDs: 1342222819-26, 1342222846-54, 1342222879-80, 1342222897-901.\n\nPublished - Viero_2015.pdf
Submitted - 1505.06242v2.pdf
", "abstract": "We report contributions to cosmic infrared background (CIB) intensities originating from known galaxies and their faint companions at submillimeter wavelengths. Using the publicly available UltraVISTA catalog and maps at 250, 350, and 500 \u03bcm from the Herschel Multi-tiered Extragalactic Survey, we perform a novel measurement that exploits the fact that uncataloged sources may bias stacked flux densities\u2014particularly if the resolution of the image is poor\u2014and intentionally smooth the images before stacking and summing intensities. By smoothing the maps we are capturing the contribution of faint (undetected in K_S ~ 23.4) sources that are physically associated, or correlated, with the detected sources. We find that the cumulative CIB increases with increased smoothing, reaching 9.82 \u00b1 0.78, 5.77 \u00b1 0.43 and 2.32 \u00b1 0.19 nWm^(-2) sr^(-1) at 250, 350, and 500 \u03bcm at 300 arscec FWHM. This corresponds to a fraction of the fiducial CIB of 0.94 \u00b1 0.23, 1.07 \u00b1 0.31, and 0.97 \u00b1 0.26 at 250, 350, and 500 \u03bcm, where the uncertainties are dominated by those of the absolute CIB. We then propose, with a simple model combining parametric descriptions for stacked flux densities and stellar mass functions, that emission from galaxies with log(M/M\u2299) > 8.5 can account for most of the measured total intensities and argue against contributions from extended, diffuse emission. Finally, we discuss prospects for future survey instruments to improve the estimates of the absolute CIB levels, and observe any potentially remaining emission at z > 4.", "date": "2015-08-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "809", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L22", "id_number": "CaltechAUTHORS:20151013-152701423", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151013-152701423", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories of China" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1088/2041-8205/809/2/L22", "primary_object": { "basename": "1505.06242v2.pdf", "url": "https://authors.library.caltech.edu/records/e91z1-dhv08/files/1505.06242v2.pdf" }, "related_objects": [ { "basename": "Viero_2015.pdf", "url": "https://authors.library.caltech.edu/records/e91z1-dhv08/files/Viero_2015.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Viero, M. P.; Moncelsi, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/0n4f5-18q51", "eprint_id": 71221, "eprint_status": "archive", "datestamp": "2023-08-22 15:51:43", "lastmod": "2023-10-23 15:30:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Spangelo-S-C", "name": { "family": "Spangelo", "given": "Sara C." } }, { "id": "Katti-R-M", "name": { "family": "Katti", "given": "Raj M." } }, { "id": "Unwin-S-C", "name": { "family": "Unwin", "given": "Stephen C." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "Jamie J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "All-sky survey mission observing scenario strategy", "ispublished": "pub", "full_text_status": "public", "keywords": "all-sky survey; observing strategy; scheduling; SPHEREx", "note": "\u00a9 2015 Society of Photo-Optical Instrumentation Engineers (SPIE). \n\nReceived Nov. 3, 2014; accepted for publication Jul. 6, 2015; published online Aug. 7, 2015. \n\nThe authors acknowledge Olivier Dore, Timothy Kock, Kirk Breitenbach, Hemali Vyas, Dustin Crumb, and Anthony Pullen for their contributions. Part of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.\n\nPublished - JATIS_1_3_037001.pdf
", "abstract": "This paper develops an observing strategy for space missions performing all-sky surveys, where a single spacecraft maps the celestial sphere subject to realistic constraints. The strategy is flexible, accommodates targeted observations of specific areas of the sky, and achieves the desired trade-off between survey goals. This paper focuses on missions operating in low Earth orbit with interactive and dynamic thermal and stray-light constraints due to the Sun, Earth, and Moon. The approach is applicable to broader mission classes, such as those that operate in different orbits or that survey the Earth. First, the instrument and spacecraft configuration is optimized to enable visibility of the targeted observations throughout the year. Second, a constraint-based strategy is presented for scheduling the observations throughout the year subject to a simplified subset of the constraints. Third, a heuristic-based scheduling algorithm is developed to assign the all-sky observations over short planning horizons. The constraint-based approach guarantees solution feasibility. The approach is applied to the proposed SPHEREx mission, which includes coverage of the north and south celestial poles, galactic plane, and a uniform coverage all-sky survey that maps the entire celestial sphere twice per year. Visualizations demonstrate how the all-sky survey achieves its redundancy requirements over time.", "date": "2015-07", "date_type": "published", "publication": "Journal of Astronomical Telescopes, Instruments, and Systems", "volume": "1", "number": "3", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "pagerange": "Art. No. 037001", "id_number": "CaltechAUTHORS:20161018-105132302", "issn": "2329-4124", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161018-105132302", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1117/1.JATIS.1.3.037001", "primary_object": { "basename": "JATIS_1_3_037001.pdf", "url": "https://authors.library.caltech.edu/records/0n4f5-18q51/files/JATIS_1_3_037001.pdf" }, "resource_type": "article", "pub_year": "2015", "author_list": "Spangelo, Sara C.; Katti, Raj M.; et el." }, { "id": "https://authors.library.caltech.edu/records/9qejz-3wk07", "eprint_id": 59168, "eprint_status": "archive", "datestamp": "2023-08-22 15:44:25", "lastmod": "2023-10-23 20:08:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hui-Howard", "name": { "family": "Hui", "given": "H." } }, { "id": "Kefeli-S", "name": { "family": "Kefeli", "given": "S." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "BICEP2/Keck Array. IV. Optical Characterization and Performance of the BICEP2 and Keck Array Experiments", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization", "note": "\u00a9 2015 American Astronomical Society. \n\nReceived 2015 February 3; accepted 2015 April 24; published 2015 June 18. \n\nBICEP2 was supported by the National Science Foundation (NSF) under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). The Keck Array was supported by the NSF under grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota), and ANT-1145248 (Stanford), and by the W. M. Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Computations presented in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard. The analysis effort at Stanford and SLAC was partially supported by the U.S. Department of Energy Office of Science. The receiver development was supported in part by a grant from the W. M. Keck Foundation. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. We thank the staff of the US Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. Most special thanks go to our heroic winter-overs Robert Schwarz and Steffen Richter. We thank all those who have contributed past efforts to the BICEP/Keck Array series of experiments, including the BICEP1-team, as well as our colleagues on the SPIDER team with whom we coordinated receiver and detector development efforts at Caltech.\n\nPublished - 0004-637X_806_2_206.pdf
Submitted - 1502.00596v2.pdf
", "abstract": "bicep2 and the Keck Array are polarization-sensitive microwave telescopes that observe the cosmic microwave background (CMB) from the South Pole at degree angular scales in search of a signature of inflation imprinted as B-mode polarization in the CMB. bicep2 was deployed in late 2009, observed for three years until the end of 2012 at 150 GHz with 512 antenna-coupled transition edge sensor bolometers, and has reported a detection of B-mode polarization on degree angular scales. The Keck Array was first deployed in late 2010 and will observe through 2016 with five receivers at several frequencies (95, 150, and 220 GHz). bicep2 and the Keck Array share a common optical design and employ the field-proven bicep1 strategy of using small-aperture, cold, on-axis refractive optics, providing excellent control of systematics while maintaining a large field of view. This design allows for full characterization of far-field optical performance using microwave sources on the ground. Here we describe the optical design of both instruments and report a full characterization of the optical performance and beams of bicep2 and the Keck Array at 150 GHz.", "date": "2015-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "806", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 206", "id_number": "CaltechAUTHORS:20150804-084849060", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150804-084849060", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT-1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "corp_creators": { "items": [ "BICEP2 Collaboration", "KECK ARRAY Collaborations" ] }, "doi": "10.1088/0004-637X/806/2/206", "primary_object": { "basename": "0004-637X_806_2_206.pdf", "url": "https://authors.library.caltech.edu/records/9qejz-3wk07/files/0004-637X_806_2_206.pdf" }, "related_objects": [ { "basename": "1502.00596v2.pdf", "url": "https://authors.library.caltech.edu/records/9qejz-3wk07/files/1502.00596v2.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/nqkdn-k5r69", "eprint_id": 58985, "eprint_status": "archive", "datestamp": "2023-08-20 06:52:11", "lastmod": "2023-10-23 19:56:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Arai-T", "name": { "family": "Arai", "given": "T." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Kim-M-G", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Lanz-A", "name": { "family": "Lanz", "given": "A." } }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Lee-H-M", "name": { "family": "Lee", "given": "H. M." } }, { "id": "Sano-K", "name": { "family": "Sano", "given": "K." } }, { "id": "Smidt-J", "name": { "family": "Smidt", "given": "J." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Nakagawa-Takao", "name": { "family": "Nakagawa", "given": "T." } }, { "id": "Onishi-Yosuke", "name": { "family": "Onishi", "given": "Y." } }, { "id": "Korngut-P-M", "name": { "family": "Korngut", "given": "P." } }, { "id": "Shirahata-Mai", "name": { "family": "Shirahata", "given": "M." } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Measurements of the Mean Diffuse Galactic Light Spectrum in the 0.95\u20131.65 \u03bcm Band from CIBER", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction \u2013 ISM: general \u2013 scattering", "note": "\u00a9 2015 The American Astronomical Society.\n\nReceived 2015 February 24; accepted 2015 April 6; published 2015 June 9.\n\nThis work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. CIBER was supported by KAKENHI (2034, 18204018, 19540250, 21340047, 21111004, and 26800112) from the Japan Society for the Promotion of Science (JSPS), and the Ministry of Education, Culture, Sports, Science, and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from the Korea Astronomy and Space Science Institute (KASI). We would like to acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range. P. K. and M.Z. acknowledge support from a NASA Postdoctoral Fellowship, A.C. acknowledges support from an NSF CAREER award, and T.A. acknowledges support from the JSPS Research Fellowship for Young Scientists. A.C. acknowledges support from an NSF CAREER award AST-0645427 and NSF AST-1313319. H.M.L acknowledges support from grant 2012R1A4A1028713. We thank T.D. Brandt for kindly providing data and models.\n\nPublished - 0004-637X_806_1_69.pdf
Submitted - 1503.04926v2.pdf
", "abstract": "We report measurements of the diffuse galactic light (DGL) spectrum in the near-infrared, spanning the wavelength range 0.95\u20131.65 \u03bcm by the Cosmic Infrared Background ExpeRiment. Using the low-resolution spectrometer calibrated for absolute spectro-photometry, we acquired long-slit spectral images of the total diffuse sky brightness toward six high-latitude fields spread over four sounding rocket flights. To separate the DGL spectrum from the total sky brightness, we correlated the spectral images with a 100 \u03bcm intensity map, which traces the dust column density in optically thin regions. The measured DGL spectrum shows no resolved features and is consistent with other DGL measurements in the optical and at near-infrared wavelengths longer than 1.8 \u03bcm. Our result implies that the continuum is consistently reproduced by models of scattered starlight in the Rayleigh scattering regime with a few large grains.", "date": "2015-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "806", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 69", "id_number": "CaltechAUTHORS:20150722-134424163", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150722-134424163", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "JPL Director's Research and Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "2034" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "26800112" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "National Research Foundation of Korea", "grant_number": "2012R1A4A1028713" } ] }, "doi": "10.1088/0004-637X/806/1/69", "primary_object": { "basename": "0004-637X_806_1_69.pdf", "url": "https://authors.library.caltech.edu/records/nqkdn-k5r69/files/0004-637X_806_1_69.pdf" }, "related_objects": [ { "basename": "1503.04926v2.pdf", "url": "https://authors.library.caltech.edu/records/nqkdn-k5r69/files/1503.04926v2.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Arai, T.; Matsuura, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/bdpxz-qvr82", "eprint_id": 58649, "eprint_status": "archive", "datestamp": "2023-09-15 05:03:38", "lastmod": "2023-10-23 21:13:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "Lingyu" } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco" } }, { "id": "Ross-N-P", "name": { "family": "Ross", "given": "Nicholas P." }, "orcid": "0000-0003-1830-6473" }, { "id": "Asboth-V", "name": { "family": "Asboth", "given": "Viktoria" } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "Matthieu" }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "Jamie" }, "orcid": "0000-0002-5710-5212" }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "Dave" }, "orcid": "0000-0002-9548-5033" }, { "id": "Conley-A", "name": { "family": "Conley", "given": "Alex" } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "Duncan" }, "orcid": "0000-0003-1748-2010" }, { "id": "Hajian-A", "name": { "family": "Hajian", "given": "Amir" } }, { "id": "Han-Jiaxin", "name": { "family": "Han", "given": "Jiaxin" }, "orcid": "0000-0002-8010-6715" }, { "id": "Lagache-Guilaine", "name": { "family": "Lagache", "given": "Guilaine" }, "orcid": "0000-0003-1492-2519" }, { "id": "Marsden-G", "name": { "family": "Marsden", "given": "Gaelen" } }, { "id": "Myers-A", "name": { "family": "Myers", "given": "Adam" } }, { "id": "Norberg-P", "name": { "family": "Norberg", "given": "Peder" }, "orcid": "0000-0002-5875-0440" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "Sebastian" }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "Mat" }, "orcid": "0000-0002-6689-6271" }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "Myrto" } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "Bernhard" } }, { "id": "Wang-Wenting", "name": { "family": "Wang", "given": "Wenting" } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Mike" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Co-evolution of black hole growth and star formation from a\n cross-correlation analysis between quasars and the cosmic infrared background", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: haloes; galaxies: high-redshift; quasars: general; submillimetre: galaxies", "note": "\u00a9 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2015 March 11. Received 2015 March 9; in original form 2014 June 20. First published online April 14, 2015.\n\nLW and PN acknowledge support from an ERC StG grant (DEGAS-\n259586). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese\nMonbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is\nhttp://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical\nInstitute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group,\nthe German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University,\nNew York University, Ohio State University, Pennsylvania\nState University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University.\n\nPublished - MNRAS-2015-Wang-4476-93.pdf
Submitted - 1406.7181v1.pdf
", "abstract": "We present the first cross-correlation measurement between Sloan Digital Sky Survey type 1 quasars and the cosmic infrared background (CIB) measured by Herschel. The quasars cover the redshift range 0.15 < z < 3.5 where most of the CIB originates. We detect the sub-millimetre emission of the quasars, which dominates on small scales, and correlated emission from dusty star-forming galaxies (DSFGs) dominant on larger scales. The mean flux of the Data Release 7 (DR7) quasars (median redshift \u3008z\u3009 = 1.4) is 11.1, 7.1 and 3.6 mJy at 250, 350 and 500 \u03bcm, respectively, while the mean flux of the DR9 quasars (\u3008z\u3009 = 2.5) is 5.7, 5.0 and 1.8 mJy at 250, 350 and 500 \u03bcm, respectively. Assuming a modified blackbody spectral energy distribution with a power law in the mid-infrared, we infer that the mean infrared luminosity of the DR7 and DR9 quasars is 10^(12.4) and 10^(12.8)\u2009L_\u2299, respectively. The correlated emission arises from DSFGs in the same halo as the quasar (the one-halo term) and DSFGs in separate haloes correlated with the quasar-hosting halo (the two-halo term). Using a simple halo model, we find that most quasars are hosted by central galaxies. The host halo mass scale of the DR7 central and satellite quasars is 10^(12.4 \u00b1 0.9) and 10^(13.6 \u00b1 0.4) M_\u2299, respectively. The host halo mass scale of the DR9 central and satellite quasars is 10^(12.3 \u00b1 0.6) and 10^(12.8 \u00b1 0.4) M_\u2299, respectively. Thus, the halo environment of the central quasars is similar to that of the most actively star-forming galaxies, which supports the view that dusty starburst and quasar activity are evolutionarily linked.", "date": "2015-06-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "449", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "4476-4493", "id_number": "CaltechAUTHORS:20150629-075947984", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150629-075947984", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "DEGAS-259586" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" } ] }, "doi": "10.1093/mnras/stv559", "primary_object": { "basename": "1406.7181v1.pdf", "url": "https://authors.library.caltech.edu/records/bdpxz-qvr82/files/1406.7181v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2015-Wang-4476-93.pdf", "url": "https://authors.library.caltech.edu/records/bdpxz-qvr82/files/MNRAS-2015-Wang-4476-93.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Wang, Lingyu; Viero, Marco; et el." }, { "id": "https://authors.library.caltech.edu/records/9wvj8-b8a66", "eprint_id": 59384, "eprint_status": "archive", "datestamp": "2023-08-20 05:39:40", "lastmod": "2023-10-23 20:32:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust", "ispublished": "pub", "full_text_status": "public", "keywords": "ISM: general \u2013 dust, extinction \u2013 ISM: magnetic fields \u2013 ISM: clouds \u2013 submillimeter: ISM", "note": "\u00a9 2015 ESO. Article published by EDP Sciences. \n\nReceived 28 April 2014; Accepted 30 January 2015; Published online 13 April 2015. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/M CTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ ERC grant agreement no 267934 and from a joint agreement between University of S\u00e3o Paulo, Brazil, and COFECUB, France (grant nos. USP 2007.1.433.14.2 and COFECUB Uc Te 114/08). We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC). HEASARC/LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa24082-14.pdf
Submitted - 1405.0871v1.pdf
", "abstract": "This paper presents an overview of the polarized sky as seen by Planck HFI at 353 GHz, which is the most sensitive Planck channel for dust polarization. We construct and analyse maps of dust polarization fraction and polarization angle at 1\u00b0 resolution, taking into account noise bias and possible systematic effects. The sensitivity of the Planck HFI polarization measurements allows for the first time a mapping of Galactic dust polarized emission on large scales, including low column density regions. We find that the maximum observed dust polarization fraction is high (p_(max) = 19.8%), in particular in some regions of moderate hydrogen column density (N_H < 2 \u00d7 10^(21) cm^(-2)). The polarization fraction displays a large scatter at N_H below a few 10^(21) cm^(-2). There is a general decrease in the dust polarization fraction with increasing column density above N_H \u2243 1 \u00d7 10^(21) cm-2 and in particular a sharp drop above N_H \u2243 1.5 \u00d7 10^(22) cm^(-2). We characterize the spatial structure of the polarization angle using the angle dispersion function. We find that the polarization angle is ordered over extended areas of several square degrees, separated by filamentary structures of high angle dispersion function. These appear as interfaces where the sky projection of the magnetic field changes abruptly without variations in the column density. The polarization fraction is found to be anti-correlated with the dispersion of polarization angles. These results suggest that, at the resolution of 1\u00b0, depolarization is due mainly to fluctuations in the magnetic field orientation along the line of sight, rather than to the loss of grain alignment in shielded regions. We also compare the polarization of thermal dust emission with that of synchrotron measured with Planck, low-frequency radio data, and Faraday rotation measurements toward extragalactic sources. These components bear resemblance along the Galactic plane and in some regions such as the Fan and North Polar Spur regions. The poor match observed in other regions shows, however, that dust, cosmic-ray electrons, and thermal electrons generally sample different parts of the line of sight.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A104", "id_number": "CaltechAUTHORS:20150811-094459251", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150811-094459251", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "University of S\u00e3o Paulo", "grant_number": "USP 2007.1.433.14.2" }, { "agency": "COFECUB", "grant_number": "Uc Te 114/08" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424082", "primary_object": { "basename": "aa24082-14.pdf", "url": "https://authors.library.caltech.edu/records/9wvj8-b8a66/files/aa24082-14.pdf" }, "related_objects": [ { "basename": "1405.0871v1.pdf", "url": "https://authors.library.caltech.edu/records/9wvj8-b8a66/files/1405.0871v1.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/nmk5g-1gd96", "eprint_id": 96862, "eprint_status": "archive", "datestamp": "2023-08-20 05:43:04", "lastmod": "2023-10-20 21:34:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Beichman-C-A", "name": { "family": "Beichman", "given": "C." }, "orcid": "0000-0002-5627-5471" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 dust, extinction \u2013 ISM: clouds \u2013 ISM: magnetic fields \u2013 submillimeter: ISM", "note": "\u00a9 2015 ESO. Article published by EDP Sciences.\n\nReceived 28 April 2014; Accepted 3 December 2014; Published online 13 April 2015.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007\u22122013) / ERC grant agreement No. 267934. This research has made use of the SIMBAD database and the VizieR catalogue access tool, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System Service.\n\nPublished - aa24087-14.pdf
Submitted - 1405.0873.pdf
", "abstract": "The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust. In addition to the information on the direction of the Galactic magnetic field, this also brings new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the visible. Comparison of the polarization of the emission and of the interstellar polarization on selected lines of sight probed by stars provides unique new diagnostics of the emission and light scattering properties of dust, and therefore of the important dust model parameters, composition, size, and shape. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, p_V, and the optical depth in the V band to the star, \u03c4_V. Toward these stars we measure the submillimetre polarized intensity, P_S, and total intensity, I_S, in the Planck 353\u2009GHz channel. We compare the column density measure in the visible, E(B \u2212 V), with that inferred from the Planck product map of the submillimetre dust optical depth and compare the polarization direction (position angle) in the visible with that in the submillimetre. For those lines of sight through the diffuse interstellar medium with comparable values of the estimated column density and polarization directions close to orthogonal, we correlate properties in the submillimetre and visible to find two ratios, R_(S/V) = (P_S/I_S) / (p_V/\u03c4_V) and R_(P/p) = P_S/p_V, the latter focusing directly on the polarization properties of the aligned grain population alone. We find R_(S /V) = 4.2, with statistical and systematic uncertainties 0.2 and 0.3, respectively, and R_(P/p) = 5.4 MJy sr^(-1), with uncertainties 0.2 and 0.3 MJy sr^(-1), respectively. Our estimate of R_(S/V) is compatible with predictions based on a range of polarizing dust models that have been developed for the diffuse interstellar medium. This estimate provides new empirical validation of many of the common underlying assumptions of the models, but is not yet very discriminating among them. However, our estimate of R_(P/p) is not compatible with predictions, which are too low by a factor of about 2.5. This more discriminating diagnostic, R_(P/p), indicates that changes to the optical properties in the models of the aligned grain population are required. These new diagnostics, together with the spectral dependence in the submillimetre from Planck, will be important for constraining and understanding the full complexity of the grain models, and for interpreting the Planck thermal dust polarization and refinement of the separation of this contamination of the cosmic microwave background.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A106", "id_number": "CaltechAUTHORS:20190701-110759480", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-110759480", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424087", "primary_object": { "basename": "1405.0873.pdf", "url": "https://authors.library.caltech.edu/records/nmk5g-1gd96/files/1405.0873.pdf" }, "related_objects": [ { "basename": "aa24087-14.pdf", "url": "https://authors.library.caltech.edu/records/nmk5g-1gd96/files/aa24087-14.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/ac7wy-khp84", "eprint_id": 96863, "eprint_status": "archive", "datestamp": "2023-08-20 05:43:11", "lastmod": "2023-10-20 21:34:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results. XXII. Frequency dependence of thermal\u2009emission\u2009from\u2009Galactic\u2009dust\u2009in\u2009intensity and polarization", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 ISM: general \u2013 Galaxy: general \u2013 radiation mechanisms: general \u2013 submillimeter: ISM \u2013 infrared: ISM", "note": "\u00a9 2015 ESO. Article published by EDP Sciences.\n\nReceived 28 April 2014; Accepted 9 December 2014; Published online 13 April 2015.\n\nThe Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and J.A. (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A detailed description of the Planck Collaboration and a list of its members can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC). HEASARC/LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa24088-14.pdf
Accepted Version - 1405.0874.pdf
", "abstract": "Planck has mapped the intensity and polarization of the sky at microwave frequencies with unprecedented sensitivity. We use these data to characterize the frequency dependence of dust emission. We make use of the Planck 353\u2009GHz I, Q, and U Stokes maps as dust templates, and cross-correlate them with the Planck and WMAP data at 12 frequencies from 23 to 353\u2009GHz, over circular patches with 10\u00b0 radius. The cross-correlation analysis is performed for both intensity and polarization data in a consistent manner. The results are corrected for the chance correlation between the templates and the anisotropies of the cosmic microwave background. We use a mask that focuses our analysis on the diffuse interstellar medium at intermediate Galactic latitudes. We determine the spectral indices of dust emission in intensity and polarization between 100 and 353\u2009GHz, for each sky patch. Both indices are found to be remarkably constant over the sky. The mean values, 1.59 \u00b1 0.02 for polarization and 1.51 \u00b1 0.01 for intensity, for a mean dust temperature of 19.6\u2009K, are close, but significantly different (3.6\u03c3). We determine the mean spectral energy distribution (SED) of the microwave emission, correlated with the 353\u2009GHz dust templates, by averaging the results of the correlation over all sky patches. We find that the mean SED increases for decreasing frequencies at \u03bd< 60\u2009GHz for both intensity and polarization. The rise of the polarization SED towards low frequencies may be accounted for by a synchrotron component correlated with dust, with no need for any polarization of the anomalous microwave emission. We use a spectral model to separate the synchrotron and dust polarization and to characterize the spectral dependence of the dust polarization fraction. The polarization fraction (p) of the dust emission decreases by (21 \u00b1 6)% from 353 to 70 GHz. We discuss this result within the context of existing dust models. The decrease in p could indicate differences in polarization efficiency among components of interstellar dust (e.g., carbon versus silicate grains). Our observational results provide inputs to quantify and optimize the separation between Galactic and cosmological polarization.", "date": "2015-04", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "576", "publisher": "EDP Sciences", "pagerange": "Art. No. A107", "id_number": "CaltechAUTHORS:20190701-112037165", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-112037165", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Distributed European Infrastructure for Supercomputing Applications (DEISA)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201424088", "primary_object": { "basename": "aa24088-14.pdf", "url": "https://authors.library.caltech.edu/records/ac7wy-khp84/files/aa24088-14.pdf" }, "related_objects": [ { "basename": "1405.0874.pdf", "url": "https://authors.library.caltech.edu/records/ac7wy-khp84/files/1405.0874.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Dor\u00e9, O.; et el." }, { "id": "https://authors.library.caltech.edu/records/bv7yz-e4e53", "eprint_id": 54466, "eprint_status": "archive", "datestamp": "2023-08-20 05:21:24", "lastmod": "2023-10-20 16:30:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-Peter-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Ahmed-Z", "name": { "family": "Ahmed", "given": "Z." } }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Alexander-Kate-D", "name": { "family": "Alexander", "given": "K. 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E." } }, { "id": "Tomasi-M", "name": { "family": "Tomasi", "given": "M." } }, { "id": "Tristram-M", "name": { "family": "Tristram", "given": "M." } }, { "id": "Tucci-M", "name": { "family": "Tucci", "given": "M." } }, { "id": "Turner-A-D", "name": { "family": "Turner", "given": "A. D." } }, { "id": "Valenziano-L", "name": { "family": "Valenziano", "given": "L." } }, { "id": "Valiviita-J", "name": { "family": "Valiviita", "given": "J." } }, { "id": "Van-Tent-B", "name": { "family": "Van Tent", "given": "B." } }, { "id": "Vibert-L", "name": { "family": "Vibert", "given": "L." } }, { "id": "Vielva-P", "name": { "family": "Vielva", "given": "P." } }, { "id": "Vieregg-A-G", "name": { "family": "Vieregg", "given": "A. G." } }, { "id": "Villa-F", "name": { "family": "Villa", "given": "F." } }, { "id": "Wade-L-A", "name": { "family": "Wade", "given": "L. A." } }, { "id": "Wandelt-Benjamin-D", "name": { "family": "Wandelt", "given": "B. D." }, "orcid": "0000-0002-5854-8269" }, { "id": "Watson-R", "name": { "family": "Watson", "given": "R." } }, { "id": "Weber-A-C", "name": { "family": "Weber", "given": "A. C." } }, { "id": "Wehus-I-K", "name": { "family": "Wehus", "given": "I. K." } }, { "id": "White-M", "name": { "family": "White", "given": "M." } }, { "id": "White-S-D-M", "name": { "family": "White", "given": "S. D. M." } }, { "id": "Willmert-J", "name": { "family": "Willmert", "given": "J." } }, { "id": "Wong-C-L", "name": { "family": "Wong", "given": "C. L." } }, { "id": "Yoon-K-W", "name": { "family": "Yoon", "given": "K. W." } }, { "id": "Yvon-D", "name": { "family": "Yvon", "given": "D." } }, { "id": "Zacchei-A", "name": { "family": "Zacchei", "given": "A." } }, { "id": "Zonca-A", "name": { "family": "Zonca", "given": "A." } } ] }, "title": "A Joint Analysis of BICEP2/Keck Array and Planck Data", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2015 American Physical Society. \n\n(Received 21 January 2015; published 9 March 2015) \n\nBICEP2 was supported by the U.S. National Science Foundation under Grants No. ANT-0742818 and No. ANT-1044978 (Caltech and Harvard) and No. ANT-0742592 and No. ANT-1110087 (Chicago and Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The Keck Array project was supported by the National Science Foundation under Grants No. ANT-1145172 (Harvard), No. ANT-1145143 (Minnesota) and No. ANT-1145248 (Stanford), and from the Keck Foundation (Caltech). We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. The Planck Collaboration acknowledges the support of the following: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found in Ref. [52].\n\nPublished - PhysRevLett.114.101301.pdf
Submitted - 1502.00612v1.pdf
", "abstract": "We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400\u2009\u2009deg2 patch of sky centered on RA 0 h, Dec. \u221257.5\u00b0. The combined maps reach a depth of 57 nK deg in Stokes Q and U in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2\u2009\u2009\u03bcK deg in Q and U at 143 GHz). We detect 150\u00d7353 cross-correlation in B modes at high significance. We fit the single- and cross-frequency power spectra at frequencies \u2265150\u2009\u2009GHz to a lensed-\u039bCDM model that includes dust and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r), using a prior on the frequency spectral behavior of polarized dust emission from previous Planck analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the r constraint. Finally, we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for r, and yields an upper limit r0.05<0.12 at 95% confidence. Marginalizing over dust and r, lensing B modes are detected at 7.0\u03c3 significance.", "date": "2015-03-09", "date_type": "published", "publication": "Physical Review Letters", "volume": "114", "number": "10", "publisher": "American Physical Society", "pagerange": "Art. No. 101301", "id_number": "CaltechAUTHORS:20150205-194356590", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150205-194356590", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT- 1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "NSF", "grant_number": "ANT-1145172" }, { "agency": "NSF", "grant_number": "ANT-1145143" }, { "agency": "NSF", "grant_number": "ANT-1145248" }, { "agency": "W. M. Keck Foundation" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "CSIC and RES (Spain)" }, { "agency": "Tekes and CSC (Finland)" }, { "agency": "Deutschen Zentrums f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "PRACE (EU)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Academy of Finland" }, { "agency": "European Research Council (ERC)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration", "BICEP2 Collaboration" ] }, "doi": "10.1103/PhysRevLett.114.101301", "primary_object": { "basename": "1502.00612v1.pdf", "url": "https://authors.library.caltech.edu/records/bv7yz-e4e53/files/1502.00612v1.pdf" }, "related_objects": [ { "basename": "PhysRevLett.114.101301.pdf", "url": "https://authors.library.caltech.edu/records/bv7yz-e4e53/files/PhysRevLett.114.101301.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Ade, P. A. R.; Aghanim, N.; et el." }, { "id": "https://authors.library.caltech.edu/records/gxw3z-v5994", "eprint_id": 55835, "eprint_status": "archive", "datestamp": "2023-08-20 04:25:12", "lastmod": "2023-10-20 23:16:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Valtchanov-I", "name": { "family": "Valtchanov", "given": "I." }, "orcid": "0000-0001-9930-7886" }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Bertoldi-F", "name": { "family": "Bertoldi", "given": "F." }, "orcid": "0000-0002-1707-1775" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Ibar-E", "name": { "family": "Ibar", "given": "E." } }, { "id": "Karim-A", "name": { "family": "Karim", "given": "A." }, "orcid": "0000-0002-8414-9579" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Nordon-R", "name": { "family": "Nordon", "given": "R." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M." }, "orcid": "0000-0002-6689-6271" }, { "id": "Pozzi-F", "name": { "family": "Pozzi", "given": "F." } }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Rodighiero-G", "name": { "family": "Rodighiero", "given": "G." }, "orcid": "0000-0002-9415-2296" }, { "id": "Rosario-D", "name": { "family": "Rosario", "given": "D." } }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I." } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Wuyts-S", "name": { "family": "Wuyts", "given": "S." } } ] }, "title": "The far-infrared/radio correlation and radio spectral index of galaxies in the SFR\u2013M_\u2217 plane up to z \u223c 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: formation, galaxies: starburst galaxies: high-redshift, infrared: galaxies", "note": "\u00a9 2014 ESO. Received: 6 September 2014. Accepted: 21 October 2014. Published online 15 December 2014. \n\nWe thank the anonymous referee for suggestions which greatly enhanced this work. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA\n(USA). Support for BM was provided by the DFG priority programme 1573 The physics of the interstellar medium. R.J.I. acknowledges support from the European Research Council in the form of Advanced Grant, cosmicism. E.I. acknowledges funding from CONICYT/FONDECYT postdoctoral project N\u25e6:3130504. F.B. and A.K. acknowledge support by the Collaborative Research Council 956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft (DFG).\n\nPublished - aa24937-14.pdf
Submitted - 1410.7412v1.pdf
", "abstract": "We study the evolution of the radio spectral index and far-infrared/radio correlation (FRC) across the star-formation rate \u2013 stellar masse (i.e. SFR\u2013M_\u2217) plane up to z ~ 2. We start from a stellar-mass-selected sample of galaxies with reliable SFR and redshift estimates. We then grid the SFR\u2013M_\u2217 plane in several redshift ranges and measure the infrared luminosity, radio luminosity, radio spectral index, and ultimately the FRC index (i.e. q_(FIR)) of each SFR\u2013M_\u2217\u2013z bin. The infrared luminosities of our SFR\u2013M_\u2217\u2013z bins are estimated using their stacked far-infrared flux densities inferred from observations obtained with the Herschel Space Observatory. Their radio luminosities and radio spectral indices (i.e. \u03b1, where S_\u03bd \u221d \u03bd^(\u2212\u03b1)) are estimated using their stacked 1.4 GHz and 610 MHz flux densities from the Very Large Array and Giant Metre-wave Radio Telescope, respectively. Our far-infrared and radio observations include the most widely studied blank extragalactic fields \u2013 GOODS-N, GOODS-S, ECDFS, and COSMOS \u2013 covering a total sky area of ~2.0\u2009deg^2. Using this methodology, we constrain the radio spectral index and FRC index of star-forming galaxies with M_\u2217 > 10^(10) M_\u2299 and 0", "date": "2015-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "573", "publisher": "EDP Sciences", "pagerange": "Art. No. A45", "id_number": "CaltechAUTHORS:20150317-091500633", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150317-091500633", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)" }, { "agency": "European Research Council (ERC)", "grant_number": "COSMICISM" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3130504" }, { "agency": "Commissariat \u00e0 l'\u00e9nergie atomique (CEA)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" } ] }, "doi": "10.1051/0004-6361/201424937", "primary_object": { "basename": "1410.7412v1.pdf", "url": "https://authors.library.caltech.edu/records/gxw3z-v5994/files/1410.7412v1.pdf" }, "related_objects": [ { "basename": "aa24937-14.pdf", "url": "https://authors.library.caltech.edu/records/gxw3z-v5994/files/aa24937-14.pdf" } ], "resource_type": "article", "pub_year": "2015", "author_list": "Magnelli, B.; Ivison, R. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/nmsv1-0kk43", "eprint_id": 53001, "eprint_status": "archive", "datestamp": "2023-08-20 04:05:59", "lastmod": "2023-10-18 21:52:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "Michael" } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "Lingyu" } }, { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "Julie" }, "orcid": "0000-0003-2376-8971" }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "Duncan" }, "orcid": "0000-0003-1748-2010" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "Seb" }, "orcid": "0000-0001-7862-1032" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "Jamie" }, "orcid": "0000-0002-5710-5212" }, { "id": "Clarke-C", "name": { "family": "Clarke", "given": "Charlotte" } }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "David" }, "orcid": "0000-0002-9548-5033" }, { "id": "Ibar-E", "name": { "family": "Ibar", "given": "Edo" } }, { "id": "Gonzalez-Solares-E", "name": { "family": "Gonzalez-Solares", "given": "Eduardo" } }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "Lucia" }, "orcid": "0000-0003-3948-7621" }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Smith-A-J", "name": { "family": "Smith", "given": "Anthony J." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "Mattia" }, "orcid": "0000-0002-6748-0577" }, { "id": "Valtchanov-I", "name": { "family": "Valtchanov", "given": "Ivan" }, "orcid": "0000-0001-9930-7886" } ] }, "title": "Detailed modelling of a large sample of Herschel sources in the Lockman Hole: identification of cold dust and of lensing candidates through their anomalous SEDs", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: strong, galaxies: evolution, galaxies: starburst, cosmology: observations, infrared: galaxies, submillimetre: galaxies", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 September 18. Received 2014 September 17; in original form 2014 May 6. First published online October 31, 2014.\n\nSPIRE has been developed by a consortium of institutes\nled by Cardiff Univ. (UK) and including Univ. Lethbridge\n(Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua\n(Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). The Dark Cosmology Centre (JW) is funded by the Danish National Research Foundation.\nThe data presented in this paper are available through the\nHerschel Database in Marseille HeDaM.3 SJO acknowledges support from the Science and Technology Facilities Council (grant numbers ST/L000652/1) and from the European Commission Research Executive Agency REA (Grant Agreement Number 607254). EI acknowledges funding from CONICYT/FONDECYT postdoctoral project no.: 3130504.\n\nPublished - 3848.full.pdf
Submitted - 1409.5136v1.pdf
Supplemental Material - MRRspireSCATfig.pdf
", "abstract": "We have studied in detail a sample of 967 SPIRE sources with 5\u03c3 detections at 350 and 500\u2009\u03bcm and associations with Spitzer-SWIRE 24\u2009\u03bcm galaxies in the HerMES-Lockman survey area, fitting their mid- and far-infrared, and submillimetre, spectral energy distributions (SEDs) in an automatic search with a set of six infrared templates. For almost 300 galaxies, we have modelled their SEDs individually to ensure the physicality of the fits. We confirm the need for the new cool and cold cirrus templates, and also of the young starburst template, introduced in earlier work. We also identify 109 lensing candidates via their anomalous SEDs and provide a set of colour\u2013redshift constraints which allow lensing candidates to be identified from combined Herschel and Spitzer data. The picture that emerges of the submillimetre galaxy population is complex, comprising ultraluminous and hyperluminous starbursts, lower luminosity galaxies dominated by interstellar dust emission, lensed galaxies and galaxies with surprisingly cold (10\u201313\u2009K) dust. 11\u2009per\u2009cent of 500\u2009\u03bcm selected sources are lensing candidates. 70\u2009per\u2009cent of the unlensed sources are ultraluminous infrared galaxies and 26\u2009per\u2009cent are hyperluminous. 34\u2009per\u2009cent are dominated by optically thin interstellar dust ('cirrus') emission, but most of these are due to cooler dust than is characteristic of our Galaxy. At the highest infrared luminosities we see SEDs dominated by M82, Arp 220 and young starburst types, in roughly equal proportions.", "date": "2014-12-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "445", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3848-3861", "id_number": "CaltechAUTHORS:20141218-082850497", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141218-082850497", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA" }, { "agency": "Danish National Research Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/L000652/1" }, { "agency": "European Commission Research Executive Agency REA", "grant_number": "607254" }, { "agency": "Fondo Nacional de Desarrollo Cient\u00edfico y Tecnol\u00f3gico (FONDECYT)", "grant_number": "3130504" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "doi": "10.1093/mnras/stu1959", "primary_object": { "basename": "1409.5136v1.pdf", "url": "https://authors.library.caltech.edu/records/nmsv1-0kk43/files/1409.5136v1.pdf" }, "related_objects": [ { "basename": "3848.full.pdf", "url": "https://authors.library.caltech.edu/records/nmsv1-0kk43/files/3848.full.pdf" }, { "basename": "MRRspireSCATfig.pdf", "url": "https://authors.library.caltech.edu/records/nmsv1-0kk43/files/MRRspireSCATfig.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Rowan-Robinson, Michael; Wang, Lingyu; et el." }, { "id": "https://authors.library.caltech.edu/records/drfb3-fwe29", "eprint_id": 53790, "eprint_status": "archive", "datestamp": "2023-08-22 14:32:09", "lastmod": "2023-10-19 22:13:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Calanog-J-A", "name": { "family": "Calanog", "given": "J. A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "Lens Models of Herschel-selected Galaxies from High-resolution Near-IR Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: star formation; gravitational lensing: strong; submillimeter: galaxies", "note": "\u00a9 2014 American Astronomical Society. Received 2014 June 5; accepted 2014 October 20; published 2014 December 8.\n\nWe thank the anonymous referee and Ian Smail for their\nthoughtful feedback and insightful comments that improved\nthe paper. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\nSupport for programs GO-12194 and GO-12488 was provided\nby NASA through a grant from the Space Telescope Science\nInstitute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS Web site is http://www.h-atlas.org/. This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist.\nThe data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES/). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\nJ.A.C., A.C., B.M., C.M.C., J.M.O., N.T., and C.T. acknowledge support from NSF AST-1313319. M.N. acknowledges financial support from ASI/INAF agreement I/072/09/0 and from PRIN-INAF 2012 project Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astro-physical Large Area Survey. L.D., S.J.M., and R.J.I. acknowledge support from the European Research Council (ERC) in the form of Advanced Investigator program, COSMICISM. This work was supported in part by the National Science Foundation under grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the\nUniversity of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing\nCARMA development and operations are supported by the\nNational Science Foundation under a cooperative agreement,\nand by the CARMA partner universities. The Sub-millimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The Dark Cosmology Centre is funded by the Danish National Research Foundation (DNRF).\n\nPublished - 0004-637X_797_2_138.pdf
Submitted - 1406.1487v2.pdf
", "abstract": "We present Keck-Adaptive Optics and Hubble Space Telescope high resolution near-infrared (IR) imaging for 500 \u00b5m bright candidate lensing systems identified by the Herschel Multi-tiered Extragalactic Survey and Herschel Astrophysical Terahertz Large Area Survey. Out of 87 candidates with near-IR imaging, 15 (~17%) display clear near-IR lensing morphologies. We present near-IR lens models to reconstruct and recover basic rest-frame optical morphological properties of the background galaxies from 12 new systems. Sources with the largest near-IR magnification factors also tend to be the most compact, consistent with the size bias predicted from simulations and previous lensing models for submillimeter galaxies (SMGs). For four new sources that also have high-resolution submillimeter maps, we test for differential lensing between the stellar and dust components and find that the 880 \u00b5m magnification factor (\u00b5_(880)) is ~1.5 times higher than the near-IR magnification factor (\u00b5_(NIR)), on average. We also find that the stellar emission is ~2 times more extended in size than dust. The rest-frame optical properties of our sample of Herschel-selected lensed SMGs are consistent with those of unlensed SMGs, which suggests that the two populations are similar.", "date": "2014-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "797", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 138", "id_number": "CaltechAUTHORS:20150115-125936396", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150115-125936396", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/072/09/0" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "European Research Council (ERC)" }, { "agency": "NSF", "grant_number": "PHYS-1066293" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Caltech Associates" }, { "agency": "University of Chicago" }, { "agency": "State of California" }, { "agency": "State of Illinois" }, { "agency": "State of Maryland" }, { "agency": "NSF" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Smithsonian Institution" }, { "agency": "Academia Sinica" }, { "agency": "Danish National Research Foundation" }, { "agency": "United Kingdom Space Agency (UKSA)" } ] }, "doi": "10.1088/0004-637X/797/2/138", "primary_object": { "basename": "0004-637X_797_2_138.pdf", "url": "https://authors.library.caltech.edu/records/drfb3-fwe29/files/0004-637X_797_2_138.pdf" }, "related_objects": [ { "basename": "1406.1487v2.pdf", "url": "https://authors.library.caltech.edu/records/drfb3-fwe29/files/1406.1487v2.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Calanog, J. A.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/a2qz6-ky869", "eprint_id": 52222, "eprint_status": "archive", "datestamp": "2023-08-22 14:15:45", "lastmod": "2023-10-18 19:40:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gralla-M-B", "name": { "family": "Gralla", "given": "Megan B." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael B." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "A measurement of the millimetre emission and the Sunyaev\u2013Zel'dovich effect associated with low-frequency radio sources", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: haloes; galaxies: statistics; radio continuum: galaxies", "note": "\u00a9 2014 The Authors.\nPublished by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 August 4. Received 2014 August 4; in original form 2013 October 30.\nFirst published online September 29, 2014.\n\nThis work was supported by the US National Science Foundation through awards AST-0408698 and AST-0965625 for the ACT project, as well as awards PHY-0855887 and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astron\u00f3mico Atacama in northern Chile under the auspices of the Comisi\u00f3n Nacional de Investigaci\u00f3n Cient\u00edfica y Tecnol\u00f3gica de Chile (CONICYT). Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund \u2013 Research Excellence; and the University of Toronto. MBG and TAM acknowledge support from Johns Hopkins University. RD, PA, FR and GM received funding from the Chilean grants FONDECYT 11100147 and BASAL (CATA). This research made use of ASTROPY, a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013).\n\nPublished - MNRAS-2014-Gralla-460-78.pdf
Submitted - 1310.8281v2.pdf
", "abstract": "We present a statistical analysis of the millimetre-wavelength properties of 1.4\u2009GHz-selected sources and a detection of the Sunyaev\u2013Zel'dovich (SZ) effect associated with the haloes that host them. We stack data at 148, 218 and 277\u2009GHz from the Atacama Cosmology Telescope at the positions of a large sample of radio AGN selected at 1.4\u2009GHz. The thermal SZ effect associated with the haloes that host the AGN is detected at the 5\u03c3 level through its spectral signature, representing a statistical detection of the SZ effect in some of the lowest mass haloes (average M_(200) \u2248 10^(13) M\u2299 h^(\u22121)_(70) studied to date. The relation between the SZ effect and mass (based on weak lensing measurements of radio galaxies) is consistent with that measured by Planck for local bright galaxies. In the context of galaxy evolution models, this study confirms that galaxies with radio AGN also typically support hot gaseous haloes. Adding Herschel observations allows us to show that the SZ signal is not significantly contaminated by dust emission. Finally, we analyse the contribution of radio sources to the angular power spectrum of the cosmic microwave background.", "date": "2014-11-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "445", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "460-478", "id_number": "CaltechAUTHORS:20141201-110542030", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141201-110542030", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0408698" }, { "agency": "NSF", "grant_number": "AST-0965625" }, { "agency": "NSF", "grant_number": "PHY-0855887" }, { "agency": "NSF", "grant_number": "PHY-1214379" }, { "agency": "Princeton University" }, { "agency": "University of Pennsylvania" }, { "agency": "Canada Foundation for Innovation (CFI)" }, { "agency": "Johns Hopkins University" }, { "agency": "FONDECYT", "grant_number": "11100147" }, { "agency": "BASAL Center for Astrophysics and Associated Technologies (CATA)" } ] }, "doi": "10.1093/mnras/stu1592", "primary_object": { "basename": "1310.8281v2.pdf", "url": "https://authors.library.caltech.edu/records/a2qz6-ky869/files/1310.8281v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Gralla-460-78.pdf", "url": "https://authors.library.caltech.edu/records/a2qz6-ky869/files/MNRAS-2014-Gralla-460-78.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Gralla, Megan B.; Bock, James; et el." }, { "id": "https://authors.library.caltech.edu/records/6g8rc-6xc34", "eprint_id": 52624, "eprint_status": "archive", "datestamp": "2023-08-22 14:15:11", "lastmod": "2023-10-18 21:02:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "Georgios E." }, "orcid": "0000-0002-4872-2294" }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Hopwood-R", "name": { "family": "Hopwood", "given": "R." } }, { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J.-S." } }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Pearson-C-P", "name": { "family": "Pearson", "given": "C." }, "orcid": "0000-0001-6139-649X" }, { "id": "Alonso-Herrera-A", "name": { "family": "Alonso-Herrera", "given": "Almudena" }, "orcid": "0000-0001-6794-2519" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "D." }, "orcid": "0000-0002-9548-5033" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Griffin-M-J", "name": { "family": "Griffin", "given": "M. J." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "I." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Swinyard-B-M", "name": { "family": "Swinyard", "given": "B. M." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Thatte-N", "name": { "family": "Thatte", "given": "N." } }, { "id": "Valtchanov-I", "name": { "family": "Valtchanov", "given": "I." }, "orcid": "0000-0001-9930-7886" }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" } ] }, "title": "A Far-Infrared Spectroscopic Survey of Intermediate Redshift (Ultra) Luminous Infrared Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: star formation; gamma rays: ISM; infrared: galaxies; infrared: general", "note": "\u00a9 2014 American Astronomical Society. Received 2014 June 18; accepted 2014 September 16; published 2014 November 5.\n\nWe warmly thank the referee for constructive comments and\nsuggestions. G.E.M. and D.R. acknowledge support from STFC\nthrough grant ST/K00106X/1. G.E.M. acknowledges support\nfrom the John Fell Oxford University Press (OUP) Research\nFund and the University of Oxford. A.A.-H. acknowledges\nfunding through the Universidad de Cantabria August G. Linares Programme. This work includes observations made with IRAM, which is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). Based on observations made with ESO Telescopes at the APEX Observatory under programme ID\n090.B-0708A and 091.B-0312A. This paper uses data from\nHerschel's photometer SPIRE. SPIRE has been developed by\na consortium of institutes led by Cardiff University (UK) and including: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA).\n\nPublished - 0004-637X_796_1_63.pdf
Submitted - 1409.5605v1.pdf
", "abstract": "We present Herschel far-IR photometry and spectroscopy as well as ground-based CO observations of an intermediate redshift (0.21 \u2264 z \u2264 0.88) sample of Herschel-selected (ultra)-luminous infrared galaxies (L_(IR) > 10^(11.5) L_\u2609). With these measurements, we trace the dust continuum, far-IR atomic line emission, in particular [C II] 157.7 \u03bcm, as well as the molecular gas of z ~ 0.3 luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) and perform a detailed investigation of the interstellar medium of the population. We find that the majority of Herschel-selected intermediate redshift (U)LIRGs have L_(CII)/L_(FIR) ratios that are a factor of about 10 higher than that of local ULIRGs and comparable to that of local normal and high-z star-forming galaxies. Using our sample to bridge local and high-z [C II] observations, we find that the majority of galaxies at all redshifts and all luminosities follow an L_(CII) \u2013L_(FIR) relation with a slope of unity, from which local ULIRGs and high- z active-galactic-nucleus-dominated sources are clear outliers. We also confirm that the strong anti-correlation between the L_(CII)/L_(FIR) ratio and the far-IR color L_0/L_(100) observed in the local universe holds over a broad range of redshifts and luminosities, in the sense that warmer sources exhibit lower L_(CII)/L_(FIR) at any epoch. Intermediate redshift ULIRGs are also characterized by large molecular gas reservoirs and by lower star formation efficiencies compared to that of local ULIRGs. The high L_(CII)/L_(FIR) ratios, the moderate star formation efficiencies (L_(IR)/L'_(CO) or L_(IR/M_(H_2), and the relatively low dust temperatures of our sample (which are also common characteristics of high-z star-forming galaxies with ULIRG-like luminosities) indicate that the evolution of the physical properties of (U)LIRGs between the present day and z > 1 is already significant by z ~ 0.3.", "date": "2014-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "796", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 63", "id_number": "CaltechAUTHORS:20141212-102043065", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141212-102043065", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K00106X/1" }, { "agency": "University of Oxford John Fell Oxford University Press (OUP) Research Fund" }, { "agency": "Universidad de Cantabria August G. Linares Programme" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" } ] }, "doi": "10.1088/0004-637X/796/1/63", "primary_object": { "basename": "0004-637X_796_1_63.pdf", "url": "https://authors.library.caltech.edu/records/6g8rc-6xc34/files/0004-637X_796_1_63.pdf" }, "related_objects": [ { "basename": "1409.5605v1.pdf", "url": "https://authors.library.caltech.edu/records/6g8rc-6xc34/files/1409.5605v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Magdis, Georgios E.; Rigopoulou, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/sycsy-0ab45", "eprint_id": 51370, "eprint_status": "archive", "datestamp": "2023-08-20 03:38:20", "lastmod": "2023-10-20 23:17:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" }, { "id": "Smidt-J", "name": { "family": "Smidt", "given": "Joseph" } }, { "id": "Arai-Toshiaki", "name": { "family": "Arai", "given": "Toshiaki" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Gong-Yan", "name": { "family": "Gong", "given": "Yan" } }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "Min Gyu" } }, { "id": "Korngut-P", "name": { "family": "Korngut", "given": "Phillip" } }, { "id": "Lam-Anson", "name": { "family": "Lam", "given": "Anson" } }, { "id": "Lee-Dae-Hee", "name": { "family": "Lee", "given": "Dae Hee" } }, { "id": "Matsumoto-Toshio", "name": { "family": "Matsumoto", "given": "Toshio" }, "orcid": "0000-0001-6066-5221" }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "Shuji" }, "orcid": "0000-0002-5698-9634" }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "Uk Won" } }, { "id": "Roudier-G", "name": { "family": "Roudier", "given": "Gael" } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "Kohji" } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "Takehiko" } } ] }, "title": "On the origin of near-infrared extragalactic background light anisotropy", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 American Association for the Advancement of Science. \n\n1 July 2014; accepted 3 October 2014.\n\nOur thanks to O. Dor\u00e9, J. Filippini, and K. Ganga for useful\nconversations and comments throughout the course of this work and K. Helgason for kindly providing models of the statistics of the near-infrared CIB. The authors acknowledge the excellent support from the\nNASA sounding rockets program that was essential in developing, testing, qualifying, launching, and recovering our payloads. The CIBER auto- and cross-power spectra are available for public download at http://ciber.caltech.edu/zemcovetal. This work was supported by\nNASA APRA research grants NNX07AI54G, NNG05WC18G,\nNNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was\nprovided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. Japanese participation in CIBER was supported by KAKENHI (20\u00b734, 18204018, 19540250, 21340047, and 21111004) from Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports,\nScience and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from Korea Astronomy and Space Science Institute (KASI). M.Z. and P.K. acknowledge support from NASA Postdoctoral Program fellowships, A.C. acknowledges support\nfrom an NSF CAREER award AST-0645427 and NSF AST-1313319, and K.T. acknowledges support from the JSPS Research Fellowship for Young Scientists. This publication makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the\nUniversity of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work made use of images and/or data products provided by the National Optical Astronomy Observatory (NOAO) Deep Wide-Field Survey (NDWFS), which is supported by NOAO, operated by AURA, Inc., under a cooperative agreement with the\nNational Science Foundation.\n\nSubmitted - 1411.1411v1.pdf
Supplemental Material - Zemcov.SM.pdf
", "abstract": "Extragalactic background light (EBL) anisotropy traces variations in the total production of photons over cosmic history and may contain faint, extended components missed in galaxy point-source surveys. Infrared EBL fluctuations have been attributed to primordial galaxies and black holes at the epoch of reionization (EOR) or, alternately, intrahalo light (IHL) from stars tidally stripped from their parent galaxies at low redshift. We report new EBL anisotropy measurements from a specialized sounding rocket experiment at 1.1 and 1.6 micrometers. The observed fluctuations exceed the amplitude from known galaxy populations, are inconsistent with EOR galaxies and black holes, and are largely explained by IHL emission. The measured fluctuations are associated with an EBL intensity that is comparable to the background from known galaxies measured through number counts and therefore a substantial contribution to the energy contained in photons in the cosmos.", "date": "2014-11-07", "date_type": "published", "publication": "Science", "volume": "346", "number": "6210", "publisher": "American Association for the Advancement of Science", "pagerange": "732-735", "id_number": "CaltechAUTHORS:20141106-112913256", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141106-112913256", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07A154G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NSF", "grant_number": "AST-1313319" } ] }, "doi": "10.1126/science.1258168", "primary_object": { "basename": "1411.1411v1.pdf", "url": "https://authors.library.caltech.edu/records/sycsy-0ab45/files/1411.1411v1.pdf" }, "related_objects": [ { "basename": "Zemcov.SM.pdf", "url": "https://authors.library.caltech.edu/records/sycsy-0ab45/files/Zemcov.SM.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Zemcov, Michael; Smidt, Joseph; et el." }, { "id": "https://authors.library.caltech.edu/records/jj0c8-yb582", "eprint_id": 52039, "eprint_status": "archive", "datestamp": "2023-08-20 03:36:09", "lastmod": "2023-10-18 19:17:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Clarke-C", "name": { "family": "Clarke", "given": "C." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Guo-K", "name": { "family": "Guo", "given": "K." } }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S." } }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G." }, "orcid": "0000-0002-4872-2294" }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Marsden-G", "name": { "family": "Marsden", "given": "G." } }, { "id": "Norberg-P", "name": { "family": "Norberg", "given": "P." }, "orcid": "0000-0002-5875-0440" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "Roehlly-Y", "name": { "family": "Roehlly", "given": "Y." } }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Smith-A-J", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: point source catalogues from Herschel-SPIRE observations II", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical\n techniques: photometric\n catalogues\n surveys\n infrared: galaxies\n submillimetre: galaxies", "note": "\u00a9 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2014 August 1. Received 2014 August 1. In original form 2013 December 12. First published online September 15, 2014.\n\nLWis supported by UK's Science and Technology Facilities Council grant ST/F002858/1 and an ERC StG grant (DEGAS-259586). The data presented in this paperwill be released through the HeDaM (hedam.lam.fr/HerMES). SPIRE has been developed by a Consortium of Institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).\n\nPublished - MNRAS-2014-Wang-2870-83.pdf
Submitted - 1312.0552v1.pdf
", "abstract": "The Herschel Multi-tiered Extragalactic Survey (HerMES) is the largest Guaranteed Time Key Programme on the Herschel Space Observatory. With a wedding cake survey strategy, it consists of nested fields with varying depth and area totalling \u223c380 deg^2. In this paper, we present deep point source catalogues extracted from Herschel-Spectral and Photometric Imaging Receiver (SPIRE) observations of all HerMES fields, except for the later addition of the 270 deg^2 HerMES Large-Mode Survey (HeLMS) field. These catalogues constitute the second Data Release (DR2) made in 2013 October. A sub-set of these catalogues, which consists of bright sources extracted from Herschel-SPIRE observations completed by 2010 May\u20091 (covering \u223c74 deg^2) were released earlier in the first extensive data release in 2012 March. Two different methods are used to generate the point source catalogues, the sussextractor point source extractor used in two earlier data releases (EDR and EDR2) and a new source detection and photometry method. The latter combines an iterative source detection algorithm, starfinder, and a De-blended SPIRE Photometry algorithm. We use end-to-end Herschel-SPIRE simulations with realistic number counts and clustering properties to characterize basic properties of the point source catalogues, such as the completeness, reliability, photometric and positional accuracy. Over 500 000 catalogue entries in HerMES fields (except HeLMS) are released to the public through the HeDAM (Herschel Database in Marseille) website (http://hedam.lam.fr/HerMES).", "date": "2014-11-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "444", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2870-2883", "id_number": "CaltechAUTHORS:20141121-102020063", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141121-102020063", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "European Research Council (ERC)", "grant_number": "DEGAS-259586" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" } ] }, "doi": "10.1093/mnras/stu1569", "primary_object": { "basename": "1312.0552v1.pdf", "url": "https://authors.library.caltech.edu/records/jj0c8-yb582/files/1312.0552v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Wang-2870-83.pdf", "url": "https://authors.library.caltech.edu/records/jj0c8-yb582/files/MNRAS-2014-Wang-2870-83.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Wang, L.; Viero, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/76tne-hae05", "eprint_id": 96852, "eprint_status": "archive", "datestamp": "2023-08-20 03:34:43", "lastmod": "2023-10-20 21:34:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Matsumura-Tomotake", "name": { "family": "Matsumura", "given": "T." } }, { "id": "Mei-Simona", "name": { "family": "Mei", "given": "S." }, "orcid": "0000-0002-2849-559X" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. I. Overview of products and scientific results", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmic background radiation \u2013 space vehicles: instruments \u2013 instrumentation: detectors", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 21 March 2013; Accepted 17 May 2014; Published online 29 October 2014.\n\nPlanck is too large a project to allow full acknowledgement of all contributions by individuals, institutions, industries, and funding agencies. The main entities involved in the mission operations are as follows. The European Space Agency operates the satellite via its Mission Operations Centre located at ESOC (Darmstadt, Germany) and coordinates scientific operations via the Planck Science Office located at ESAC (Madrid, Spain). Two Consortia, comprising around 100 scientific institutes within Europe, the USA, and Canada, and funded by agencies from the participating countries, developed the scientific instruments LFI and HFI, and continue to operate them via Instrument Operations Teams located in Trieste (Italy) and Orsay (France). The Consortia are also responsible for scientific processing of the acquired data. The Consortia are led by the Principal Investigators: J.-L. Puget in France for HFI (funded principally by CNES and CNRS/INSU-IN2P3) and N. Mandolesi in Italy for LFI (funded principally via ASI). NASA's UK Planck Project, based at JPL and involving scientists at many UK institutions, contributes significantly to the efforts of these two Consortia. A third Consortium, led by H. U. Norgaard-Nielsen and supported by the Danish Natural Research Council, contributed to the reflector programme. The author list for this paper has been selected by the Planck Science Team from the Planck Collaboration, and is composed of individuals from all of the above entities who have made multi-year contributions to the development of the mission. It does not pretend to be inclusive of all contributions to Planck. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at (http://www.rssd.esa.int/index.php?project=PLANCK& page=Planck_ Collaboration). The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, and JA (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).\n\nPublished - aa21529-13.pdf
Submitted - 1303.5062.pdf
", "abstract": "The European Space Agency's Planck satellite, dedicated to studying the early Universe and its subsequent evolution, was launched 14 May 2009 and has been scanning the microwave and submillimetre sky continuously since 12 August 2009. In March 2013, ESA and the Planck Collaboration released the initial cosmology products based on the first 15.5\u2009months of Planck data, along with a set of scientific and technical papers and a web-based explanatory supplement. This paper gives an overview of the mission and its performance, the processing, analysis, and characteristics of the data, the scientific results, and the science data products and papers in the release. The science products include maps of the cosmic microwave background (CMB) and diffuse extragalactic foregrounds, a catalogue of compact Galactic and extragalactic sources, and a list of sources detected through the Sunyaev-Zeldovich effect. The likelihood code used to assess cosmological models against the Planck data and a lensing likelihood are described. Scientific results include robust support for the standard six-parameter \u039bCDM model of cosmology and improved measurements of its parameters, including a highly significant deviation from scale invariance of the primordial power spectrum. The Planck values for these parameters and others derived from them are significantly different from those previously determined. Several large-scale anomalies in the temperature distribution of the CMB, first detected by WMAP, are confirmed with higher confidence. Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at greater than 25\u03c3. Planck finds no evidence for non-Gaussianity in the CMB. Planck's results agree well with results from the measurements of baryon acoustic oscillations. Planck finds a lower Hubble constant than found in some more local measures. Some tension is also present between the amplitude of matter fluctuations (\u03c38) derived from CMB data and that derived from Sunyaev-Zeldovich data. The Planck and WMAP power spectra are offset from each other by an average level of about 2% around the first acoustic peak. Analysis of Planck polarization data is not yet mature, therefore polarization results are not released, although the robust detection of E-mode polarization around CMB hot and cold spots is shown graphically.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A1", "id_number": "CaltechAUTHORS:20190701-084039975", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-084039975", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321529", "primary_object": { "basename": "1303.5062.pdf", "url": "https://authors.library.caltech.edu/records/76tne-hae05/files/1303.5062.pdf" }, "related_objects": [ { "basename": "aa21529-13.pdf", "url": "https://authors.library.caltech.edu/records/76tne-hae05/files/aa21529-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/s33jy-jpn50", "eprint_id": 96853, "eprint_status": "archive", "datestamp": "2023-08-20 03:34:53", "lastmod": "2023-10-20 21:34:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. VI. High Frequency Instrument data processing", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis \u2013 cosmic background radiation \u2013 cosmology: observations \u2013 surveys", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 26 March 2013; Accepted 22 July 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration.\n\nPublished - aa21570-13.pdf
Accepted Version - 1303.5067.pdf
", "abstract": "We describe the processing of the 531 billion raw data samples from the High Frequency Instrument (HFI), which we performed to produce six temperature maps from the first 473 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545, and 857GHz with an angular resolution ranging from 9.\u03017 to 4.\u03016. The detector noise per (effective) beam solid angle is respectively, 10, 6 , 12, and 39\u2009\u03bcK in the four lowest HFI frequency channels (100\u2212353GHz) and 13 and 14\u2009kJy sr^(-1) in the 545 and 857\u2009GHz channels. Relative to the 143\u2009GHz channel, these two high frequency channels are calibrated to within 5% and the 353\u2009GHz channel to the percent level. The 100 and 217\u2009GHz channels, which together with the 143\u2009GHz channel determine the high-multipole part of the CMB power spectrum (50 <\u2113 < 2500), are calibrated relative to 143\u2009GHz to better than 0.2%.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A6", "id_number": "CaltechAUTHORS:20190701-085818699", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-085818699", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321570", "primary_object": { "basename": "1303.5067.pdf", "url": "https://authors.library.caltech.edu/records/s33jy-jpn50/files/1303.5067.pdf" }, "related_objects": [ { "basename": "aa21570-13.pdf", "url": "https://authors.library.caltech.edu/records/s33jy-jpn50/files/aa21570-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/rm1w3-fgf92", "eprint_id": 96851, "eprint_status": "archive", "datestamp": "2023-08-20 03:34:34", "lastmod": "2023-10-20 21:34:11", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. VIII. HFI photometric calibration and mapmaking", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 surveys \u2013 methods: data analysis", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 21 March 2013; Accepted 8 March 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members with the technical or scientific activities they have been involved into, can be found at http://www.rssd.esa.int/index.php?project=PLANCK&page=PlanckCollaboration.\n\nPublished - aa21538-13.pdf
Submitted - 1303.5069.pdf
", "abstract": "This paper describes the methods used to produce photometrically calibrated maps from the Planck High Frequency Instrument (HFI) cleaned, time-ordered information. HFI observes the sky over a broad range of frequencies, from 100 to 857\u2009\u2009GHz. To obtain the best calibration accuracy over such a large range, two different photometric calibration schemes have to be used. The 545 and 857\u2009GHz data are calibrated by comparing flux-density measurements of Uranus and Neptune with models of their atmospheric emission. The lower frequencies (below 353\u2009\u2009GHz) are calibrated using the solar dipole. A component of this anisotropy is time-variable, owing to the orbital motion of the satellite in the solar system. Photometric calibration is thus tightly linked to mapmaking, which also addresses low-frequency noise removal. By comparing observations taken more than one year apart in the same configuration, we have identified apparent gain variations with time. These variations are induced by non-linearities in the read-out electronics chain. We have developed an effective correction to limit their effect on calibration. We present several methods to estimate the precision of the photometric calibration. We distinguish relative uncertainties (between detectors, or between frequencies) and absolute uncertainties. Absolute uncertainties lie in the range from 0.54% to 10% from 100 to 857\u2009\u2009GHz. We describe the pipeline used to produce the maps from the HFI timelines, based on the photometric calibration parameters, and the scheme used to set the zero level of the maps a posteriori. We also discuss the cross-calibration between HFI and the SPIRE instrument on board Herschel. Finally we summarize the basic characteristics of the set of HFI maps included in the 2013 Planck data release.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A8", "id_number": "CaltechAUTHORS:20190701-075622398", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-075622398", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321538", "primary_object": { "basename": "1303.5069.pdf", "url": "https://authors.library.caltech.edu/records/rm1w3-fgf92/files/1303.5069.pdf" }, "related_objects": [ { "basename": "aa21538-13.pdf", "url": "https://authors.library.caltech.edu/records/rm1w3-fgf92/files/aa21538-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/265xd-cxd57", "eprint_id": 96859, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:43", "lastmod": "2023-10-20 21:34:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Abergel-A", "name": { "family": "Abergel", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XI. All-sky model of thermal dust emission", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis \u2013 ISM: general \u2013 dust, extinction \u2013 infrared: ISM \u2013 submillimeter: ISM \u2013 opacity", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 4 December 2013; Accepted 4 September 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbuk agakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa23195-13.pdf
Accepted Version - 1312.1300.pdf
", "abstract": "This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857\u2009GHz, and IRAS 100 \u03bcm data. Using a modified blackbody fit to the data we present all-sky maps of the dust optical depth, temperature, and spectral index over the 353\u20133000\u2009GHz range. This model is a good representation of the IRAS and Planck data at 5\u2032 between 353 and 3000\u2009GHz (850 and 100 \u03bcm). It shows variations of the order of 30% compared with the widely-used model of Finkbeiner, Davis, and Schlegel. The Planck data allow us to estimate the dust temperature uniformly over the whole sky, down to an angular resolution of 5\u2032, providing an improved estimate of the dust optical depth compared to previous all-sky dust model, especially in high-contrast molecular regions where the dust temperature varies strongly at small scales in response to dust evolution, extinction, and/or local production of heating photons. An increase of the dust opacity at 353\u2009GHz, \u03c4_(353)/N_H, from the diffuse to the denser interstellar medium (ISM) is reported. It is associated with a decrease in the observed dust temperature, T_(obs), that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H\u2009I column densities lower than 10^(20)\u2009cm^(-2) that could be the signature of dust in the warm ionized medium. In the diffuse ISM at high Galactic latitude, we report an anticorrelation between \u03c4_(353)/N_H and T_(obs) while the dust specific luminosity, i.e., the total dust emission integrated over frequency (the radiance) per hydrogen atom, stays about constant, confirming one of the Planck Early Results obtained on selected fields. This effect is compatible with the view that, in the diffuse ISM, T_(obs) responds to spatial variations of the dust opacity, due to variations of dust properties, in addition to (small) variations of the radiation field strength. The implication is that in the diffuse high-latitude ISM \u03c4_(353) is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of \u03c4_(353) with dust extinction estimated using colour excess measurements on stars is strong. To estimate Galactic E(B\u2212 V) in extragalactic fields at high latitude we develop a new method based on the thermal dust radiance, instead of the dust optical depth, calibrated to E(B \u2212 V) using reddening measurements of quasars deduced from Sloan Digital Sky Survey data.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A11", "id_number": "CaltechAUTHORS:20190701-102824126", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-102824126", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" }, { "agency": "European Research Council (ERC)", "grant_number": "267934" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Participating Institutions" }, { "agency": "NSF" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Higher Education Funding Council for England" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201323195", "primary_object": { "basename": "1312.1300.pdf", "url": "https://authors.library.caltech.edu/records/265xd-cxd57/files/1312.1300.pdf" }, "related_objects": [ { "basename": "aa23195-13.pdf", "url": "https://authors.library.caltech.edu/records/265xd-cxd57/files/aa23195-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Abergel, A.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/qmf7j-v0192", "eprint_id": 96854, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:02", "lastmod": "2023-10-20 21:34:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R. R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XII. Diffuse component separation", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 26 March 2013; Accepted 18 December 2013; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. The authors acknowledge the support provided by the Advanced Computing and e-Science team at IFCA. This work made use of the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa21580-13.pdf
Submitted - 1303.5072.pdf
", "abstract": "Planck has produced detailed all-sky observations over nine frequency bands between 30 and 857 GHz. These observations allow robust reconstruction of the primordial cosmic microwave background (CMB) temperature fluctuations over nearly the full sky, as well as new constraints on Galactic foregrounds, including thermal dust and line emission from molecular carbon monoxide (CO). This paper describes the component separation framework adopted by Planck for many cosmological analyses, including CMB power spectrum determination and likelihood construction on large angular scales, studies of primordial non-Gaussianity and statistical isotropy, the integrated Sachs-Wolfe effect, gravitational lensing, and searches for topological defects. We test four foreground-cleaned CMB maps derived using qualitatively different component separation algorithms. The quality of our reconstructions is evaluated through detailed simulations and internal comparisons, and shown through various tests to be internally consistent and robust for CMB power spectrum and cosmological parameter estimation up to \u2113 = 2000. The parameter constraints on \u039bCDM cosmologies derived from these maps are consistent with those presented in the cross-spectrum based Planck likelihood analysis. We choose two of the CMB maps for specific scientific goals. We also present maps and frequency spectra of the Galactic low-frequency, CO, and thermal dust emission. The component maps are found to provide a faithful representation of the sky, as evaluated by simulations, with the largest bias seen in the CO component at 3%. For the low-frequency component, the spectral index varies widely over the sky, ranging from about \u03b2 = \u22124 to \u2212 2. Considering both morphology and prior knowledge of the low frequencycomponents, the index map allows us to associate a steep spectral index (\u03b2< \u22123.2) with strong anomalous microwave emission, corresponding to a spinning dust spectrum peaking below 20 GHz, a flat index of \u03b2> \u22122.3 with strong free-free emission, and intermediate values with synchrotron emission.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A12", "id_number": "CaltechAUTHORS:20190701-091146023", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-091146023", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321580", "primary_object": { "basename": "1303.5072.pdf", "url": "https://authors.library.caltech.edu/records/qmf7j-v0192/files/1303.5072.pdf" }, "related_objects": [ { "basename": "aa21580-13.pdf", "url": "https://authors.library.caltech.edu/records/qmf7j-v0192/files/aa21580-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/f0k4w-rq416", "eprint_id": 96855, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:11", "lastmod": "2023-10-20 21:34:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Chen-Xi-Tracy-IPAC", "name": { "family": "Chen", "given": "X." }, "orcid": "0000-0001-9152-6224" }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XIV. Zodiacal emission", "ispublished": "pub", "full_text_status": "public", "keywords": "zodiacal dust \u2013 interplanetary medium \u2013 cosmic background radiation", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 25 March 2013; Accepted 4 March 2014; Published online 29 October 2014.\n\nThis paper benefited from exchanges with Dale Fixsen, Tom Kelsall and Janet Weiland. We acknowledge the IN2P3 Computer Center (http://cc.in2p3.fr) for providing a significant amount of the computing resources and services needed for this work. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration.\n\nPublished - aa21562-13.pdf
Submitted - 1303.5074.pdf
", "abstract": "The Planck satellite provides a set of all-sky maps at nine frequencies from 30\u2009GHz to 857\u2009GHz. Planets, minor bodies, and diffuse interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through different columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model \u2013 a diffuse cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are different from those in the diffuse cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the cosmic microwave background (CMB) results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small solar system bodies.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A14", "id_number": "CaltechAUTHORS:20190701-092236114", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-092236114", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321562", "primary_object": { "basename": "1303.5074.pdf", "url": "https://authors.library.caltech.edu/records/f0k4w-rq416/files/1303.5074.pdf" }, "related_objects": [ { "basename": "aa21562-13.pdf", "url": "https://authors.library.caltech.edu/records/f0k4w-rq416/files/aa21562-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/a1jcx-ecf68", "eprint_id": 96856, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:20", "lastmod": "2023-10-20 21:34:26", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Paladini-Roberta", "name": { "family": "Paladini", "given": "R." }, "orcid": "0000-0002-5158-243X" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XV. CMB power spectra and likelihood", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmological parameters \u2013 cosmology: observations \u2013 methods: data analysis", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 26 March 2013; Accepted 5 May 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members with the technical or scientific activities they have been involved into, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We acknowledge the use of the CLASS Boltzmann code (Lesgourgues 2011) and the Monte Python package (Audren et al. 2013) in earlier stages of this work. The likelihood code and some of the validation work was built on the library pmclib from the CosmoPMC package (Kilbinger et al. 2011). This research used resources of the IN2P3 Computer Center (http://cc.in2p3.fr) as well as of the Planck-HFI data processing centre infrastructures hosted at the Institut d'Astrophysique de Paris (France) and financially supported by CNES.\n\nPublished - aa21573-13.pdf
Submitted - 1303.5075.pdf
", "abstract": "This paper presents the Planck 2013 likelihood, a complete statistical description of the two-point correlation function of the CMB temperature fluctuations that accounts for all known relevant uncertainties, both instrumental and astrophysical in nature. We use this likelihood to derive our best estimate of the CMB angular power spectrum from Planck over three decades in multipole moment, \u2113, covering 2 \u2264 \u2113 \u2264 2500. The main source of uncertainty at \u2113 \u2272 1500 is cosmic variance. Uncertainties in small-scale foreground modelling and instrumental noise dominate the error budget at higher \u2113s. For \u2113 < 50, our likelihood exploits all Planck frequency channels from 30 to 353 GHz, separating the cosmological CMB signal from diffuse Galactic foregrounds through a physically motivated Bayesian component separation technique. At \u2113 \u2265 50, we employ a correlated Gaussian likelihood approximation based on a fine-grained set of angular cross-spectra derived from multiple detector combinations between the 100, 143, and 217 GHz frequency channels, marginalising over power spectrum foreground templates. We validate our likelihood through an extensive suite of consistency tests, and assess the impact of residual foreground and instrumental uncertainties on the final cosmological parameters. We find good internal agreement among the high-\u2113 cross-spectra with residuals below a few \u03bcK^2 at \u2113 \u2272 1000, in agreement with estimated calibration uncertainties. We compare our results with foreground-cleaned CMB maps derived from all Planck frequencies, as well as with cross-spectra derived from the 70 GHz Planck map, and find broad agreement in terms of spectrum residuals and cosmological parameters. We further show that the best-fit \u039bCDM cosmology is in excellent agreement with preliminary PlanckEE and TE polarisation spectra. We find that the standard \u039bCDM cosmology is well constrained by Planck from the measurements at \u2113 \u2272 1500. One specific example is the spectral index of scalar perturbations, for which we report a 5.4\u03c3 deviation from scale invariance, n_s = 1. Increasing the multipole range beyond \u2113 \u2243 1500 does not increase our accuracy for the \u039bCDM parameters, but instead allows us to study extensions beyond the standard model. We find no indication of significant departures from the \u039bCDM framework. Finally, we report a tension between the Planck best-fit \u039bCDM model and the low-\u2113 spectrum in the form of a power deficit of 5\u201310% at \u2113 \u2272 40, with a statistical significance of 2.5\u20133\u03c3. Without a theoretically motivated model for this power deficit, we do not elaborate further on its cosmological implications, but note that this is our most puzzling finding in an otherwise remarkably consistent data set.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A15", "id_number": "CaltechAUTHORS:20190701-095024014", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-095024014", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321573", "primary_object": { "basename": "1303.5075.pdf", "url": "https://authors.library.caltech.edu/records/a1jcx-ecf68/files/1303.5075.pdf" }, "related_objects": [ { "basename": "aa21573-13.pdf", "url": "https://authors.library.caltech.edu/records/a1jcx-ecf68/files/aa21573-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/zp3n1-aam71", "eprint_id": 96857, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:27", "lastmod": "2023-10-20 21:34:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-M-D", "name": { "family": "Seiffert", "given": "M. D." } }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XXIII. Isotropy and statistics of the CMB", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation \u2013 cosmology: observations \u2013 cosmology: miscellaneous", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 21 March 2013; Accepted 11 January 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We acknowledge the use of resources from the Norewegian national super computing facilities NOTUR. The modal and KSW bispectrum estimator analysis was performed on the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. We further acknowledge the computer resources and technical assistance provided by the Spanish Supercomputing Network nodes at Universidad de Cantabria and Universidad Polit\u00e9cnica de Madrid as well as by the Advanced Computing and e-Science team at IFCA. Some of the results in this paper have been derived using the HEALPix package.\n\nPublished - aa21534-13.pdf
Accepted Version - 1303.5083.pdf
", "abstract": "The two fundamental assumptions of the standard cosmological model \u2013 that the initial fluctuations are statistically isotropic and Gaussian \u2013 are rigorously tested using maps of the cosmic microwave background (CMB) anisotropy from the Planck satellite. The detailed results are based on studies of four independent estimates of the CMB that are compared to simulations using a fiducial \u039bCDM model and incorporating essential aspects of the Planck measurement process. Deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask choice, and frequency dependence. Many of these anomalies were previously observed in the WMAP data, and are now confirmed at similar levels of significance (about 3\u03c3). However, we find little evidence of non-Gaussianity, with the exception of a few statistical signatures that seem to be associated with specific anomalies. In particular, we find that the quadrupole-octopole alignment is also connected to a low observed variance in the CMB signal. A power asymmetry is now found to persist on scales corresponding to about \u2113 = 600 and can be described in the low-\u2113 regime by a phenomenological dipole modulation model. However, any primordial power asymmetry is strongly scale-dependent and does not extend toarbitrarily small angular scales. Finally, it is plausible that some of these features may be reflected in the angular power spectrum of the data, which shows a deficit of power on similar scales. Indeed, when the power spectra of two hemispheres defined by a preferred direction are considered separately, one shows evidence of a deficit in power, while its opposite contains oscillations between odd and even modes that may be related to the parity violation and phase correlations also detected in the data. Although these analyses represent a step forward in building an understanding of the anomalies, a satisfactory explanation based on physically motivated models is still lacking.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A23", "id_number": "CaltechAUTHORS:20190701-100009602", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-100009602", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321534", "primary_object": { "basename": "1303.5083.pdf", "url": "https://authors.library.caltech.edu/records/zp3n1-aam71/files/1303.5083.pdf" }, "related_objects": [ { "basename": "aa21534-13.pdf", "url": "https://authors.library.caltech.edu/records/zp3n1-aam71/files/aa21534-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/fg01x-gs803", "eprint_id": 96858, "eprint_status": "archive", "datestamp": "2023-08-20 03:35:34", "lastmod": "2023-10-20 21:34:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Aghanim-Nabila", "name": { "family": "Aghanim", "given": "N." }, "orcid": "0000-0002-6688-8992" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-Sergi-R", "name": { "family": "Hildebrandt", "given": "S. R." }, "orcid": "0000-0003-0220-0009" }, { "id": "Pr\u00e9zeau-Gary", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-Graca-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Seiffert-Michael-D", "name": { "family": "Seiffert", "given": "M. D." }, "orcid": "0000-0002-7536-9393" }, { "id": "Rusholme-Benjamin", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-Brendan-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck 2013 results. XXVII. Doppler boosting of the CMB: Eppur si muove", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 cosmic background radiation \u2013 reference systems \u2013 relativistic processes", "note": "\u00a9 2014 ESO. Article published by EDP Sciences.\n\nReceived 23 March 2013; Accepted 3 January 2014; Published online 29 October 2014.\n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. Some of the results in this paper have been derived using the HEALPix package. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. We acknowledge support from the Science and Technology Facilities Council [grant number ST/I000976/1].\n\nPublished - aa21556-13.pdf
Accepted Version - 1303.5087.pdf
", "abstract": "Our velocity relative to the rest frame of the cosmic microwave background (CMB) generates a dipole temperature anisotropy on the sky which has been well measured for more than 30 years, and has an accepted amplitude of v/c = 1.23 \u00d7 10^(-3), or v = 369. In addition to this signal generated by Doppler boosting of the CMB monopole, our motion also modulates and aberrates the CMB temperature fluctuations (as well as every other source of radiation at cosmological distances). This is an order 10^(-3) effect applied to fluctuations which are already one part in roughly 10^5, so it is quite small. Nevertheless, it becomes detectable with the all-sky coverage, high angular resolution, and low noise levels of the Planck satellite. Here we report a first measurement of this velocity signature using the aberration and modulation effects on the CMB temperature anisotropies, finding a component in the known dipole direction, (l,b) = (264\u00b0,48\u00b0), of 384 km s^(-1) \u00b1 78 km s^(-1) (stat.) \u00b1 115 km s^(-1) (syst.). This is a significant confirmation of the expected velocity.", "date": "2014-11", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "571", "publisher": "EDP Sciences", "pagerange": "Art. No. A27", "id_number": "CaltechAUTHORS:20190701-101108014", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190701-101108014", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Econom\u00eda, Industria y Competitividad (MINECO)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "Spanish Supercomputing Network (RES)" }, { "agency": "Finnish Ministry of Employment and the Economy" }, { "agency": "Academy of Finland" }, { "agency": "Finnish IT Center for Science (CSC)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "State Secretariat for Education and Research (Switzerland)" }, { "agency": "Swiss Space Office (SSO)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" }, { "agency": "Partnership for Advanced Computing in Europe (PRACE)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321556", "primary_object": { "basename": "aa21556-13.pdf", "url": "https://authors.library.caltech.edu/records/fg01x-gs803/files/aa21556-13.pdf" }, "related_objects": [ { "basename": "1303.5087.pdf", "url": "https://authors.library.caltech.edu/records/fg01x-gs803/files/1303.5087.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Aghanim, N.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/5jb6x-t5j12", "eprint_id": 51457, "eprint_status": "archive", "datestamp": "2023-08-22 13:53:04", "lastmod": "2023-10-18 16:44:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Georgakakis-A", "name": { "family": "Georgakakis", "given": "A." } }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bonzini-M", "name": { "family": "Bonzini", "given": "M." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Ibar-E", "name": { "family": "Ibar", "given": "E." } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G." }, "orcid": "0000-0002-4872-2294" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Pannella-M", "name": { "family": "Pannella", "given": "M." } }, { "id": "Paolillo-M", "name": { "family": "Paolillo", "given": "M." }, "orcid": "0000-0003-4210-7693" }, { "id": "Rosario-D", "name": { "family": "Rosario", "given": "D." } }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Villforth-C", "name": { "family": "Villforth", "given": "C." } } ] }, "title": "Linking the X-ray and infrared properties of star-forming galaxies at z < 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: general; galaxies: high-redshift; galaxies: starburst; submillimetre: general; X-rays: galaxies", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2014 July 16. Received 2014 July 15; in original form 2014 June 13.\n\nThis paper uses data from Herschel's photometers SPIRE and\nPACS. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). The scientific results reported in this paper are based to a significant degree on observations made by the Chandra X-ray Observatory.\n\nPublished - MNRAS-2014-Symeonidis-3728-40.pdf
Submitted - 1407.4511v1.pdf
", "abstract": "We present the most complete study to date of the X-ray emission from star formation in high-redshift (median z = 0.7; z < 1.5), IR-luminous (L_(IR) = 10^(10)\u201310^(13) L_\u2299) galaxies detected by Herschel's PACS and SPIRE instruments. For our purpose, we take advantage of the deepest X-ray data to date, the Chandra Deep Fields (North and South). Sources which host AGN are removed from our analysis by means of multiple AGN indicators. We find an AGN fraction of 18 \u00b1 2 per cent amongst our sample and note that AGN entirely dominate at values of log [L_X/L_(IR)] > \u22123 in both hard and soft X-ray bands. From the sources which are star formation dominated, only a small fraction are individually X-ray detected and for the bulk of the sample we calculate average X-ray luminosities through stacking. We find an average soft X-ray to infrared ratio of log \u3008L_(SX)/L_(IR)\u3009 = \u22124.3 and an average hard X-ray to infrared ratio of log \u3008L_(HX)/L_(IR)\u3009 = \u22123.8. We report that the X-ray/IR correlation is approximately linear through the entire range of LIR and z probed and, although broadly consistent with the local (z < 0.1) one, it does display some discrepancies. We suggest that these discrepancies are unlikely to be physical, i.e. due to an intrinsic change in the X-ray properties of star-forming galaxies with cosmic time, as there is no significant evidence for evolution of the L_X/L_(IR) ratio with redshift. Instead, they are possibly due to selection effects and remaining AGN contamination. We also examine whether dust obscuration in the galaxy plays a role in attenuating X-rays from star formation, by investigating changes in the L_X/L_(IR) ratio as a function of the average dust temperature. We conclude that X-rays do not suffer any measurable attenuation in the host galaxy.", "date": "2014-10-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "443", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3728-3740", "id_number": "CaltechAUTHORS:20141107-142352785", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141107-142352785", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" } ] }, "doi": "10.1093/mnras/stu1441", "primary_object": { "basename": "1407.4511v1.pdf", "url": "https://authors.library.caltech.edu/records/5jb6x-t5j12/files/1407.4511v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Symeonidis-3728-40.pdf", "url": "https://authors.library.caltech.edu/records/5jb6x-t5j12/files/MNRAS-2014-Symeonidis-3728-40.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Symeonidis, M.; Georgakakis, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/xk7rp-3pf45", "eprint_id": 50026, "eprint_status": "archive", "datestamp": "2023-08-22 13:35:57", "lastmod": "2023-10-17 22:27:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G. P." } } ] }, "title": "BICEP2. II. Experiment and three-year Data Set", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; instrumentation: polarimeters; telescopes", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2014 April 15; accepted 2014 July 15; published 2014 August 14. \n\nBicep2 was supported by the U.S. National Science Foundation\nunder grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development\nFund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W. M. Keck Foundation. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed past efforts to the Bicep/Keck Array series of experiments, including the Bicep1 and Keck Array teams, as well as our colleagues on the Spider team with whom we coordinated receiver and detector development efforts at Caltech. We dedicate this paper to the memory of Andrew Lange, whom we sorely miss.\n\nPublished - 0004-637X_792_1_62.pdf
Submitted - 1403.4302v3.pdf
", "abstract": "We report on the design and performance of the BICEP2 instrument and on its three-year data set. BICEP2 was designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 1\u00b0-5\u00b0(\u2113 = 40-200), near the expected peak of the B-mode polarization signature of primordial gravitational waves from cosmic inflation. Measuring B-modes requires dramatic improvements in sensitivity combined with exquisite control of systematics. The BICEP2 telescope observed from the South Pole with a 26 cm aperture and cold, on-axis, refractive optics. BICEP2 also adopted a new detector design in which beam-defining slot antenna arrays couple to transition-edge sensor (TES) bolometers, all fabricated on a common substrate. The antenna-coupled TES detectors supported scalable fabrication and multiplexed readout that allowed BICEP2 to achieve a high detector count of 500 bolometers at 150 GHz, giving unprecedented sensitivity to B-modes at degree angular scales. After optimization of detector and readout parameters, BICEP2 achieved an instrument noise-equivalent temperature of 15.8 \u00b5K\u221as. The full data set reached Stokes Q and U map depths of 87.2 nK in square-degree pixels (5.'2 \u03bcK) over an effective area of 384 deg^2 within a 1000 deg^2 field. These are the deepest CMB polarization maps at degree angular scales to date. The power spectrum analysis presented in a companion paper has resulted in a significant detection of B-mode polarization at degree scales.", "date": "2014-09-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "792", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 62", "id_number": "CaltechAUTHORS:20140925-103717168", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140925-103717168", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT-1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "W. M. Keck Foundation" } ] }, "corp_creators": { "items": [ "BICEP2 Collaboration" ] }, "doi": "10.1088/0004-637X/792/1/62", "primary_object": { "basename": "0004-637X_792_1_62.pdf", "url": "https://authors.library.caltech.edu/records/xk7rp-3pf45/files/0004-637X_792_1_62.pdf" }, "related_objects": [ { "basename": "1403.4302v3.pdf", "url": "https://authors.library.caltech.edu/records/xk7rp-3pf45/files/1403.4302v3.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/0c0h2-ptn58", "eprint_id": 45854, "eprint_status": "archive", "datestamp": "2023-08-20 02:41:43", "lastmod": "2023-10-26 18:30:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Staniszewski-Z", "name": { "family": "Staniszewski", "given": "Z." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Brevik-J", "name": { "family": "Brevik", "given": "J." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Gong-Y", "name": { "family": "Gong", "given": "Y." } }, { "id": "Hailey-Dunsheath-S", "name": { "family": "Hailey-Dunsheath", "given": "S." }, "orcid": "0000-0002-8504-7988" }, { "id": "O'Brient-R", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Santos-M", "name": { "family": "Santos", "given": "M." } }, { "id": "Shirokoff-E", "name": { "family": "Shirokoff", "given": "E." } }, { "id": "Silva-M", "name": { "family": "Silva", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Tomographic Ionized-Carbon Mapping Experiment (TIME) CII Imaging Spectrometer", "ispublished": "pub", "full_text_status": "restricted", "keywords": "Spectrometer, Reionization, Intensity, Mapping, TES, KID", "note": "\u00a9 2014 Springer Science+Business Media New York. \n\nReceived: 21 August 2013. Accepted: 4 February 2014. Published online: 12 May 2014. \n\nWe would like to thank the Keck Institute for Space Studies at Caltech and JPL for support of this concept study. Funding for R. O'Brient provided by the NASA Postdoctoral Program.", "abstract": "The Tomographic Ionized-Carbon Mapping Experiment (TIME) and TIME-Pilot are proposed imaging spectrometers to measure reionization and large scale structure at redshifts 5\u20139. We seek to exploit the 158 \u03bcm restframe emission of [CII], which becomes measurable at 200\u2013300 GHz at reionization redshifts. Here we describe the scientific motivation, give an overview of the proposed instrument, and highlight key technological developments underway to enable these measurements.", "date": "2014-09", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "176", "number": "5-6", "publisher": "Springer", "pagerange": "767-772", "id_number": "CaltechAUTHORS:20140520-145421640", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140520-145421640", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Keck Institute for Space Studies (KISS)" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "JPL" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" } ] }, "doi": "10.1007/s10909-014-1126-4", "resource_type": "article", "pub_year": "2014", "author_list": "Staniszewski, Z.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/ecff8-sth11", "eprint_id": 48647, "eprint_status": "archive", "datestamp": "2023-08-22 13:14:00", "lastmod": "2023-10-17 19:30:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } } ] }, "title": "HerMES: The Rest-Frame UV Emission and A Lensing Model for the z=6.34 Luminous Dusty Starburst Galaxy HFLS3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; gravitational lensing: strong; infrared: galaxies; submillimeter: galaxies", "note": "\u00a9 2014 American Astronomical Society. Received 2014 April 6; accepted 2014 May 16; published 2014 July 1. Financial support for this work was provided by NASA through grant HST-GO-13045 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Additional support for A.C., W.O., J.C., J.L.W., and\nC.M.C. was from NSF with AST-1313319. We thank E. da\nCunha for help with Magphys. Dark Cosmology Centre is\nfunded by the Danish National Research Foundation (J.L.W.\nand D.W.). S.O. acknowledges support from the Science and\nTechnology Facilities Council [grant No. ST/I000976/1].\nSPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES).\n\nPublished - 0004-637X_790_1_40.pdf
Submitted - 1404.1378v1.pdf
", "abstract": "We discuss the rest-frame ultraviolet emission from the starbursting galaxy HFLS3 at a redshift of 6.34. The galaxy was discovered in Herschel/SPIRE data due to its red color in the submillimeter wavelengths from 250 to 500 \u03bcm. Keck/NIRC2 K s -band adaptive optics imaging data showed two potential near-IR counterparts near HFLS3. Previously, the northern galaxy was taken to be in the foreground at z = 2.1, while the southern galaxy was assumed to be HFLS3's near-IR counterpart. The recently acquired Hubble/WFC3 and Advanced Camera for Surveys (ACS) imaging data show conclusively that both optically bright galaxies are in the foreground at z < 6. A new lensing model based on the Hubble imaging data and the millimeter-wave continuum emission yields a magnification factor of 2.2 \u00b1 0.3, with a 95% confidence upper limit on the magnification of 3.5. When corrected for lensing, the instantaneous star formation rate is 1320 M_\u2609 yr^(\u20131), with the 95% confidence lower limit around 830 M_\u2609 yr^(\u20131). The dust and stellar masses of HFLS3 from the same spectral energy distribution (SED) models are at the level of 3 \u00d7 10^8 M_\u2609 and ~5 \u00d7 10^(10) M_\u2609, respectively, with large systematic uncertainties on assumptions related to the SED model. With Hubble/WFC3 images, we also find diffuse near-IR emission about 0.5 arcsec (~3 kpc) to the southwest of HFLS3 that remains undetected in the ACS imaging data. The emission has a photometric redshift consistent with either z ~ 6 or a dusty galaxy template at z ~ 2.", "date": "2014-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "790", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 40", "id_number": "CaltechAUTHORS:20140818-092419872", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140818-092419872", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "HST-GO-13045" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "NSF", "grant_number": "AST-1313319" }, { "agency": "Danish National Research Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" } ] }, "doi": "10.1088/0004-637X/790/1/40", "primary_object": { "basename": "0004-637X_790_1_40.pdf", "url": "https://authors.library.caltech.edu/records/ecff8-sth11/files/0004-637X_790_1_40.pdf" }, "related_objects": [ { "basename": "1404.1378v1.pdf", "url": "https://authors.library.caltech.edu/records/ecff8-sth11/files/1404.1378v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Cooray, Asantha; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/05xha-ds549", "eprint_id": 46424, "eprint_status": "archive", "datestamp": "2023-08-20 01:30:17", "lastmod": "2023-10-26 19:44:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P." }, "orcid": "0000-0002-7963-7420" }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z. K." } } ] }, "title": "Detection of B-Mode Polarization at Degree Angular Scales by BICEP2", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 American Physical Society. Published by the American Physical Society under the terms of the Creative Commons Attribution 3.0 License. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. \n\nReceived 4 April 2014; revised manuscript received 13 June 2014; published 19 June 2014. \n\nBICEP2 was supported by the U.S. National Science Foundation under Grants No. ANT-0742818 and No. ANT-1044978 (Caltech and Harvard) and ANT-0742592 and ANT-1110087 (Chicago and Minnesota). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and Grants No. 06-ARPA206-0040 and No. 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. The receiver development was supported in part by a grant from the W. M. Keck Foundation. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The analysis effort at Stanford and SLAC is partially supported by the U.S. Department of Energy Office of Science. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. We thank the staff of the U.S. Antarctic Program and in particular the South Pole Station without whose help this research would not have been possible. We thank all those who have contributed past efforts to the BICEP\u2013Keck Array series of experiments, including the BICEP1 and Keck Array teams. We thank all those in the astrophysics community who have contributed feedback on the public preprint of this paper, and particularly two anonymous referees for their detailed and constructive recommendations. This work would not have been possible without the late Andrew Lange, whom we sorely miss.\n\nPublished - PhysRevLett.112.241101.pdf
Submitted - 1403.3985v2.pdf
", "abstract": "We report results from the BICEP2 experiment, a cosmic microwave background (CMB) polarimeter specifically designed to search for the signal of inflationary gravitational waves in the B-mode power spectrum around \u2113\u223c80. The telescope comprised a 26 cm aperture all-cold refracting optical system equipped with a focal plane of 512 antenna coupled transition edge sensor 150 GHz bolometers each with temperature sensitivity of \u2248300\u2009\u2009\u03bcK_(CMB)\u221as. BICEP2 observed from the South Pole for three seasons from 2010 to 2012. A low-foreground region of sky with an effective area of 380 square deg was observed to a depth of 87 nK deg in Stokes Q and U. In this paper we describe the observations, data reduction, maps, simulations, and results. We find an excess of B-mode power over the base lensed-\u039bCDM expectation in the range 30<\u2113<150, inconsistent with the null hypothesis at a significance of >5\u03c3. Through jackknife tests and simulations based on detailed calibration measurements we show that systematic contamination is much smaller than the observed excess. Cross correlating against WMAP 23 GHz maps we find that Galactic synchrotron makes a negligible contribution to the observed signal. We also examine a number of available models of polarized dust emission and find that at their default parameter values they predict power \u223c(5\u201310)\u00d7 smaller than the observed excess signal (with no significant cross-correlation with our maps). However, these models are not sufficiently constrained by external public data to exclude the possibility of dust emission bright enough to explain the entire excess signal. Cross correlating BICEP2 against 100 GHz maps from the BICEP1 experiment, the excess signal is confirmed with 3\u03c3 significance and its spectral index is found to be consistent with that of the CMB, disfavoring dust at 1.7\u03c3. The observed B-mode power spectrum is well fit by a lensed-\u039bCDM+tensor theoretical model with tensor-to-scalar ratio r=0.20^(+0.07)_(\u22120.05), with r=0 disfavored at 7.0\u03c3. Accounting for the contribution of foreground, dust will shift this value downward by an amount which will be better constrained with upcoming data sets.", "date": "2014-06-20", "date_type": "published", "publication": "Physical Review Letters", "volume": "112", "number": "24", "publisher": "American Physical Society", "pagerange": "Art. No. 241101", "id_number": "CaltechAUTHORS:20140623-073320912", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140623-073320912", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0742818" }, { "agency": "NSF", "grant_number": "ANT-1044978" }, { "agency": "NSF", "grant_number": "ANT-0742592" }, { "agency": "NSF", "grant_number": "ANT-1110087" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA", "grant_number": "06-ARPA206-0040" }, { "agency": "NASA", "grant_number": "10-SAT10-0017" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Harvard University" }, { "agency": "Department of Energy (DOE)" } ] }, "corp_creators": { "items": [ "BICEP2 Collaboration" ] }, "doi": "10.1103/PhysRevLett.112.241101", "primary_object": { "basename": "1403.3985v2.pdf", "url": "https://authors.library.caltech.edu/records/05xha-ds549/files/1403.3985v2.pdf" }, "related_objects": [ { "basename": "PhysRevLett.112.241101.pdf", "url": "https://authors.library.caltech.edu/records/05xha-ds549/files/PhysRevLett.112.241101.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/jy2na-vdq62", "eprint_id": 46302, "eprint_status": "archive", "datestamp": "2023-08-22 12:43:36", "lastmod": "2023-10-26 19:39:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "Julie L." }, "orcid": "0000-0003-2376-8971" }, { "id": "Malhotra-S", "name": { "family": "Malhotra", "given": "S." }, "orcid": "0000-0002-9226-5350" }, { "id": "Zheng-Zheng", "name": { "family": "Zheng", "given": "Z." } }, { "id": "Finkelstein-S-L", "name": { "family": "Finkelstein", "given": "S." }, "orcid": "0000-0001-8519-1130" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Calanog-J-A", "name": { "family": "Calanog", "given": "J." } }, { "id": "Ciardullo-R", "name": { "family": "Ciardullo", "given": "R." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Gawiser-E", "name": { "family": "Gawiser", "given": "E." } }, { "id": "Gronwall-C", "name": { "family": "Gronwall", "given": "C." } }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S." } }, { "id": "Ibar-Eduardo", "name": { "family": "Ibar", "given": "E." } }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Marsden-G", "name": { "family": "Marsden", "given": "G." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Rhoads-J", "name": { "family": "Rhoads", "given": "J." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Smith-A-J", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Wang-L", "name": { "family": "Wang", "given": "L." }, "orcid": "0000-0002-9803-166X" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Constraining the Ly\u03b1 Escape Fraction with Far-infrared Observations of Ly\u03b1 Emitters", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: star formation; submillimeter: general", "note": "\u00a9 2014 American Astronomical Society. Received 2013 December 16; accepted 2014 March 18; published 2014 April 29. We thank Ian Smail and Fabian Walter for helpful discussions and feedback on this manuscript. J.L.W., A.C., and D.R. thank the Aspen Center for Physics for hospitality during the conception, writing, and editing of this paper. This work is supported in part by the NSF under Grant Numbers PHY-1066293 and AST-1055919. S.M. and J.R. thank the DARK Cosmology Centre and Nordea Fonden in Copenhagen, Denmark, for hospitality during the course of this work. The Dark Cosmology Centre is funded by the Danish National Research Foundation. We acknowledge support from the Science and Technology Facilities Council (grant number ST/I000976/1). Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, under programmes 078.F-9028(A), 079.F-9500(A), 080.A-3023(A), and 081.F-9500(A). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists, and a mission scientist. HerMES is described in Oliver et al. (2012). The data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). \nFacilities: APEX (LABOCA), Herschel (SPIRE)\n\nPublished - 0004-637X_787_1_9.pdf
Submitted - 1312.4963v2.pdf
", "abstract": "We study the far-infrared properties of 498 Ly\u03b1 emitters (LAEs) at z = 2.8, 3.1, and 4.5 in the Extended Chandra Deep Field-South, using 250, 350, and 500 \u03bcm data from the Herschel Multi-tiered Extragalactic Survey and 870 \u03bcm data from the LABOCA ECDFS Submillimeter Survey. None of the 126, 280, or 92 LAEs at z = 2.8, 3.1, and 4.5, respectively, are individually detected in the far-infrared data. We use stacking to probe the average emission to deeper flux limits, reaching 1\u03c3 depths of ~0.1 to 0.4 mJy. The LAEs are also undetected at \u22653\u03c3 in the stacks, although a 2.5\u03c3 signal is observed at 870 \u03bcm for the z = 2.8 sources. We consider a wide range of far-infrared spectral energy distributions (SEDs), including an M82 and an Sd galaxy template, to determine upper limits on the far-infrared luminosities and far-infrared-derived star formation rates of the LAEs. These star formation rates are then combined with those inferred from the Ly\u03b1 and UV emission to determine lower limits on the LAEs' Ly\u03b1 escape fraction (f_(esc)(Ly\u03b1)). For the Sd SED template, the inferred LAEs f_(esc)(Ly\u03b1) are \u227330% (1\u03c3) at z = 2.8, 3.1, and 4.5, which are all significantly higher than the global f_(esc)(Ly\u03b1) at these redshifts. Thus, if the LAEs f_(esc)(Ly\u03b1) follows the global evolution, then they have warmer far-infrared SEDs than the Sd galaxy template. The average and M82 SEDs produce lower limits on the LAE f_(esc)(Ly\u03b1) of ~10%-20% (1\u03c3), all of which are slightly higher than the global evolution of f_(esc)(Ly\u03b1), but consistent with it at the 2\u03c3-3\u03c3 level.", "date": "2014-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "787", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 9", "id_number": "CaltechAUTHORS:20140617-094634128", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140617-094634128", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "NSF", "grant_number": "AST-1055919" }, { "agency": "Danish National Research Foundation" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1088/0004-637X/787/1/9", "primary_object": { "basename": "1312.4963v2.pdf", "url": "https://authors.library.caltech.edu/records/jy2na-vdq62/files/1312.4963v2.pdf" }, "related_objects": [ { "basename": "0004-637X_787_1_9.pdf", "url": "https://authors.library.caltech.edu/records/jy2na-vdq62/files/0004-637X_787_1_9.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Wardlow, Julie L.; Malhotra, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/nj69c-e0v92", "eprint_id": 41533, "eprint_status": "archive", "datestamp": "2023-08-22 12:41:32", "lastmod": "2023-10-24 23:49:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pullen-A-R", "name": { "family": "Pullen", "given": "Anthony R." } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "Olivier" }, "orcid": "0000-0001-7432-2932" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "Jamie" }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Intensity Mapping across Cosmic Times with the Ly\u03b1 Line", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; diffuse radiation; intergalactic medium; large-scale structure of universe", "note": "\u00a9 2014 The American Astronomical Society. \n\nReceived 2013 December 13; accepted 2014 March 22; published 2014 April 24. \n\nWe thank P. Capak, A. Cooray, S. Furlanetto, Y. Gong, C. Hirata, A. Lidz, G. Rudie, M. Viero, and M. Zemcov for helpful comments and useful discussions. Part of the research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. A.P. was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Oak Ridge Associated Universities through a contract with NASA. This work was supported by the Keck Institute of Space Studies and we thank colleagues at the \"First Billion Years\" for stimulating discussions, in particular J. Bowman and A. Readhead for organizing it.\n\nPublished - Pullen_2014_ApJ_786_111.pdf
Submitted - 1309.2295v1.pdf
", "abstract": "We present a quantitative model of Ly\u03b1 emission throughout cosmic history and determine the prospects for intensity mapping spatial fluctuations in the Ly\u03b1 signal. Since (1) our model assumes at z > 6 the minimum star formation required to sustain reionization and (2) is based at z < 6 on a luminosity function (LF) extrapolated from the few observed bright Ly\u03b1 emitters, this should be considered a lower limit. Mapping the line emission allows probes of reionization, star formation, and large-scale structure (LSS) as a function of redshift. While Ly\u03b1 emission during reionization has been studied, we also predict the postreionization signal to test predictions of the intensity and motivate future intensity mapping probes of reionization. We include emission from massive dark matter halos and the intergalactic medium (IGM) in our model. We find agreement with current, measured LFs of Ly\u03b1 emitters at z < 8. However, diffuse IGM emission, not associated with Ly\u03b1 emitters, dominates the intensity up to z ~ 10. While our model is applicable for deep-optical or near-infrared observers like the James Webb Space Telescope, only intensity mapping will detect the diffuse IGM emission. We also construct a three-dimensional power spectrum model of the Ly\u03b1 emission. Finally, we consider the prospects of an intensity mapper for measuring Ly\u03b1 fluctuations while identifying interloper contamination for removal. Our results suggest that while the reionization signal is challenging, Ly\u03b1 fluctuations can be an interesting new probe of LSS at late times when used in conjunction with other lines, e.g., H\u03b1, to monitor low-redshift foreground confusion.", "date": "2014-05-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "786", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 111", "id_number": "CaltechAUTHORS:20130925-143816733", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130925-143816733", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Postdoctoral Program" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Keck Institute for Space Studies (KISS)" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" } ] }, "doi": "10.1088/0004-637X/786/2/111", "primary_object": { "basename": "Pullen_2014_ApJ_786_111.pdf", "url": "https://authors.library.caltech.edu/records/nj69c-e0v92/files/Pullen_2014_ApJ_786_111.pdf" }, "related_objects": [ { "basename": "1309.2295v1.pdf", "url": "https://authors.library.caltech.edu/records/nj69c-e0v92/files/1309.2295v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Pullen, Anthony R.; Dor\u00e9, Olivier; et el." }, { "id": "https://authors.library.caltech.edu/records/yg9t6-gkj85", "eprint_id": 45992, "eprint_status": "archive", "datestamp": "2023-08-20 00:09:25", "lastmod": "2023-10-26 18:35:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Clements-D-L", "name": { "family": "Clements", "given": "D. L." }, "orcid": "0000-0002-9548-5033" }, { "id": "Braglia-F-G", "name": { "family": "Braglia", "given": "F. G." } }, { "id": "Hyde-A-K", "name": { "family": "Hyde", "given": "A. K." } }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "I." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cava-A", "name": { "family": "Cava", "given": "A." } }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Gonzales-Solares-E-A", "name": { "family": "Gonzales Solares", "given": "E. A." }, "orcid": "0000-0001-9123-0626" }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Marsden-G", "name": { "family": "Marsden", "given": "G." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Smith-A-J", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Vieira-J", "name": { "family": "Vieira", "given": "J." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "J." }, "orcid": "0000-0003-2376-8971" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "De-Zotti-G", "name": { "family": "de Zotti", "given": "G." }, "orcid": "0000-0003-2868-2595" } ] }, "title": "Herschel Multitiered Extragalactic Survey: clusters of dusty galaxies uncovered by Herschel and Planck", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high redshift\n galaxies: starburst\n submillimetre: galaxies", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 November 19. Received 2013 November 19; in original form 2013 November 13. First published online: February 11, 2014.\n\nBased in part on observations with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia\nand with important participation from NASA.\n\nBased in part on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded\nby ESA Member States, NASA & Canada.\n\nSPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The development of Planck has been supported by ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal). The development of Planck has been supported by ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN(Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES). The authors would like to thank Mattia Negrello for the provision of Fig. 14. This work is funded in part by the UK STFC and UKSA. SJO, LW and AS acknowledge support from the Science and Technology Facilities Council [grant number ST/I000976/1], GdZ acknowledges financial support by ASI/INAF agreement I/072/09/0. Lucia Marchetti, and Mattia Vaccari were supported by the Italian Space Agency\n(ASI Herschel Science Contract I/005/07/0).\n\nPublished - MNRAS-2014-Clements-1193-211.pdf
", "abstract": "The potential for Planck to detect clusters of dusty, star-forming galaxies at z > 1 is tested by examining the Herschel-SPIRE images of Planck Early Release Compact Source Catalog sources lying in fields observed by the Herschel Multitiered Extragalactic Survey. Of the 16 Planck sources that lie in the \u223c90 sq. deg. examined, we find that 12 are associated with single bright Herschel sources. The remaining four are associated with overdensities of Herschel sources, making them candidate clusters of dusty, star-forming galaxies. We use complementary optical/near-IR data for these 'clumps' to test this idea, and find evidence for the presence of galaxy clusters in all four cases. We use photometric redshifts and red sequence galaxies to estimate the redshifts of these clusters, finding that they range from 0.8 to 2.3. These redshifts imply that the Herschel sources in these clusters, which contribute to the detected Planck flux, are forming stars very rapidly, with typical total cluster star formation rates >1000\u2009M_\u2299\u2009yr^(\u22121). The high-redshift clusters discovered in these observations are used to constrain the epoch of cluster galaxy formation, finding that the galaxies in our clusters are 1\u20131.5 Gyr old at z \u223c 1\u20132. Prospects for the discovery of further clusters of dusty galaxies are discussed, using not only all sky Planck surveys, but also deeper, smaller area, Herschel surveys.", "date": "2014-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "439", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1193-1211", "id_number": "CaltechAUTHORS:20140530-091456467", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-091456467", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "CSIC (Spain)" }, { "agency": "Ministerio de Econom\u00eda y Competitividad (MICINN)" }, { "agency": "JA (Spain)" }, { "agency": "Tekes (Finland)" }, { "agency": "AoF (Finland)" }, { "agency": "CSC (Finland)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "PRACE (EU)" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/072/09/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/0" } ] }, "doi": "10.1093/mnras/stt2253", "primary_object": { "basename": "MNRAS-2014-Clements-1193-211.pdf", "url": "https://authors.library.caltech.edu/records/yg9t6-gkj85/files/MNRAS-2014-Clements-1193-211.pdf" }, "resource_type": "article", "pub_year": "2014", "author_list": "Clements, D. L.; Braglia, F. G.; et el." }, { "id": "https://authors.library.caltech.edu/records/nbd7v-hvw47", "eprint_id": 45990, "eprint_status": "archive", "datestamp": "2023-08-20 00:09:19", "lastmod": "2023-10-26 18:35:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Delvecchio-I", "name": { "family": "Delvecchio", "given": "I." }, "orcid": "0000-0001-8706-2252" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Tracing the cosmic growth of supermassive black holes to z \u223c 3 with Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: nuclei, infrared: galaxies.", "note": "\u00a9 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 January 16. Received 2013 December 30; in original form 2013 November 14. First published online: February 25, 2014.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nThis paper uses data from Herschel's photometers PACS and SPIRE. PACS has been developed by a consortium of institutes led by MPE (Germany) and including: UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy) and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI,Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). ID is deeply grateful to Iary Davidzon, Andrea Negri, Fabio Vito and Alessandro Marconi for inspiring discussions and suggestions. ID also thanks Elisabeta Lusso for useful tests on codes for SED decomposition and Micol Bolzonella for kindly providing a tool to estimate error bars.\n\nPublished - MNRAS-2014-Delvecchio-2736-54.pdf
Submitted - 1401.4503v1.pdf
", "abstract": "We study a sample of Herschel selected galaxies within the Great Observatories Origins Deep Survey-South and the Cosmic Evolution Survey fields in the framework of the Photodetector Array Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the rich multiwavelength photometric data sets available in both fields, we perform a broad-band spectral energy distribution decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability of revealing AGN activity increases for bright (L_(1\u22121000) > 10^(11) L_\u2299) star-forming galaxies at z > 0.3, becoming about 80 per cent for the brightest (L_(1\u22121000) > 10^(12) L_\u2299) infrared (IR) galaxies at z \u2265 1. Finally, we reconstruct the AGN bolometric luminosity function and the supermassive black hole growth rate across cosmic time up to z \u223c 3 from a far-IR perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at z \u223c 2 and reproducing the observed local black hole mass density with consistent values of the radiative efficiency \u03f5_(rad) (\u223c0.07).", "date": "2014-04", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "439", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2736-2754", "id_number": "CaltechAUTHORS:20140530-074307694", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140530-074307694", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "ASI/INAF (Italy)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "CSA (Canada)" }, { "agency": "NAOC (China)" }, { "agency": "CEA (France)" }, { "agency": "CNES (France)" }, { "agency": "CNRS (France)" }, { "agency": "ASI (Italy)" }, { "agency": "MCINN (Spain)" }, { "agency": "SNSB (Sweden)" }, { "agency": "STFC (UK)" }, { "agency": "UKSA (UK)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stu130", "primary_object": { "basename": "1401.4503v1.pdf", "url": "https://authors.library.caltech.edu/records/nbd7v-hvw47/files/1401.4503v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2014-Delvecchio-2736-54.pdf", "url": "https://authors.library.caltech.edu/records/nbd7v-hvw47/files/MNRAS-2014-Delvecchio-2736-54.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Delvecchio, I. and Bock, J." }, { "id": "https://authors.library.caltech.edu/records/bv451-xa169", "eprint_id": 46099, "eprint_status": "archive", "datestamp": "2023-08-22 11:59:32", "lastmod": "2023-10-26 18:41:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J.-S." } }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G." }, "orcid": "0000-0002-4872-2294" }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } }, { "id": "Dai-Y-Sophia", "name": { "family": "Dai", "given": "Y. Sophia" }, "orcid": "0000-0002-7928-416X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S." } }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "D. L." }, "orcid": "0000-0002-9548-5033" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Smith-A-J-S", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M." }, "orcid": "0000-0002-6689-6271" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I." } }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "G. G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Webb-T-M-A", "name": { "family": "Webb", "given": "T. M. A." } }, { "id": "Efstathiou-Andreas", "name": { "family": "Efstathiou", "given": "A." }, "orcid": "0000-0002-2612-4840" } ] }, "title": "HerMES: Spectral Energy Distributions of Submillimeter Galaxies at z > 4", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; galaxies: formation; infrared: galaxies", "note": "\u00a9 2014 American Astronomical Society. Received 2013 March 14; accepted 2014 January 25; published 2014 March 4. \n\nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nThis work is based in part on observations made with the\nSpitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC,\nUniv. Colorado (USA). This development has been supported\nby national funding agencies: CSA (Canada); NAOC (China);\nCEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain);\nSNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\nFacilities: Herschel (SPIRE), Spitzer (IRAC, MIPS).\n\nPublished - 0004-637X_784_1_52.pdf
Submitted - 1401.6079v1.pdf
", "abstract": "We present a study of the infrared properties for a sample of seven spectroscopically confirmed submillimeter galaxies (SMGs) at z > 4.0. By combining ground-based near-infrared, Spitzer IRAC and MIPS, Herschel SPIRE, and ground-based submillimeter/millimeter photometry, we construct their spectral energy distributions (SEDs) and a composite model to fit the SEDs. The model includes a stellar emission component at \u03bb_(rest) < 3.5 \u03bcm, a hot dust component peaking at \u03bb_(rest) ~ 5 \u03bcm, and cold dust component which becomes significant for \u03bb_(rest) > 50 \u03bcm. Six objects in the sample are detected at 250 and 350 \u03bcm. The dust temperatures for the sources in this sample are in the range of 40-80 K, and their L_(FIR) ~ 10^(13) L_\u2609 qualifies them as hyper-luminous infrared galaxies. The mean FIR-radio index for this sample is around \u3008q\u3009 = 2.2 indicating no radio excess in their radio emission. Most sources in the sample have 24 \u03bcm detections corresponding to a rest-frame 4.5 \u03bcm luminosity of Log_(10)(L_(4.5)/L_\u2609) = 11 ~ 11.5. Their L_(4.5)/L_(FIR) ratios are very similar to those of starburst-dominated SMGs at z ~ 2. The L_(CO) \u2013 L_(FIR) relation for this sample is consistent with that determined for local ULIRGs and SMGs at z ~ 2. We conclude that SMGs at z > 4 are hotter and more luminous in the FIR but otherwise very similar to those at z ~ 2. None of these sources show any sign of the strong QSO phase being triggered.", "date": "2014-03-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "784", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 52", "id_number": "CaltechAUTHORS:20140605-113014540", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140605-113014540", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/784/1/52", "primary_object": { "basename": "0004-637X_784_1_52.pdf", "url": "https://authors.library.caltech.edu/records/bv451-xa169/files/0004-637X_784_1_52.pdf" }, "related_objects": [ { "basename": "1401.6079v1.pdf", "url": "https://authors.library.caltech.edu/records/bv451-xa169/files/1401.6079v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Huang, J.-S.; Rigopoulou, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/tqmf8-3e041", "eprint_id": 46113, "eprint_status": "archive", "datestamp": "2023-08-19 23:58:48", "lastmod": "2023-10-26 18:41:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kaufman-J-P", "name": { "family": "Kaufman", "given": "J. P." } }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J." }, "orcid": "0000-0001-8217-6832" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Richter-S", "name": { "family": "Richter", "given": "S." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Self-calibration of BICEP1 three-year data and constraints on astrophysical polarization rotation", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2014 American Physical Society.\n\nReceived 22 January 2014; published 24 March 2014.\n\nBICEP1 was supported by NSF Grant No. OPP-0230438,\nCaltech Presidents Discovery Fund, Caltech Presidents\nFund PF-471, JPL Research and Technology\nDevelopment Fund, and the late J. Robinson. This analysis\nwas supported in part by NSF CAREER Award No. AST-\n1255358 and the Harvard College Observatory, and J. M.\nK. acknowledges support from an Alfred P. Sloan Research\nFellowship. B. G. K acknowledges support from NSF\nPECASE Award No. AST-0548262. N. J.M.'s research\nwas supported by an appointment to the NASA\nPostdoctoral Program at Goddard Space Flight Center,\nadministered by Oak Ridge Associated Universities\nthrough a contract with NASA. M. S. acknowledges\nsupport from a grant from Joan and Irwin Jacobs. We\nthank the South Pole Station staff for helping make our\nobserving seasons a success. We also thank our colleagues\nin the ACBAR, BOOMERANG, QUAD, BOLOCAM,\nSPT, WMAP and Planck experiments, as well as Kim\nGriest, Amit Yadav, and Casey Conger for advice and\nhelpful discussions, and Kathy Deniston and Irene Coyle\nfor logistical and administrative support. We thank Patrick\nShopbell for computational support at Caltech and the FAS\nScience Division Research Computing Group at Harvard\nUniversity for providing support to run all the computations\nfor this paper on the Odyssey cluster.\n\nPublished - PhysRevD.89.062006.pdf
Submitted - 1312.7877v1.pdf
", "abstract": "Cosmic microwave background (CMB) polarimeters aspire to measure the faint B-mode signature predicted to arise from inflationary gravitational waves. They also have the potential to constrain cosmic birefringence, rotation of the polarization of the CMB arising from parity-violating physics, which would produce nonzero expectation values for the CMB's temperature to B-mode correlation (TB) and E-mode to B-mode correlation (EB) spectra. However, instrumental systematic effects can also cause these TB and EB correlations to be nonzero. In particular, an overall miscalibration of the polarization orientation of the detectors produces TB and EB spectra which are degenerate with isotropic cosmological birefringence, while also introducing a small but predictable bias on the BB spectrum. We find that Bicep1 three-year spectra, which use our standard calibration of detector polarization angles from a dielectric sheet, are consistent with a polarization rotation of \u03b1=\u22122.77\u00b0\u00b10.86\u00b0(statistical)\u00b11.3\u00b0(systematic). We have revised the estimate of systematic error on the polarization rotation angle from the two-year analysis by comparing multiple calibration methods. We also account for the (negligible) impact of measured beam systematic effects. We investigate the polarization rotation for the Bicep1 100 GHz and 150 GHz bands separately to investigate theoretical models that produce frequency-dependent cosmic birefringence. We find no evidence in the data supporting either of these models or Faraday rotation of the CMB polarization by the Milky Way galaxy's magnetic field. If we assume that there is no cosmic birefringence, we can use the TB and EB spectra to calibrate detector polarization orientations, thus reducing bias of the cosmological B-mode spectrum from leaked E-modes due to possible polarization orientation miscalibration. After applying this \"self-calibration\" process, we find that the upper limit on the tensor-to-scalar ratio decreases slightly, from r<0.70 to r<0.65 at 95% confidence.", "date": "2014-03-15", "date_type": "published", "publication": "Physical Review D", "volume": "89", "number": "6", "publisher": "American Physical Society", "pagerange": "Art. No. 062006", "id_number": "CaltechAUTHORS:20140606-082619092", "issn": "2470-0010", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140606-082619092", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0230438" }, { "agency": "Caltech Presidents Discovery Fund" }, { "agency": "Caltech Presidents Fund", "grant_number": "PF-471" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NSF", "grant_number": "AST-1255358" }, { "agency": "Harvard College Observatory" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0548262" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "Joan and Irwin Jacobs" } ] }, "doi": "10.1103/PhysRevD.89.062006", "primary_object": { "basename": "1312.7877v1.pdf", "url": "https://authors.library.caltech.edu/records/tqmf8-3e041/files/1312.7877v1.pdf" }, "related_objects": [ { "basename": "PhysRevD.89.062006.pdf", "url": "https://authors.library.caltech.edu/records/tqmf8-3e041/files/PhysRevD.89.062006.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Kaufman, J. P.; Aikin, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/evx99-aq474", "eprint_id": 46254, "eprint_status": "archive", "datestamp": "2023-08-22 11:56:34", "lastmod": "2023-10-26 19:37:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Barkats-D", "name": { "family": "Barkats", "given": "D." } }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J." }, "orcid": "0000-0001-8217-6832" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Richter-S", "name": { "family": "Richter", "given": "S." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Degree-scale Cosmic Microwave Background Polarization Measurements from Three Years of BICEP1 Data", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization", "note": "\u00a9 2014 American Astronomical Society. Received 2013 October 4; accepted 2014 January 7; published 2014 February 14. Bicep1 was supported by NSF grant No. OPP-0230438,\nCaltech President's Discovery Fund, Caltech President's Fund\nPF-471, JPL Research and Technology Development Fund, and\nthe late J. Robinson. This analysis was supported in part by NSF\nCAREER award No. AST-1255358 and the Harvard College\nObservatory, and J.M.K. acknowledges support from an Alfred\nP. Sloan Research Fellowship. B.G.K acknowledges support\nfrom NSF PECASE Award No. AST-0548262. We thank the South Pole Station staff for helping make our observing seasons\na success.We also thank our colleagues in Acbar, Boomerang,\nQUaD, Bolocam, SPT, WMAP, and Planck for advice and helpful discussions, and Kathy Deniston and Irene Coyle for\nlogistical and administrative support. We thank Patrick Shopbell for computational support at Caltech and the FAS Science Division Research Computing Group at Harvard University for providing support to run all the computations for this paper on\nthe Odyssey cluster.\n\nPublished - 0004-637X_783_2_67.pdf
Submitted - 1310.1422v2.pdf
", "abstract": "BICEP1 is a millimeter-wavelength telescope designed specifically to measure the inflationary B-mode polarization of the cosmic microwave background at degree angular scales. We present results from an analysis of the data acquired during three seasons of observations at the South Pole (2006-2008). This work extends the two-year result published in Chiang et al., with additional data from the third season and relaxed detector-selection criteria. This analysis also introduces a more comprehensive estimation of band power window functions, improved likelihood estimation methods, and a new technique for deprojecting monopole temperature-to-polarization leakage that reduces this class of systematic uncertainty to a negligible level. We present maps of temperature, E- and B-mode polarization, and their associated angular power spectra. The improvement in the map noise level and polarization spectra error bars are consistent with the 52% increase in integration time relative to Chiang et al. We confirm both self-consistency of the polarization data and consistency with the two-year results. We measure the angular power spectra at 21 \u2264 \u2113 \u2264 335 and find that the EE spectrum is consistent with Lambda cold dark matter cosmology, with the first acoustic peak of the EE spectrum now detected at 15\u03c3. The BB spectrum remains consistent with zero. From B-modes only, we constrain the tensor-to-scalar ratio to r = 0.03^(+0.27)_(-0.23), or r < 0.70 at 95% confidence level.", "date": "2014-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "783", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 67", "id_number": "CaltechAUTHORS:20140612-151743927", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140612-151743927", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0230438" }, { "agency": "Caltech President's Discovery Fund" }, { "agency": "Caltech President's Fund", "grant_number": "PF-471" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NSF", "grant_number": "AST-1255358" }, { "agency": "Harvard College Observatory" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF", "grant_number": "AST-0548262" } ] }, "corp_creators": { "items": [ "BICEP1 Collaboration" ] }, "doi": "10.1088/0004-637X/783/2/67", "primary_object": { "basename": "0004-637X_783_2_67.pdf", "url": "https://authors.library.caltech.edu/records/evx99-aq474/files/0004-637X_783_2_67.pdf" }, "related_objects": [ { "basename": "1310.1422v2.pdf", "url": "https://authors.library.caltech.edu/records/evx99-aq474/files/1310.1422v2.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Barkats, D.; Aikin, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/cj808-0d466", "eprint_id": 41525, "eprint_status": "archive", "datestamp": "2023-08-22 11:34:32", "lastmod": "2023-10-24 23:48:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "The Herschel Stripe 82 Survey (HerS): Maps and Early Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; infrared: galaxies; large-scale structure of universe; submillimeter: galaxies", "note": "\u00a9 2014 American Astronomical Society. \n\nReceived 2013 August 20; accepted 2014 January 2; published 2014 January 20. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nThe authors warmly thank Duncan Hanson, Brandon Hensley, Edward Chapin, and Lyman Page for their input and participation. We also thank the anonymous referee, whose comments have greatly improved this paper. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the University of Sussex (UK); and Caltech, JPL, NHSC, the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\n\nPublished - 0067-0049_210_2_22.pdf
Submitted - 1308.4399v1.pdf
", "abstract": "We present the first set of maps and band-merged catalog from the Herschel Stripe 82 Survey (HerS). Observations at 250, 350, and 500 \u03bcm were taken with the Spectral and Photometric Imaging Receiver instrument aboard the Herschel Space Observatory. HerS covers 79 deg^2 along the SDSS Stripe 82 to an average depth of 13.0, 12.9, and 14.8 mJy beam\u20131 (including confusion) at 250, 350, and 500 \u03bcm, respectively. HerS was designed to measure correlations with external tracers of the dark matter density field\u2014either point-like (i.e., galaxies selected from radio to X-ray) or extended (i.e., clusters and gravitational lensing)\u2014in order to measure the bias and redshift distribution of intensities of infrared-emitting dusty star-forming galaxies and active galactic nuclei. By locating HerS in Stripe 82, we maximize the overlap with available and upcoming cosmological surveys. The band-merged catalog contains 3.3 \u00d7 10^4 sources detected at a significance of \u2273 3\u03c3 (including confusion noise). The maps and catalog are available at http://www.astro.caltech.edu/hers/.", "date": "2014-02", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "210", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 22", "id_number": "CaltechAUTHORS:20130925-111749774", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130925-111749774", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1088/0067-0049/210/2/22", "primary_object": { "basename": "0067-0049_210_2_22.pdf", "url": "https://authors.library.caltech.edu/records/cj808-0d466/files/0067-0049_210_2_22.pdf" }, "related_objects": [ { "basename": "1308.4399v1.pdf", "url": "https://authors.library.caltech.edu/records/cj808-0d466/files/1308.4399v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Viero, M. P.; Moncelsi, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/p0t3n-wjk07", "eprint_id": 43776, "eprint_status": "archive", "datestamp": "2023-08-22 11:30:34", "lastmod": "2023-10-25 23:51:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Hopwood-R", "name": { "family": "Hopwood", "given": "R." } }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G. E." }, "orcid": "0000-0002-4872-2294" }, { "id": "Thatte-N", "name": { "family": "Thatte", "given": "N." } }, { "id": "Swinyard-B-M", "name": { "family": "Swinyard", "given": "B. M." } }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J.-S." } }, { "id": "Alonso-Herrero-A", "name": { "family": "Alonso-Herrero", "given": "A." }, "orcid": "0000-0001-6794-2519" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "D." }, "orcid": "0000-0002-9548-5033" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Griffin-M-J", "name": { "family": "Griffin", "given": "M. J." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Pearson-C", "name": { "family": "Pearson", "given": "C." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Smith-A", "name": { "family": "Smith", "given": "A." }, "orcid": "0000-0002-1938-4660" }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Valtchanov-I", "name": { "family": "Valtchanov", "given": "I." }, "orcid": "0000-0001-9930-7886" }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } } ] }, "title": "Herschel Observations of Far-infrared Cooling Lines in Intermediate Redshift (Ultra)-luminous Infrared Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: starburst; infrared: galaxies; infrared: ISM", "note": "\u00a9 2014 American Astronomical Society. Received 2013 October 11; accepted 2013 December 6; published 2014 January 6. \n\nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nWe thank the anonymous referee for his/her insightful comments.\nD.R. and G.E.M. acknowledge support from grant\nST/K00106X/1 and the John Fell Oxford University Press\n(OUP) Research Fund (G.E.M.). This Letter is based on data\nfrom Herschel's SPIRE-FTS. SPIRE has been developed by\na consortium of institutes led by Cardiff University (UK) and including: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC,\nUKSA (UK); and NASA (USA).\nFacilities: Herschel, IRAM:30m, APEX\n\nPublished - 2041-8205_781_1_L15.pdf
Submitted - 1401.2300v1.pdf
", "abstract": "We report the first results from a spectroscopic survey of the [C II] 158 \u03bcm line from a sample of intermediate redshift (0.2 10^(11.5) L_\u2609), using the Spectral and Photometric Imaging REceiver-Fourier Transform Spectrometer on board the Herschel Space Observatory. This is the first survey of [C II] emission, an important tracer of star formation, at a redshift range where the star formation rate density of the universe increases rapidly. We detect strong [C II] 158 \u03bcm line emission from over 80% of the sample. We find that the [C II] line is luminous, in the range (0.8-4) \u00d7 10^(\u20133) of the far-infrared continuum luminosity of our sources, and appears to arise from photodissociation regions on the surface of molecular clouds. The L [C_(II)]/L_(IR) ratio in our intermediate redshift (U)LIRGs is on average ~10 times larger than that of local ULIRGs. Furthermore, we find that the L [C_(II)]/L_(IR) and L [C_(II)]/L_(CO(1-0)) ratios in our sample are similar to those of local normal galaxies and high-z star-forming galaxies. ULIRGs at z ~ 0.5 show many similarities to the properties of local normal and high-z star-forming galaxies. Our findings strongly suggest that rapid evolution in the properties of the star-forming regions of (U)LIRGs is likely to have occurred in the last 5 billion years.", "date": "2014-01-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "781", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L15", "id_number": "CaltechAUTHORS:20140211-111507479", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140211-111507479", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/K00106X/1" }, { "agency": "John Fell Oxford University Press (OUP) Research Fund" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1088/2041-8205/781/1/L15", "primary_object": { "basename": "1401.2300v1.pdf", "url": "https://authors.library.caltech.edu/records/p0t3n-wjk07/files/1401.2300v1.pdf" }, "related_objects": [ { "basename": "2041-8205_781_1_L15.pdf", "url": "https://authors.library.caltech.edu/records/p0t3n-wjk07/files/2041-8205_781_1_L15.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Rigopoulou, D.; Hopwood, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/7vp5x-kb465", "eprint_id": 44525, "eprint_status": "archive", "datestamp": "2023-08-22 11:26:35", "lastmod": "2023-10-26 14:22:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" } ] }, "title": "HerMES: dust attenuation and star formation activity in ultraviolet-selected samples from z \u223c 4 to \u223c 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical; galaxies: star formation; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 October 9. Received 2013 October 9; in original form 2013 July 30.\n\nWe thank the referee for useful comments and suggestions. SH\nand VB acknowledge support from the Centre National d'Etudes\nSpatiales. We thank the COSMOS team for sharing data essential to this study. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM\n(http://hedam.oamp.fr/HerMES).\n\nPublished - MNRAS-2014-Heinis-1268-83.pdf
", "abstract": "We study the link between observed ultraviolet (UV) luminosity, stellar mass and dust attenuation within rest-frame UV-selected samples at z \u223c 4,\u2009 \u223c 3 and \u223c1.5. We measure by stacking at 250, 350 and 500\u2009\u03bcm in the Herschel/Spectral and Photometric Imaging Receiver images from the Herschel Multi-Tiered Extragalactic Survey (HerMES) program the average infrared luminosity as a function of stellar mass and UV luminosity. We find that dust attenuation is mostly correlated with stellar mass. There is also a secondary dependence with UV luminosity: at a given UV luminosity, dust attenuation increases with stellar mass, while at a given stellar mass it decreases with UV luminosity. We provide new empirical recipes to correct for dust attenuation given the observed UV luminosity and the stellar mass. Our results also enable us to put new constraints on the average relation between star formation rate (SFR) and stellar mass at z \u223c 4, \u223c3 and \u223c1.5. The SFR\u2013stellar mass relations are well described by power laws (SFR\u221dM^(0.7__\u2217), with the amplitudes being similar at z \u223c 4 and \u223c3, and decreasing by a factor of 4 at z \u223c 1.5 at a given stellar mass. We further investigate the evolution with redshift of the specific SFR. Our results are in the upper range of previous measurements, in particular at z \u223c 3, and are consistent with a plateau at 3 < z < 4. Current model predictions (either analytic, semi-analytic or hydrodynamic) are inconsistent with these values, as they yield lower predictions than the observations in the redshift range we explore. We use these results to discuss the star formation histories of galaxies in the framework of the main sequence of star-forming galaxies. Our results suggest that galaxies at high redshift (2.5 < z < 4) stay around 1 Gyr on the main sequence. With decreasing redshift, this time increases such that z = 1 main-sequence galaxies with 108", "date": "2014-01-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "437", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1268-1283", "id_number": "CaltechAUTHORS:20140326-101000362", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140326-101000362", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'Etudes Spatiales (CNES)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/stt1960", "primary_object": { "basename": "MNRAS-2014-Heinis-1268-83.pdf", "url": "https://authors.library.caltech.edu/records/7vp5x-kb465/files/MNRAS-2014-Heinis-1268-83.pdf" }, "resource_type": "article", "pub_year": "2014", "author_list": "Heinis, S.; Buat, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/d44q1-ks913", "eprint_id": 43598, "eprint_status": "archive", "datestamp": "2023-08-22 11:22:22", "lastmod": "2023-10-25 23:41:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. Darren" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Sayers-J", "name": { "family": "Sayers", "given": "J." }, "orcid": "0000-0002-8213-3784" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: Candidate High-redshift Galaxies Discovered with Herschel/SPIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter: galaxies", "note": "\u00a9 2014 American Astronomical Society. Received 2013 July 12; accepted 2013 October 25; published 2013 December 13.\n\nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nThis material is based upon work supported by the National\nAeronautics and Space Administration under grant No. 12-\nADAP12-0139 issued through the ADAP program. Part of this\nwork was performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). The SPIRE data presented in paper this have been released through the Herschel Database in Marseille, HeDAM (http://hedam.oamp.fr/HerMES). Some of this material is based upon work at the Caltech Submillimeter Observatory, which was operated by the California Institute of Technology under cooperative\nagreement with the National Science Foundation (AST-\n0838261). The Submillimeter Array is a joint project between\nthe Smithsonian Astrophysical Observatory and the Academia\nSinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Based in part on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement and the CARMA partner universities. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership\namong the California Institute of Technology, the University\nof California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Based in part on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. This research made use of Astropy (http://www.astropy.org), a community-developed core Python package for Astronomy (Astropy Collaboration 2013). This research has made use of NASA's Astrophysics Data System Bibliographic Services. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\nFacilities: Herschel (SPIRE), CSO (Bolocam, Z-Spec),\nCARMA, SMA, IRAM:Interferometer, Keck:I (LRIS), GTC\n(OSIRIS), MERLIN.\n\nPublished - 0004-637X_780_1_75.pdf
Submitted - 1310.7583v1.pdf
", "abstract": "We present a method for selecting z > 4 dusty, star-forming galaxies (DSFGs) using Herschel/Spectral and Photometric Imaging Receiver 250/350/500 \u03bcm flux densities to search for red sources. We apply this method to 21 deg^2 of data from the HerMES survey to produce a catalog of 38 high-z candidates. Follow-up of the first five of these sources confirms that this method is efficient at selecting high-z DSFGs, with 4/5 at z = 4.3-6.3 (and the remaining source at z = 3.4), and that they are some of the most luminous dusty sources known. Comparison with previous DSFG samples, mostly selected at longer wavelengths (e.g., 850 \u03bcm) and in single-band surveys, shows that our method is much more efficient at selecting high-z DSFGs, in the sense that a much larger fraction are at z > 3. Correcting for the selection completeness and purity, we find that the number of bright (S_(500\u03bcm) \u2265 30 mJy), red Herschel sources is 3.3 \u00b1 0.8 deg^(\u20132). This is much higher than the number predicted by current models, suggesting that the DSFG population extends to higher redshifts than previously believed. If the shape of the luminosity function for high-z DSFGs is similar to that at z ~ 2, rest-frame UV based studies may be missing a significant component of the star formation density at z = 4-6, even after correction for extinction.", "date": "2014-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "780", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 75", "id_number": "CaltechAUTHORS:20140131-080059273", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140131-080059273", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "12- ADAP12-0139" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "Smithsonian Institution" }, { "agency": "Academia Sinica" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Caltech Associates" }, { "agency": "University of Chicago" }, { "agency": "State of California" }, { "agency": "State of Illinois" }, { "agency": "State of Maryland" }, { "agency": "CARMA partner universities" }, { "agency": "W. M. Keck Foundation" } ] }, "doi": "10.1088/0004-637X/780/1/75", "primary_object": { "basename": "0004-637X_780_1_75.pdf", "url": "https://authors.library.caltech.edu/records/d44q1-ks913/files/0004-637X_780_1_75.pdf" }, "related_objects": [ { "basename": "1310.7583v1.pdf", "url": "https://authors.library.caltech.edu/records/d44q1-ks913/files/1310.7583v1.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Dowell, C. Darren; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/jjach-q5025", "eprint_id": 44185, "eprint_status": "archive", "datestamp": "2023-08-19 22:53:58", "lastmod": "2023-10-26 00:16:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck intermediate results XIII. Constraints on peculiar velocities", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations, cosmic background radiation, large-scale structure of Universe, galaxies: clusters: general", "note": "\u00a9 2014 ESO. \n\nReceived 15 February 2013. Accepted 18 November 2013. Published online 13 January 2014. \n\nThe development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/Planck. The authors from the consortia funded principally by CNES, CNRS, ASI, NASA, and Danish Natural Research Council acknowledge the use of the pipeline running infrastructures Magique3 at Institut d'Astrophysique de Paris (France), CPAC at Cambridge (UK), and USPDC at\nIPAC (USA). We acknowledge the use of the HEALPix package, WMAP data and the LAMBDA archive http://lambda.gsfc.nasa.gov).\n\nPublished - aa21299-13.pdf
Submitted - 1303.5090v2.pdf
", "abstract": "Using Planck data combined with the Meta Catalogue of X-ray detected Clusters of galaxies (MCXC), we address the study of peculiar motions by searching for evidence of the kinetic Sunyaev-Zeldovich effect (kSZ). By implementing various filters designed to extract the kSZ generated at the positions of the clusters, we obtain consistent constraints on the radial peculiar velocity average, root mean square (rms), and local bulk flow amplitude at different depths. For the whole cluster sample of average redshift 0.18, the measured average radial peculiar velocity with respect to the cosmic microwave background (CMB) radiation at that redshift, i.e., the kSZ monopole, amounts to 72 \u00b1 60 km\u2009s^(-1). This constitutes less than 1% of the relative Hubble velocity of the cluster sample with respect to our local CMB frame. While the linear \u039bCDM prediction for the typical cluster radial velocity rms at z = 0.15 is close to 230 km\u2009s^(-1), the upper limit imposed by Planck data on the cluster subsample corresponds to 800 km\u2009s^(-1) at 95% confidence level, i.e., about three times higher. Planck data also set strong constraints on the local bulk flow in volumes centred on the Local Group. There is no detection of bulk flow as measured in any comoving sphere extending to the maximum redshift covered by the cluster sample. A blind search for bulk flows in this sample has an upper limit of 254 km\u2009s^(-1) (95% confidence level) dominated by CMB confusion and instrumental noise, indicating that the Universe is largely homogeneous on Gpc scales. In this context, in conjunction with supernova observations, Planck is able to rule out a large class of inhomogeneous void models as alternatives to dark energy or modified gravity. The Planck constraints on peculiar velocities and bulk flows are thus consistent with the \u039bCDM scenario.", "date": "2014-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "561", "publisher": "EDP Sciences", "pagerange": "Art. No. A97", "id_number": "CaltechAUTHORS:20140306-131731569", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140306-131731569", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "European Space Agency (ESA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "NASA" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "CSIC (Spain)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MICINN)" }, { "agency": "Junta de Andaluc\u00eda" }, { "agency": "RES (Spain)" }, { "agency": "Tekes (Finland)" }, { "agency": "Academy of Finland" }, { "agency": "CSC (Finland)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "SER/SSO (Switzerland)" }, { "agency": "Research Council of Norway" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "PRACE (EU)" }, { "agency": "Danish Natural Research Council" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Institut national du patrimoine (INP)" }, { "agency": "Ministro da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" } ] }, "corp_creators": { "items": [ "Planck Collaboration" ] }, "doi": "10.1051/0004-6361/201321299", "primary_object": { "basename": "1303.5090v2.pdf", "url": "https://authors.library.caltech.edu/records/jjach-q5025/files/1303.5090v2.pdf" }, "related_objects": [ { "basename": "aa21299-13.pdf", "url": "https://authors.library.caltech.edu/records/jjach-q5025/files/aa21299-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/2p2hz-h5d70", "eprint_id": 44186, "eprint_status": "archive", "datestamp": "2023-08-19 22:54:05", "lastmod": "2023-10-26 00:16:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "The evolution of the dust temperatures of galaxies in the SFR\u2013M_\u2217 plane up to z ~ 2", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, infrared: galaxies, galaxies: starburst", "note": "\u00a9 2014 ESO. Received 5 July 2013. Accepted 11 November 2013. \nPublished online 07 January 2014.\n\nHerschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA.\n\nPACS has been developed by a consortium of institutes\nled by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by funding agencies BMVIT (Austria) ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). D.E. received support of the European Community\nFramework Programme 7, FP7-SPACE Astrodeep, grant agreement No. 312725\n\nPublished - aa22217-13.pdf
Submitted - 1311.2956v1.pdf
", "abstract": "We study the evolution of the dust temperature of galaxies in the SFR\u2212 M\u2217 plane up to z ~ 2 using far-infrared and submillimetre observations from the Herschel Space Observatory taken as part of the PACS Evolutionary Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time key programmes. Starting from a sample of galaxies with reliable star-formation rates (SFRs), stellar masses (M_\u2217) and redshift estimates, we grid the SFR\u2212 M_\u2217parameter space in several redshift ranges and estimate the mean dust temperature (T_(dust)) of each SFR\u2013M_\u2217 \u2212 z bin. Dust temperatures are inferred using the stacked far-infrared flux densities (100\u2013500\u2009 \u03bcm) of our SFR\u2013M_\u2217 \u2212 z bins. At all redshifts, the dust temperature of galaxies smoothly increases with rest-frame infrared luminosities (L_(IR)), specific SFRs (SSFR; i.e., SFR/M_\u2217), and distances with respect to the main sequence (MS) of the SFR\u2212 M_\u2217 plane (i.e., \u0394log (SSFR)_(MS) = log [SSFR(galaxy)/SSFR_(MS)(M_\u2217,z)]). The T_(dust) \u2212 SSFR and T_(dust) \u2212 \u0394log (SSFR)_(MS) correlations are statistically much more significant than the T_(dust) \u2212 LIR one. While the slopes of these three correlations are redshift-independent, their normalisations evolve smoothly from z = 0 and z ~ 2. We convert these results into a recipe to derive T_(dust) from SFR, M_\u2217 and z, valid out to z ~ 2 and for the stellar mass and SFR range covered by our stacking analysis. The existence of a strong T_(dust) \u2212 \u0394log (SSFR)_(MS) correlation provides us with several pieces of information on the dust and gas content of galaxies. Firstly, the slope of the T_(dust) \u2212 \u0394log (SSFR)_(MS) correlation can be explained by the increase in the star-formation efficiency (SFE; SFR/M_(gas)) with \u0394log (SSFR)_(MS) as found locally by molecular gas studies. Secondly, at fixed \u0394log (SSFR)_(MS), the constant dust temperature observed in galaxies probing wide ranges in SFR and M_\u2217 can be explained by an increase or decrease in the number of star-forming regions with comparable SFE enclosed in them. And thirdly, at high redshift, the normalisation towards hotter dust temperature of the T_(dust) \u2212 \u0394log (SSFR)_(MS) correlation can be explained by the decrease in the metallicities of galaxies or by the increase in the SFE of MS galaxies. All these results support the hypothesis that the conditions prevailing in the star-forming regions of MS and far-above-MS galaxies are different. MS galaxies have star-forming regions with low SFEs and thus cold dust, while galaxies situated far above the MS seem to be in a starbursting phase characterised by star-forming regions with high SFEs and thus hot dust.", "date": "2014-01", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "561", "publisher": "EDP Sciences", "pagerange": "Art. No. A86", "id_number": "CaltechAUTHORS:20140306-150020894", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140306-150020894", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "ASI/INAF (Italy)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "CSA (Canada)" }, { "agency": "NAOC (China)" }, { "agency": "CEA (France)" }, { "agency": "CNES (France)" }, { "agency": "CNRS (France)" }, { "agency": "ASI (Italy)" }, { "agency": "MCINN (Spain)" }, { "agency": "SNSB (Sweden)" }, { "agency": "STFC (UK)" }, { "agency": "UKSA (UK)" }, { "agency": "NASA" }, { "agency": "European Community Framework Programme 7 (FP7-SPACE Astrodeep)", "grant_number": "312725" } ] }, "doi": "10.1051/0004-6361/201322217", "primary_object": { "basename": "1311.2956v1.pdf", "url": "https://authors.library.caltech.edu/records/2p2hz-h5d70/files/1311.2956v1.pdf" }, "related_objects": [ { "basename": "aa22217-13.pdf", "url": "https://authors.library.caltech.edu/records/2p2hz-h5d70/files/aa22217-13.pdf" } ], "resource_type": "article", "pub_year": "2014", "author_list": "Magnelli, B. and Bock, J." }, { "id": "https://authors.library.caltech.edu/records/7zn0x-8s882", "eprint_id": 43423, "eprint_status": "archive", "datestamp": "2023-08-22 11:05:32", "lastmod": "2023-10-25 23:32:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bussmann-R-S", "name": { "family": "Bussmann", "given": "R. S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "Gravitational Lens Models Based on Submillimeter Array Imaging of Herschel-selected Strongly Lensed Sub-millimeter Galaxies at z > 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: fundamental parameters; galaxies: halos; galaxies: high-redshift; gravitational lensing: strong", "note": "\u00a9 2013 American Astronomical Society. Received 2013 August 31; accepted 2013 October 11; published 2013 November 22. The results described in this paper are based on observations obtained with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The Herschel-ATLAS is a project with Herschel. The H-ATLAS Web site is http://www.h-atlas.org/. US participants in HATLAS acknowledge support from NASA through a contract from JPL. This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists, and a mission scientist.\nHerMES is described in Oliver et al. (2012). The HerMES data\npresented in this paper will be released through the Herschel Database in Marseille HeDaM (36). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). R.S.B. acknowledges support from the SMA Fellowship program. H.F, A.C., and J.L.W. acknowledge support from NSF CAREER AST-0645427. A portion of this work was completed at the Aspen Center for Physics during a 2013 summer workshop on dusty galaxies at high redshift. R.S.B. acknowledges the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation Grant No. PHY-1066293. S.J.O., L.W., and A.S. acknowledge support from the Science and Technology Facilities Council (grant No. ST/I000976/1). M.N. acknowledges financial support from PRIN INAF 2012\nproject \"Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Large Area Survey.\" A.O. and R.G. acknowledge support from the Programme National Cosmologie et Galaxies (PNCG). J.G.N. acknowledges financial support from Spanish CSIC for 36 http://hedam.oamp.fr/HerMES a JAE-DOC fellowship and partial financial support from the Spanish Ministerio de Ciencia e Innovacion project AYA2010-\n21766-C03-01. I.P.-F., P.M.-N., N.L. and A.S. acknowledge support from the Spanish grant AYA2010-21697-C05-04. We thank K. Rosenfeld for assistance in implementing the visibility-plane aspect of the lens modeling software used in this paper. We thank the anonymous referee for a timely review that provided useful comments and helped improved the clarity of the manuscript. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\nObservations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research\nin Astronomy, Inc., under a cooperative agreement with\nthe NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Minist\u00e9rio da Ci\u00eancia, Tecnologia e Inova\u00e7\u00e3o (Brazil) and Ministerio de Ciencia, Tecnolog\u00eda e Innovaci\u03ccn Productiva (Argentina). The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias.\nFacilities: SMA, MMT, Gemini: South, ING: Herschel,\nVLT: Melipal\n\nPublished - 0004-637X_779_1_25.pdf
Submitted - 1309.0836v2.pdf
", "abstract": "Strong gravitational lenses are now being routinely discovered in wide-field surveys at (sub-)millimeter wavelengths. We present Submillimeter Array (SMA) high-spatial resolution imaging and Gemini-South and Multiple Mirror Telescope optical spectroscopy of strong lens candidates discovered in the two widest extragalactic surveys conducted by the Herschel Space Observatory: the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS) and the Herschel Multi-tiered Extragalactic Survey (HerMES). From a sample of 30 Herschel sources with S_(500) > 100 mJy, 21 are strongly lensed (i.e., multiply imaged), 4 are moderately lensed (i.e., singly imaged), and the remainder require additional data to determine their lensing status. We apply a visibility-plane lens modeling technique to the SMA data to recover information about the masses of the lenses as well as the intrinsic (i.e., unlensed) sizes (r_(half)) and far-infrared luminosities (L_(FIR)) of the lensed submillimeter galaxies (SMGs). The sample of lenses comprises primarily isolated massive galaxies, but includes some groups and clusters as well. Several of the lenses are located at z_(lens) > 0.7, a redshift regime that is inaccessible to lens searches based on Sloan Digital Sky Survey spectroscopy. The lensed SMGs are amplified by factors that are significantly below statistical model predictions given the 500 \u03bcm flux densities of our sample. We speculate that this may reflect a deficiency in our understanding of the intrinsic sizes and luminosities of the brightest SMGs. The lensed SMGs span nearly one decade in L_(FIR) (median L_(FIR) = 7.9 \u00d7 10^(12) L_\u2609) and two decades in FIR luminosity surface density (median \u03a3_(FIR) = 6.0 \u00d7 10^(11) L_\u2609 kpc^(\u20132)). The strong lenses in this sample and others identified via (sub-)mm surveys will provide a wealth of information regarding the astrophysics of galaxy formation and evolution over a wide range in redshift.", "date": "2013-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "779", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 25", "id_number": "CaltechAUTHORS:20140117-085640459", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140117-085640459", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "SMA Fellowship Program" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Programme National Cosmologie et Galaxies (PNCG)" }, { "agency": "CSIC JAE-DOC fellowship" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2010- 21766-C03-01" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "AYA2010-21697-C05-04" }, { "agency": "Smithsonian Institution" }, { "agency": "Academia Sinica" } ] }, "doi": "10.1088/0004-637X/779/1/25", "primary_object": { "basename": "1309.0836v2.pdf", "url": "https://authors.library.caltech.edu/records/7zn0x-8s882/files/1309.0836v2.pdf" }, "related_objects": [ { "basename": "0004-637X_779_1_25.pdf", "url": "https://authors.library.caltech.edu/records/7zn0x-8s882/files/0004-637X_779_1_25.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Bussmann, R. S.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/z6k01-pg348", "eprint_id": 43424, "eprint_status": "archive", "datestamp": "2023-08-22 11:05:38", "lastmod": "2023-10-25 23:32:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "L." }, "orcid": "0000-0002-4242-3015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: The Contribution to the Cosmic Infrared Background from Galaxies Selected by Mass and Redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: evolution; infrared: galaxies; large-scale structure of universe; submillimeter: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 April 1; accepted 2013 October 18; published 2013 November 22.\n\nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nThe authors warmly thank Duncan Hanson, PhilKorngut, Zak\nStaniszewski, and Yoshihiro Ueda. We also thank the anonymous\nreferee, whose careful comments greatly improved this\npaper. Much credit belongs to C. Barth Netterfield and Enzo\nPascale for inspiring the simultaneous stacking algorithm, and to whom we are thankful. SPIRE has been developed by a\nconsortium of institutes led by Cardiff Univ. (UK) and including:\nUniv. Lethbridge (Canada); NAOC (China); CEA, LAM\n(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC,\nUniv. Colorado (USA). This development has been supported\nby national funding agencies: CSA (Canada); NAOC (China);\nCEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain);\nSNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\n\nPublished - 0004-637X_779_1_32.pdf
Submitted - 1304.0446v2.pdf
", "abstract": "We quantify the fraction of the cosmic infrared background (CIB) that originates from galaxies identified in the UV/optical/near-infrared by stacking 81,250 (~35.7 arcmin^(\u20132)) K-selected sources (K_(AB) < 24.0) split according to their rest-frame U \u2013 V versus V \u2013 J colors into 72,216 star-forming and 9034 quiescent galaxies, on maps from Spitzer/MIPS (24 \u03bcm), Herschel/PACS (100, 160 \u03bcm), Herschel/SPIRE (250, 350, 500 \u03bcm), and AzTEC (1100 \u03bcm). The fraction of the CIB resolved by our catalog is (69% \u00b1 15%) at 24 \u03bcm, (78% \u00b1 17%) at 70 \u03bcm, (58% \u00b1 13%) at 100 \u03bcm, (78% \u00b1 18%) at 160 \u03bcm, (80% \u00b1 17%) at 250 \u03bcm, (69% \u00b1 14%) at 350 \u03bcm, (65% \u00b1 12%) at 500 \u03bcm, and (45% \u00b1 8%) at 1100 \u03bcm. Of that total, about 95% originates from star-forming galaxies, while the remaining 5% is from apparently quiescent galaxies. The CIB at \u03bb \u227e 200 \u03bcm appears to be sourced predominantly from galaxies at z \u227e 1, while at \u03bb \u2273 200 \u03bcm the bulk originates from 1 \u227e z \u227e 2. Galaxies with stellar masses log(M/M_\u2609) = 9.5-11 are responsible for the majority of the CIB, with those in the log(M/M_\u2609) = 9.5-10 bin contributing mostly at \u03bb < 250 \u03bcm, and those in the log(M/M_\u2609) = 10-11 bin dominating at \u03bb > 350 \u03bcm. The contribution from galaxies in the log(M/M_\u2609) = 9.0-9.5 (lowest) and log(M/M_\u2609) = 11.0-12.0 (highest) stellar-mass bins contribute the least\u2014both of order 5%\u2014although the highest stellar-mass bin is a significant contributor to the luminosity density at z \u2273 2. The luminosities of the galaxies responsible for the CIB shifts from combinations of \"normal\" and luminous infrared galaxies (LIRGs) at \u03bb \u227e 160 \u03bcm, to LIRGs at 160 \u227e \u03bb \u227e 500 \u03bcm, to finally LIRGs and ultra-luminous infrared galaxies at \u03bb \u2273 500 \u03bcm. Stacking analyses were performed using SIMSTACK, a novel algorithm designed to account for possible biases in the stacked flux density due to clustering. It is made available to the public at www.astro.caltech.edu/~viero/viero_homepage/toolbox.html.", "date": "2013-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "779", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 32", "id_number": "CaltechAUTHORS:20140117-095413552", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140117-095413552", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1088/0004-637X/779/1/32", "primary_object": { "basename": "0004-637X_779_1_32.pdf", "url": "https://authors.library.caltech.edu/records/z6k01-pg348/files/0004-637X_779_1_32.pdf" }, "related_objects": [ { "basename": "1304.0446v2.pdf", "url": "https://authors.library.caltech.edu/records/z6k01-pg348/files/1304.0446v2.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Viero, M. P.; Moncelsi, L.; et el." }, { "id": "https://authors.library.caltech.edu/records/fstgf-6gv87", "eprint_id": 43440, "eprint_status": "archive", "datestamp": "2023-08-22 11:06:12", "lastmod": "2023-10-25 23:32:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bothwell-M-S", "name": { "family": "Bothwell", "given": "M. S." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Downes-T-P", "name": { "family": "Downes", "given": "T. P." } } ] }, "title": "SPT 0538\u201350: Physical Conditions in the Interstellar Medium of a Strongly Lensed Dusty Star-forming Galaxy at z = 2.8", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: individual; gravitational lensing: strong; submillimeter: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 July 3; accepted 2013 September 11; published 2013 November 26. We thank the anonymous referee who provided comments that helped improve the clarity of this manuscript. The authors\nwould like to thank N. Rangwala for sharing the M82 CO flux\ndensities. M.S.B. would like to acknowledge the hospitality of the Aspen Center for Physics, where some of this manuscript was written. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Support is provided by National Science Foundation grants AST-1009649, ANT-0638937, PHY-1125897, and PHYS-1066293. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00957. S and #2011.0.00958. S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility\nof the National Science Foundation operated under a cooperative agreement by Associated Universities, Inc. Partial support for this work was provided by NASA through grant HST-GO-12659 from the Space Telescope Science Institute and awards for Herschel analysis issued by JPL/Caltech for OT1_dmarrone_1, OT1_jvieira_4, and OT2_jvieira_5. \nFacilities: HST/WFC3, Spitzer/IRAC, ALMA, APEX,\nATCA, VLT:Kueyen, SMA, Herschel\n\nPublished - 0004-637X_779_1_67.pdf
Submitted - 1309.3275v1.pdf
", "abstract": "We present observations of SPT-S J053816\u20135030.8, a gravitationally lensed dusty star-forming galaxy (DSFG) at z = 2.7817 that was first discovered at millimeter wavelengths by the South Pole Telescope. SPT 0538\u201350 is typical of the brightest sources found by wide-field millimeter-wavelength surveys, being lensed by an intervening galaxy at moderate redshift (in this instance, at z = 0.441). We present a wide array of multi-wavelength spectroscopic and photometric data on SPT 0538\u201350, including data from ALMA, Herschel PACS and SPIRE, Hubble, Spitzer, the Very Large Telescope, ATCA, APEX, and the Submillimeter Array. We use high-resolution imaging from the Hubble Space Telescope to de-blend SPT 0538\u201350, separating DSFG emission from that of the foreground lens. Combined with a source model derived from ALMA imaging (which suggests a magnification factor of 21 \u00b1 4), we derive the intrinsic properties of SPT 0538\u201350, including the stellar mass, far-IR luminosity, star formation rate, molecular gas mass, and\u2014using molecular line fluxes\u2014the excitation conditions within the interstellar medium. The derived physical properties argue that we are witnessing compact, merger-driven star formation in SPT 0538\u201350 similar to local starburst galaxies and unlike that seen in some other DSFGs at this epoch.", "date": "2013-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "779", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 67", "id_number": "CaltechAUTHORS:20140121-072415768", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140121-072415768", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Smithsonian Institution" }, { "agency": "Academia Sinica" }, { "agency": "NSF", "grant_number": "AST-1009649" }, { "agency": "NSF", "grant_number": "ANT-0638937" }, { "agency": "NSF", "grant_number": "PHY-1125897" }, { "agency": "NSF", "grant_number": "PHYS-1066293" }, { "agency": "NASA Space Telescope Science Institute", "grant_number": "HST-GO-12659" } ] }, "doi": "10.1088/0004-637X/779/1/67", "primary_object": { "basename": "0004-637X_779_1_67.pdf", "url": "https://authors.library.caltech.edu/records/fstgf-6gv87/files/0004-637X_779_1_67.pdf" }, "related_objects": [ { "basename": "1309.3275v1.pdf", "url": "https://authors.library.caltech.edu/records/fstgf-6gv87/files/1309.3275v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Bothwell, M. S.; Vieira, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/r2b11-jdy32", "eprint_id": 43229, "eprint_status": "archive", "datestamp": "2023-08-22 11:03:25", "lastmod": "2023-10-25 23:22:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-Nicholas", "name": { "family": "Lee", "given": "Nicholas" } }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "Caitlin M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" }, { "id": "Hung-Chao-Ling", "name": { "family": "Hung", "given": "Chao-Ling" }, "orcid": "0000-0002-6879-3639" }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "Emeric" } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "Olivier" }, "orcid": "0000-0002-7303-4397" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "Herve" }, "orcid": "0000-0002-1371-5705" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "Peter" }, "orcid": "0000-0003-3578-6843" }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "Jeyhan S." }, "orcid": "0000-0001-9187-3605" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "Isaac" } }, { "id": "Salvato-Mara", "name": { "family": "Salvato", "given": "Mara" }, "orcid": "0000-0001-7116-9303" }, { "id": "Aravena-M", "name": { "family": "Aravena", "given": "M." }, "orcid": "0000-0002-6290-3198" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } } ] }, "title": "Multi-wavelength SEDs of Herschel-selected Galaxies in the COSMOS Field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; infrared: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 June 24; accepted 2013 September 27; published 2013 November 12. D. B. Sanders and C. M. Casey acknowledge the hospitality\nof the Aspen Center for Physics, which is supported by the\nNational Science Foundation grant No. PHY-1066293. C. M.\nCasey is generously supported by a Hubble Fellowship from\nSpace Telescope Science Institute, grant HST-HF-51268.01-A.\nCOSMOS is based on observations with the NASA/ESA\nHubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555; also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; and the Canada\u2013France\u2013Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven,\nCSL, IMEC (Belgium); CEA, LAM (France);MPIA (Germany);\nINAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).\nSPIRE has been developed by a consortium of institutes led\nby Cardiff University (UK) and including Univ. Lethbridge\n(Canada); NAOC (China); CEA, LAM (France); IFSI, Univ.\nPadua (Italy); IAC (Spain); Stockholm Observatory (Sweden);\nImperial College London, RAL, UCL-MSSL, UKATC, Univ.\nSussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA).\nThis development has been supported by national funding\nagencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS\n(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC\n(UK); and NASA (USA).\n\nPublished - 0004-637X_778_2_131.pdf
Submitted - 1310.0474v1.pdf
", "abstract": "We combine Herschel Photodetector Array Camera and Spectrometer and Spectral and Photometric Imaging Receiver maps of the full 2 deg^2 Cosmic Evolution Survey (COSMOS) field with existing multi-wavelength data to obtain template and model-independent optical-to-far-infrared spectral energy distributions (SEDs) for 4218 Herschel-selected sources with log(L_(IR)/L_\u2609) = 9.4-13.6 and z = 0.02-3.54. Median SEDs are created by binning the optical to far-infrared (FIR) bands available in COSMOS as a function of infrared luminosity. Herschel probes rest-frame wavelengths where the bulk of the infrared radiation is emitted, allowing us to more accurately determine fundamental dust properties of our sample of infrared luminous galaxies. We find that the SED peak wavelength (\u03bbpeak) decreases and the dust mass (M_(dust)) increases with increasing total infrared luminosity (L_(IR)). In the lowest infrared luminosity galaxies (log(L_(IR)/L_\u2609) = 10.0-11.5), we see evidence of polycyclic aromatic hydrocarbon (PAH) features (\u03bb ~ 7-9 \u03bcm), while in the highest infrared luminosity galaxies (L_(IR) > 10^(12) L_\u2609) we see an increasing contribution of hot dust and/or power-law emission, consistent with the presence of heating from an active galactic nucleus (AGN). We study the relationship between stellar mass and star formation rate of our sample of infrared luminous galaxies and find no evidence that Herschel-selected galaxies follow the SFR/M_* \"main sequence\" as previously determined from studies of optically selected, star-forming galaxies. Finally, we compare the mid-infrared to FIR properties of our infrared luminous galaxies using the previously defined diagnostic, IR8 \u2261 L_(IR)/L_8, and find that galaxies with L_(IR) \u2273 10^(11.3) L_\u2609 tend to systematically lie above (\u00d7 3-5) the IR8 \"infrared main sequence,\" suggesting either suppressed PAH emission or an increasing contribution from AGN heating.", "date": "2013-12-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "778", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 131", "id_number": "CaltechAUTHORS:20140106-131441483", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140106-131441483", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "PHY-1066293" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51268.01-A" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/778/2/131", "primary_object": { "basename": "0004-637X_778_2_131.pdf", "url": "https://authors.library.caltech.edu/records/r2b11-jdy32/files/0004-637X_778_2_131.pdf" }, "related_objects": [ { "basename": "1310.0474v1.pdf", "url": "https://authors.library.caltech.edu/records/r2b11-jdy32/files/1310.0474v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Lee, Nicholas; Sanders, D. B.; et el." }, { "id": "https://authors.library.caltech.edu/records/hsgzy-enj48", "eprint_id": 42866, "eprint_status": "archive", "datestamp": "2023-08-22 10:55:24", "lastmod": "2023-10-25 23:06:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The SCUBA-2 Cosmology Legacy Survey: demographics of the 450-\u03bcm population", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: starburst; submillimetre: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 August 20. Received 2013 August 9; in original form 2013 May 15.\n\nFirst published online: September 28, 2013.\n\nWe thank the anonymous referee for suggestions which greatly\nenhanced this work. We also thank B. Sidthorpe and W. Holland for many useful discussions related to the reduction and analysis of SCUBA-2 imaging. JSD acknowledges the support of the Royal Society via a Wolfson Research Merit award and the support of the European Research\nCouncil via the award of an Advanced Grant. IRS acknowledges support from STFC (ST/I001573/1), a Leverhulme\nFellowship, the ERC Advanced Investigator programme\nDUSTYGAL and a Royal Society/Wolfson Merit Award. LW and SJO were supported by the Science and Technology\nFacilities Council (grant number ST/I000976/1). Many thanks to the JCMT telescope operators: J.Hoge, J. Wouterloot\nand W.Montgomerie, without whom these observations would\nnot be possible. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada and (until 2013 March 31) the Netherlands Organisation for Scientific Research. Additional funds for the construction of\nSCUBA-2 were provided by the Canada Foundation for Innovation. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK), including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). All the data used in this analysis are available through the JCMT, Herschel, HST and Spitzer archives.\n\nPublished - MNRAS-2013-Roseboom-430-48.pdf
Submitted - 1308.4443.pdf
Supplemental Material - 3409207_Supplementary_Data.zip
Supplemental Material - tablea1_cosmos.txt
Supplemental Material - tablea2_uds.txt
Supplemental Material - tablea3_seds.txt
", "abstract": "We investigate the multiwavelength properties of a sample of 450-\u03bcm-selected sources from the SCUBA-2 Cosmology Legacy Survey. A total of 69 sources were identified above 4\u03c3 in deep SCUBA-2 450-\u03bcm observations overlapping the UDS and COSMOS fields and covering 210\u2009arcmin^2 to a typical depth of \u03c3_450 = 1.5\u2009mJy. Reliable cross-identifications are found for 58 sources (84\u2009per\u2009cent) in Spitzer and Hubble Space Telescope WFC3/IR data. The photometric redshift distribution (dN/dz) of 450-\u03bcm-selected sources is presented, showing a broad peak in the redshift range 1 < z < 3 and a median of z = 1.4. Combining the SCUBA-2 photometry with Herschel SPIRE data from HerMES, the submm spectral energy distribution (SED) is examined via the use of modified blackbody fits, yielding aggregate values for the IR luminosity, dust temperature and emissivity of \u3008LIR\u3009 = 10^(12 \u00b1 0.8)\u2009L_\u2299, \u3008T_D\u3009 = 42 \u00b1 11\u2009K and \u3008\u03b2_D\u3009 = 1.6 \u00b1 0.5, respectively. The relationship between these SED parameters and the physical properties of galaxies is investigated, revealing correlations between TD and LIR and between \u03b2D and both stellar mass and effective radius. The connection between the star formation rate (SFR) and stellar mass is explored, with 24\u2009per\u2009cent of 450-\u03bcm sources found to be 'starbursts', i.e. displaying anomalously high specific SFRs. However, both the number density and observed properties of these 'starburst' galaxies are found to be consistent with the population of normal star-forming galaxies.", "date": "2013-11-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "436", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "430-448", "id_number": "CaltechAUTHORS:20131205-150159773", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131205-150159773", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)", "grant_number": "DUSTYGAL 321334" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I001573/1" }, { "agency": "Leverhulme Trust" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" } ] }, "doi": "10.1093/mnras/stt1577", "primary_object": { "basename": "1308.4443.pdf", "url": "https://authors.library.caltech.edu/records/hsgzy-enj48/files/1308.4443.pdf" }, "related_objects": [ { "basename": "3409207_Supplementary_Data.zip", "url": "https://authors.library.caltech.edu/records/hsgzy-enj48/files/3409207_Supplementary_Data.zip" }, { "basename": "MNRAS-2013-Roseboom-430-48.pdf", "url": "https://authors.library.caltech.edu/records/hsgzy-enj48/files/MNRAS-2013-Roseboom-430-48.pdf" }, { "basename": "tablea1_cosmos.txt", "url": "https://authors.library.caltech.edu/records/hsgzy-enj48/files/tablea1_cosmos.txt" }, { "basename": "tablea2_uds.txt", "url": "https://authors.library.caltech.edu/records/hsgzy-enj48/files/tablea2_uds.txt" }, { "basename": "tablea3_seds.txt", "url": "https://authors.library.caltech.edu/records/hsgzy-enj48/files/tablea3_seds.txt" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Roseboom, I. G.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/qe785-gv857", "eprint_id": 42990, "eprint_status": "archive", "datestamp": "2023-08-19 22:17:23", "lastmod": "2023-10-25 23:11:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sayers-J", "name": { "family": "Sayers", "given": "J." }, "orcid": "0000-0002-8213-3784" }, { "id": "Mroczkowski-T-K", "name": { "family": "Mroczkowski", "given": "T." }, "orcid": "0000-0003-3816-5372" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Korngut-P-M", "name": { "family": "Korngut", "given": "P. M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bulbul-Esra", "name": { "family": "Bulbul", "given": "E." } }, { "id": "Czakon-N-G", "name": { "family": "Czakon", "given": "N. G." } }, { "id": "Egami-Eichi", "name": { "family": "Egami", "given": "E." } }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Koch-P-M", "name": { "family": "Koch", "given": "P. M." }, "orcid": "0000-0003-2777-5861" }, { "id": "Lin-Kai-Yang", "name": { "family": "Lin", "given": "K.-Y." }, "orcid": "0000-0002-8698-7277" }, { "id": "Mantz-A-B", "name": { "family": "Mantz", "given": "A." }, "orcid": "0000-0002-8031-1217" }, { "id": "Molnar-S-M", "name": { "family": "Molnar", "given": "S. M." }, "orcid": "0000-0002-4227-956X" }, { "id": "Moustakas-L-A", "name": { "family": "Moustakas", "given": "L." }, "orcid": "0000-0003-3030-2360" }, { "id": "Pierpaoli-Elena", "name": { "family": "Pierpaoli", "given": "E." }, "orcid": "0000-0002-7957-8993" }, { "id": "Rawle-T-D", "name": { "family": "Rawle", "given": "T. D." } }, { "id": "Reese-E-D", "name": { "family": "Reese", "given": "E. D." }, "orcid": "0000-0002-8700-7082" }, { "id": "Rex-M", "name": { "family": "Rex", "given": "M." } }, { "id": "Shitanishi-Jennifer-A", "name": { "family": "Shitanishi", "given": "J. A." } }, { "id": "Siegel-S-R", "name": { "family": "Siegel", "given": "S. R." }, "orcid": "0000-0003-2631-6217" }, { "id": "Umetsu-Keiichi", "name": { "family": "Umetsu", "given": "K." }, "orcid": "0000-0002-7196-4822" } ] }, "title": "A Measurement of the Kinetic Sunyaev-Zel'dovich Signal Toward MACS J0717.5+3745", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual (MACS J0717.5+3745) \u2013 galaxies: clusters: intracluster medium", "note": "\u00a9 2013 The American Astronomical Society. \n\nReceived 2013 July 12; accepted 2013 September 25; published 2013 November 1. \n\nWe acknowledge the assistance of: the day crew and Hilo\nstaff of the Caltech Submillimeter Observatory, who provided\ninvaluable assistance during data-taking for this data set; Kathy\nDeniston, Barbara Wertz, and Diana Bisel, who provided effective\nadministrative support at Caltech and in Hilo; the\nBolocam observations were partially supported by the Gordon\nand Betty Moore Foundation. J.S. was supported by\nNSF/AST-0838261, NASA/NNX11AB07G, and the Norris\nFoundation CCAT Postdoctoral Fellowship; support for T.M.\nwas provided by NASA through Einstein Fellowship Program\ngrant No. PF0-110077 awarded by the Chandra X-ray Center,\nwhich is operated by the Smithsonian Astrophysical Observatory\nfor NASA under contract NAS8-03060; P.M.K. was supported\nby a NASA Postdoctoral Program Fellowship; N.C. was\npartially supported by a NASA Graduate Student Research Fellowship;\nA.M. was partially supported by NSF/AST-0838187\nand NSF/AST-1140019; E.P. and J.A.S. were partially supported by NASA/\nNNX07AH59G; S.S. was supported by NASA\nEarth and Space Science Fellowship NASA/NNX12AL62H;\nK.U. acknowledges partial support from the National Science\nCouncil of Taiwan grant NSC100-2112-M-001-008-MY3 and\nfrom the Academia Sinica Career Development Award. A portion\nof this research was carried out at the Jet Propulsion Laboratory,\nCalifornia Institute of Technology, under a contract with the\nNational Aeronautics and Space Administration. This research\nmade use of the Caltech Submillimeter Observatory, which was\noperated at the time by the California Institute of Technology\nunder cooperative agreement with the National Science Foundation\n(NSF/AST-0838261). This work is also based in part on\nobservations made with Herschel, a European Space Agency\nCornerstone Mission with a significant participation by NASA.\nPartial support for this work was provided by NASA through an\naward issued by JPL/Caltech. \n\nFacilities: CSO, CXO, Herschel, XMM\n\nPublished - 0004-637X_778_1_52.pdf
Submitted - 1312.3680v1.pdf
", "abstract": "We report our analysis of MACS J0717.5+3745 using 140 and 268 GHz Bolocam data collected at the Caltech Submillimeter Observatory. We detect extended Sunyaev-Zel'dovich (SZ) effect signal at high significance in both Bolocam bands, and we employ Herschel-SPIRE observations to subtract the signal from dusty background galaxies in the 268 GHz data. We constrain the two-band SZ surface brightness toward two of the sub-clusters of MACS J0717.5+3745: the main sub-cluster (named C), and a sub-cluster identified in spectroscopic optical data to have a line-of-sight velocity of +3200 km s^(\u20131) (named B). We determine the surface brightness in two separate ways: via fits of parametric models and via direct integration of the images. For both sub-clusters, we find consistent surface brightnesses from both analysis methods. We constrain spectral templates consisting of relativistically corrected thermal and kinetic SZ signals, using a jointly-derived electron temperature from Chandra and XMM-Newton under the assumption that each sub-cluster is isothermal. The data show no evidence for a kinetic SZ signal toward sub-cluster C, but they do indicate a significant kinetic SZ signal toward sub-cluster B. The model-derived surface brightnesses for sub-cluster B yield a best-fit, line-of-sight velocity of v_z = +3450 \u00b1 900 km s^(\u20131), with (1 \u2013 Prob[v_z \u2265 0]) = 1.3 \u00d7 10^(\u20135) (4.2\u03c3 away from 0 for a Gaussian distribution). The directly integrated sub-cluster B SZ surface brightnesses provide a best-fit v_z = +2550 \u00b1 1050 km s^(\u20131), with (1 \u2013 Prob[vz \u2265 0]) = 2.2 \u00d7 10^(\u20133) (2.9\u03c3).", "date": "2013-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "778", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 52", "id_number": "CaltechAUTHORS:20131212-125628354", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131212-125628354", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "NASA", "grant_number": "NNX11AB07G" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF0-110077" }, { "agency": "NASA", "grant_number": "NAS8-03060" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NASA Graduate Student Research Fellowship" }, { "agency": "NSF", "grant_number": "AST-0838187" }, { "agency": "NSF", "grant_number": "AST-1140019" }, { "agency": "NASA", "grant_number": "NNX07AH59G" }, { "agency": "NASA Earth and Space Science Fellowship", "grant_number": "NNX12AL62H" }, { "agency": "National Science Council (Taipei)", "grant_number": "NSC100-2112-M-001-008-MY3" }, { "agency": "Academia Sinica" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1088/0004-637X/778/1/52", "primary_object": { "basename": "0004-637X_778_1_52.pdf", "url": "https://authors.library.caltech.edu/records/qe785-gv857/files/0004-637X_778_1_52.pdf" }, "related_objects": [ { "basename": "1312.3680v1.pdf", "url": "https://authors.library.caltech.edu/records/qe785-gv857/files/1312.3680v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Sayers, J.; Mroczkowski, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/8fg87-zwj76", "eprint_id": 42272, "eprint_status": "archive", "datestamp": "2023-08-19 21:50:27", "lastmod": "2023-10-25 15:48:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hanson-D", "name": { "family": "Hanson", "given": "D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Padin-S", "name": { "family": "Padin", "given": "S." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Detection of B-Mode Polarization in the Cosmic Microwave Background with Data from the South Pole Telescope", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 American Physical Society.\n\nReceived 22 July 2013; published 30 September 2013.\n\nThe SPT is supported by the National Science Foundation\nthrough Grant No. ANT-0638937, with partial support provided\nby NSF Grant No. PHY-1125897. Support for the\ndevelopment and construction of SPTpol were provided by\nthe Gordon and Betty Moore Foundation through Grant\nNo. GBMF 947 to the University of Chicago, a gift from\nthe Kavli Foundation, and NSF Grant No. 0959620. Herschel\nis an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia\nand with important participation from NASA. This research\nused resources of the National Energy Research Scientific\nComputing Center, which is supported by the Office of\nScience of the U.S. Department of Energy under Award\nNo. DE-AC02-05CH11231. It also used resources of the\nCLUMEQ supercomputing consortium, part of the\nCompute Canada network. Research at Argonne National\nLaboratory and use of the Center for Nanoscale Materials\nare supported by theOffice of Science of the U.S. Department\nof Energy under Award No. DE-AC02-06CH11357. The\nMcGill group acknowledges funding from the National\nSciences and Engineering Research Council of Canada,\nCanada Research Chairs Program, and the Canadian\nInstitute for Advanced Research. The C. U. Boulder group\nacknowledges support from NSF Grant No. AST-0956135.\nWe thank P. Hargrave at Cardiff University for antireflection coating the SPTpol lens, A. Datesman for his work on TES detectors at Argonne, R. Divan for microfabrication support at Argonne, and the members of the Truce Collaboration for their efforts in the design of the 150 GHz polarization detectors, in particular D. Becker, J. Britton, M. D. Niemack, and K.W. Yoon at NIST. We thank M. Lueker, T. Plagge, Z. Staniszewski, E. Shirokoff, H. Spieler, and R. Williamson for their considerable contributions to the SPT program. D. H. was supported by the Lorne Trottier Chair program in Astrophysics and Cosmology at McGill and by the CITA National Fellowship program. R.K. acknowledges support from NASA Hubble Fellowship Grant No. HF-51275.\n\nPublished - PhysRevLett.111.141301.pdf
Submitted - 1307.5830v2.pdf
", "abstract": "Gravitational lensing of the cosmic microwave background generates a curl pattern in the observed polarization. This \"B-mode\" signal provides a measure of the projected mass distribution over the entire observable Universe and also acts as a contaminant for the measurement of primordial gravity-wave signals. In this Letter we present the first detection of gravitational lensing B modes, using first-season data from the polarization-sensitive receiver on the South Pole Telescope (SPTpol). We construct a template for the lensing B-mode signal by combining E-mode polarization measured by SPTpol with estimates of the lensing potential from a Herschel-SPIRE map of the cosmic infrared background. We compare this template to the B modes measured directly by SPTpol, finding a nonzero correlation at 7.7\u03c3 significance. The correlation has an amplitude and scale dependence consistent with theoretical expectations, is robust with respect to analysis choices, and constitutes the first measurement of a powerful cosmological observable.", "date": "2013-10-04", "date_type": "published", "publication": "Physical Review Letters", "volume": "111", "number": "14", "publisher": "American Physical Society", "pagerange": "Art. No. 141301", "id_number": "CaltechAUTHORS:20131106-111142604", "issn": "0031-9007", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131106-111142604", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0638937" }, { "agency": "NSF", "grant_number": "PHY-1125897" }, { "agency": "Gordon and Betty Moore Foundation", "grant_number": "GBMF 947" }, { "agency": "Kavli Foundation" }, { "agency": "NSF", "grant_number": "0959620" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-05CH11231" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-06CH11357" }, { "agency": "National Sciences and Engineering Research Council of Canada" }, { "agency": "Canada Research Chairs Program" }, { "agency": "Canadian Institute for Advanced Research" }, { "agency": "NSF", "grant_number": "AST-0956135" }, { "agency": "Lorne Trottier Chair program in Astrophysics and Cosmology" }, { "agency": "CITA National Fellowship program" }, { "agency": "NASA Hubble Fellowship", "grant_number": "HF-51275" } ] }, "corp_creators": { "items": [ "SPTpol Collaboration" ] }, "doi": "10.1103/PhysRevLett.111.141301", "primary_object": { "basename": "1307.5830v2.pdf", "url": "https://authors.library.caltech.edu/records/8fg87-zwj76/files/1307.5830v2.pdf" }, "related_objects": [ { "basename": "PhysRevLett.111.141301.pdf", "url": "https://authors.library.caltech.edu/records/8fg87-zwj76/files/PhysRevLett.111.141301.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Hanson, D.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/nycbc-g0q47", "eprint_id": 42903, "eprint_status": "archive", "datestamp": "2023-08-19 21:40:10", "lastmod": "2023-10-25 23:08:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ibar-E", "name": { "family": "Ibar", "given": "E." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Herschel reveals the obscured star formation in HiZELS H\u03b1 emitters at z = 1.47", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift, galaxies: starburst, galaxies: star formation, galaxies: statistics, infrared: galaxies, submillimetre: galaxies.", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 July 4. Received 2013 July 3; in original form 2012 November 30. \nFirst published online: August 8, 2013.\n\nWe thank the anonymous referee for the useful comments that helped improve this paper. EI agradece el financiamento de CONICYT/FONDECYT por el proyecto de postdoctorado N\u25e6:3130504. DS acknowledges financial support from the Netherland Organization for Scientific research (NWO) through a Veni fellowship. IS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. RJI acknowledges support in the form of ERC Advanced Investigator programme, COSMI-CISM. The HiZELS data are based on observations obtained using both the Wide Field Camera on the 3.8-m United Kingdom Infrared\nTelescope (operated by the Joint Astronomy Centre on behalf\nof the Science and Technology Facilities Council of the UK) and Suprime-Cam on the 8.2-m Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This research has made use of data from the HerMES project (http://hermes.sussex. ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. The data presented in this paper will be released through the HerMES database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES). SPIRE has been developed by\na consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM\n(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB\n(Sweden); STFC, UKSA (UK); and NASA (USA). PACS has\nbeen developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy) and CICYT/MCYT (Spain). This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.\n\nPublished - MNRAS-2013-Ibar-3218-35.pdf
Submitted - 1307.3556v1.pdf
", "abstract": "We describe the far-infrared (far-IR; rest-frame 8\u20131000-\u03bcm) properties of a sample of 443 H\u03b1-selected star-forming galaxies in the Cosmic Evolution Survey (COSMOS) and Ultra Deep Survey (UDS) fields detected by the High-redshift Emission Line Survey (HiZELS) imaging survey. Sources are identified using narrow-band filters in combination with broad-band photometry to uniformly select H\u03b1 (and [O\u2009ii] if available) emitters in a narrow redshift slice at z = 1.47 \u00b1 0.02. We use a stacking approach in Spitzer-MIPS mid-IR, Herschel-PACS/SPIRE far-IR [from the PACS Evolutionary Prove (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES)] and AzTEC mm-wave images to describe their typical far-IR properties. We find that HiZELS galaxies with observed H\u03b1 luminosities of L(H\u03b1)_(obs) \u2248 10^(8.1-9.1) L_\u2299 ( \u2248 10^(41.7-42.7) erg s^(\u22121)) have bolometric far-IR luminosities of typical luminous IR galaxies, L(8\u22121000\u03bcm)\u224810^(11.41)^(+0.04)_(\u22120.06) L_\u2299. Combining the H\u03b1 and far-IR luminosities, we derive median star formation rates (SFRs) of SFR_(H\u03b1), FIR = 32 \u00b1 5 M_\u2299 yr^(\u22121) and H\u03b1 extinctions of A_(H\u03b1) = 1.0 \u00b1 0.2 mag. Perhaps surprisingly, little difference is seen in typical HiZELS extinction levels compared to local star-forming galaxies. We confirm previous empirical stellar mass (M_*)\u2009to\u2009A_(H\u03b1) relations and the little or no evolution up to z = 1.47. For HiZELS galaxies (or similar samples) we provide an empirical parametrization of the SFR as a function of rest-frame (u \u2212 z) colours and 3.6-\u03bcm photometry \u2013 a useful proxy to aid in the absence of far-IR detections in high-z galaxies. We find that the observed H\u03b1 luminosity is a dominant SFR tracer when rest-frame (u \u2212 z) colours are \u22720.9 mag or when Spitzer-3.6-\u03bcm photometry is fainter than 22 mag (Vega) or when stellar masses are lower than 10^(9.7)\u2009M_\u2299. We do not find any correlation between the [O\u2009ii]/H\u03b1 and far-IR luminosity, suggesting that this emission line ratio does not trace the extinction of the most obscured star-forming regions, especially in massive galaxies where these dominate. The luminosity-limited HiZELS sample tends to lie above of the so-called main sequence for star-forming galaxies, especially at low stellar masses, indicating high star formation efficiencies in these galaxies. This work has implications for SFR indicators and suggests that obscured star formation is linked to the assembly of stellar mass, with deeper potential wells in massive galaxies providing dense, heavily obscured environments in which stars can form rapidly.", "date": "2013-10", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "434", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3218-3235", "id_number": "CaltechAUTHORS:20131209-121026664", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131209-121026664", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "CONICYT/FONDECYT", "grant_number": "3130504" }, { "agency": "Netherlands Organization for Scientific Research (NWO) Veni Fellowship" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Leverhulme Fellowship" }, { "agency": "ERC Advanced Investigator Programme DUSTYGAL" }, { "agency": "Royal Society Wolfson Merit Award" }, { "agency": "ERC Advanced Investigator Programme COSMI-CISM" }, { "agency": "CSA (Canada)" }, { "agency": "NAOC (China)" }, { "agency": "CEA (France)" }, { "agency": "CNES (France)" }, { "agency": "CNRS (France)" }, { "agency": "ASI (Italy)" }, { "agency": "MCINN (Spain)" }, { "agency": "SNSB (Sweden)" }, { "agency": "STFC (UK)" }, { "agency": "UKSA (UK)" }, { "agency": "NASA" }, { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1093/mnras/stt1258", "primary_object": { "basename": "1307.3556v1.pdf", "url": "https://authors.library.caltech.edu/records/nycbc-g0q47/files/1307.3556v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Ibar-3218-35.pdf", "url": "https://authors.library.caltech.edu/records/nycbc-g0q47/files/MNRAS-2013-Ibar-3218-35.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Ibar, E.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/5v2k0-sv027", "eprint_id": 43274, "eprint_status": "archive", "datestamp": "2023-08-19 21:41:53", "lastmod": "2023-10-25 23:24:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G. E." }, "orcid": "0000-0002-4872-2294" }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Hurley-P", "name": { "family": "Hurley", "given": "P." } }, { "id": "Alonso-Herrero-A", "name": { "family": "Alonso-Herrero", "given": "A." }, "orcid": "0000-0001-6794-2519" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S." } }, { "id": "Charmandaris-V", "name": { "family": "Charmandaris", "given": "V." }, "orcid": "0000-0002-2688-1956" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dai-Y-Sophia", "name": { "family": "Dai", "given": "Y. Sophia" }, "orcid": "0000-0002-7928-416X" }, { "id": "Dale-D-A", "name": { "family": "Dale", "given": "D. A." }, "orcid": "0000-0002-5782-9093" }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "D." }, "orcid": "0000-0002-7631-647X" }, { "id": "Feltre-A", "name": { "family": "Feltre", "given": "A." } }, { "id": "Hatziminaoglou-E", "name": { "family": "Hatziminaoglou", "given": "E." } }, { "id": "Huang-J-S", "name": { "family": "Huang", "given": "J.-S." } }, { "id": "Morrison-G-E", "name": { "family": "Morrison", "given": "G." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M." }, "orcid": "0000-0002-6689-6271" }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Shi-Y", "name": { "family": "Shi", "given": "Y." } } ] }, "title": "Mid- to far-infrared properties of star-forming galaxies and active galactic nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: active, galaxies: starburst, galaxies: star formation, infrared: galaxies", "note": "\u00a9 2013 ESO. Article published by EDP Sciences. \n\nReceived 8 July 2013. Accepted 23 August 2013. Published online 22 October 2013. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nGEM acknowledges support from the John Fell Oxford University Press (OUP) Research Fund and the University of Oxford. A.A.-H. acknowledges funding through the Universidad de Cantabria August G.\nLinares Programme. VC acknowledges partial support from the EU FP7 Grant PIRSES-GA-20120316788. This paper uses data from Herschel's photometer SPIRE. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA).\n\nPublished - aa22226-13.pdf
Submitted - 1309.3922v1.pdf
", "abstract": "We study the mid- to far-IR properties of a 24 \u03bcm-selected flux-limited sample (S_(24)> 5\u2009mJy) of 154 intermediate redshift (\u27e8 z \u27e9 ~ 0.15), infrared luminous galaxies, drawn from the 5 Milli-Jansky Unbiased Spitzer Extragalactic Survey. By combining existing mid-IR spectroscopy and new Herschel SPIRE submm photometry from the Herschel Multi-tiered Extragalactic Survey, we derived robust total infrared luminosity (L_(IR)) and dust mass (M_(dust)) estimates and infered the relative contribution of the AGN to the infrared energy budget of the sources. We found that the total (8\u22121000 \u03bcm) infrared emission of galaxies with weak 6.2 \u03bcm PAH emission (EW_(6.2) \u2264 0.2 \u03bcm) is dominated by AGN activity, while for galaxies with EW_(6.2)> 0.2 \u03bcm more than 50% of the L_(IR) arises from star formation. We also found that for galaxies detected in the 250\u2013500 \u03bcm Herschel bands an AGN has a statistically insignificant effect on the temperature of the cold dust and the far-IR colours of the host galaxy, which are primarily shaped by star formation activity. For star-forming galaxies we reveal an anti-correlation between the L_(IR)-to-rest-frame 8 \u03bcm luminosity ratio, IR8 \u2261 L_(IR)/L_8\u2009 and the strength of PAH features. We found that this anti-correlation is primarily driven by variations in the PAHs emission, and not by variations in the 5\u221215 \u03bcm mid-IR continuum emission. Using the [Ne\u2009iii]/[Ne\u2009ii] line ratio as a tracer of the hardness of the radiation field, we confirm that galaxies with harder radiation fields tend to exhibit weaker PAH features, and found that they have higher IR8 values and higher dust-mass-weighted luminosities (L_(IR)/M_(dust)), the latter being a proxy for the dust temperature (T_d). We argue that these trends originate either from variations in the environment of the star-forming regions or are caused by variations in the age of the starburst. Finally, we provide scaling relations that will allow estimating L_(IR), based on single-band observations with the mid-infrared instrument, on board the upcoming James Webb Space Telescope.", "date": "2013-10", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "558", "publisher": "EDP Sciences", "pagerange": "Art. No. A136", "id_number": "CaltechAUTHORS:20140108-140820993", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140108-140820993", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "John Fell Oxford University Press (OUP) Research Fund" }, { "agency": "University of Oxford" }, { "agency": "Universidad de Cantabria August G. Linares Programme" }, { "agency": "European Research Council (ERC)", "grant_number": "PIRSES-GA-20120316788" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201322226", "primary_object": { "basename": "1309.3922v1.pdf", "url": "https://authors.library.caltech.edu/records/5v2k0-sv027/files/1309.3922v1.pdf" }, "related_objects": [ { "basename": "aa22226-13.pdf", "url": "https://authors.library.caltech.edu/records/5v2k0-sv027/files/aa22226-13.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Magdis, G. E.; Rigopoulou, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/w3vvb-xne59", "eprint_id": 41898, "eprint_status": "archive", "datestamp": "2023-08-22 10:23:33", "lastmod": "2023-10-25 14:53:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Feltre-A", "name": { "family": "Feltre", "given": "A." } }, { "id": "Hatziminaoglou-E", "name": { "family": "Hatziminaoglou", "given": "E." } }, { "id": "Hern\u00e1n-Caballero-A", "name": { "family": "Hern\u00e1n-Caballero", "given": "A." } }, { "id": "Fritz-J", "name": { "family": "Fritz", "given": "J." } }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-D", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Gonzalez-Solares-E-A", "name": { "family": "Gonzalez-Solares", "given": "E. A." } }, { "id": "Ibar-E", "name": { "family": "Ibar", "given": "E." } }, { "id": "Isaak-K-G", "name": { "family": "Isaak", "given": "K. G." } }, { "id": "Lo-Faro-B", "name": { "family": "Lo Faro", "given": "B." } }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" } ] }, "title": "The roles of star formation and AGN activity of IRS sources in the HerMES fields", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: starburst; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2013 The Royal Astronomical Society.\n\nAccepted 2013 June 25; Received 2013 June 25; In original form 2013 April 3.\n\nSPIRE has been developed by a consortium of institutes led\nby Cardiff Univ. (UK), including Univ. Lethbridge (Canada);\nNAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);\nIAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and\nCaltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The SPIRE data presented in this paper are available through the HerMES Database in Marseille (HeDaM; http://hedam.oamp.fr/HerMES). The Cornell Atlas of Spitzer/IRS Sources (CASSIS) is a product of the Infrared Science Center at Cornell University, supported by NASA and JPL. Funding for the creation and distribution of the SDSS Archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho and the Max Planck Society. The SDSS website is http://www.sdss.org/. Much of the analysis presented in this work was done with TOPCAT (http://www.star.bris.ac.uk/\u223cmbt/topcat/), developed by M. Taylor.\n\nPublished - MNRAS-2013-Feltre-2426-37.pdf
Submitted - 1306.5946v1.pdf
", "abstract": "In this work, we explore the impact of the presence of an active galactic nucleus (AGN) on the mid- and far-infrared (IR) properties of galaxies as well as the effects of simultaneous AGN and starburst activity in the same galaxies. To do this, we apply a multicomponent, multiband spectral synthesis technique to a sample of 250\u2009\u03bcm selected galaxies of the Herschel Multi-tiered Extragalactic Survey (HerMES), with Infrared Spectrograph (IRS) spectra available for all galaxies. Our results confirm that the inclusion of the IRS spectra plays a crucial role in the spectral analysis of galaxies with an AGN component improving the selection of the best-fitting hot dust (torus) model.\n\nWe find a correlation between the obscured star formation rate, SFR_IR, derived from the IR luminosity of the starburst component, and SFRPAH, derived from the luminosity of the PAH features, L_PAH, with SFR_FIR taking higher values than SFR_PAH. The correlation is different for AGN- and starburst-dominated objects. The ratio of L_PAH to that of the starburst component, L_PAH/L_SB, is almost constant for AGN-dominated objects but decreases with increasing L_SB for starburst-dominated objects. SFR_FIR increases with the accretion luminosity, L_acc, with the increase less prominent for the very brightest, unobscured AGN-dominated sources.\n\nWe find no correlation between the masses of the hot (AGN-heated) and cold (starburst-heated) dust components. We interpret this as a non-constant fraction of gas driven by the gravitational effects to the AGN while the starburst is ongoing. We also find no evidence of the AGN affecting the temperature of the cold dust component, though this conclusion is mostly based on objects with a non-dominant AGN component. We conclude that our findings do not provide evidence that the presence of AGN affects the star formation process in the host galaxy, but rather that the two phenomena occur simultaneously over a wide range of luminosities.", "date": "2013-09-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "434", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2426-2437", "id_number": "CaltechAUTHORS:20131011-132251886", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131011-132251886", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "JPL" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" } ] }, "doi": "10.1093/mnras/stt1177", "primary_object": { "basename": "1306.5946v1.pdf", "url": "https://authors.library.caltech.edu/records/w3vvb-xne59/files/1306.5946v1.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Feltre-2426-37.pdf", "url": "https://authors.library.caltech.edu/records/w3vvb-xne59/files/MNRAS-2013-Feltre-2426-37.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Feltre, A.; Hatziminaoglou, E.; et el." }, { "id": "https://authors.library.caltech.edu/records/0f1h8-3ps49", "eprint_id": 42059, "eprint_status": "archive", "datestamp": "2023-08-22 10:23:09", "lastmod": "2023-10-25 15:04:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Calanog-J-A", "name": { "family": "Calanog", "given": "J. A." } }, { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "J." }, "orcid": "0000-0003-2376-8971" }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "Hai" }, "orcid": "0000-0001-9608-6395" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Assef-R-J", "name": { "family": "Assef", "given": "R. J." }, "orcid": "0000-0002-9508-3667" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Ibar-Eduardo", "name": { "family": "Ibar", "given": "E." } }, { "id": "Kartaltepe-J", "name": { "family": "Kartaltepe", "given": "J." }, "orcid": "0000-0001-9187-3605" }, { "id": "Magdis-G", "name": { "family": "Magdis", "given": "G." } }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "I." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: The Far-infrared Emission from Dust-obscured Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: luminosity function, mass function; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2013 April 16, accepted for publication 2013 July 22. Published 2013 September 5. We thank the anonymous referee for useful comments that helped improve this paper. We thank Jason Melbourne for insightful discussions. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel\nKey Programme utilizing Guaranteed Time from the SPIRE\ninstrument team, ESAC scientists, and a mission scientist.\nThe data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES/). We our thankful to the COSMOS collaboration for granting us access to their catalogs and we gratefully acknowledge the contributions of the entire COSMOS team that have made this work possible. More information on the COSMOS survey is available at http://hermes.sussex.ac.uk/. This work is based (in\npart) on observations made with the Spitzer Space Telescope,\nwhich is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge support from a GAANN fellowship (to J.A.C.), NSF CAREER AST-0645427 (A.C. and H.F.), and NASA funds to the US HerMES team through JPL. S.O. acknowledges\nsupport from the Science and Technology Facilities Council\n[grant number ST/I000976/1]. Some of the data (spectroscopic redshifts) presented here were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of\nTechnology, the University of California, and the National\nAeronautics and Space Administration. The Observatory was\nmade possible by the generous financial support of the W.\nM. Keck Foundation. The authors wish to recognize and\nacknowledge the very significant cultural role and reverence\nthat the summit of Mauna Kea has always had within the\nindigenous Hawaiian community.We are most fortunate to have\nthe opportunity to conduct observations from this mountain.\nFacilities: Herschel (SPIRE), Spitzer (IRAC, MIPS), Subaru\n(Suprime Cam), Keck:II (DEIMOS)\n\nPublished - 0004-637X_775_1_61.pdf
Submitted - 1307.6967v1.pdf
", "abstract": "Dust-obscured galaxies (DOGs) are an ultraviolet-faint, infrared-bright galaxy population that reside at z ~ 2 and are believed to be in a phase of dusty star-forming and active galactic nucleus (AGN) activity. We present far-infrared (far-IR) observations of a complete sample of DOGs in the 2 deg^2 of the Cosmic Evolution Survey. The 3077 DOGs have \u3008z\u3009 = 1.9 \u00b1 0.3 and are selected from 24 \u03bcm and r^+ observations using a color cut of r^+ \u2013 [24] \u2265 7.5 (AB mag) and S_(24) \u2265 100 \u03bcJy. Based on the near-IR spectral energy distributions, 47% are bump DOGs (star formation dominated) and 10% are power-law DOGs (AGN-dominated). We use SPIRE far-IR photometry from the Herschel Multi-tiered Extragalactic Survey to calculate the IR luminosity and characteristic dust temperature for the 1572 (51%) DOGs that are detected at 250 \u03bcm (\u22653\u03c3). For the remaining 1505 (49%) that are undetected, we perform a median stacking analysis to probe fainter luminosities. Herschel-detected and undetected DOGs have average luminosities of (2.8 \u00b1 0.4) \u00d7 10^(12) L_\u2609 and (0.77 \u00b1 0.08) \u00d7 10^(12) L_\u2609, and dust temperatures of (33 \u00b1 7) K and (37 \u00b1 5) K, respectively. The IR luminosity function for DOGs with S_(24) \u2265 100 \u03bcJy is calculated, using far-IR observations and stacking. DOGs contribute 10%-30% to the total star formation rate (SFR) density of the universe at z = 1.5-2.5, dominated by 250 \u03bcm detected and bump DOGs. For comparison, DOGs contribute 30% to the SFR density for all z = 1.5-2.5 galaxies with S_(24) \u2265 100 \u03bcJy. DOGs have a large scatter about the star formation main sequence and their specific SFRs show that the observed phase of star formation could be responsible for their total observed stellar mass at z ~ 2.", "date": "2013-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "775", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 61", "id_number": "CaltechAUTHORS:20131025-085434310", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131025-085434310", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "GAANN fellowship" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/775/1/61", "primary_object": { "basename": "0004-637X_775_1_61.pdf", "url": "https://authors.library.caltech.edu/records/0f1h8-3ps49/files/0004-637X_775_1_61.pdf" }, "related_objects": [ { "basename": "1307.6967v1.pdf", "url": "https://authors.library.caltech.edu/records/0f1h8-3ps49/files/1307.6967v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Calanog, J. A.; Wardlow, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/j2zzr-t8803", "eprint_id": 41786, "eprint_status": "archive", "datestamp": "2023-09-26 23:52:37", "lastmod": "2023-10-24 14:55:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Griffin-M-J", "name": { "family": "Griffin", "given": "M. J." } }, { "id": "North-C-E", "name": { "family": "North", "given": "C. E." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Amaral-Rogers-A", "name": { "family": "Amaral-Rogers", "given": "A." } }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Conversi-L", "name": { "family": "Conversi", "given": "L." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Ferlet-M-J", "name": { "family": "Ferlet", "given": "M." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Lim-Tanya-L", "name": { "family": "Lim", "given": "T." } }, { "id": "Pearson-C-P", "name": { "family": "Pearson", "given": "C." }, "orcid": "0000-0001-6139-649X" }, { "id": "Pohlen-M", "name": { "family": "Pohlen", "given": "M." } }, { "id": "Sibthorpe-B", "name": { "family": "Sibthorpe", "given": "B." } }, { "id": "Spencer-L", "name": { "family": "Spencer", "given": "L." } }, { "id": "Swinyard-B", "name": { "family": "Swinyard", "given": "B." } }, { "id": "Valtchanov-I", "name": { "family": "Valtchanov", "given": "I." }, "orcid": "0000-0001-9930-7886" } ] }, "title": "Flux calibration of broad-band far-infrared and submillimetre photometric instruments: theory and application to Herschel-SPIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "instrumentation: photometers; methods: observational; techniques: photometric; submillimetre: general", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 June 5. Received 2013 May 21; in original form 2013 February 8.\n\nFirst published online: July 24, 2013.\n\nHerschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with\nimportant participation from NASA.\nSPIRE has been developed by a consortium of institutes led\nby Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada);\nNAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);\nIAC (Spain); Stockholm Observatory (Sweden); Imperial College\nLondon, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and\nCaltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada);\nNAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN\n(Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\nThis research made use of APLPY, an open-source plotting package\nfor PYTHON hosted at http://aplpy.github.com\n\nPublished - stt999.pdf
Submitted - 1306_1778v1.pdf
", "abstract": "Photometric instruments operating at far-infrared to millimetre wavelengths often have broad spectral passbands (\u03bb/\u0394\u03bb \u223c 3 or less), especially those operating in space. A broad passband can result in significant variation of the beam profile and aperture efficiency across the passband, effects which thus far have not generally been taken into account in the flux calibration of such instruments. With absolute calibration uncertainties associated with the brightness of primary calibration standards now in the region of 5\u2009per\u2009cent or less, variation of the beam properties across the passband can be a significant contributor to the overall calibration accuracy for extended emission. We present a calibration framework which takes such variations into account for both antenna-coupled and absorber-coupled focal plane architectures. The scheme covers point source and extended source cases, and also the intermediate case of a semi-extended source profile. We apply the new method to the Spectral and Photometric Imaging Receiver (SPIRE) photometer on board the Herschel Space Observatory.", "date": "2013-09", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "434", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "992-1004", "id_number": "CaltechAUTHORS:20131009-091455399", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131009-091455399", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "University of California" }, { "agency": "NASA" } ] }, "doi": "10.1093/mnras/stt999", "primary_object": { "basename": "1306_1778v1.pdf", "url": "https://authors.library.caltech.edu/records/j2zzr-t8803/files/1306_1778v1.pdf" }, "related_objects": [ { "basename": "stt999.pdf", "url": "https://authors.library.caltech.edu/records/j2zzr-t8803/files/stt999.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Griffin, M. J.; North, C. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/0xgjc-9j766", "eprint_id": 41074, "eprint_status": "archive", "datestamp": "2023-09-26 23:51:29", "lastmod": "2023-10-24 14:54:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Griffin-M-J", "name": { "family": "Griffin", "given": "M. J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Conversi-L", "name": { "family": "Conversi", "given": "L." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Lim-Tanya-L", "name": { "family": "Lim", "given": "T." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "North-C-E", "name": { "family": "North", "given": "C. E." } }, { "id": "Papageorgiou-A", "name": { "family": "Papageorgiou", "given": "A." }, "orcid": "0000-0002-3039-9257" }, { "id": "Pearson-C-P", "name": { "family": "Pearson", "given": "C. P." }, "orcid": "0000-0001-6139-649X" }, { "id": "Pohlen-M", "name": { "family": "Pohlen", "given": "M." } }, { "id": "Polehampton-E-T", "name": { "family": "Polehampton", "given": "E. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Sibthorpe-B", "name": { "family": "Sibthorpe", "given": "B." } }, { "id": "Spencer-L-D", "name": { "family": "Spencer", "given": "L. D." } }, { "id": "Swinyard-B-M", "name": { "family": "Swinyard", "given": "B. M." } }, { "id": "Valtchanov-I", "name": { "family": "Valtchanov", "given": "I." }, "orcid": "0000-0001-9930-7886" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" } ] }, "title": "Flux calibration of the Herschel-SPIRE photometer", "ispublished": "pub", "full_text_status": "public", "keywords": "instrumentation: photometers", "note": "\u00a9 2013 The Authors.\nPublished by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 May 29. Received 2013 May 29; in original form 2013 April 30.\n\nFirst published online: July 5, 2013.\n\nHerschel is a European Space Agency (ESA) space observatory with science\ninstruments provided by European-led Principal Investigator consortia\nand with important participation from NASA.\n\nWe thank the reviewer for the helpful comments on this paper.\nSPIRE has been developed by a consortium of institutes led by\nCardiff Univ. (UK) and including: Univ. Lethbridge (Canada);\nNAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);\nIAC (Spain); Stockholm Observatory (Sweden); Imperial College\nLondon, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and\nCaltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada);\nNAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN\n(Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA).\nHIPE is a joint development by the Herschel Science Ground Segment\nConsortium, consisting of ESA, the NASA Herschel Science\nCenter and the HIFI, PACS and SPIRE consortia.\n\nPublished - MNRAS-2013-Bendo-3062-78.pdf
Submitted - 1306_1217_FluxcalibrationHerschel.pdf
", "abstract": "We describe the procedure used to flux calibrate the three-band submillimetre photometer in the Spectral and Photometric Imaging Receiver instrument on the Herschel Space Observatory. This includes the equations describing the calibration scheme, a justification for using Neptune as the primary calibration source, a description of the observations and data processing procedures used to derive flux calibration parameters (for converting from voltage to flux density) for every bolometer in each array, an analysis of the error budget in the flux calibration for the individual bolometers and tests of the flux calibration on observations of primary and secondary calibrators. The procedure for deriving the flux calibration parameters is divided into two parts. In the first part, we use observations of astronomical sources in conjunction with the operation of the photometer internal calibration source to derive the unscaled derivatives of the flux calibration curves. To scale the calibration curves in Jy beam^(\u22121) V^(\u22121), we then use observations of Neptune in which the beam of each bolometer is mapped using a very fine scan pattern. The total instrumental uncertainties in the flux calibration for most individual bolometers is \u223c0.5\u2009 per\u2009cent, although a few bolometers have uncertainties of \u223c1\u20135\u2009 per\u2009cent because of issues with the Neptune observations. Based on application of the flux calibration parameters to Neptune observations performed using typical scan map observing modes, we determined that measurements from each array as a whole have instrumental uncertainties of 1.5\u2009 per\u2009cent. This is considerably less than the absolute calibration uncertainty associated with the model of Neptune, which is estimated at 4 \u2009per\u2009cent.", "date": "2013-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "433", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3062-3078", "id_number": "CaltechAUTHORS:20130904-083919768", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130904-083919768", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "doi": "10.1093/mnras/stt948", "primary_object": { "basename": "1306_1217_FluxcalibrationHerschel.pdf", "url": "https://authors.library.caltech.edu/records/0xgjc-9j766/files/1306_1217_FluxcalibrationHerschel.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Bendo-3062-78.pdf", "url": "https://authors.library.caltech.edu/records/0xgjc-9j766/files/MNRAS-2013-Bendo-3062-78.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Bendo, G. J.; Griffin, M. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/b4a7x-55663", "eprint_id": 28629, "eprint_status": "archive", "datestamp": "2023-08-22 09:57:10", "lastmod": "2023-10-24 18:01:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Arai-T", "name": { "family": "Arai", "given": "T." } }, { "id": "Battle-J", "name": { "family": "Battle", "given": "J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V." } }, { "id": "Keating-B", "name": { "family": "Keating", "given": "B." } }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Mason-P", "name": { "family": "Mason", "given": "P." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "U. W." } }, { "id": "Renbarger-T", "name": { "family": "Renbarger", "given": "T." } }, { "id": "Sullivan-I", "name": { "family": "Sullivan", "given": "I." } }, { "id": "Suzuki-K", "name": { "family": "Suzuki", "given": "K." } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "T." } } ] }, "title": "The Cosmic Infrared Background Experiment (CIBER): A Sounding Rocket Payload to Study the Near Infrared Extragalactic Background Light", "ispublished": "pub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars; diffuse radiation; infrared: diffuse background; instrumentation: spectrographs; space vehicles: instruments; zodiacal dust", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2011 September 9; accepted 2011 November 20; published 2013 August 1.\n\nThis work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. Japanese participation in CIBER was supported by KAKENHI (20\u202234, 18204018, 19540250, 21340047 and 21111004) from Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports, Science and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from Korea Astronomy and Space science Institute (KASI).\n\nWe would like to acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range. We also acknowledge the work of the Genesia Corporation for technical support of the CIBER optics, and M.C. Runyan and an anonymous referee for helpful comments on this manuscript. M.Z. acknowledges support from a NASA Postdoctoral Fellowship, A.C. acknowledges support from an NSF CAREER award, B.K. acknowledges support from a UCSD Hellman Faculty Fellowship, and K.T. acknowledges support from the JSPS Research Fellowship for Young Scientists.\n\nPublished - 0067-0049_207_2_31.pdf
Submitted - 1112.1424v1.pdf
", "abstract": "The Cosmic Infrared Background Experiment (CIBER) is a suite of four instruments designed to study the near infrared (IR) background light from above the Earth's atmosphere. The instrument package comprises two imaging telescopes designed to characterize spatial anisotropy in the extragalactic IR background caused by cosmological structure during the epoch of reionization, a low resolution spectrometer to measure the absolute spectrum of the extragalactic IR background, and a narrow band spectrometer optimized to measure the absolute brightness of the Zodiacal light foreground. In this paper we describe the design and characterization of the CIBER payload. The detailed mechanical, cryogenic, and electrical design of the system are presented, including all system components common to the four instruments. We present the methods and equipment used to characterize the instruments before and after flight, and give a detailed description of CIBER's flight profile and configurations. CIBER is designed to be recoverable and has flown twice, with modifications to the payload having been informed by analysis of the first flight data. All four instruments performed to specifications during the second flight, and the scientific data from this flight are currently being analyzed.", "date": "2013-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "207", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 31", "id_number": "CaltechAUTHORS:20120103-144402759", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120103-144402759", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "JPL Director's Research and Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "NASA Postdoctoral Fellowship" }, { "agency": "NSF" }, { "agency": "UCSD Hellman Faculty Fellowship" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0067-0049/207/2/31", "primary_object": { "basename": "1112.1424v1.pdf", "url": "https://authors.library.caltech.edu/records/b4a7x-55663/files/1112.1424v1.pdf" }, "related_objects": [ { "basename": "0067-0049_207_2_31.pdf", "url": "https://authors.library.caltech.edu/records/b4a7x-55663/files/0067-0049_207_2_31.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Zemcov, M.; Arai, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/dmfsk-trq97", "eprint_id": 41377, "eprint_status": "archive", "datestamp": "2023-08-22 10:00:07", "lastmod": "2023-10-24 23:41:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Arai-T", "name": { "family": "Arai", "given": "T." } }, { "id": "Battle-J", "name": { "family": "Battle", "given": "J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brown-S", "name": { "family": "Brown", "given": "S." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V." } }, { "id": "Keating-B", "name": { "family": "Keating", "given": "B." } }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lykke-K", "name": { "family": "Lykke", "given": "K." } }, { "id": "Mason-P", "name": { "family": "Mason", "given": "P." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Murata-K", "name": { "family": "Murata", "given": "K." } }, { "id": "Nam-U-W", "name": { "family": "Nam", "given": "U. W." } }, { "id": "Renbarger-T", "name": { "family": "Renbarger", "given": "T." } }, { "id": "Smith-A", "name": { "family": "Smith", "given": "A." }, "orcid": "0000-0002-1938-4660" }, { "id": "Sullivan-I", "name": { "family": "Sullivan", "given": "I." } }, { "id": "Suzuki-K", "name": { "family": "Suzuki", "given": "K." } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "T." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Cosmic Infrared Background Experiment (CIBER): The Low Resolution Spectrometer", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; infrared: diffuse background; instrumentation: spectrographs; methods: laboratory; space vehicles: instruments; techniques: spectroscopic", "note": "\u00a9 2013 American Astronomical Society. Received 2011 August 4; accepted 2011 September 26; published 2013 August 1. \n\nThis work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, and NNX07AJ24G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and\nDevelopment Fund. Japanese participation in CIBER was supported by KAKENHI (20\u00b734, 18204018, 19540250, 21340047,\n21111004, and 24111717) from the (JSPS) and the Ministry of Education, Culture, Sports, Science, and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from the Korea Astronomy and Space science Institute (KASI). We would like to acknowledge the dedicated efforts of the sounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range. We also acknowledge the work of the Genesia Corporation for technical support of the CIBER optics. K.T. acknowledges support from the JSPS Research Fellowship for the Young Scientists, M. Z. acknowledges support from a NASA Postdoctoral Fellowship, and A.C. acknowledges support from an NSF CAREER award. We thank the referee for useful suggestions which have improved this manuscript. Certain commercial equipment, instruments, or materials are\nidentified in this paper to foster understanding. Such identification does not imply recommendation or endorsement by the National Institute of Standards and Technology, nor does it imply that the materials or equipment identified are necessarily the best available for the purpose.\n\nPublished - 0067-0049_207_2_33.pdf
Submitted - 1112.4217v2.pdf
", "abstract": "Absolute spectrophotometric measurements of diffuse radiation at 1 \u03bcm to 2 \u03bcm are crucial to our understanding of the radiative content of the universe from nucleosynthesis since the epoch of reionization, the composition and structure of the zodiacal dust cloud in our solar system, and the diffuse galactic light arising from starlight scattered by interstellar dust. The Low Resolution Spectrometer (LRS) on the rocket-borne Cosmic Infrared Background Experiment is a \u03bb/\u0394\u03bb ~ 15-30 absolute spectrophotometer designed to make precision measurements of the absolute near-infrared sky brightness between 0.75 \u03bcm <\u03bb < 2.1 \u03bcm. This paper presents the optical, mechanical, and electronic design of the LRS, as well as the ground testing, characterization, and calibration measurements undertaken before flight to verify its performance. The LRS is shown to work to specifications, achieving the necessary optical and sensitivity performance. We describe our understanding and control of sources of systematic error for absolute photometry of the near-infrared extragalactic background light.", "date": "2013-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "207", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 33", "id_number": "CaltechAUTHORS:20130918-094659482", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130918-094659482", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "JPL Director's Research and Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20\u00b734" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "24111717" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NSF" } ] }, "doi": "10.1088/0067-0049/207/2/33", "primary_object": { "basename": "1112.4217v2.pdf", "url": "https://authors.library.caltech.edu/records/dmfsk-trq97/files/1112.4217v2.pdf" }, "related_objects": [ { "basename": "0067-0049_207_2_33.pdf", "url": "https://authors.library.caltech.edu/records/dmfsk-trq97/files/0067-0049_207_2_33.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Tsumura, K.; Arai, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/9fca0-rf749", "eprint_id": 41192, "eprint_status": "archive", "datestamp": "2023-08-19 20:55:47", "lastmod": "2023-10-24 23:31:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Korngut-P-M", "name": { "family": "Korngut", "given": "P. M." } }, { "id": "Renbarger-T", "name": { "family": "Renbarger", "given": "T." } }, { "id": "Arai-T", "name": { "family": "Arai", "given": "T." } }, { "id": "Battle-J", "name": { "family": "Battle", "given": "J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brown-S-W", "name": { "family": "Brown", "given": "S. W." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Keating-B", "name": { "family": "Keating", "given": "B." } }, { "id": "Kim-M-G", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Lanz-A", "name": { "family": "Lanz", "given": "A." } }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lykke-K-R", "name": { "family": "Lykke", "given": "K. R." } }, { "id": "Mason-P", "name": { "family": "Mason", "given": "P." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "U. W." } }, { "id": "Shultz-B", "name": { "family": "Shultz", "given": "B." } }, { "id": "Smith-A-W", "name": { "family": "Smith", "given": "A. W." } }, { "id": "Sullivan-I", "name": { "family": "Sullivan", "given": "I." } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "T." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Cosmic Infrared Background Experiment (CIBER): The Narrow-Band Spectrometer", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: diffuse background \u2013 instrumentation: spectrographs \u2013 methods: laboratory \u2013 space vehicles:\ninstruments \u2013 techniques: spectroscopic \u2013 zodiacal dust", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2012 November 9; accepted 2013 June 4; published 2013 August 1.\n\nThis work was supported by NASA APRA research\nGrants NNX07AI54G, NNG05WC18G, NNX07AG43G,\nNNX07AJ24G, and NNX10AE12G. Initial support was provided\nby an award to J.B. from the Jet Propulsion Laboratory's\nDirector's Research and Development Fund. Japanese participation\nin CIBER was supported by KAKENHI (20.34, 18204018,\n19540250, 21340047, and 21111004) from the Japan Society for\nthe Promotion of Science (JSPS) and the Ministry of Education,\nCulture, Sports, Science, and Technology (MEXT). Korean participation\nin CIBER was supported by the Pioneer Project from\nthe Korea Astronomy and Space science Institute (KASI).\n\nCertain commercial equipment, instruments, or materials are\nidentified in this paper to foster understanding. Such identification\ndoes not imply recommendation or endorsement by the\nNational Institute of Standards and Technology, nor does it imply\nthat the materials or equipment identified are necessarily the\nbest available for the purpose.\nThis work utilizes SOLIS data obtained by the NSO Integrated\nSynoptic Program (NISP),managed by the National Solar\nObservatory, which is operated by the Association of Universities\nfor Research in Astronomy (AURA), Inc. under a cooperative\nagreement with the National Science Foundation.\nWe acknowledge the dedicated efforts of the sounding rocket\nstaff at the NASA Wallops Flight Facility and the White Sands\nMissile Range. We also acknowledge the work of the Genesia\nCorporation for technical support of the CIBER optics. A.C.\nacknowledges support from an NSF CAREER award, B.K. acknowledges\nsupport from a UCSD Hellman Faculty Fellowship,\nK.T. acknowledges support from the JSPS Research Fellowship\nfor Young Scientists, and M.Z. and P.M.K acknowledge support\nfrom NASA Postdoctoral Fellowships.\n\nPublished - 0067-0049_207_2_34.pdf
Submitted - 1307.0016v1.pdf
", "abstract": "We have developed a near-infrared spectrometer designed to measure the absolute intensity of the solar 854.2 nm Ca II Fraunhofer line, scattered by interplanetary dust, in the zodiacal light (ZL) spectrum. Based on the known equivalent line width in the solar spectrum, this measurement can derive the zodiacal brightness, testing models of the ZL based on morphology that are used to determine the extragalactic background light in absolute photometry measurements. The spectrometer is based on a simple high-resolution tipped filter placed in front of a compact camera with wide-field refractive optics to provide the large optical throughput and high sensitivity required for rocket-borne observations. We discuss the instrument requirements for an accurate measurement of the absolute ZL brightness, the measured laboratory characterization, and the instrument performance in flight.", "date": "2013-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "207", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 34", "id_number": "CaltechAUTHORS:20130909-135918200", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130909-135918200", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "JPL Director's Research and Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20.34" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "NSF" }, { "agency": "UCSD Hellman Faculty Fellowship" }, { "agency": "NASA Postdoctoral Program" } ] }, "doi": "10.1088/0067-0049/207/2/34", "primary_object": { "basename": "0067-0049_207_2_34.pdf", "url": "https://authors.library.caltech.edu/records/9fca0-rf749/files/0067-0049_207_2_34.pdf" }, "related_objects": [ { "basename": "1307.0016v1.pdf", "url": "https://authors.library.caltech.edu/records/9fca0-rf749/files/1307.0016v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Korngut, P. M.; Renbarger, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/rn66n-v7k08", "eprint_id": 41379, "eprint_status": "archive", "datestamp": "2023-08-22 10:00:13", "lastmod": "2023-10-24 23:41:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Sullivan-I", "name": { "family": "Sullivan", "given": "I." } }, { "id": "Arai-T", "name": { "family": "Arai", "given": "T." } }, { "id": "Battle-J", "name": { "family": "Battle", "given": "J." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V." } }, { "id": "Keating-B", "name": { "family": "Keating", "given": "B." } }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Lam-A-C", "name": { "family": "Lam", "given": "A. C." } }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Mason-P", "name": { "family": "Mason", "given": "P." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Mitchell-Wynne-K", "name": { "family": "Mitchell-Wynne", "given": "K." } }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "U. W." } }, { "id": "Renbarger-T", "name": { "family": "Renbarger", "given": "T." } }, { "id": "Smidt-J", "name": { "family": "Smidt", "given": "J." } }, { "id": "Suzuki-K", "name": { "family": "Suzuki", "given": "K." } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "T." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Cosmic Infrared Background Experiment (CIBER): The Wide-field Imagers", "ispublished": "pub", "full_text_status": "public", "keywords": "dark ages, reionization, first stars; diffuse radiation; infrared: diffuse background; instrumentation: miscellaneous; space vehicles: instruments", "note": "\u00a9 2013 American Astronomical Society. Received 2011 October 21; accepted 2012 June 20; published 2013 August 1. \n\nThis work was supported by NASA APRA research grants NNX07AI54G, NNG05WC18G, NNX07AG43G, NNX07AJ24G, and NNX10AE12G. Initial support was provided by an award to J.B. from the Jet Propulsion Laboratory's Director's Research and Development Fund. Japanese participation in CIBER was supported by KAKENHI (20\u00b734, 18204018, 19540250, 21340047, and 21111004) from the Japan Society for the Promotion of Science (JSPS) and the Ministry of Education, Culture, Sports, Science, and Technology (MEXT). Korean participation in CIBER was supported by the Pioneer Project from the Korea Astronomy and Space Science Institute (KASI). This publication makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the\nNational Science Foundation. This work made use of images\nand/or data products provided by the NOAO Deep Wide-Field\nSurvey (NDWFS), which is supported by the National Optical\nAstronomy Observatory, operated by AURA, Inc., under a\ncooperative agreement with the National Science Foundation.\nWe would like to acknowledge the dedicated efforts of the\nsounding rocket staff at the NASA Wallops Flight Facility and the White Sands Missile Range. We also acknowledge the work of the Genesia Corporation for technical support of the CIBER optics. Our thanks to Y. Gong for sharing the REBL curves shown in Figure 1. A.C. acknowledges support from an NSF CAREER award, B.K. acknowledges support from a UCSD Hellman Faculty Fellowship, K.T. acknowledges support from the JSPS Research Fellowship for Young Scientists, and M.Z. acknowledges support from a NASA Postdoctoral Program\nFellowship.\nFacility: CIBER\n\nPublished - 0067-0049_207_2_32.pdf
Submitted - 1206.4702v1.pdf
", "abstract": "We have developed and characterized an imaging instrument to measure the spatial properties of the diffuse near-infrared extragalactic background light (EBL) in a search for fluctuations from z > 6 galaxies during the epoch of reionization. The instrument is part of the Cosmic Infrared Background Experiment (CIBER), designed to observe the EBL above Earth's atmosphere during a suborbital sounding rocket flight. The imaging instrument incorporates a 2\u00b0 \u00d7 2\u00b0 field of view to measure fluctuations over the predicted peak of the spatial power spectrum at 10 arcmin, and 7\" \u00d7 7\" pixels, to remove lower redshift galaxies to a depth sufficient to reduce the low-redshift galaxy clustering foreground below instrumental sensitivity. The imaging instrument employs two cameras with \u0394\u03bb/\u03bb ~ 0.5 bandpasses centered at 1.1 \u03bcm and 1.6 \u03bcm to spectrally discriminate reionization extragalactic background fluctuations from local foreground fluctuations. CIBER operates at wavelengths where the electromagnetic spectrum of the reionization extragalactic background is thought to peak, and complements fluctuation measurements by AKARI and Spitzer at longer wavelengths. We have characterized the instrument in the laboratory, including measurements of the sensitivity, flat-field response, stray light performance, and noise properties. Several modifications were made to the instrument following a first flight in 2009 February. The instrument performed to specifications in three subsequent flights, and the scientific data are now being analyzed.", "date": "2013-08", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "207", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 32", "id_number": "CaltechAUTHORS:20130918-101520290", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130918-101520290", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "NASA", "grant_number": "NNX10AE12G" }, { "agency": "JPL Director's Research and Development Fund" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20\u00b734" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "Korea Astronomy and Space Science Institute (KASI)" }, { "agency": "National Optical Astronomy Observatory (NOAO)" }, { "agency": "NSF" }, { "agency": "UCSD Hellman Faculty Fellowship" }, { "agency": "NASA Postdoctoral Program" } ] }, "doi": "10.1088/0067-0049/207/2/32", "primary_object": { "basename": "0067-0049_207_2_32.pdf", "url": "https://authors.library.caltech.edu/records/rn66n-v7k08/files/0067-0049_207_2_32.pdf" }, "related_objects": [ { "basename": "1206.4702v1.pdf", "url": "https://authors.library.caltech.edu/records/rn66n-v7k08/files/1206.4702v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Bock, J. J.; Sullivan, I.; et el." }, { "id": "https://authors.library.caltech.edu/records/khv1r-jcd61", "eprint_id": 39944, "eprint_status": "archive", "datestamp": "2023-08-22 09:55:16", "lastmod": "2023-10-24 17:19:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" } ] }, "title": "HerMES: Cosmic Infrared Background Anisotropies and the Clustering of Dusty Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: formation; galaxies: halos; large-scale structure of universe", "note": "\u00a9 2013 American Astronomical Society.\n\nReceived 2012 August 22; accepted 2013 May 28; published 2013 July 8.\n\nWe thank Aur\u00e9lien Benoit-Levy, Kevin Blagrave, Olivier\nDor\u00e9, Duncan Hanson, Amir Hajian, Peter Martin, Mattia Negrello, Aurelie P\u00b4enin, Anthony Pullen, and Christian Reichardt for valuable discussions. We also thank Olivier Dor\u00e9, Cien Shang, and Jun-Qing Xia for kindly providing their halo model curves. Finally, we sincerely thank the referee for helping improve this paper considerably.\nL.W. acknowledges support from UK's Science and Technology\nFacilities Council grant ST/F002858/1 and an ERC StG\ngrant (DEGAS-259586). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM\n(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC,\nUniv. Colorado (USA). This development has been supported\nby national funding agencies: CSA (Canada); NAOC (China);\nCEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain);\nSNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPublished - 0004-637X_772_1_77.pdf
Submitted - 1208.5049v3.pdf
", "abstract": "We present measurements of the auto- and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500 \u03bcm (1200, 860, and 600 GHz) from observations totaling ~70 deg^2 made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy \u03b4I/I = 14% \u00b1 4%, detecting signatures arising from the clustering of dusty star-forming galaxies in both the linear (2-halo) and nonlinear (1-halo) regimes; and that the transition from the 2- to 1-halo terms, below which power originates predominantly from multiple galaxies within dark matter halos, occurs at k_\u03b8 ~ 0.10-0.12 arcmin^\u20131 (\u2113 ~ 2160-2380), from 250 to 500 \u03bcm. New to this paper is clear evidence of a dependence of the Poisson and 1-halo power on the flux-cut level of masked sources\u2014suggesting that some fraction of the more luminous sources occupy more massive halos as satellites, or are possibly close pairs. We measure the cross-correlation power spectra between bands, finding that bands which are farthest apart are the least correlated, as well as hints of a reduction in the correlation between bands when resolved sources are more aggressively masked. In the second part of the paper, we attempt to interpret the measurements in the framework of the halo model. With the aim of fitting simultaneously with one model the power spectra, number counts, and absolute CIB level in all bands, we find that this is achievable by invoking a luminosity-mass relationship, such that the luminosity-to-mass ratio peaks at a particular halo mass scale and declines toward lower and higher mass halos. Our best-fit model finds that the halo mass which is most efficient at hosting star formation in the redshift range of peak star-forming activity, z ~ 1-3, is log(M_peak/M_\u2609) ~ 12.1 \u00b1 0.5, and that the minimum halo mass to host infrared galaxies is log(M_min/M_\u2609) ~ 10.1 \u00b1 0.6.", "date": "2013-07-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "772", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 77", "id_number": "CaltechAUTHORS:20130815-100959854", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130815-100959854", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "European Research Council (ERC)", "grant_number": "DEGAS-259586" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1088/0004-637X/772/1/77", "primary_object": { "basename": "0004-637X_772_1_77.pdf", "url": "https://authors.library.caltech.edu/records/khv1r-jcd61/files/0004-637X_772_1_77.pdf" }, "related_objects": [ { "basename": "1208.5049v3.pdf", "url": "https://authors.library.caltech.edu/records/khv1r-jcd61/files/1208.5049v3.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Viero, M. P.; Zemcov, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/d1j3a-5aw41", "eprint_id": 39865, "eprint_status": "archive", "datestamp": "2023-08-22 09:49:15", "lastmod": "2023-10-24 17:15:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Holder-G-P", "name": { "family": "Holder", "given": "G. P." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Padin-S", "name": { "family": "Padin", "given": "S." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "A Cosmic Microwave Background Lensing Mass Map and Its Correlation with the Cosmic Infrared Background", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; galaxies: structure", "note": "\u00a9 2013 American Astronomical Society. Received 2013 March 28; accepted 2013 June 5; published 2013 June 19. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support provided by\nNSF grant PHY-1125897, the Kavli Foundation, and the Gordon\nand Betty Moore Foundation. The McGill group acknowledges\nfunding from the National Sciences and Engineering Research\nCouncil of Canada, Canada Research Chairs program, and\nthe Canadian Institute for Advanced Research. Work at\nHarvard is supported by grant AST-1009012. S. Bhattacharya acknowledges support from NSF grant AST-1009811, R.Keisler\nfrom NASA Hubble Fellowship grant HF-51275.01, B. Benson\nfrom a KICP Fellowship, M. Dobbs from an Alfred P. Sloan\nResearch Fellowship, and O. Zahn from a BCCP fellowship.\n\nPublished - 2041-8205_771_1_L16.pdf
Submitted - 1303.5048v1.pdf
", "abstract": "We use a temperature map of the cosmic microwave background (CMB) obtained using the South Pole Telescope at 150 GHz to construct a map of the gravitational convergence to z ~ 1100, revealing the fluctuations in the projected mass density. This map shows individual features that are significant at the ~4\u03c3 level, providing the first image of CMB lensing convergence. We cross-correlate this map with Herschel/SPIRE maps covering 90 deg2 at wavelengths of 500, 350, and 250 \u03bcm. We show that these submillimeter (submm) wavelength maps are strongly correlated with the lensing convergence map, with detection significances in each of the three submm bands ranging from 6.7\u03c3 to 8.8\u03c3. We fit the measurement of the cross power spectrum assuming a simple constant bias model and infer bias factors of b = 1.3-1.8, with a statistical uncertainty of 15%, depending on the assumed model for the redshift distribution of the dusty galaxies that are contributing to the Herschel/SPIRE maps.", "date": "2013-07-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "771", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L16", "id_number": "CaltechAUTHORS:20130812-093103295", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130812-093103295", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0638937" }, { "agency": "NSF", "grant_number": "PHY-1125897" }, { "agency": "Kavli Foundation" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "National Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Research Chairs program" }, { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "NSF", "grant_number": "AST-1009012" }, { "agency": "NSF", "grant_number": "AST-1009811" }, { "agency": "NASA Hubble Fellowship grant", "grant_number": "HF-51275.01" }, { "agency": "KICP Fellowship" }, { "agency": "Alfred P. Sloan Research Fellowship" }, { "agency": "BCCP Fellowship" } ] }, "doi": "10.1088/2041-8205/771/1/L16", "primary_object": { "basename": "1303.5048v1.pdf", "url": "https://authors.library.caltech.edu/records/d1j3a-5aw41/files/1303.5048v1.pdf" }, "related_objects": [ { "basename": "2041-8205_771_1_L16.pdf", "url": "https://authors.library.caltech.edu/records/d1j3a-5aw41/files/2041-8205_771_1_L16.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Holder, G. P.; Viero, M. P.; et el." }, { "id": "https://authors.library.caltech.edu/records/6wazf-6sy97", "eprint_id": 39620, "eprint_status": "archive", "datestamp": "2023-08-19 20:27:43", "lastmod": "2023-10-24 17:00:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Fu-Hai", "name": { "family": "Fu", "given": "Hai" }, "orcid": "0000-0001-9608-6395" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "The rapid assembly of an elliptical galaxy of 400 billion solar masses at a redshift of 2.3", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 Nature Publishing Group, a division of Macmillan Publishers Limited.\n\nReceived 15 February; accepted 12 April 2013. Published online 22 May.\n\nCorrected online 19 June 2013--The x and y axis labels of Fig. 1b were corrected.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This research has made use of data from the HerMES project\n(http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme using Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. SPIRE has been developed by a consortium of institutes led by Cardiff\nUniversity (UK) and including the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, the University of Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the University of Sussex (UK); and Caltech/JPL, IPAC and the University of Colorado (USA).\nThis development has been supported by the following national funding agencies: CSA (Canada); NAOC (China); CEA, CNES and CNRS (France); ASI (Italy); MCINN (Spain);\nSNSB (Sweden); STFC (UK); and NASA (USA). The data presented in this paper will be released through the HeDaM Database in Marseille at http://hedam.oamp.fr/HerMES.\n\n\nAuthor Contributions: H.F. and A.C. wrote the manuscript and led the project. C.F., R.J.I.,\nD.A.R., M.G., R.S.B. and A.I.H. contributed significantly to the taking and analysis of the\nfollow-up data with various instruments. All other co-authors of this paper contributed\nextensively and equally by their varied contributions to the HerMES project, planning of\nHerMES observations, analysis of HerMES data, and by commenting on this\nmanuscript as part of an internal review process.\n\nSubmitted - 1305.4930v1.pdf
Supplemental Material - nature12184-s1.pdf
", "abstract": "Stellar archaeology shows that massive elliptical galaxies formed rapidly about ten billion years ago with star-formation rates of above several hundred solar masses per year. Their progenitors are probably the submillimetre bright galaxies at redshifts z greater than 2. Although the mean molecular gas mass (5\u2009\u00d7\u200910^(10) solar masses) of the submillimetre bright galaxies can explain the formation of typical elliptical galaxies, it is inadequate to form elliptical galaxies4 that already have stellar masses above 2\u2009\u00d7\u200910^(11) solar masses at z\u2009\u2248\u20092. Here we report multi-wavelength high-resolution observations of a rare merger of two massive submillimetre bright galaxies at z = 2.3. The system is seen to be forming stars at a rate of 2,000 solar masses per year. The star-formation efficiency is an order of magnitude greater than that of normal galaxies, so the gas reservoir will be exhausted and star formation will be quenched in only around 200 million years. At a projected separation of 19\u2009 kiloparsecs, the two massive starbursts are about to merge and form a passive elliptical galaxy with a stellar mass of about 4\u2009\u00d7\u200910^(11) solar masses. We conclude that gas-rich major galaxy mergers with intense star formation can form the most massive elliptical galaxies by z\u2009\u2248\u20091.5.", "date": "2013-06-20", "date_type": "published", "publication": "Nature", "volume": "498", "number": "7454", "publisher": "Nature Publishing Group", "pagerange": "338-341", "id_number": "CaltechAUTHORS:20130729-100444888", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130729-100444888", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "doi": "10.1038/nature12184", "primary_object": { "basename": "nature12184-s1.pdf", "url": "https://authors.library.caltech.edu/records/6wazf-6sy97/files/nature12184-s1.pdf" }, "related_objects": [ { "basename": "1305.4930v1.pdf", "url": "https://authors.library.caltech.edu/records/6wazf-6sy97/files/1305.4930v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Fu, Hai; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/e13v9-n4q19", "eprint_id": 39650, "eprint_status": "archive", "datestamp": "2023-08-19 20:25:21", "lastmod": "2023-10-20 22:19:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gruppioni-C", "name": { "family": "Gruppioni", "given": "C." }, "orcid": "0000-0002-5836-4056" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Herschel PEP/HerMES luminosity function \u2013 I. Probing the evolution of PACS selected Galaxies to z \u2243 4", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active \u2013 galaxies: evolution \u2013 galaxies: luminosity function, mass function\n\u2013 galaxies: starburst \u2013 cosmology: observations \u2013 infrared: galaxies", "note": "\u00a9 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 February 18. Received 2013 February 13; in original form 2012 October 23. First published online: April 16, 2013. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPACS has been developed by a consortium of institutes led by MPE (Germany) and including: UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); and IAC (Spain). This\ndevelopment has been supported by the funding agencies BMVIT\n(Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR\n(Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE\nhas been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI,Univ. Padua (Italy); IAC (Spain); StockholmObservatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). CG and FP acknowledge financial contribution from the contracts PRIN-INAF 1.06.09.05 and ASI-INAF I00507/1 and I005110. PM thanks the University of Trieste for the grant FRA2009. The authors thank an anonymous referee for the helpful comments that greatly improved the quality of the paper.\n\nPublished - MNRAS-2013-Gruppioni-23-52.pdf
Submitted - 1302.5209v2.pdf
Erratum - stt1748.pdf
", "abstract": "We exploit the deep and extended far-IR data sets (at 70, 100 and 160 \u03bcm) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 \u03bcm, to derive the evolution of the rest-frame 35-, 60-, 90- and total infrared (IR) luminosity functions (LFs) up to z \u223c 4. We detect very strong luminosity evolution for the total IR LF (L_IR \u221d (1 + z)^3.55 \u00b1 0.10) up to z \u223c 2, and \u221d (1 + z)^(1.62 \u00b1 0.51) at 2 < z \u2272 4) combined with a density evolution (\u221d(1 + z)^(\u22120.57 \u00b1 0.22) up to z \u223c 1 and \u221d (1 + z)^(\u22123.92 \u00b1 0.34) at 1 < z \u2272 4). In agreement with previous findings, the IR luminosity density (\u03c1IR) increases steeply to z \u223c 1, then flattens between z \u223c 1 and z \u223c 3 to decrease at z \u2273 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to \u03c1IR. Galaxies occupying the well-established SFR\u2013stellar mass main sequence (MS) are found to dominate both the total IR LF and \u03c1IR at all redshifts, with the contribution from off-MS sources (\u22650.6 dex above MS) being nearly constant (\u223c20 per cent of the total \u03c1IR) and showing no significant signs of increase with increasing z over the whole 0.8 < z < 2.2 range. Sources with mass in the range 10 \u2264 log(M/M_\u2299) \u2264 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (\u22732) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies.", "date": "2013-06-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "432", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "23-52", "id_number": "CaltechAUTHORS:20130730-104305133", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130730-104305133", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "1.06.09.05" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I00507/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I005110" }, { "agency": "University of Trieste", "grant_number": "FRA2009" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stt308", "primary_object": { "basename": "1302.5209v2.pdf", "url": "https://authors.library.caltech.edu/records/e13v9-n4q19/files/1302.5209v2.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Gruppioni-23-52.pdf", "url": "https://authors.library.caltech.edu/records/e13v9-n4q19/files/MNRAS-2013-Gruppioni-23-52.pdf" }, { "basename": "stt1748.pdf", "url": "https://authors.library.caltech.edu/records/e13v9-n4q19/files/stt1748.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Gruppioni, C.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/vrdmq-8pg94", "eprint_id": 39269, "eprint_status": "archive", "datestamp": "2023-08-19 20:21:09", "lastmod": "2023-10-24 16:37:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } } ] }, "title": "HerMES: A Deficit in the Surface Brightness of the Cosmic Infrared Background due to Galaxy Cluster Gravitational Lensing", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation", "note": "\u00a9 2013 The American Astronomical Society.\n\nReceived 2013 April 3; accepted 2013 April 26; published 2013 May 15.\n\nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\n\n\nSPIRE has been developed by a consortium of institutes\nled by Cardiff University (UK) and including: University of\nLethbridge (Canada); NAOC (China); CEA, LAM (France);\nIFSI, University of Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, University of Sussex (UK); Caltech, JPL,\nNHSC, University of Colorado (USA). This development has\nbeen supported by national funding agencies: CSA (Canada);\nNAOC (China); CEA, CNES, CNRS (France); ASI (Italy);\nMCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and\nNASA (USA).\nHCSS/HSpot/HIPE are joint developments by the Herschel\nScience Ground Segment Consortium, consisting of ESA, the\nNASA Herschel Science Center, and the HIFI, PACS and SPIRE\nconsortia.\nThis work is based in part on archival data obtained with\nthe Spitzer Space Telescope, which is operated by JPL/Caltech\nunder a contract with NASA.\nSupport for this work was provided by NASA.\n\nPublished - 2041-8205_769_2_L31.pdf
Submitted - 1303.6725v1.pdf
", "abstract": "We have observed four massive galaxy clusters with the SPIRE instrument on the Herschel Space Observatory and measure a deficit of surface brightness within their central region after removing detected sources. We simulate the effects of instrumental sensitivity and resolution, the source population, and the lensing effect of the clusters to estimate the shape and amplitude of the deficit. The amplitude of the central deficit is a strong function of the surface density and flux distribution of the background sources. We find that for the current best fitting faint end number counts, and excellent lensing models, the most likely amplitude of the central deficit is the full intensity of the cosmic infrared background (CIB). Our measurement leads to a lower limit to the integrated total intensity of the CIB of I_250 \u00b5m > 0.69^(+0.03)_(-0.03) (stat)^(+0.11)_(-0.06)(sys.) MJy sr^(-1), with more CIB possible from both low-redshift sources and from sources within the target clusters. It should be possible to observe this effect in existing high angular resolution data at other wavelengths where the CIB is bright, which would allow tests of models of the faint source component of the CIB.", "date": "2013-06-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "769", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L31", "id_number": "CaltechAUTHORS:20130709-110259992", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130709-110259992", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1088/2041-8205/769/2/L31", "primary_object": { "basename": "2041-8205_769_2_L31.pdf", "url": "https://authors.library.caltech.edu/records/vrdmq-8pg94/files/2041-8205_769_2_L31.pdf" }, "related_objects": [ { "basename": "1303.6725v1.pdf", "url": "https://authors.library.caltech.edu/records/vrdmq-8pg94/files/1303.6725v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Zemcov, M.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/144mv-ftm42", "eprint_id": 39864, "eprint_status": "archive", "datestamp": "2023-08-22 09:30:54", "lastmod": "2023-10-24 17:15:43", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Gruppioni-C", "name": { "family": "Gruppioni", "given": "C." }, "orcid": "0000-0002-5836-4056" }, { "id": "Cucciati-O", "name": { "family": "Cucciati", "given": "O." }, "orcid": "0000-0002-9336-7551" }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S." } }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "J. S." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Nordon-R", "name": { "family": "Nordon", "given": "R." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "Popesso-P", "name": { "family": "Popesso", "given": "P." } }, { "id": "Pozzi-F", "name": { "family": "Pozzi", "given": "F." } }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } } ] }, "title": "Herschel PEP/HerMES: the redshift evolution (0 \u2264 z \u2264 4) of dust attenuation and of the total (UV+IR) star formation rate density", "ispublished": "pub", "full_text_status": "public", "keywords": "early Universe; cosmology: observations; galaxies: star formation; infrared: galaxies; galaxies: starburst; ultraviolet: galaxies", "note": "\u00a9 2013 ESO. Article published by EDP Sciences.\n\nReceived 5 April 2013; Accepted 29 April 2013.\n\nPublished online 05 June 2013.\n\n\nPACS has been developed by a consortium of institutes\nled by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT\n(Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory\n(Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden);\nSTFC, UKSA (UK); and NASA (USA). The authors acknowledge financial contribution from the contracts PRIN-INAF 1.06.09.05 and ASI-INAF I00507/1 and I005110. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, OAMP (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL,\nUCL-MSSL, UKATC, University of Sussex (UK); and Caltech/ JPL, IPAC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC\n(UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM; http://hedam.oamp.fr/HerMES). This work makes use of TOPCAT (http://www.star.bristol.ac.uk/?mbt/topcat/).\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPublished - aa21651-13.pdf
Submitted - 1304.7000v2.pdf
", "abstract": "Using new homogeneous luminosity functions (LFs) in the far-ultraviolet (FUV) from VVDS and in the far-infrared (FIR) from Herschel/PEP and Herschel/HerMES, we studied the evolution of the dust attenuation with redshift. With this information, we were able to estimate the redshift evolution of the total (FUV + FIR) star formation rate density (SFRD_TOT). By integrating SFRD_TOT, we followed the mass building and analyzed the redshift evolution of the stellar mass density (SMD). This article aims at providing a complete view of star formation from the local Universe to z ~ 4 and, using assumptions on earlier star formation history, compares this evolution with previously published data in an attempt to draw a homogeneous picture of the global evolution of star formation in galaxies. Our main conclusions are that: 1) the dust attenuation A_FUV is found to increase from z = 0 to z ~ 1.2 and then starts to decrease until our last data point at z = 3.6; 2) the estimated SFRD confirms published results to z ~ 2. At z > 2, we observe either a plateau or a small increase up to z ~ 3 and then a likely decrease up to z = 3.6; 3) the peak of AFUV is delayed with respect to the plateau of SFRD_TOT and a probable origin might be found in the evolution of the bright ends of the FUV and FIR LFs; 4) using assumptions (exponential rise and linear rise with time) for the evolution of the star formation density from z = 3.6 to z_form = 10, we integrated SFRDTOT and obtained a good agreement with the published SMDs.", "date": "2013-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "554", "publisher": "EDP Sciences", "pagerange": "Art. No. A70", "id_number": "CaltechAUTHORS:20130812-092251046", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130812-092251046", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "1.06.09.05" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I00507/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I005110" }, { "agency": "Stockholm Observatory" } ] }, "doi": "10.1051/0004-6361/201321651", "primary_object": { "basename": "1304.7000v2.pdf", "url": "https://authors.library.caltech.edu/records/144mv-ftm42/files/1304.7000v2.pdf" }, "related_objects": [ { "basename": "aa21651-13.pdf", "url": "https://authors.library.caltech.edu/records/144mv-ftm42/files/aa21651-13.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Burgarella, D.; Buat, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/kzms5-yq422", "eprint_id": 38923, "eprint_status": "archive", "datestamp": "2023-08-22 09:24:10", "lastmod": "2023-10-24 14:52:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Capak-P", "name": { "family": "Capak", "given": "P. L." }, "orcid": "0000-0003-3578-6843" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Herschel census of infrared SEDs through cosmic time", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimetre: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. \n\nAccepted 2013 February 19. Received 2013 February 4; in original form 2012 October 21. First published online: April 1, 2013. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nThis paper uses data from Herschel's photometers SPIRE and\nPACS. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain).\n\nPublished - MNRAS-2013-Symeonidis-2317-40.pdf
Accepted Version - 1302.4895.pdf
", "abstract": "Using Herschel data from the deepest SPIRE and PACS surveys (HerMES and PEP) in COSMOS, GOODS-S and GOODS-N, we examine the dust properties of infrared (IR)-luminous (L_IR > 10^10 L_\u2299) galaxies at 0.1 < z < 2 and determine how these evolve with cosmic time. The unique angle of this work is the rigorous analysis of survey selection effects, making this the first study of the star-formation-dominated, IR-luminous population within a framework almost entirely free of selection biases. We find that IR-luminous galaxies have spectral energy distributions (SEDs) with broad far-IR peaks characterized by cool/extended dust emission and average dust temperatures in the 25\u201345 K range. Hot (T > 45\u2009K) SEDs and cold (T < 25\u2009K), cirrus-dominated SEDs are rare, with most sources being within the range occupied by warm starbursts such as M82 and cool spirals such as M51. We observe a luminosity\u2013temperature (L-T) relation, where the average dust temperature of log [L_IR/L_\u2299] \u223c 12.5 galaxies is about 10 K higher than that of their log [L_IR/L_\u2299] \u223c 10.5 counterparts. However, although the increased dust heating in more luminous systems is the driving factor behind the L-T relation, the increase in dust mass and/or starburst size with luminosity plays a dominant role in shaping it. Our results show that the dust conditions in IR-luminous sources evolve with cosmic time: at high redshift, dust temperatures are on average up to 10 K lower than what is measured locally (z \u2272 0.1). This is manifested as a flattening of the L-T relation, suggesting that (ultra)luminous infrared galaxies [(U)LIRGs] in the early Universe are typically characterized by a more extended dust distribution and/or higher dust masses than local equivalent sources. Interestingly, the evolution in dust temperature is luminosity dependent, with the fraction of LIRGs with T < 35 K showing a two-fold increase from z \u223c 0 to z \u223c 2, whereas that of ULIRGs with T < 35 K shows a six-fold increase. Our results suggest a greater diversity in the IR-luminous population at high redshift, particularly for ULIRGs.", "date": "2013-05-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "431", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2317-2340", "id_number": "CaltechAUTHORS:20130612-134204476", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130612-134204476", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1093/mnras/stt330", "primary_object": { "basename": "1302.4895.pdf", "url": "https://authors.library.caltech.edu/records/kzms5-yq422/files/1302.4895.pdf" }, "related_objects": [ { "basename": "MNRAS-2013-Symeonidis-2317-40.pdf", "url": "https://authors.library.caltech.edu/records/kzms5-yq422/files/MNRAS-2013-Symeonidis-2317-40.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Symeonidis, M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/jej8e-7k075", "eprint_id": 38838, "eprint_status": "archive", "datestamp": "2023-08-22 09:13:24", "lastmod": "2023-10-23 23:31:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D. G." }, "orcid": "0000-0003-1748-2010" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Amblard-A", "name": { "family": "Amblard", "given": "A." } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S." } }, { "id": "Ibar-Eduardo", "name": { "family": "Ibar", "given": "E." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Marsden-G", "name": { "family": "Marsden", "given": "G." } }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Smith-A-J", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Connecting stellar mass and star-formation rate to dark matter halo mass out to z \u223c 2", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical; cosmology: observations; large-scale structure of Universe; infrared: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2013 January 31. Received 2013 January 25; in original form 2012 March 22.\n\nFirst published online: March 7, 2013.\n\nWe thank the anonymous referee for constructive comments. We\nalso thank Cheng Li for providing the SDSS clustering measurements and the stellar mass function, Rachel Mandelbaum for the stellar mass m\u2217\u2013halo mass Mh relation from weak lensing, Surhud More for them\u2217\u2212Mh relation from satellite kinematics, Alexi Leauthaud for the m\u2217\u2212Mh relation, Samir Salim for the conditional dependence\nof specific star-formation rate on m\u2217 in the local Universe,\nBenjamin Moster for useful discussions on the CSMF, Anthony\nLewis for useful discussion on MCMC methods and Peder Norberg for general discussions. LW acknowledges support from UK's Science and Technology Facilities Council grant ST/F002858/1 and an ERC StG grant (DEGAS-259586). SJO is supported by UK's Science and Technology Facilities Council grant ST/F002858/1. The data presented in this paper will be released through the Herschel data base in Marseille HeDaM (hedam.oamp.fr/herMES). SPIRE has been developed\nby a consortium of institutes led by Cardiff Univ. (UK) and\nincluding Univ. Lethbridge (Canada); NAOC (China); CEA, LAM\n(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).\n\nPublished - MNRAS-2013-Wang-648-61.pdf
", "abstract": "We have constructed an extended halo model (EHM) which relates the total stellar mass and star-formation rate (SFR) to halo mass (M_h). An empirical relation between the distribution functions of total stellar mass of galaxies and host halo mass, tuned to match the spatial density of galaxies over 0 < z < 2 and the clustering properties at z \u223c 0, is extended to include two different scenarios describing the variation of SFR on M_h. We also present new measurements of the redshift evolution of the average SFR for star-forming galaxies of different stellar masses up to z = 2, using data from the Herschel Multi-tiered Extragalactic Survey for infrared bright galaxies. Combining the EHM with the halo accretion histories from numerical simulations, we trace the stellar mass growth and star-formation history in haloes spanning a range of masses. We find that: (1) the intensity of the star-forming activity in haloes in the probed mass range has steadily decreased from z \u223c 2 to 0; (2) at a given epoch, haloes in the mass range between a few times 10^(11)\u2009M_\u2299 and a few times 10^(12)\u2009M_\u2299 are the most efficient at hosting star formation; (3) the peak of SFR density shifts to lower mass haloes over time; and (4) galaxies that are forming stars most actively at z \u223c 2 evolve into quiescent galaxies in today's group environments, strongly supporting previous claims that the most powerful starbursts at z \u223c 2 are progenitors of today's elliptical galaxies.", "date": "2013-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "431", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "648-661", "id_number": "CaltechAUTHORS:20130606-115901445", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130606-115901445", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "European Research Council (ERC)", "grant_number": "DEGAS-259586" } ] }, "doi": "10.1093/mnras/stt190", "primary_object": { "basename": "MNRAS-2013-Wang-648-61.pdf", "url": "https://authors.library.caltech.edu/records/jej8e-7k075/files/MNRAS-2013-Wang-648-61.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Wang, L.; Farrah, D. G.; et el." }, { "id": "https://authors.library.caltech.edu/records/qj7sp-ywb34", "eprint_id": 38246, "eprint_status": "archive", "datestamp": "2023-08-19 19:35:53", "lastmod": "2023-10-23 19:58:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Kov\u00e1cs-A", "name": { "family": "Kov\u00e1cs", "given": "A." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxies and clusters", "note": "\u00a9 2013 Macmillan Publishers Limited.\n\nReceived 4 October 2012; accepted 27 February 2013.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This research has made use of data from the HerMES project. HerMES is a Herschel Key Programme using guaranteed time from the SPIRE instrument team, ESAC scientists and a mission scientist. See Supplementary Information for further acknowledgements.\n\nAuthor Contributions: D.A.R. had the overall lead of the project. C.M.B., D.L.C., I.P.-F.,\nR.J.I., C.B., H.F., J.D.V. and R.N. contributed significantly to the taking and analysis of the\nfollow-up data with different instruments by leading several telescope proposals and\nanalysis efforts. C.D.D. led the selection of the parent sample. A. Conley, J.W., J.C., A.\nCooray, P.H. and J.K. contributed significantly to the data analysis and to fitting and\nmodelling the results. All other authors contributed to the proposals, source selection,\ndata analysis and interpretation, in particular through work on the primary Herschel\nSPIRE data in which the source was discovered through the HerMES consortium(led by\nJ.B. and S.J.O.). All authors have reviewed, discussed, and commented on the\nmanuscript.\n\nAccepted Version - 1304.4256.pdf
Supplemental Material - nature12050-s1.pdf
", "abstract": "Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts\u2014that is, increased rates of star formation\u2014in the most massive dark-matter haloes at early epochs. However, it remains unknown how soon after the Big Bang massive starburst progenitors exist. The measured redshift (z) distribution of dusty, massive starbursts has long been suspected to be biased low in z owing to selection effects, as confirmed by recent findings of systems with redshifts as high as ~5 (refs 2\u20134). Here we report the identification of a massive starburst galaxy at z = 6.34 through a submillimetre colour-selection technique. We unambiguously determined the redshift from a suite of molecular and atomic fine-structure cooling lines. These measurements reveal a hundred billion solar masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at least 40 per cent of the baryonic mass. A 'maximum starburst' converts the gas into stars at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoch. Despite the overall downturn in cosmic star formation towards the highest redshifts, it seems that environments mature enough to form the most massive, intense starbursts existed at least as early as 880 million years after the Big Bang.", "date": "2013-04-18", "date_type": "published", "publication": "Nature", "volume": "496", "number": "7445", "publisher": "Nature Publishing Group", "pagerange": "329-333", "id_number": "CaltechAUTHORS:20130502-132215358", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130502-132215358", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "doi": "10.1038/nature12050", "primary_object": { "basename": "1304.4256.pdf", "url": "https://authors.library.caltech.edu/records/qj7sp-ywb34/files/1304.4256.pdf" }, "related_objects": [ { "basename": "nature12050-s1.pdf", "url": "https://authors.library.caltech.edu/records/qj7sp-ywb34/files/nature12050-s1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Riechers, Dominik A.; Bradford, C. M.; et el." }, { "id": "https://authors.library.caltech.edu/records/74sxd-qy156", "eprint_id": 38269, "eprint_status": "archive", "datestamp": "2023-08-22 09:06:56", "lastmod": "2023-10-23 19:59:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Weiss-Axel", "name": { "family": "Wei\u00df", "given": "A." }, "orcid": "0000-0003-4678-3939" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Downes-T-P", "name": { "family": "Downes", "given": "T. P." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Padin-S", "name": { "family": "Padin", "given": "S." } }, { "id": "Shirokoff-E", "name": { "family": "Shirokoff", "given": "E." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z." } } ] }, "title": "ALMA Redshifts of Millimeter-selected Galaxies from the SPT Survey: The Redshift Distribution of Dusty Star-forming Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; early universe; galaxies: evolution; galaxies: high-redshift; ISM: molecules", "note": "\u00a9 2013 American Astronomical Society. Received 2012 October 31; accepted 2013 February 15; published 2013 March 28. The authors thank A. Blain and N. Scoville for many useful\ndiscussions related to this work, and A. Benson, C. Baugh,\nC. Hayward, and C. Lacey for providing us with the predicted\nredshift distributions from their models and useful discussions regarding their implications. This paper makes use of the following ALMA data:ADS/JAO.ALMA#2011.0.00957.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. Based on observations taken with European Southern Observatory Very Large Telescope, Paranal, Chile, with program ID 088.A-0902(C), and with the Atacama Pathfinder Experiment under program IDs 086.A-0793(A), 086.A-1002(A), 087.A-0815(A) and 087.A-0968(A). APEX is a collaboration between the Max-Planck-Institut f\u00fcr Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. This research has made use of the NASA/IPAC Extragalactic\nDatabase (NED) which is operated by the Jet Propulsion\nLaboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support through PHY-1125897, the Kavli Foundation and the Gordon and Betty Moore Foundation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Partial support for this work was provided by NASA through grant HST-GO-12659 from the Space Telescope Science Institute. This work is based in part on observations made with Herschel, a European\nSpace Agency Cornerstone Mission with significant participation by NASA, and supported through an award issued by JPL/Caltech for OT2_jvieira_5. T.R.G. gratefully acknowledges support from a STFC Advanced Fellowship.\n\nPublished - 0004-637X_767_1_88.pdf
Submitted - 1303.2726v1.pdf
", "abstract": "Using the Atacama Large Millimeter/submillimeter Array, we have conducted a blind redshift survey in the 3 mm atmospheric transmission window for 26 strongly lensed dusty star-forming galaxies (DSFGs) selected with the South Pole Telescope. The sources were selected to have S_(1.4mm) > 20 mJy and a dust-like spectrum and, to remove low-z sources, not have bright radio (S_843MHz) < 6 mJy) or far-infrared counterparts (S_(100\u03bcm) < 1 Jy, S_(60\u03bcm) < 200 mJy). We robustly detect 44 line features in our survey, which we identify as redshifted emission lines of ^(12)CO, ^(13)CO, C I, H_2O, and H_2O^+. We find one or more spectral features in 23 sources yielding a ~90% detection rate for this survey; in 12 of these sources we detect multiple lines, while in 11 sources we detect only a single line. For the sources with only one detected line, we break the redshift degeneracy with additional spectroscopic observations if available, or infer the most likely line identification based on photometric data. This yields secure redshifts for ~70% of the sample. The three sources with no lines detected are tentatively placed in the redshift desert between 1.7 < z < 2.0. The resulting mean redshift of our sample is z = 3.5. This finding is in contrast to the redshift distribution of radio-identified DSFGs, which have a significantly lower mean redshift of z = 2.3 and for which only 10%-15% of the population is expected to be at z > 3. We discuss the effect of gravitational lensing on the redshift distribution and compare our measured redshift distribution to that of models in the literature.", "date": "2013-04-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "767", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 88", "id_number": "CaltechAUTHORS:20130503-143501568", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130503-143501568", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "NSF", "grant_number": "ANT-0638937" }, { "agency": "NSF", "grant_number": "PHY-1125897" }, { "agency": "Kavli Foundation" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "NASA Space Telescope Science Institute", "grant_number": "HST-GO-12659" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "STFC Advanced Fellowship" } ] }, "doi": "10.1088/0004-637X/767/1/88", "primary_object": { "basename": "0004-637X_767_1_88.pdf", "url": "https://authors.library.caltech.edu/records/74sxd-qy156/files/0004-637X_767_1_88.pdf" }, "related_objects": [ { "basename": "1303.2726v1.pdf", "url": "https://authors.library.caltech.edu/records/74sxd-qy156/files/1303.2726v1.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Wei\u00df, A.; Vieira, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/3ay9y-z6y07", "eprint_id": 37678, "eprint_status": "archive", "datestamp": "2023-08-19 19:06:17", "lastmod": "2023-10-23 17:56:14", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Padin-S", "name": { "family": "Padin", "given": "S." } }, { "id": "Shirokoff-E", "name": { "family": "Shirokoff", "given": "E." } }, { "id": "Staniszewski-Z", "name": { "family": "Staniszewski", "given": "Z." } } ] }, "title": "Dusty starburst galaxies in the early Universe as revealed by gravitational lensing", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2013 Macmillan Publishers Limited.\n\nReceived 28 August 2012; accepted 12 February 2013.\nPublished online 13 March 2013.\nThe SPT is supported by the National Science Foundation, the\nKavli Foundation and the Gordon and Betty Moore Foundation. ALMA is a partnership\nof ESO (representing its member states), NSF (USA) and NINS (Japan), together with\nNRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with Chile. The Joint ALMA\nObservatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy\nObservatory is a facility of the NSF operated under cooperative agreement by\nAssociated Universities, Inc. Partial support for this work was provided by NASA from\nthe Space Telescope Science Institute. This work is based in part on observations made\nwith Herschel, a European Space Agency Cornerstone Mission with significant\nparticipation by NASA. Work at McGill University is supported by NSERC, the CRC\nprogramme and CIfAR.\n\nAuthor Contributions: J.D.V. and D.P.M. wrote the text. S.C.C. took and reduced optical\nimages and spectroscopy. A.W., C.D.B. and D.P.M. analysed the ALMA spectra. D.P.M.,\nJ.S.S. and Y.D.H. analysed the ALMA imaging data. J.D.V. reduced and analysed the\nHerschel data. Y.D.H. constructed the lens models. C.D.F. reduced optical images. All\nother authors (listed alphabetically) have contributed as part of the South Pole\nTelescope collaboration, by their involvement with the construction of the instrument,\nthe initial discovery of the sources, multi-wavelength follow-up, and/or contributions to\nthe text.\n\nSupplemental Material - nature12001-s1.pdf
", "abstract": "In the past decade, our understanding of galaxy evolution has been revolutionized by the discovery that luminous, dusty starburst galaxies were 1,000 times more abundant in the early Universe than at present. It has, however, been difficult to measure the complete redshift distribution of these objects, especially at the highest redshifts (z\u2009>\u20094). Here we report a redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources. High-resolution imaging demonstrates that these sources are strongly gravitationally lensed by foreground galaxies. We detect spectral lines in 23 out of 26 sources and multiple lines in 12 of those 23 sources, from which we obtain robust, unambiguous redshifts. At least 10 of the sources are found to lie at z\u2009>\u20094, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought. Models of lens geometries in the sample indicate that the background objects are ultra-luminous infrared galaxies, powered by extreme bursts of star formation.", "date": "2013-03-21", "date_type": "published", "publication": "Nature", "volume": "495", "number": "7441", "publisher": "Nature Publishing Group", "pagerange": "344-347", "id_number": "CaltechAUTHORS:20130328-134810813", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130328-134810813", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF" }, { "agency": "Kavli Foundation" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "NASA Space Telescope Science Institute (STSCI)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "CRC Programme" }, { "agency": "Canadian Institute for Advanced Research (CIfAR)" } ] }, "doi": "10.1038/nature12001", "primary_object": { "basename": "nature12001-s1.pdf", "url": "https://authors.library.caltech.edu/records/3ay9y-z6y07/files/nature12001-s1.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Vieira, J. D.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/h7xgg-91v51", "eprint_id": 38924, "eprint_status": "archive", "datestamp": "2023-08-22 08:54:20", "lastmod": "2023-10-24 14:52:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hildebrandt-H", "name": { "family": "Hildebrandt", "given": "H." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "Inferring the mass of submillimetre galaxies by exploiting\n their gravitational magnification of background galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: weak; galaxies: high-redshift; submillimetre: galaxies", "note": "\u00a9 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.\n\nAccepted 2012 December 6. Received 2012 November 26; in original form 2012 November 11.\n\nFirst published online: January 7, 2013.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. The HerMES data were accessed through the HeDaM data base (http://hedam.oamp.fr) operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille. The optical data are based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada\u2013France\u2013Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre, as part of the Canada\u2013France\u2013Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. HH is supported by the Marie Curie IOF 252760, a CITA National Fellowship and the DFG grant Hi 1495/2-1. LvW is supported by NSERC and CIfAR. DS acknowledges support by NSERC and CSA. TE is supported by the Deutsche Forschungsgemeinschaft through project ER 327/3-1 and the Transregional Collaborative Research Centre TR 33 \u2013 'The Dark Universe'. RFJvdB acknowledges support from the Netherlands Organisation for Scientic Research grant number 639.042.814.\nAuthor Contributions: HH led the analysis and wrote the draft version of the paper. LvW and DS contributed significantly in the development of this project through ideas and discussions on a daily basis. MB provided the redshift distribution of the submillimetre galaxies. TE led the optical data reduction and calibration. RFJvdB\nprovided the luminosity function estimate of the background galaxies. All other co-authors contributed extensively and equally by their varied contributions to the SPIRE instrument, the Herschelmission, analysis of SPIRE and HerMES data, planning of HerMES observations and scientific support of HerMES and by commenting on this manuscript as part of an internal review process.\n\nPublished - MNRAS-2013-Hildebrandt-3230-7.pdf
", "abstract": "Dust emission at submillimetre wavelengths allows us to trace the early phases of star formation in the Universe. In order to understand the physical processes involved in this mode of star formation, it is essential to gain knowledge about the dark matter structures \u2013 most importantly their masses \u2013 that submillimetre galaxies live in. Here we use the magnification effect of gravitational lensing to determine the average mass and dust content of submillimetre galaxies with 250\u2009\u03bcm flux densities of S_250 > 15\u2009mJy selected using data from the Herschel Multi-tiered Extragalactic Survey. The positions of hundreds of submillimetre foreground lenses are cross-correlated with the positions of background Lyman-break galaxies at z \u223c 3\u20135 selected using optical data from the Canada\u2013France\u2013Hawaii Telescope Legacy Survey. We detect a cross-correlation signal at the 7\u03c3 level over a sky area of 1\u2009deg^2, with \u223c80 per cent of this signal being due to magnification, whereas the remaining \u223c20 per cent comes from dust extinction. Adopting some simple assumptions for the dark matter and dust profiles and the redshift distribution enables us to estimate the average mass of the haloes hosting the submillimetre galaxies to be log\u2009_(10)[M_200/M_\u2299] = \n13.17^(+0.05)_(\u22120.08)(stat.) and their average dust mass fraction (at radii of >10\u2009kpc) to be M_dust/M_200 \u2248 6 \u00d7 10^(\u22125). This supports the picture that submillimetre galaxies are dusty, forming stars at a high rate, reside in massive group-sized haloes and are a crucial phase in the assembly and evolution of structure in the Universe.", "date": "2013-03-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "429", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3230-3237", "id_number": "CaltechAUTHORS:20130612-134247579", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130612-134247579", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Marie Curie Fellowship", "grant_number": "252760" }, { "agency": "CITA National Fellowship" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "Hi 1495/2-1" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "ER 327/3-1" }, { "agency": "Deutsche Forschungsgemeinschaft (DFG)", "grant_number": "TR 33" }, { "agency": "Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)", "grant_number": "639.042.814" } ] }, "local_group": { "items": [ { "id": "COSMOS" } ] }, "doi": "10.1093/mnras/sts585", "primary_object": { "basename": "MNRAS-2013-Hildebrandt-3230-7.pdf", "url": "https://authors.library.caltech.edu/records/h7xgg-91v51/files/MNRAS-2013-Hildebrandt-3230-7.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Hildebrandt, H.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/7dajn-9ee75", "eprint_id": 37723, "eprint_status": "archive", "datestamp": "2023-08-22 08:52:13", "lastmod": "2023-10-23 17:59:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Moyerman-S", "name": { "family": "Moyerman", "given": "S." } }, { "id": "Aiken-R", "name": { "family": "Aiken", "given": "R." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Richter-S", "name": { "family": "Richter", "given": "S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "Scientific Verification of Faraday Rotation Modulators: Detection of Diffuse Polarized Galactic Emission", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: structure; instrumentation: polarimeters; techniques: polarimetric", "note": "\u00a9 2013 American Astronomical Society. Received 2012 December 2; accepted 2013 January 16; published 2013 February 15. S.M. gratefully acknowledges the American Association\nof University Women for a fellowship supporting this research. B.G.K. also acknowledges NSF PECASE Award No.\nAST-0548262. G.R. gratefully acknowledges support by the\nNASA Science Mission Directorate via the US Planck project.\nBICEP is supported by NSF grant OPP-0230438, Caltech\nDiscovery Fund, Caltech Presidents Fund PF-471, JPL Research\nand Technology Fund, and the late J. Robinson.\n\nPublished - 0004-637X_765_1_64.pdf
", "abstract": "The design and performance of a wide bandwidth linear polarization modulator based on the Faraday effect is described. Faraday Rotation Modulators (FRMs) are solid-state polarization switches that are capable of modulation up to 10 kHz. Six FRMs were utilized during the 2006 observing season in the Background Imaging of Cosmic Extragalactic Polarization (BICEP) experiment; three FRMs were used at each of BICEP's 100 and 150 GHz frequency bands. The technology was verified through high signal-to-noise detection of Galactic polarization using two of the six FRMs during four observing runs in 2006. The features exhibit strong agreement with BICEP's measurements of the Galaxy using non-FRM pixels and with the Galactic polarization models. This marks the first detection of high signal-to-noise mm-wave celestial polarization using fast, active optical modulation. The performance of the FRMs during periods when they were not modulated was also analyzed and compared to results from BICEP's 43 pixels without FRMs.", "date": "2013-03-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "765", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 64", "id_number": "CaltechAUTHORS:20130402-120630257", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130402-120630257", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "American Association of University Women" }, { "agency": "NSF", "grant_number": "AST-0548262" }, { "agency": "NASA" }, { "agency": "NSF", "grant_number": "OPP-0230438" }, { "agency": "Caltech Discovery Fund" }, { "agency": "Caltech President's Fund", "grant_number": "PF-471" }, { "agency": "JPL Research and Technology Fund" } ] }, "doi": "10.1088/0004-637X/765/1/64", "primary_object": { "basename": "0004-637X_765_1_64.pdf", "url": "https://authors.library.caltech.edu/records/7dajn-9ee75/files/0004-637X_765_1_64.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Moyerman, S.; Aiken, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/z2dt4-3x583", "eprint_id": 38314, "eprint_status": "archive", "datestamp": "2023-08-22 08:48:25", "lastmod": "2023-10-23 20:02:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Omont-A", "name": { "family": "Omont", "given": "A." }, "orcid": "0000-0002-4721-3922" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" } ] }, "title": "H_2O emission in high-z ultra-luminous infrared galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter: galaxies; radio lines: galaxies", "note": "\u00a9 2013 ESO. Article published by EDP Sciences. \n\nReceived 28 November 2012. Accepted 7 January 2013. Published online 05 March 2013. \n\nHerschel (Pilbratt et al. 2010) is an ESA space observatory with science\ninstruments provided by European-led Principal Investigator consortia\nand with important participation from NASA.\n\nBased on observations carried out with the IRAM Plateau de Bure interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The authors are grateful to the IRAM staff for\ntheir support. US participants in H-ATLAS acknowledge support from NASA through a contract from JPL. Italian participants in H-ATLAS acknowledge a financial contribution from the agreement ASI-INAF I/009/10/0. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ.\nPadua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). M. J. Micha\u0142owski acknowledges the support of a FWO-Pegasus Marie Curie Fellowship.\n\nPublished - aa20811-12.pdf
", "abstract": "Using the IRAM Plateau de Bure interferometer (PdBI), we report the detection of water vapor in six new lensed ultra-luminous starburst galaxies at high redshift, discovered in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). The sources are detected either in the 2_(02)\u22121_(11) or 2_(11)\u22122_(02) H_2O emission lines with integrated line fluxes ranging from 1.8 to 14 Jy km s^(-1). The corresponding apparent luminosities are \u03bcL_(H2O) ~ 3\u221212 \u00d7 10^8\u2009L_\u2299, where \u03bc is the lensing magnification factor (3 < \u03bc < 12). These results confirm that H_2O lines are among the strongest molecular lines in high-z ultra-luminous starburst galaxies, with intensities almost comparable to those of the high-J CO lines, and similar profiles and line widths (~200\u2212900 km s^(-1)). With the current sensitivity of the PdBI, the water lines can therefore easily be detected in high-z lensed galaxies (with F(500 \u03bcm)\u2009>\u2009100\u2009mJy) discovered in the Herschel surveys. Correcting the luminosities for amplification, using existing lensing models, L_(H2O) is found to have a strong dependence on the infrared luminosity, varying as ~L_(IR)^(1.2). This relation, which needs to be confirmed with better statistics, may indicate a role of radiative (infrared) excitation of the H_2O lines, and implies that high-z galaxies with L_(IR) \u2273 10^(13)\u2009L_\u2299 tend to be very strong emitters in water vapor, that have no equivalent in the local universe.", "date": "2013-03", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "551", "publisher": "EDP Sciences", "pagerange": "Art. No. A115", "id_number": "CaltechAUTHORS:20130507-093655427", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130507-093655427", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)", "grant_number": "I/009/10/0" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO)" }, { "agency": "Marie Curie Fellowship" } ] }, "doi": "10.1051/0004-6361/201220811", "primary_object": { "basename": "aa20811-12.pdf", "url": "https://authors.library.caltech.edu/records/z2dt4-3x583/files/aa20811-12.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Omont, A.; Riechers, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/80pgd-kvp22", "eprint_id": 38943, "eprint_status": "archive", "datestamp": "2023-08-19 14:46:10", "lastmod": "2023-10-24 14:53:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Heinis-S", "name": { "family": "Heinis", "given": "S." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Farrah-Duncan", "name": { "family": "Farrah", "given": "D." }, "orcid": "0000-0003-1748-2010" }, { "id": "Ibar-Eduardo", "name": { "family": "Ibar", "given": "E." } }, { "id": "Ilbert-Olivier", "name": { "family": "Ilbert", "given": "O." }, "orcid": "0000-0002-7303-4397" }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G." }, "orcid": "0000-0002-4872-2294" }, { "id": "Marsden-G", "name": { "family": "Marsden", "given": "G." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "Rodighiero-G", "name": { "family": "Rodighiero", "given": "G." }, "orcid": "0000-0002-9415-2296" }, { "id": "Roehlly-Y", "name": { "family": "Roehlly", "given": "Y." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Smith-A-J", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HERMES: unveiling obscured star formation \u2013 the far-infrared luminosity function of ultraviolet-selected galaxies at z \u223c 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical\n galaxies: luminosity function\n infrared: galaxies\n ultraviolet: galaxies", "note": "\u00a9 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2012 November 12. Received 2012 October 31; in original form 2012 April 5. First published online: December 13, 2012. We thank the referee for a careful reading and detailed, constructive comments which helped improving the paper. SH and VB thank the French Space Agency (CNES) for financial support. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA,LAM(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory\n(Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden);\nSTFC, UKSA (UK); and NASA (USA). We thank the COSMOS collaboration for sharing data used in this paper.\nThe data presented in this paper will be released through\nthe Herschel Database in Marseille (HeDaM, http://hedam.\noamp.fr/HerMES), operated by CeSAM and hosted by the\nLaboratoire d'Astrophysique de Marseille.\n\nPublished - MNRAS-2013-Heinis-1113-32.pdf
", "abstract": "We study the far-infrared and sub-millimetre properties of a sample of ultraviolet (UV) selected galaxies at z \u223c 1.5. Using stacking at 250, 350 and 500\u2009\u03bcm from Herschel Space Observatory Spectral and Photometric Imaging Receiver (SPIRE) imaging of the Cosmological Evolution Survey (COSMOS) field obtained within the Herschel Multi-tiered Extragalactic Survey (HERMES) key programme, we derive the mean infrared (IR) luminosity as a function of both UV luminosity and slope of the UV continuum \u03b2. The IR to UV luminosity ratio is roughly constant over most of the UV luminosity range we explore. We also find that the IR to UV luminosity ratio is correlated with \u03b2. We observe a correlation that underestimates the correlation derived from low-redshift starburst galaxies, but is in good agreement with the correlation derived from local normal star-forming galaxies. Using these results we reconstruct the IR luminosity function of our UV-selected sample. This luminosity function recovers the IR luminosity functions measured from IR-selected samples at the faintest luminosities (L_(IR) \u223c 10^(11)\u2009L_\u2299), but might underestimate them at the bright-end (L_(IR) \u2273 5 \u00d7 10^(11)\u2009L_\u2299). For galaxies with 10^(11) < L_(IR)/L_\u2299 < 10^(13), the IR luminosity function of an UV selection recovers (given the differences in IR-based estimates) 52\u201365 to 89\u2013112\u2009per\u2009cent of the star formation rate density derived from an IR selection. The cosmic star formation rate density derived from this IR luminosity function is 61\u201376 to 100\u2013133\u2009per\u2009cent of the density derived from IR selections at the same epoch. Assuming the latest Herschel results and conservative stacking measurements, we use a toy model to fully reproduce the far-IR luminosity function from our UV selection at z \u223c 1.5. This suggests that a sample around 4 mag deeper (i.e. reaching u^* \u223c 30\u2009mag) and a large dispersion of the IR to UV luminosity ratio are required.", "date": "2013-02-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "429", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "1113-1132", "id_number": "CaltechAUTHORS:20130613-104444434", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130613-104444434", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "doi": "10.1093/mnras/sts397", "primary_object": { "basename": "MNRAS-2013-Heinis-1113-32.pdf", "url": "https://authors.library.caltech.edu/records/80pgd-kvp22/files/MNRAS-2013-Heinis-1113-32.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Heinis, S.; Buat, V.; et el." }, { "id": "https://authors.library.caltech.edu/records/tbew4-6sd35", "eprint_id": 64745, "eprint_status": "archive", "datestamp": "2023-08-22 08:39:53", "lastmod": "2023-10-17 21:50:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silva-M-B", "name": { "family": "Silva", "given": "Marta B." }, "orcid": "0000-0003-0209-4816" }, { "id": "Santos-M-G", "name": { "family": "Santos", "given": "Mario G." }, "orcid": "0000-0003-3892-3073" }, { "id": "Gong-Yan", "name": { "family": "Gong", "given": "Yan" } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Intensity Mapping of Lyman-alpha Emission During the Epoch of Reionization", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: theory; diffuse radiation; large-scale structure of universe", "note": "\u00a9 2013 The American Astronomical Society. \n\nReceived 2012 May 10. Accepted 2012 November 30. Published 2013 January 17. \n\nThis work was supported by FCT-Portugal with the grant SFRH/BD/51373/2011 for M.B.S. and under grant PTDC/FIS/100170/2008 for M.B.S. and M.G.S. \n\nA.C. and Y.G. acknowledge support from NSF CAREER AST-0645427 and NASA NNX10AD42G at UCI. \n\nM.B.S. was a long-term Visiting Student at UCI, supported by NSF CAREER AST-0645427, when this work was initiated, and she thanks the Department of Physics and Astronomy at UCI for hospitality during her stay.\n\nPublished - pdf.pdf
Submitted - silva.pdf
", "abstract": "We calculate the absolute intensity and anisotropies of the Ly\u03b1 radiation field present during the epoch of reionization. We consider emission from both galaxies and the intergalactic medium (IGM) and take into account the main contributions to the production of Ly\u03b1 photons: recombinations, collisions, continuum emission from galaxies, and scattering of Lyn photons in the IGM. We find that the emission from individual galaxies dominates over the IGM with a total Ly\u03b1 intensity (times frequency) of about (1.43-3.57) \u00d7 10^(\u20138) erg s^(\u20131) cm^(\u20132) sr^(\u20131) at a redshift of 7. This intensity level is low, so it is unlikely that the Ly\u03b1 background during reionization can be established by an experiment aiming at an absolute background light measurement. Instead, we consider Ly\u03b1 intensity mapping with the aim of measuring the anisotropy power spectrum that has rms fluctuations at the level of 1 \u00d7 10^(\u20131)6 [erg s^(\u20131) cm^(\u20132) sr^(\u20131)]^2 at a few Mpc scales. These anisotropies could be measured with a spectrometer at near-IR wavelengths from 0.9 to 1.4 \u03bcm with fields in the order of 0.5 to 1 deg^2. We recommend that existing ground-based programs using narrowband filters also pursue intensity fluctuations to study statistics on the spatial distribution of faint Ly\u03b1 emitters. We also discuss the cross-correlation signal with 21 cm experiments that probe H I in the IGM during reionization. A dedicated sub-orbital or space-based Ly\u03b1 intensity mapping experiment could provide a viable complimentary approach to probe reionization, when compared to 21 cm experiments, and is likely within experimental reach.", "date": "2013-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "763", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 132", "id_number": "CaltechAUTHORS:20160224-150511943", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160224-150511943", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "SFRH/BD/51373/2011" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PTDC/FIS/100170/2008" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NASA", "grant_number": "NNX10AD42G" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "Keck Institute for Space Studies (KISS)" } ] }, "local_group": { "items": [ { "id": "Keck-Institute-for-Space-Studies" } ] }, "doi": "10.1088/0004-637X/763/2/132", "primary_object": { "basename": "silva.pdf", "url": "https://authors.library.caltech.edu/records/tbew4-6sd35/files/silva.pdf" }, "related_objects": [ { "basename": "pdf.pdf", "url": "https://authors.library.caltech.edu/records/tbew4-6sd35/files/pdf.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Silva, Marta B.; Santos, Mario G.; et el." }, { "id": "https://authors.library.caltech.edu/records/z6krb-2av20", "eprint_id": 37091, "eprint_status": "archive", "datestamp": "2023-08-19 14:36:54", "lastmod": "2023-10-23 16:07:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Silva-M-B", "name": { "family": "Silva", "given": "Marta B." }, "orcid": "0000-0003-0209-4816" }, { "id": "Santos-M-G", "name": { "family": "Santos", "given": "Mario G." }, "orcid": "0000-0003-3892-3073" }, { "id": "Gong-Yan", "name": { "family": "Gong", "given": "Yan" } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Intensity Mapping of Ly\u03b1 Emission during the Epoch of Reionization", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: theory, diffuse radiation, large-scale structure of universe", "note": "\u00a9 2013 American Astronomical Society. \n\nReceived 2012 May 10; accepted 2012 November 30; published 2013 January 17. \n\nThis work was supported by FCT-Portugal with the grant SFRH/BD/51373/2011 for M.B.S. and under grant PTDC/FIS/100170/2008 for M.B.S. and M.G.S. A.C. and Y.G. acknowledge support from NSF CAREER AST-0645427 and NASA NNX10AD42G at UCI. M.B.S. was a long-term Visiting Student at UCI, supported by NSF CAREER AST-0645427, when this work was initiated, and she thanks the Department of Physics and Astronomy at UCI for hospitality during her stay.\n\nPublished - 0004-637X_763_2_132.pdf
Submitted - 1205.1493v2.pdf
", "abstract": "We calculate the absolute intensity and anisotropies of the Ly\u03b1 radiation field present during the epoch of reionization. We consider emission from both galaxies and the intergalactic medium (IGM) and take into account the main contributions to the production of Ly\u03b1 photons: recombinations, collisions, continuum emission from galaxies, and scattering of Lyn photons in the IGM. We find that the emission from individual galaxies dominates over the IGM with a total Ly\u03b1 intensity (times frequency) of about (1.43-3.57) \u00d7 10^(\u20138) erg s^(\u20131) cm^(\u20132) sr^(\u20131) at a redshift of 7. This intensity level is low, so it is unlikely that the Ly\u03b1 background during reionization can be established by an experiment aiming at an absolute background light measurement. Instead, we consider Ly\u03b1 intensity mapping with the aim of measuring the anisotropy power spectrum that has rms fluctuations at the level of 1 \u00d7 10^(\u201316) [erg s^(\u20131) cm^(\u20132) sr^(\u20131)]^2 at a few Mpc scales. These anisotropies could be measured with a spectrometer at near-IR wavelengths from 0.9 to 1.4 \u03bcm with fields in the order of 0.5 to 1 deg^2. We recommend that existing ground-based programs using narrow band filters also pursue intensity fluctuations to study statistics on the spatial distribution of faint Ly\u03b1 emitters. We also discuss the cross-correlation signal with 21 cm experiments that probe H I in the IGM during reionization. A dedicated sub-orbital or space-based Ly\u03b1 intensity mapping experiment could provide a viable complimentary approach to probe reionization, when compared to 21 cm experiments, and is likely within experimental reach.", "date": "2013-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "763", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 132", "id_number": "CaltechAUTHORS:20130222-154521694", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130222-154521694", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "SFRH/BD/51373/2011" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PTDC/ FIS/100170/2008" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NASA", "grant_number": "NNX10AD42G" } ] }, "doi": "10.1088/0004-637X/763/2/132", "primary_object": { "basename": "0004-637X_763_2_132.pdf", "url": "https://authors.library.caltech.edu/records/z6krb-2av20/files/0004-637X_763_2_132.pdf" }, "related_objects": [ { "basename": "1205.1493v2.pdf", "url": "https://authors.library.caltech.edu/records/z6krb-2av20/files/1205.1493v2.pdf" } ], "resource_type": "article", "pub_year": "2013", "author_list": "Silva, Marta B.; Santos, Mario G.; et el." }, { "id": "https://authors.library.caltech.edu/records/0j5xh-pz447", "eprint_id": 36777, "eprint_status": "archive", "datestamp": "2023-08-22 08:18:11", "lastmod": "2023-10-23 15:46:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lo-Faro-B", "name": { "family": "Lo Faro", "given": "B." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "The Complex Physics of Dusty Star-forming Galaxies at High Redshifts as Revealed by Herschel and Spitzer", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: general; galaxies: interactions; galaxies: starburst", "note": "\u00a9 2013 American Astronomical Society. Received 2012 July 20; accepted 2012 November 19; published 2012 December 20.\n\nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\n\nWe acknowledge support from ASI (Herschel Science Contract\nI/005/11/0). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM(France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA)\n\nPublished - 0004-637X_762_2_108.pdf
", "abstract": "We combine far-infrared photometry from Herschel (PEP/HerMES) with deep mid-infrared spectroscopy from Spitzer to investigate the nature and the mass assembly history of a sample of 31 luminous and ultraluminous infrared galaxies ((U)LIRGs) at z ~ 1 and 2 selected in GOODS-S with 24 \u03bcm fluxes between 0.2 and 0.5 mJy. We model the data with a self-consistent physical model (GRASIL) which includes a state-of-the-art treatment of dust extinction and reprocessing. We find that all of our galaxies appear to require massive populations of old (>1 Gyr) stars and, at the same time, to host a moderate ongoing activity of star formation (SFR \u2264 100 M_\u2609 yr^(\u20131)). The bulk of the stars appear to have been formed a few Gyr before the observation in essentially all cases. Only five galaxies of the sample require a recent starburst superimposed on a quiescent star formation history. We also find discrepancies between our results and those based on optical-only spectral energy distribution (SED) fitting for the same objects; by fitting their observed SEDs with our physical model we find higher extinctions (by \u0394A_V ~ 0.81 and 1.14) and higher stellar masses (by \u0394log(M_\u2605) ~ 0.16 and 0.36 dex) for z ~ 1 and z ~ 2 (U)LIRGs, respectively. The stellar mass difference is larger for the most dust-obscured objects. We also find lower SFRs than those computed from L IR using the Kennicutt relation due to the significant contribution to the dust heating by intermediate-age stellar populations through \"cirrus\" emission (~73% and ~66% of the total L IR for z ~ 1 and z ~ 2 (U)LIRGs, respectively).", "date": "2013-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "762", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 108", "id_number": "CaltechAUTHORS:20130205-104441854", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130205-104441854", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "ASI Herschel Science Contract", "grant_number": "I/005/11/0" }, { "agency": "BMVIT (Austria)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "CEA/CNES (France)" }, { "agency": "DLR (Germany)" }, { "agency": "ASI/INAF (Italy)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "CSA (Canada)" }, { "agency": "NAOC (China)" }, { "agency": "CEA (France)" }, { "agency": "CNES (France)" }, { "agency": "CNRS (France)" }, { "agency": "ASI (Italy)" }, { "agency": "MCINN (Spain)" }, { "agency": "SNSB (Sweden)" }, { "agency": "STFC (UK)" }, { "agency": "UKSA (UK)" }, { "agency": "NASA" } ] }, "doi": "10.1088/0004-637X/762/2/108", "primary_object": { "basename": "0004-637X_762_2_108.pdf", "url": "https://authors.library.caltech.edu/records/0j5xh-pz447/files/0004-637X_762_2_108.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Lo Faro, B. and Bock, J." }, { "id": "https://authors.library.caltech.edu/records/w0brf-s4j82", "eprint_id": 36770, "eprint_status": "archive", "datestamp": "2023-08-22 08:09:53", "lastmod": "2023-10-23 15:45:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "Julie L." }, "orcid": "0000-0003-2376-8971" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "J. M." }, "orcid": "0000-0003-2251-0602" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Yan-Lin", "name": { "family": "Yan", "given": "L." }, "orcid": "0000-0003-1710-9339" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: Candidate Gravitationally Lensed Galaxies and Lensing Statistics at Submillimeter Wavelengths", "ispublished": "pub", "full_text_status": "public", "keywords": "gravitational lensing: strong; submillimeter: galaxies", "note": "\u00a9 2013 American Astronomical Society. Received 2012 May 16; accepted 2012 November 9; published 2012 December 14. We thank Elisabetta Valiante for providing the redshift\ndistributions from her model and an anonymous referee for\nthoughtful feedback. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI\n(Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists, and a mission scientist. HerMES is described in Oliver et al. (2012). The data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES/). J.L.W., A.C., F.d.B., C.F., S.K., H.F., and J.C. acknowledge partial support from NSF CAREER AST-0645427 (to A.C. at UCI). S.J.O., L.W., and A.S. acknowledge support from the Science and Technology Facilities Council (grant No.ST/F002858/1 and grant No. ST/I000976/1) at U. of Sussex.\nA.F., G.M., L.M., and M.V. were supported by the Italian Space Agency (ASI \"Herschel Science\" Contract I/005/07/0). D.R. acknowledges support from NASA through a Spitzer Space\nTelescope grant. Support for program numbers GO-12194 and GO-12488 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and\nSpace Administration. The Observatory was made possible\nby the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute\nof Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation; the Kenneth T. and Eileen L. Norris Foundation; the James S. McDonnell Foundation; the Associates of the California Institute of Technology; the\nUniversity of Chicago; the states of California, Illinois, and Maryland; and the National Science Foundation. Ongoing\nCARMA development and operations are supported by the \nNational Science Foundation under a cooperative agreement\nand by the CARMA partner universities. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, in the island of La Palma. The GTC observations are part of the International Time Programme 2010\u20132011 (PI: PerezFournon).\nFacilities: Herschel (SPIRE),CARMA,GBT(Zpectrometer),\nVLA, Keck:II (NIRC2), Keck:I (LRIS), SMA,\nIRAM:Interferometer, IRAM:30m, HST (WFC3), Spitzer\n(IRAC, MIPS), GTC (OSIRIS).\n\nPublished - 0004-637X_762_1_59.pdf
", "abstract": "We present a list of 13 candidate gravitationally lensed submillimeter galaxies (SMGs) from 95 deg^2 of the Herschel Multi-tiered Extragalactic Survey, a surface density of 0.14 \u00b1 0.04 deg^(\u20132). The selected sources have 500 \u03bcm flux densities (S_(500)) greater than 100 mJy. Gravitational lensing is confirmed by follow-up observations in 9 of the 13 systems (70%), and the lensing status of the four remaining sources is undetermined. We also present a supplementary sample of 29 (0.31 \u00b1 0.06 deg^(\u20132)) gravitationally lensed SMG candidates with S_(500) = 80-100 mJy, which are expected to contain a higher fraction of interlopers than the primary candidates. The number counts of the candidate lensed galaxies are consistent with a simple statistical model of the lensing rate, which uses a foreground matter distribution, the intrinsic SMG number counts, and an assumed SMG redshift distribution. The model predicts that 32%-74% of our S_(500) \u2265 100 mJy candidates are strongly gravitationally lensed (\u03bc \u2265 2), with the brightest sources being the most robust; this is consistent with the observational data. Our statistical model also predicts that, on average, lensed galaxies with S_(500) = 100 mJy are magnified by factors of ~9, with apparently brighter galaxies having progressively higher average magnification, due to the shape of the intrinsic number counts. 65% of the sources are expected to have intrinsic 500 \u03bcm flux densities less than 30 mJy. Thus, samples of strongly gravitationally lensed SMGs, such as those presented here, probe below the nominal Herschel detection limit at 500 \u03bcm. They are good targets for the detailed study of the physical conditions in distant dusty, star-forming galaxies, due to the lensing magnification, which can lead to spatial resolutions of ~0.\"01 in the source plane.", "date": "2013-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "762", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 59", "id_number": "CaltechAUTHORS:20130205-093943506", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130205-093943506", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Academia Sinica" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/01" }, { "agency": "NASA", "grant_number": "GO-12194" }, { "agency": "NASA", "grant_number": "GO-12488" }, { "agency": "NASA", "grant_number": "NAS5-26555" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Smithsonian Institution" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Caltech Associates" }, { "agency": "University of Chicago" }, { "agency": "States of California, Illinois, and Maryland" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/762/1/59", "primary_object": { "basename": "0004-637X_762_1_59.pdf", "url": "https://authors.library.caltech.edu/records/w0brf-s4j82/files/0004-637X_762_1_59.pdf" }, "resource_type": "article", "pub_year": "2013", "author_list": "Wardlow, Julie L.; Cooray, Asantha; et el." }, { "id": "https://authors.library.caltech.edu/records/evcmr-gm882", "eprint_id": 36315, "eprint_status": "archive", "datestamp": "2023-08-22 07:57:38", "lastmod": "2023-10-20 23:00:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } } ] }, "title": "A Population of z > 2 Far-infrared Herschel-SPIRE-selected Starbursts", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society. Received 2012 July 20; accepted 2012 October 12; published 2012 December 4. C.M.C. is generously supported by a Hubble Fellowship from\nSpace Telescope Science Institute, grant HST-HF-51268.01-A.\nThe data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work would not be possible without the hard work and dedication of the Keck Observatory night and day staff; special thanks to Marc Kassis, Luca Rizzi, and Greg Wirth for help and advice\nwhile observing. The analysis pipeline used to reduce the\nDEIMOS data was developed at UC Berkeley with support from\nNSF grant AST-0071048. Spire has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI and Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, and Univ. Sussex (UK); and Caltech, JPL, NHSC, and Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\nThis research has made use of data from the HerMES project\n(http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the Spire instrument team, ESAC scientists, and a mission scientist. HerMES is described in Oliver et al. (2012). The Spire data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES).\n\nPublished - 0004-637X_761_2_139.pdf
", "abstract": "We present spectroscopic observations for a sample of 36 Herschel-SPIRE 250-500 \u03bcm selected galaxies (HSGs) at 2 < z < 5 from the Herschel Multi-tiered Extragalactic Survey. Redshifts are confirmed as part of a large redshift survey of Herschel-SPIRE-selected sources covering ~0.93 deg^2 in six extragalactic legacy fields. Observations were taken with the Keck I Low Resolution Imaging Spectrometer and the Keck II DEep Imaging Multi-Object Spectrograph. Precise astrometry, needed for spectroscopic follow-up, is determined by identification of counterparts at 24 \u03bcm or 1.4 GHz using a cross-identification likelihood matching method. Individual source luminosities range from log (L_(IR)/L_\u2609) = 12.5-13.6 (corresponding to star formation rates (SFRs) 500-9000 M_\u2609 yr^(\u20131), assuming a Salpeter initial mass function), constituting some of the most intrinsically luminous, distant infrared galaxies discovered thus far. We present both individual and composite rest-frame ultraviolet spectra and infrared spectral energy distributions. The selection of these HSGs is reproducible and well characterized across large areas of the sky in contrast to most z > 2 HyLIRGs in the literature, which are detected serendipitously or via tailored surveys searching only for high-z HyLIRGs; therefore, we can place lower limits on the contribution of HSGs to the cosmic star formation rate density (SFRD) at (7 \u00b1 2) \u00d7 10^(\u20133) M_\u2609 yr^(\u20131) h^3 Mpc^\u20133 at z ~ 2.5, which is >10% of the estimated total SFRD of the universe from optical surveys. The contribution at z ~ 4 has a lower limit of 3 \u00d7 10^(\u20133) M_\u2609 yr^(\u20131) h^3 Mpc^(\u20133), \u227320% of the estimated total SFRD. This highlights the importance of extremely infrared-luminous galaxies with high SFRs to the buildup of stellar mass, even at the earliest epochs.", "date": "2012-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "761", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 139", "id_number": "CaltechAUTHORS:20130111-093810807", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130111-093810807", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51268.01-A" }, { "agency": "W. M. Keck Foundation" }, { "agency": "NSF", "grant_number": "AST-0071048" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/761/2/139", "primary_object": { "basename": "0004-637X_761_2_139.pdf", "url": "https://authors.library.caltech.edu/records/evcmr-gm882/files/0004-637X_761_2_139.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Casey, C. M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/4xnkm-5f241", "eprint_id": 36334, "eprint_status": "archive", "datestamp": "2023-08-22 07:58:09", "lastmod": "2023-10-20 23:01:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Casey-C-M", "name": { "family": "Casey", "given": "C. M." }, "orcid": "0000-0002-0930-6466" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } } ] }, "title": "A Redshift Survey of Herschel Far-infrared Selected Starbursts and Implications for Obscured Star Formation", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society. Received 2012 July 26; accepted 2012 October 15; published 2012 December 4. We thank the anonymous reviewer for a very useful, constructive\nreport that improved the manuscript. C.M.C. is generously\nsupported by a Hubble Fellowship from Space Telescope Science Institute, grant HST-HF-51268.01-A. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge\nthe very significant cultural role and reverence that\nthe summit of Mauna Kea has always had within the indigenous\nHawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This work would not be possible without the hard work and dedication of the Keck Observatory night and day staff; special thanks to Marc Kassis, Luca Rizzi and Greg Wirth for help and advice while observing. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. Thanks to Nick Scoville and Brian Siana for useful discussions which improved the paper. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).\nThis research has made use of data from the HerMES project\n(http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. HerMES is described in Oliver et al. (2012). The SPIRE data presented in this paper will be released through the HerMES Database in Marseille, HeDaM (http://hedam.oamp.fr/HerMES).\n\nPublished - 0004-637X_761_2_140.pdf
", "abstract": "We present Keck spectroscopic observations and redshifts for a sample of 767 Herschel-SPIRE selected galaxies (HSGs) at 250, 350, and 500 \u03bcm, taken with the Keck I Low Resolution Imaging Spectrometer and the Keck II DEep Imaging Multi-Object Spectrograph. The redshift distribution of these SPIRE sources from the Herschel Multitiered Extragalactic Survey peaks at z = 0.85, with 731 sources at z < 2 and a tail of sources out to z ~ 5. We measure more significant disagreement between photometric and spectroscopic redshifts (\u3008\u0394z/(1 + z_(spec))\u3009 = 0.29) than is seen in non-infrared selected samples, likely due to enhanced star formation rates and dust obscuration in infrared-selected galaxies. The infrared data are used to directly measure integrated infrared luminosities and dust temperatures independent of radio or 24 \u03bcm flux densities. By probing the dust spectral energy distribution (SED) at its peak, we estimate that the vast majority (72%-83%) of z < 2 Herschel-selected galaxies would drop out of traditional submillimeter surveys at 0.85-1 mm. We find that dust temperature traces infrared luminosity, due in part to the SPIRE wavelength selection biases, and partially from physical effects. As a result, we measure no significant trend in SPIRE color with redshift; if dust temperature were independent of luminosity or redshift, a trend in SPIRE color would be expected. Composite infrared SEDs are constructed as a function of infrared luminosity, showing the increase in dust temperature with luminosity, and subtle change in near-infrared and mid-infrared spectral properties. Moderate evolution in the far-infrared (FIR)/radio correlation is measured for this partially radio-selected sample, with q_(IR) \u221d(1 + z)^(\u20130.30\u00b10.02) at z < 2. We estimate the luminosity function and implied star formation rate density contribution of HSGs at z < 1.6 and find overall agreement with work based on 24 \u03bcm extrapolations of the LIRG, ULIRG, and total infrared contributions. This work significantly increased the number of spectroscopically confirmed infrared-luminous galaxies at z \u00bb 0 and demonstrates the growing importance of dusty starbursts for galaxy evolution studies and the build-up of stellar mass throughout cosmic time.", "date": "2012-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "761", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 140", "id_number": "CaltechAUTHORS:20130111-152856336", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130111-152856336", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51268.01-A" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/761/2/140", "primary_object": { "basename": "0004-637X_761_2_140.pdf", "url": "https://authors.library.caltech.edu/records/4xnkm-5f241/files/0004-637X_761_2_140.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Casey, C. M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/eesqf-24v95", "eprint_id": 36256, "eprint_status": "archive", "datestamp": "2023-08-22 07:55:46", "lastmod": "2023-10-20 22:56:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mroczkowski-Anthony-K", "name": { "family": "Mroczkowski", "given": "Tony" }, "orcid": "0000-0003-3816-5372" }, { "id": "Dicker-Simon-R", "name": { "family": "Dicker", "given": "Simon" }, "orcid": "0000-0002-1940-4289" }, { "id": "Sayers-Jack", "name": { "family": "Sayers", "given": "Jack" }, "orcid": "0000-0002-8213-3784" }, { "id": "Reese-Erik-D", "name": { "family": "Reese", "given": "Erik D." }, "orcid": "0000-0002-8700-7082" }, { "id": "Mason-Brian-S", "name": { "family": "Mason", "given": "Brian" } }, { "id": "Czakon-Nicole-G", "name": { "family": "Czakon", "given": "Nicole" } }, { "id": "Romero-Charles-E", "name": { "family": "Romero", "given": "Charles" } }, { "id": "Young-A-H", "name": { "family": "Young", "given": "Alexander" }, "orcid": "0000-0003-2291-6952" }, { "id": "Devlin-Mark-J", "name": { "family": "Devlin", "given": "Mark" }, "orcid": "0000-0002-3169-9761" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "Sunil" }, "orcid": "0000-0002-1098-7174" }, { "id": "Korngut-Phillip-M", "name": { "family": "Korngut", "given": "Phillip" } }, { "id": "Sarazin-Craig", "name": { "family": "Sarazin", "given": "Craig" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Koch-Patrick-M", "name": { "family": "Koch", "given": "Patrick M." }, "orcid": "0000-0003-2777-5861" }, { "id": "Lin-Kai-Yang", "name": { "family": "Lin", "given": "Kai-Yang" }, "orcid": "0000-0002-8698-7277" }, { "id": "Molnar-Sandor-M", "name": { "family": "Molnar", "given": "Sandor M." }, "orcid": "0000-0002-4227-956X" }, { "id": "Pierpaoli-Elena", "name": { "family": "Pierpaoli", "given": "Elena" }, "orcid": "0000-0002-7957-8993" }, { "id": "Umetsu-Keiichi", "name": { "family": "Umetsu", "given": "Keiichi" }, "orcid": "0000-0002-7196-4822" }, { "id": "Zemcov-Michael", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "A Multi-wavelength Study of the Sunyaev-Zel'dovich Effect in the Triple-merger Cluster MACS J0717.5+3745 with MUSTANG and Bolocam", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; X-rays: galaxies: clusters; X-rays: general", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2012 April 27; accepted 2012 October 23; published 2012 November 20. \n\nWe thank Maxim Markevitch, Simona Giacintucci, Cheng-Jiun Ma, and Dan Coe for useful discussions and input. We also thank Reinout van Weeren, Adi Zitrin, Annalisa Bonafede, and Marceau Limousin for providing radio and lensing maps and for their input, which aided tremendously in the\ninterpretation of the cluster astrophysics. We thank Marie Rex, Eiichi Egami, and Tim Rawle for their support in obtaining the 268 GHz Bolocam observations. The late-night assistance of the GBT operators was much appreciated during the observations, as was the overall support from all those at the GBT. We also thank Ashley Reichardt for her help in performing the MUSTANG observations. We are grateful for CSO administrative support from Kathy Deniston, Barbara Wertz, and Diana Bisel, and for Bolocam instrument maintenance and support from the CSO day crew. We also thank the many folks who helped in obtaining the CARMA/SZA observations presented here, particularly Tom Culverhouse, Nikolaus Volgenau, John Carpenter, and the many students and postdocs who regularly help run the array. We are especially grateful to Stephen Muchovej and Erik Leitch for their work on the pipeline that allows data from the CARMA/SZA subarray to be easily calibrated against Mars.\nMuch of the work presented here was supported by National\nScience Foundation (NSF) grant AST-1007905. Support for T.M. was provided by NASA through the Einstein Fellowship\nProgram, grant PF0-110077. Support for A.Y. was provided\nby the National Radio Astronomy Observatory (NRAO) graduate student support program. Support for P.K. was provided\nby the NASA Postdoctoral Program (NPP). J.S. was supported by NSF/AST-0838261 and NASA/NNX11AB07G. N.C. was partially supported by a NASA Graduate Student Research Fellowship. K.U. acknowledges support from the Academia Sinica Career Development Award and the National Science Council of Taiwan under grant NSC100-2112-M-001-008-MY3. The NRAO is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. The MUSTANG observations presented here were obtained with time on the GBT allocated under NRAO proposal IDs AGBT10A056 and AGBT11B001. The Bolocam data were acquired through observations at the CSO, which is operated by the California Institute of Technology under cooperative agreement with the NSF (AST-0838261). A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We also thank Nina the dog for always standing by patiently and never questioning the value of this work.\n\nPublished - 0004-637X_761_1_47.pdf
", "abstract": "We present 90, 140, and 268 GHz subarcminute resolution imaging of the Sunyaev-Zel'dovich effect (SZE) in the disturbed, intermediate-redshift (z = 0.5458) galaxy cluster MACS J0717.5+3745, a triple-merger system comprising four distinct, optically detected subclusters. Our 90 GHz SZE data result in a sensitive, 34 \u03bcJy beam^(\u20131) map of the SZE at 13\" effective resolution using the MUSTANG bolometer array on the Green Bank Telescope (GBT). Our 140 and 268 GHz SZE imaging, with resolutions of 58\" and 31\" and sensitivities of 1.8 and 3.3 mJy beam^(\u20131), respectively, was obtained through observations from the Caltech Submillimeter Observatory using Bolocam. We compare these maps to a two-dimensional pressure map derived from Chandra X-ray observations. Our MUSTANG SZE data confirm previous indications from Chandra of a pressure enhancement due to shock-heated, \u2273 20 keV gas immediately adjacent to extended radio emission seen in low-frequency radio maps of this cluster. MUSTANG also detects pressure substructure that is not well constrained by the Chandra X-ray data in the remnant core of a merging subcluster. We find that the small-scale pressure enhancements in the MUSTANG data amount to ~2% of the total pressure measured in the 140 GHz Bolocam observations. The X-ray inferred pseudo-pressure template also fails on larger scales to accurately describe the Bolocam data, particularly at the location of the subcluster with a remnant core known to have a high line-of-sight optical velocity of ~3200 km s^(\u20131). Our Bolocam data are adequately described when we add an additional component\u2014not described by a thermal SZE spectrum\u2014to the X-ray template coincident with this subcluster. Using flux densities extracted from our model fits, and marginalizing over the X-ray spectroscopic temperature constraints for the region, we fit a thermal + kinetic SZE spectrum to our Bolocam data and find that the subcluster has a best-fit line-of-sight proper velocity vz = 3600^(+3440)_(\u20132160) km s^(\u20131), in agreement with the optical velocity estimates for the subcluster. The probability v_z \u2264 0 given our measurements is 2.1%. Repeating this analysis using flux densities measured directly from our maps results in a 3.4% probability v_z \u2264 0. We note that this tantalizing result for the kinetic SZE is on resolved, subcluster scales.", "date": "2012-12-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "761", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 47", "id_number": "CaltechAUTHORS:20130109-075048169", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130109-075048169", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-1007905" }, { "agency": "NASA Einstein Fellowship", "grant_number": "PF0-110077" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "NASA", "grant_number": "NNX11AB07G" }, { "agency": "NASA Graduate Student Research Fellowship" }, { "agency": "Academia Sinica" }, { "agency": "National Science Council (Taipei)", "grant_number": "NSC100-2112-M-001-008-MY3" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/761/1/47", "primary_object": { "basename": "0004-637X_761_1_47.pdf", "url": "https://authors.library.caltech.edu/records/eesqf-24v95/files/0004-637X_761_1_47.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Mroczkowski, Tony; Dicker, Simon; et el." }, { "id": "https://authors.library.caltech.edu/records/a49bh-jb229", "eprint_id": 36032, "eprint_status": "archive", "datestamp": "2023-08-19 13:32:26", "lastmod": "2023-10-20 22:09:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Aussel-Herve", "name": { "family": "Aussel", "given": "H." }, "orcid": "0000-0002-1371-5705" }, { "id": "Berta-S", "name": { "family": "Berta", "given": "S." }, "orcid": "0000-0002-0320-1532" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C." } }, { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "D." }, "orcid": "0000-0002-7631-647X" }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Le-Floc'h-Emeric", "name": { "family": "Le Floc'h", "given": "E." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Lutz-Dieter", "name": { "family": "Lutz", "given": "D." }, "orcid": "0000-0003-0291-9582" }, { "id": "Magnelli-B", "name": { "family": "Magnelli", "given": "B." }, "orcid": "0000-0002-6777-6490" }, { "id": "Marsden-G", "name": { "family": "Marsden", "given": "G." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Pozzi-F", "name": { "family": "Pozzi", "given": "F." } }, { "id": "Riguccini-L", "name": { "family": "Riguccini", "given": "L." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Cosmic Evolution of Star Formation Enhancement in Close Major-merger Galaxy Pairs Since z = 1", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2012 American Astronomical Society. Received 2012 June 15; accepted 2012 October 3; published 2012 November 6. \nHerschel is an ESA space observatory with science instruments provided by\nEuropean-led Principal Investigator consortia and with important participation\nfrom NASA.\nDr. Xianzhong Zheng is thanked for kindly providing the\nsoftware and instructions for the \"clean stacking.\"We acknowledge support from the Science and Technology Facilities Council (grant No. ST/I000976/1). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France),\nDLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes\nled by Cardiff University (UK) and including: the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, the University of Sussex (UK); and Caltech, JPL, NHSC, the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM, http://hedam.oamp.fr/HerMES).\n\nPublished - 0004-637X_760_1_72.pdf
", "abstract": "The infrared (IR) emission of \"M_* galaxies\" (10^(10.4) \u2264 M_(star) \u2264 10^(11.0) M_\u2609) in galaxy pairs, derived using data obtained in Herschel (PEP/HerMES) and Spitzer (S-COSMOS) surveys, is compared to that of single-disk galaxies in well-matched control samples to study the cosmic evolution of the star formation enhancement induced by galaxy-galaxy interaction. Both the mean IR spectral energy distribution and mean IR luminosity of star-forming galaxies (SFGs) in SFG+SFG (S+S) pairs in the redshift bin of 0.6 < z < 1 are consistent with no star formation enhancement. SFGs in S+S pairs in a lower redshift bin of 0.2 < z < 0.6 show marginal evidence for a weak star formation enhancement. Together with the significant and strong sSFR enhancement shown by SFGs in a local sample of S+S pairs (obtained using previously published Spitzer observations), our results reveal a trend for the star formation enhancement in S+S pairs to decrease with increasing redshift. Between z = 0 and z = 1, this decline of interaction-induced star formation enhancement occurs in parallel with the dramatic increase (by a factor of ~10) of the sSFR of single SFGs, both of which can be explained by the higher gas fraction in higher-z disks. SFGs in mixed pairs (S+E pairs) do not show any significant star formation enhancement at any redshift. The difference between SFGs in S+S pairs and in S+E pairs suggests a modulation of the sSFR by the intergalactic medium (IGM) in the dark matter halos hosting these pairs.", "date": "2012-11-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "760", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 72", "id_number": "CaltechAUTHORS:20121218-105629072", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121218-105629072", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "ESA-PRODEX (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "CICYT/MCYT (Spain)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/760/1/72", "primary_object": { "basename": "0004-637X_760_1_72.pdf", "url": "https://authors.library.caltech.edu/records/a49bh-jb229/files/0004-637X_760_1_72.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Xu, C. K.; Shupe, D. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/xzmh9-cxx67", "eprint_id": 35722, "eprint_status": "archive", "datestamp": "2023-08-22 07:41:24", "lastmod": "2023-10-20 20:31:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "FMOS near-IR spectroscopy of Herschel-selected galaxies: star formation rates, metallicity and dust attenuation at z \u223c 1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; submillimetre: galaxies", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS. \n\nAccepted 2012 July 23. Received 2012 July 23; in original form 2012 January 26. Article first published online: 8 Oct. 2012. \n\nWe thank the anonymous referee for suggestions which greatly enhanced this work. IGR, SJO and LW acknowledge support from the Science and Technology Facilities Council (grant Nos ST/F002858/1 and ST/I000976/1). JSD acknowledges the support of the Royal Society via aWolfson Research Merit award and the support of the European Research Council via the award of an Advanced Grant. Based on zCOSMOS observations carried out using the Very Large Telescope at the ESO Paranal Observatory under Programme ID: LP175.A-0839. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, theMax Planck Society and theHigher Education Funding Council for England. The SDSS website is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UK ATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC and UKSA (UK); and NASA (USA). FMOS was funded jointly by STFC and the Japanese Monbukagakusho, and we gratefully acknowledge the support of the staff at the Subaru Telescope throughout the instrument commissioning phase. The data presented in this paper will be released through the Herschel Database inMarseille HeDaM (hedam.oamp.fr/HerMES).\n\nPublished - mnr21777.pdf
Accepted Version - 1207.5564.pdf
", "abstract": "We investigate the properties (e.g. star formation rate, dust attenuation, stellar mass and metallicity) of a sample of infrared (IR) luminous galaxies at z \u223c 1 via near-IR spectroscopy with Subaru-FMOS. Our sample consists of Herschel SPIRE and Spitzer MIPS selected sources in the COSMOS field with photometric redshifts in the range of 0.7 < z_phot < 1.8, which have been targeted in two pointings (0.5\u2009deg^2) with FMOS. We find a modest success rate for emission-line detections, with candidate H\u03b1 emission lines detected for 57 of 168 SPIRE sources (34\u2009per cent). By stacking the near-IR spectra we directly measure the mean Balmer decrement for the H\u03b1 and H\u03b2 lines, finding a value of \u3008E(B \u2212 V)\u3009 = 0.51 \u00b1 0.27 for \u3008LIR\u3009 = 10^12 \u2009L_\u2299 sources at \u3008z\u3009 = 1.36. By comparing star formation rates estimated from the IR and from the dust-uncorrected H\u03b1 line we find a strong relationship between dust attenuation and star formation rate. This relation is broadly consistent with that previously seen in star-forming galaxies at z \u223c 0.1. Finally, we investigate the metallicity via the N2 ratio, finding that z \u223c 1 IR-selected sources are indistinguishable from the local mass\u2013metallicity relation. We also find a strong correlation between dust attenuation and metallicity, with the most metal-rich IR sources experiencing the largest levels of dust attenuation.", "date": "2012-11-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "426", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1782-1792", "id_number": "CaltechAUTHORS:20121129-084742065", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121129-084742065", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "European Research Council (ERC)" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "NASA" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "Higher Education Funding Council for England" }, { "agency": "Royal Society" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2012.21777.x", "primary_object": { "basename": "1207.5564.pdf", "url": "https://authors.library.caltech.edu/records/xzmh9-cxx67/files/1207.5564.pdf" }, "related_objects": [ { "basename": "mnr21777.pdf", "url": "https://authors.library.caltech.edu/records/xzmh9-cxx67/files/mnr21777.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Roseboom, I. G.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/pz576-cjq62", "eprint_id": 35247, "eprint_status": "archive", "datestamp": "2023-08-22 07:06:47", "lastmod": "2023-10-20 15:53:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lupu-R-E", "name": { "family": "Lupu", "given": "R. E." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "J." }, "orcid": "0000-0001-5703-2108" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Measurements of CO Redshifts with Z-Spec for Lensed Submillimeter Galaxies Discovered in the H-ATLAS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: distances and redshifts; galaxies: high-redshift; galaxies: ISM- line: identification; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2010 September 29; accepted 2012 August 13; published 2012 September 12.\n\nWe are indebted to the staff of the Caltech Submillimeter Observatory for their unflagging support. This work was supported by NSF grant AST-0807990 to J. Aguirre and by the CSO NSF Cooperative Agreement AST-0838261. Support was provided to J. Kamenetzky by an NSF Graduate Research Fellowship. Z-spec was constructed under NASA SARA grants NAGS-11911 and NAGS-12788 and an NSF Career grant (AST-0239270) and a Research Corporation Award (RI0928) to J.\nGlenn, in collaboration with the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We acknowledge Peter Ade and his group for their filters and Lionel Duband for the 3He/4He refrigerator in Z-Spec, and are grateful for their help in the early integration of the instrument. R.L. thanks Tom Loredo for useful discussions regarding the significance of the redshift determination, and P. Papadopoulos for help improving the gas mass discussion. R.L. also thanks the anonymous referee for the thorough read and the helpful comments for improving\nthe paper. We appreciate the help of Robert Hanni and\nJon Rodriguez with observing.\n\nPublished - 0004-637X_757_2_135.pdf
", "abstract": "We present new observations from Z-Spec, a broadband 185-305 GHz spectrometer, of five submillimeter bright lensed sources selected from the Herschel-Astrophysical Terahertz Large Area Survey science demonstration phase catalog. We construct a redshift-finding algorithm using combinations of the signal to noise of all the lines falling in the Z-Spec bandpass to determine redshifts with high confidence, even in cases where the signal to noise in individual lines is low. We measure the dust continuum in all sources and secure CO redshifts for four out of five (z ~ 1.5-3). In one source, SDP.17, we tentatively identify two independent redshifts and a water line, confirmed at z = 2.308. Our sources have properties characteristic of dusty starburst galaxies, with magnification-corrected star formation rates of 10^(2\u20133) M_\u2609 yr^(\u20131). Lower limits for the dust masses (~a few 10^8 M_\u2609) and spatial extents (~1 kpc equivalent radius) are derived from the continuum spectral energy distributions, corresponding to dust temperatures between 54 and 69 K. In the local thermodynamic equilibrium (LTE) approximation, we derive relatively low CO excitation temperatures (\u2272100 K) and optical depths (\u03c4 \u2272 1). Performing a non-LTE excitation analysis using RADEX, we find that the CO lines measured by Z-Spec (from J = 4 \u2192 3 to 10 \u2192 9, depending on the galaxy) localize the best solutions to either a high-temperature/low-density region or a low/temperature/high-density region near the LTE solution, with the optical depth varying accordingly. Observations of additional CO lines, CO(1-0) in particular, are needed to constrain the non-LTE models.", "date": "2012-10-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "757", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 135", "id_number": "CaltechAUTHORS:20121101-142033089", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121101-142033089", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0807990" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA", "grant_number": "NAGS-11911" }, { "agency": "NASA", "grant_number": "NAGS-12788" }, { "agency": "NSF", "grant_number": "AST-0239270" }, { "agency": "Research Corporation", "grant_number": "RI0928" } ] }, "doi": "10.1088/0004-637X/757/2/135", "primary_object": { "basename": "0004-637X_757_2_135.pdf", "url": "https://authors.library.caltech.edu/records/pz576-cjq62/files/0004-637X_757_2_135.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Lupu, R. E.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/09spc-e4j07", "eprint_id": 34760, "eprint_status": "archive", "datestamp": "2023-08-22 06:48:53", "lastmod": "2023-10-19 21:26:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hilton-M", "name": { "family": "Hilton", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Herschel observations of a z \u223c 2 stellar mass selected galaxy sample drawn from the GOODS NICMOS Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: starburst; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS. \n\nAccepted 2012 June 11. Received 2012 June 8; in original form 2012 January 26. Article first published online: 27 Jul. 2012. \n\nWe thank the referee for many helpful comments which have improved this paper. We thank Amanda Bauer for providing the UV-based SFR measurements of GNS galaxies and useful discussions. MH and CJC acknowledge financial support from the Leverhulme Trust and STFC. Support for the GNS was also provided by NASA/STScI grant HST-GO11082. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy) and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain).\n\nPublished - mnr21499.pdf
Accepted Version - 1206.2319.pdf
", "abstract": "We present a study of the far-infrared (IR) properties of a stellar mass selected sample of 1.5 < z < 3 galaxies with log\u2009(M_*/M_\u2299) > 9.5 drawn from the Great Observatories Origins Deep Survey (GOODS) Near Infrared Camera and Multi-Object Spectrometer (NICMOS) Survey (GNS), the deepest H-band Hubble Space Telescope survey of its type prior to the installation of Wide Field Camera 3 (WFC3). We use far-IR and submm data from the Photoconductor Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) instruments on-board Herschel, taken from the PACS Evolutionary Probe (PEP) and Herschel Multi-Tiered Extragalactic Survey (HerMES) key projects, respectively. We find a total of 22 GNS galaxies, with median log\u2009(M_*/M_\u2299) = 10.8 and z = 2.0, associated with 250\u2009\u03bcm sources detected with signal-to-noise ratio (SNR) > 3. We derive mean total IR luminosity log\u2009LIR(L_\u2299) = 12.36 \u00b1 0.05 and corresponding star formation rate (SFR)_(IR + UV) = (280 \u00b1 40)\u2009M_\u2299\u2009yr^(\u22121) for these objects, and find them to have mean dust temperature T_dust \u2248 35\u2009K. We find that the SFR derived from the far-IR photometry combined with ultraviolet (UV)-based estimates of unobscured SFR for these galaxies is on average more than a factor of 2 higher than the SFR derived from extinction-corrected UV emission alone, although we note that the IR-based estimate is subject to substantial Malmquist bias. To mitigate the effect of this bias and extend our study to fainter fluxes, we perform a stacking analysis to measure the mean SFR in bins of stellar mass. We obtain detections at the 2\u20134\u03c3 level at SPIRE wavelengths for samples with log\u2009(M_*/M_\u2299) > 10. In contrast to the Herschel detected GNS galaxies, we find that estimates of SFR_(IR + UV) for the stacked samples are comparable to those derived from extinction-corrected UV emission, although the uncertainties are large. We find evidence for an increasing fraction of dust obscured star formation with stellar mass, finding SFR_(IR)/SFR_(UV) \u221d M^(0.7\u00b10.2)_*, which is likely a consequence of the mass\u2013metallicity relation.", "date": "2012-09-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "425", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "540-555", "id_number": "CaltechAUTHORS:20121008-143240324", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121008-143240324", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Leverhulme Trust" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA", "grant_number": "HST-GO11082" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2012.21499.x", "primary_object": { "basename": "mnr21499.pdf", "url": "https://authors.library.caltech.edu/records/09spc-e4j07/files/mnr21499.pdf" }, "related_objects": [ { "basename": "1206.2319.pdf", "url": "https://authors.library.caltech.edu/records/09spc-e4j07/files/1206.2319.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Hilton, M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/vdjgt-62z57", "eprint_id": 34499, "eprint_status": "archive", "datestamp": "2023-09-14 19:34:10", "lastmod": "2023-10-23 20:53:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N. Y." }, "orcid": "0000-0002-8948-1044" }, { "id": "Marshall-J", "name": { "family": "Marshall", "given": "J." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Herschel Multi-tiered Extragalactic Survey: HerMES", "ispublished": "pub", "full_text_status": "public", "keywords": "surveys; galaxies: evolution; infrared: galaxies; submillimetre: galaxies", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS.\n\nAccepted 2012 March 12. Received 2012 January 5; in original form 2011 July 20.\nArticle first published online: 6 Jul. 2012.\nWe acknowledge support from the UK Science and Technology\nFacilities Council, grant numbers ST/F002858/1 and ST/I000976/1. HCSS/HSPOT/HIPE are joint developments by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center and the HIFI, PACS and SPIRE consortia. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK) and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS\n(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC,\nUKSA (UK) and NASA (USA).\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nPublished - mnr20912.pdf
Accepted Version - 1203.2562.pdf
", "abstract": "The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling \u223c380\u2009deg^2. Fields range in size from 0.01 to \u223c20\u2009deg^2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500\u2009\u03bcm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160\u2009\u03bcm), with an additional wider component of 270\u2009deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. \n\nThe survey will detect of the order of 100\u2009000 galaxies at 5\u03c3 in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. \n\nThis paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.", "date": "2012-08-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "424", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1614-1635", "id_number": "CaltechAUTHORS:20120927-094554573", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120927-094554573", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Herschel Science Ground Segment Consortium" }, { "agency": "NASA Herschel Science Center" }, { "agency": "HIFI" }, { "agency": "PACS" }, { "agency": "SPIRE" }, { "agency": "European Space Agency (ESA)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2012.20912.x", "primary_object": { "basename": "1203.2562.pdf", "url": "https://authors.library.caltech.edu/records/vdjgt-62z57/files/1203.2562.pdf" }, "related_objects": [ { "basename": "mnr20912.pdf", "url": "https://authors.library.caltech.edu/records/vdjgt-62z57/files/mnr20912.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Oliver, S. J.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/js41s-kzx28", "eprint_id": 32677, "eprint_status": "archive", "datestamp": "2023-08-22 06:10:11", "lastmod": "2023-10-18 15:58:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dai-Y-Sophia", "name": { "family": "Dai", "given": "Y. Sophia" }, "orcid": "0000-0002-7928-416X" }, { "id": "Bergeron-J", "name": { "family": "Bergeron", "given": "Jacqueline" }, "orcid": "0000-0002-1201-873X" }, { "id": "Elvis-M", "name": { "family": "Elvis", "given": "Martin" } }, { "id": "Omont-A", "name": { "family": "Omont", "given": "Alain" }, "orcid": "0000-0002-4721-3922" }, { "id": "Huang-Jia-Sheng", "name": { "family": "Huang", "given": "Jia-Sheng" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "Jamie" }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "Giovanni" }, "orcid": "0000-0002-0670-0708" }, { "id": "Hatziminaoglou-E", "name": { "family": "Hatziminaoglou", "given": "Evanthia" } }, { "id": "Ibar-E", "name": { "family": "Ibar", "given": "Edo" } }, { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "Georgios E." }, "orcid": "0000-0002-4872-2294" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "Seb J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "Mathew J." }, "orcid": "0000-0002-6689-6271" }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "Ismael" } }, { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "Dimitra" }, "orcid": "0000-0001-6854-7545" }, { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "Myrto" } }, { "id": "Trichas-M", "name": { "family": "Trichas", "given": "Markos" } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "Joaquin D." } }, { "id": "Willmer-C-N-A", "name": { "family": "Willmer", "given": "Christopher N. A." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "A Population of Dust-rich Quasars at z ~ 1.5", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: nuclei; galaxies: starburst; infrared: galaxies; quasars: general", "note": "\u00a9 2012 The American Astronomical Society. \n\nReceived 2011 August 11; accepted 2012 April 27; published 2012 June 12. \n\nThis research has made use of data from the HerMES\nproject\u2014a Herschel Key Program utilizing Guaranteed Time\nfrom the SPIRE instrument team, ESAC scientists and a\nmission scientist. SPIRE has been developed by a consortium\nof institutes led by Cardiff University (UK) and including\nthe University of Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, the University of Padua (Italy);\nIAC (Spain); Stockholm Observatory (Sweden); Imperial\nCollege London, RAL, UCL-MSSL, UKATC, the University\nof Sussex (UK); Caltech, JPL, NHSC, the University of\nColorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA,\nCNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB\n(Sweden); STFC and UKSA (UK); and NASA (USA). The\nHerMES data were accessed through the HeDaM database\n(http://hedam.oamp.fr) operated by CeSAM and hosted by\nthe Laboratoire d'Astrophysique de Marseille. We acknowledge\nsupport from the Science and Technology Facilities\nCouncil (grant numbers ST/F002858/1 and ST/I000976/1).\nThis work is based partly on observations made with the Spitzer Space Telescope and the MMT Observatory, operated by the Jet Propulsion Laboratory, Caltech under a contract with NASA, the Smithsonian Astrophysical Observatory and the University of Arizona, respectively. Research by Y. S. D. is supported by the SAO Predoctoral Fellowship. \n\nFacilities: Herschel, MMT, Spitzer\n\nPublished - Dai2012p18933Astrophys_J.pdf
", "abstract": "We report Herschel SPIRE (250, 350, and 500 \u03bcm) detections of 32 quasars with redshifts 0.5 \u2264z < 3.6 from the Herschel Multi-tiered Extragalactic Survey (HerMES). These sources are from a MIPS 24 \u03bcm flux-limited sample of 326 quasars in the Lockman Hole Field. The extensive multi-wavelength data available in the field permit construction of the rest-frame spectral energy distributions (SEDs) from ultraviolet to the mid-infrared for all sources, and to the far-infrared (FIR) for the 32 objects. Most quasars with Herschel FIR detections show dust temperatures in the range of 25-60 K, with a mean of 34 K. The FIR luminosities range from 10^(11.3) to 10^(13.5) L_\u2609, qualifying most of their hosts as ultra- or hyper-luminous infrared galaxies. These FIR-detected quasars may represent a dust-rich population, but with lower redshifts and fainter luminosities than quasars observed at ~1 mm. However, their FIR properties cannot be predicted from shorter wavelengths (0.3-20 \u03bcm, rest frame), and the bolometric luminosities derived using the 5100 \u00c5 index may be underestimated for these FIR-detected quasars. Regardless of redshift, we observed a decline in the relative strength of FIR luminosities for quasars with higher near-infrared luminosities.", "date": "2012-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "753", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 33", "id_number": "CaltechAUTHORS:20120724-121521512", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120724-121521512", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Smithsonian Astrophysical Observatory" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/753/1/33", "primary_object": { "basename": "Dai2012p18933Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/js41s-kzx28/files/Dai2012p18933Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Dai, Y. Sophia; Bergeron, Jacqueline; et el." }, { "id": "https://authors.library.caltech.edu/records/my5dk-p7s22", "eprint_id": 32605, "eprint_status": "archive", "datestamp": "2023-08-22 06:09:21", "lastmod": "2023-10-18 14:35:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mitchell-Wynne-K", "name": { "family": "Mitchell-Wynne", "given": "K." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Gong-Y", "name": { "family": "Gong", "given": "Y." } }, { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Franceschini-A", "name": { "family": "Franceschini", "given": "A." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "M." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Marchetti-L", "name": { "family": "Marchetti", "given": "L." }, "orcid": "0000-0003-3948-7621" }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "I." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Smidt-J", "name": { "family": "Smidt", "given": "J." } }, { "id": "Smith-A", "name": { "family": "Smith", "given": "A." }, "orcid": "0000-0002-1938-4660" }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Vigroux-L", "name": { "family": "Vigroux", "given": "L." } }, { "id": "Wang-Lingyu", "name": { "family": "Wang", "given": "L." } }, { "id": "Wardlow-J-L", "name": { "family": "Wardlow", "given": "J. L." }, "orcid": "0000-0003-2376-8971" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: A Statistical Measurement of the Redshift Distribution of Herschel-SPIRE Sources Using the Cross-correlation Technique", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2012 February 29; accepted 2012 April 24; published 2012 June 11.\n\nSPIRE has been developed by a consortium of institutes led\nby Cardiff University (UK) and including: the University of\nLethbridge (Canada); NAOC (China); CEA, LAM (France);\nIFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, the University of Sussex (UK); and Caltech, JPL, NHSC, the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). The data presented in this paper will be released through the HeDaM Database in Marseille. This work made use of images and/or data products provided by the NOAO Deep Wide-Field Survey, which is supported by the National Optical Astronomy Observatory (NOAO). NOAO is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSSWeb\nsite is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, the Astrophysical Institute Potsdam, the University of Basel, the University of Cambridge, Case Western Reserve University, the University of Chicago, Drexel University, Fermilab,\nthe Institute for Advanced Study, the Japan Participation\nGroup, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, The Ohio State University, the University of Pittsburgh, the University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. K.M.W., Y.G., A.C., J.S., and J.L.W. are supported by NASA funds for U.S. participants in Herschel through an award from JPL. A.C. and Y.G. also acknowledge support from NSF CAREER AST-0645427 (to A.C.) and K.M.W. acknowledges support from a NSF REU supplement. S.O., A.S., and L.W. acknowledge support from the Science and Technology Facilities Council (grant No. ST/F002858/1) and (grant No. ST/I000976/1). A.F., L.M., and M.V. were supported by the Italian Space Agency (ASI Herschel Science Contract I/005/07/0).\n\nPublished - MitchellWynne2012p18928Astrophys_J.pdf
", "abstract": "The wide-area imaging surveys with the Herschel Space Observatory at submillimeter (sub-mm) wavelengths have now resulted in catalogs of the order of one-hundred-thousand dusty, starburst galaxies. These galaxies capture an important phase of galaxy formation and evolution, but, unfortunately, the redshift distribution of these galaxies, N(z), is still mostly uncertain due to limitations associated with counterpart identification at optical wavelengths and spectroscopic follow-up. We make a statistical estimate of N(z) using a clustering analysis of sub-mm galaxies detected at each of 250, 350 and 500 \u03bcm from the Herschel Multi-tiered Extragalactic Survey centered on the Bo\u00f6tes field. We cross-correlate Herschel galaxies against galaxy samples at optical and near-IR wavelengths from the Sloan Digital Sky Survey, the NOAO Deep Wide Field Survey, and the Spitzer Deep Wide Field Survey. We create optical and near-IR galaxy samples based on their photometric or spectroscopic redshift distributions and test the accuracy of those redshift distributions with similar galaxy samples defined with catalogs from the Cosmological Evolution Survey (COSMOS), which has superior spectroscopic coverage. We model the clustering auto- and cross-correlations of Herschel and optical/IR galaxy samples to estimate N(z) and clustering bias factors. The S_(350) > 20 mJy galaxies have a bias factor varying with redshift as b(z) = 1.0^(+1.0)_(\u20130.5)(1 + z)^1.2^(+0.3)_(\u20130.7). This bias and the redshift dependence is broadly in agreement with galaxies that occupy dark matter halos of mass in the range of 1012 to 10^(13) M_\u2609. We find that galaxy selections in all three Spectral and Photometric Imaging Receiver (SPIRE) bands share a similar average redshift, with = 1.8 \u00b1 0.2 for 250 \u03bcm selected samples, and = 1.9 \u00b1 0.2 for both 350 and 500 \u03bcm samples, while their distributions behave differently. For 250 \u03bcm selected galaxies we find the a larger number of sources with z \u2264 1 when compared with the subsequent two SPIRE bands, with 350 and 500 \u03bcm selected SPIRE samples having peaks in N(z) at progressively higher redshifts. We compare our clustering-based N(z) results to sub-mm galaxy model predictions in the literature, and with an estimate of N(z) using a stacking analysis of COSMOS 24 \u03bcm detections.", "date": "2012-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "753", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 23", "id_number": "CaltechAUTHORS:20120720-094749727", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120720-094749727", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "JPL" }, { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/0" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "COSMOS" } ] }, "doi": "10.1088/0004-637X/753/1/23", "primary_object": { "basename": "MitchellWynne2012p18928Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/my5dk-p7s22/files/MitchellWynne2012p18928Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Mitchell-Wynne, K.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/h7c7n-ksg79", "eprint_id": 32827, "eprint_status": "archive", "datestamp": "2023-08-19 11:07:44", "lastmod": "2023-10-18 16:20:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "B\u00e9thermin-Matthieu", "name": { "family": "B\u00e9thermin", "given": "M." }, "orcid": "0000-0002-3915-2015" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: deep number counts at 250 \u03bcm, 350 \u03bcm and 500 \u03bcm\n in the COSMOS and GOODS-N fields and the build-up\n of the cosmic infrared background", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations, diffuse radiation, galaxies: statistics, galaxies: photometry, submillimeter: galaxies,\nsubmillimeter: diffuse background", "note": "\u00a9 2012 ESO. Received 21 December 2011. Accepted 9 March 2012.\nPublished online: 6 June 2012. We thank the COSMOS and GOODS teams for releasing\npublicly their data. Thanks to Georges Helou for suggesting that the distribution\nof the colors is more likely log-normal than normal. MB thank Herv\u00e9 Dole\nfor his advices about stacking, and Elizabeth Fernandez for providing a mock\ncatalog from the B\u00e9thermin et al. model. SPIRE has been developed by a consortium\nof institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge\n(Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC\n(Spain); Stockholm Observatory (Sweden); Imperial College London, RAL,\nUCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado\n(USA). This development has been supported by national funding agencies: CSA\n(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN\n(Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). MB acknowledge\nfinancial support from ERC-StG grant UPGAL 240039. SJO acknowledge\nsupport from the Science and Technology Facilities Council [grant number\nST/F002858/1] and [grant number ST/I000976/1]. M.V. was supported by the\nItalian Space Agency (ASI Herschel Science Contract I/005/07/0). The data presented\nin this paper will be released through the Herschel Database in Marseille\nHeDaM (hedam.oamp.fr/HerMES).\n\nPublished - Bethermin2012p18995Astron_Astrophys.pdf
", "abstract": "Aims. The Spectral and Photometric Imaging REceiver (SPIRE) onboard the Herschel space telescope has provided confusion limited maps of deep fields at 250 \u03bcm, 350 \u03bcm, and 500 \u03bcm, as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). Unfortunately, due to confusion, only a small fraction of the cosmic infrared background (CIB) can be resolved into individually-detected sources. Our goal is to produce deep galaxy number counts and redshift distributions below the confusion limit at SPIRE wavelengths (~20 mJy), which we then use to place strong constraints on the origins of the cosmic infrared background and on models of galaxy evolution.\nMethods. We individually extracted the bright SPIRE sources (>20 mJy) in the COSMOS field with a method using the positions, the flux densities, and the redshifts of the 24 \u03bcm sources as a prior, and derived the number counts and redshift distributions of the bright SPIRE sources. For fainter SPIRE sources (<20 mJy), we reconstructed the number counts and the redshift distribution below the confusion limit using the deep 24 \u03bcm catalogs associated with photometric redshift and information provided by the stacking of these sources into the deep SPIRE maps of the GOODS-N and COSMOS fields. Finally, by integrating all these counts, we studied the contribution of the galaxies to the CIB as a function of their flux density and redshift.\nResults. Through stacking, we managed to reconstruct the source counts per redshift slice down to ~2 mJy in the three SPIRE bands, which lies about a factor 10 below the 5\u03c3 confusion limit. Our measurements place tight constraints on source population models. None of the pre-existing models are able to reproduce our results at better than 3-\u03c3. Finally, we extrapolate our counts to zero flux density in order to derive an estimate of the total contribution of galaxies to the CIB, finding 10.1_(-2.3)^(+2.6)\u2009nW\u2009m^(-2)\u2009sr^(-1), 6.5_(-1.6)^(+1.7)\u2009nW\u2009m^(-2)\u2009sr^(-1), and 2.8_(-0.8)^(+0.9)\u2009nW\u2009m^(-2)\u2009sr^(-1) at 250 \u03bcm, 350 \u03bcm, and 500 \u03bcm, respectively. These values agree well with FIRAS absolute measurements, suggesting our number counts and their extrapolation are sufficient to explain the CIB. We find that half of the CIB is emitted at z = 1.04, 1.20, and 1.25, respectively. Finally, combining our results with other works, we estimate the energy budget contained in the CIB between 8 \u03bcm and 1000 \u03bcm: 26_(-3)^(+7)\u2009nW\u2009m^(-2)\u2009sr^(-1).", "date": "2012-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "542", "publisher": "EDP Sciences", "pagerange": "Art. No. A58", "id_number": "CaltechAUTHORS:20120801-084702053", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120801-084702053", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" }, { "agency": "ERC-StG", "grant_number": "UPGAL-240039" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/1000976/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/0" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1051/0004-6361/201118698", "primary_object": { "basename": "Bethermin2012p18995Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/h7c7n-ksg79/files/Bethermin2012p18995Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "B\u00e9thermin, M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/10c8x-xqv70", "eprint_id": 31818, "eprint_status": "archive", "datestamp": "2023-08-22 05:44:58", "lastmod": "2023-10-17 21:22:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Staniszewski-Z", "name": { "family": "Staniszewski", "given": "Z." } }, { "id": "Aikin-R-W", "name": { "family": "Aikin", "given": "R. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J. P." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-R-C", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Teply-G-P", "name": { "family": "Teply", "given": "G." } } ] }, "title": "The Keck Array: A Multi Camera CMB Polarimeter at the South Pole", "ispublished": "pub", "full_text_status": "restricted", "keywords": "Transition edge sensor (TES) arrays; Cosmology; Cosmic microwave background; Inflation", "note": "\u00a9 2012 Springer Science+Business Media, LLC. \n\nReceived: 24 September 2011; Accepted: 8 January 2012; Published online: 3 April 2012. \n\nThe following individuals acknowledge additional support: Z. Staniszewski from the NASA Postdoctoral Program.", "abstract": "The Keck array is a new multi-camera Cosmic Microwave Background (CMB) polarimeter. Each camera contains 256 polarization pairs of antenna-coupled transition edge sensor (TES) bolometers. We recently deployed three of five cameras at the geographic South Pole, and plan to deploy the final two cameras in early 2012. This new telescope is an ideal instrument to search for the primordial B-mode polarization signal imprinted in the CMB by inflationary gravitational waves. We will discuss the design of the detectors and receivers, the status of current observations,\nand report on progress toward upgrading the instrument with the full compliment of polarized receivers.", "date": "2012-06", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "167", "number": "5-6", "publisher": "Springer", "pagerange": "827-833", "id_number": "CaltechAUTHORS:20120605-123408895", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120605-123408895", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Postdoctoral Program" } ] }, "doi": "10.1007/s10909-012-0510-1", "resource_type": "article", "pub_year": "2012", "author_list": "Staniszewski, Z.; Aikin, R. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/3r4a4-b1853", "eprint_id": 31775, "eprint_status": "archive", "datestamp": "2023-08-22 05:41:49", "lastmod": "2023-10-17 21:07:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Martin-P-G", "name": { "family": "Martin", "given": "Peter G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } } ] }, "title": "Evidence for Environmental Changes in the Submillimeter Dust Opacity", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; dust, extinction; evolution; infrared: ISM; ISM: structure; submillimeter: ISM", "note": "\u00a9 2012 American Astronomical Society.\n\nReceived 2011 December 22; accepted 2012 March 14; published 2012 May 1.\n\nThe BLAST collaboration acknowledges the support of NASA through grant numbers NAG5-12785, NAG5-13301, and\nNNGO-6GI11G, the Canadian Space Agency (CSA), the UK Particle Physics & Astronomy Research Council (PPARC), and\nCanada's Natural Sciences and Engineering Research Council\n(NSERC). We thank the Columbia Scientific Balloon Facility\n(CSBF) staff for their outstanding work. Finally, we appreciate the careful reading of the manuscript by the referee, B. T. Draine, which has led to some clarification and elaboration of the analysis.\n\nPublished - Martin2012p18398Astrophys_J.pdf
", "abstract": "The submillimeter opacity of dust in the diffuse interstellar medium (ISM) in the Galactic plane has been quantified using a pixel-by-pixel correlation of images of continuum emission with a proxy for column density. We used multi-wavelength continuum data: three Balloon-borne Large Aperture Submillimeter Telescope bands at 250, 350, and 500 \u03bcm and one IRAS band at 100 \u03bcm. The proxy is the near-infrared color excess, E(J \u2013 K_s), obtained from the Two Micron All Sky Survey. Based on observations of stars, we show how well this color excess is correlated with the total hydrogen column density for regions of moderate extinction. The ratio of emission to column density, the emissivity, is then known from the correlations, as a function of frequency. The spectral distribution of this emissivity can be fit by a modified blackbody, whence the characteristic dust temperature T and the desired opacity \u03c3_e(1200) at 1200 GHz or 250 \u03bcm can be obtained. We have analyzed 14 regions near the Galactic plane toward the Vela molecular cloud, mostly selected to avoid regions of high column density (N_H > 10^(22) cm^(\u20132)) and small enough to ensure a uniform dust temperature. We find \u03c3_e(1200) is typically (2-4) \u00d7 10^(\u201325) cm^2 H^(\u20131) and thus about 2-4 times larger than the average value in the local high Galactic latitude diffuse atomic ISM. This is strong evidence for grain evolution. There is a range in total power per H nucleon absorbed (and re-radiated) by the dust, reflecting changes in the strength of the interstellar radiation field and/or the dust absorption opacity. These changes in emission opacity and power affect the equilibrium T, which is typically 15 K, colder than at high latitudes. Our analysis extends, to higher opacity and lower temperature, the trend of increasing \u03c3_e(1200) with decreasing T that was found at high latitudes. The recognition of changes in the emission opacity raises a cautionary flag because all column densities deduced from dust emission maps, and the masses of compact structures within them, depend inversely on the value adopted.", "date": "2012-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "751", "number": "1", "publisher": "American Astronomical Society", "pagerange": "28", "id_number": "CaltechAUTHORS:20120601-115553413", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120601-115553413", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "doi": "10.1088/0004-637X/751/1/28", "primary_object": { "basename": "Martin2012p18398Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/3r4a4-b1853/files/Martin2012p18398Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Martin, Peter G.; Bock, James J.; et el." }, { "id": "https://authors.library.caltech.edu/records/xy831-kwb94", "eprint_id": 31829, "eprint_status": "archive", "datestamp": "2023-08-19 10:56:58", "lastmod": "2023-10-17 21:22:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Page-M-J", "name": { "family": "Page", "given": "M. J." }, "orcid": "0000-0002-6689-6271" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The suppression of star formation by powerful active galactic nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomy", "note": "\u00a9 2012 Macmillan Publishers Limited.\n\nReceived: 30 November 2011; Accepted: 29 March 2012;\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and which includes: University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN(Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). Author Contributions: This Letter represents the combined work of the HerMES collaboration, the SPIRE Instrument Team's extragalactic survey. M.J.P. planned the study, and wrote the draft version of the paper. M.S. fitted models to the spectral energy distributions of the sources and J.D.V. performed the stacking analysis. All other co-authors contributed extensively and equally by their varied contributions to the SPIRE instrument, the Herschel mission, analysis of SPIRE and HerMES data, planning of HerMES observations and scientific support of HerMES, and by commenting on this manuscript as part of an internal review process.\n\nSubmitted - 1310.4147.pdf
Supplemental Material - nature11096-s1.pdf
", "abstract": "The old, red stars that constitute the bulges of galaxies, and the massive black holes at their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accretion onto black holes. It is widely suspected, but unproved, that the tight correlation between the mass of the black hole and the mass of the stellar bulge results from the AGN quenching the surrounding star formation as it approaches its peak luminosity. X-rays trace emission from AGN unambiguously, whereas powerful star-forming galaxies are usually dust-obscured and are brightest at infrared and submillimetre wavelengths. Here we report submillimetre and X-ray observations that show that rapid star formation was common in the host galaxies of AGN when the Universe was 2\u20136 billion years old, but that the most vigorous star formation is not observed around black holes above an X-ray luminosity of 10^(44) ergs per second. This suppression of star formation in the host galaxy of a powerful AGN is a key prediction of models in which the AGN drives an outflow, expelling the interstellar medium of its host and transforming the galaxy's properties in a brief period of cosmic time.", "date": "2012-05-10", "date_type": "published", "publication": "Nature", "volume": "485", "number": "7397", "publisher": "Nature Publishing Group", "pagerange": "213-216", "id_number": "CaltechAUTHORS:20120606-132737240", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120606-132737240", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/nature11096", "primary_object": { "basename": "1310.4147.pdf", "url": "https://authors.library.caltech.edu/records/xy831-kwb94/files/1310.4147.pdf" }, "related_objects": [ { "basename": "nature11096-s1.pdf", "url": "https://authors.library.caltech.edu/records/xy831-kwb94/files/nature11096-s1.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Page, M. J.; Vieira, J. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/c7bwd-9h079", "eprint_id": 31248, "eprint_status": "archive", "datestamp": "2023-08-22 05:31:04", "lastmod": "2023-10-17 15:42:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bonetti-J-A", "name": { "family": "Bonetti", "given": "J. A." } }, { "id": "Turner-A-D", "name": { "family": "Turner", "given": "A. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Day-Peter-K", "name": { "family": "Day", "given": "P. K." } }, { "id": "Filippini-J-P", "name": { "family": "Filippini", "given": "J." }, "orcid": "0000-0001-8217-6832" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Holmes-W-A", "name": { "family": "Holmes", "given": "W." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Kenyon-M", "name": { "family": "Kenyon", "given": "M." } }, { "id": "Kovac-J-M", "name": { "family": "Kovac", "given": "J. M." } }, { "id": "Kuo-Chia-Lam", "name": { "family": "Kuo", "given": "C. L." } }, { "id": "LeDuc-H-G", "name": { "family": "LeDuc", "given": "H. G." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "O'Brient-R-C", "name": { "family": "O'Brient", "given": "R." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Runyan-M-C", "name": { "family": "Runyan", "given": "M." } }, { "id": "Staniszewski-Z-K", "name": { "family": "Staniszewski", "given": "Z." } }, { "id": "Sudiwala-R-V", "name": { "family": "Sudiwala", "given": "R." } }, { "id": "Transgrud-Amy-R", "name": { "family": "Transgrud", "given": "A." } } ] }, "title": "Characterization and Fabrication of the TES Arrays for the Spider, Keck and BICEP2 CMB Polarimeters", "ispublished": "pub", "full_text_status": "restricted", "keywords": "CMB polarization; TES", "note": "\u00a9 2012 Springer Science+Business Media. \n\nReceived: 17 July 2011. Accepted: 10 January 2012. Published online: 3 February 2012. \n\nThe research described in this publication was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with National Aeronautics and Space Administration.", "abstract": "Spider, the Keck Array, and BICEP2 are projects to study the polarization of the cosmic microwave background (CMB). All three use large format arrays of antenna-coupled, membrane-isolated, transition edge sensors (TES's). Although similar, each project requires its own set of device parameters, such as thermal conductance, time constants, and normal state resistances. We have perfected a fabrication process that achieves two primary objectives: (1) high device yields of 95% or greater, and (2) very low spreads in devices parameters. Currently our arrays are taking science data at the South Pole in both the BICEP2 and Keck array telescopes. The focal planes for Spider, a high altitude balloon mission, are on schedule for a 2012 deployment. An overview of fabrication and development is given as well as a snapshot of scientific data.", "date": "2012-05", "date_type": "published", "publication": "Journal of Low Temperature Physics", "volume": "167", "number": "3-4", "publisher": "Springer", "pagerange": "146-151", "id_number": "CaltechAUTHORS:20120501-100739165", "issn": "0022-2291", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120501-100739165", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1007/s10909-012-0529-3", "resource_type": "article", "pub_year": "2012", "author_list": "Bonetti, J. A.; Turner, A. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/d9wkw-zvg05", "eprint_id": 31500, "eprint_status": "archive", "datestamp": "2023-08-22 05:29:05", "lastmod": "2024-02-24 00:16:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Aguirre-J", "name": { "family": "Aguirre", "given": "J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Czakon-N-G", "name": { "family": "Czakon", "given": "N. G." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Lupu-R", "name": { "family": "Lupu", "given": "R." } }, { "id": "Maloney-P", "name": { "family": "Maloney", "given": "P." } }, { "id": "Mauskopf-P", "name": { "family": "Mauskopf", "given": "P." } }, { "id": "Million-E-T", "name": { "family": "Million", "given": "E." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Naylor-B", "name": { "family": "Naylor", "given": "B." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H." } }, { "id": "Rosenman-M", "name": { "family": "Rosenman", "given": "M." } }, { "name": { "family": "Sayers", "given": "J." } }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "High Spectral Resolution Measurement of the Sunyaev\u2013Zel'dovich Effect Null with Z-Spec", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; galaxies: clusters: individual (RX J1347.5-1145); galaxies: clusters: intracluster medium; submillimeter: galaxies", "note": "\u00a9 2012 American Astronomical Society. \n\nReceived 2011 September 2; accepted 2012 February 3; published 2012 March 29. \n\nOur thanks to M. Hollister for his help acquiring the Bolocam data used in this work, J. Filippini for many useful discussions on statistics, and the anonymous referee for useful suggestions which improved this manuscript. The Z-Spec team acknowledges support from the following grants for building and fielding the instrument: NASA SARA grants NAGS-11911 and NAGS-12788, and the NSF AST grant 0807990. Bolocam was constructed and commissioned using funds from NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846, NSF/AST-0229008, and NSF/AST-0206158. The Bolocam observation and data analysis efforts were also supported by the Gordon and Betty Moore Foundation. J.S. was partially supported by a NASA Post-doctoral Program fellowship, NSF/AST-0838261, and NASA/NNX11AB07G; N.C. was partially supported by the NASA Graduate Student Research Fellowship. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the application package CIAO.\n\nPublished - Zemcov2012p18111Astrophys_J.pdf
", "abstract": "The Sunyaev-Zel'dovich (SZ) effect spectrum crosses through a null where \u0394T_CMB = 0 near \u03bd_0 = 217 GHz. In a cluster of galaxies, \u03bd0 can be shifted from the canonical thermal SZ effect value by corrections to the SZ effect scattering due to the properties of the inter-cluster medium. We have measured the SZ effect in the hot galaxy cluster RX J 1347.5 \u2013 1145 with Z-Spec, an R ~ 300 grating spectrometer sensitive between 185 and 305 GHz. These data comprise a high spectral resolution measurement around the null of the SZ effect and clearly exhibit the transition from negative to positive \u0394T_CMB over the Z-Spec band. The SZ null position is measured to be \u03bd_0 = 225.8 \u00b1 2.5(stat.) \u00b1 1.2(sys.) GHz, which differs from the canonical null frequency by 3.0\u03c3 and is evidence for modifications to the canonical thermal SZ effect shape. Assuming the measured shift in \u03bd0 is due only to relativistic corrections to the SZ spectrum, we place the limit kT_e = 17.1 \u00b1 5.3 keV from the zero-point measurement alone. By simulating the response of the instrument to the sky, we are able to generate likelihood functions in {y_0, T_e, v_pec} space. For v_pec = 0 km s^(\u20131), we measure the best-fitting SZ model to be y_0 = 4.6^(+0.6)_(\u20130.9) \u00d7 10^(\u20134), T_e, 0 = 15.2^(+12)_(\u20137.4) keV. When v pec is allowed to vary, a most probable value of v_pec = + 450 \u00b1 810 km s^(\u20131) is found.", "date": "2012-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "749", "number": "2", "publisher": "American Astronomical Society", "pagerange": "114", "id_number": "CaltechAUTHORS:20120516-092304643", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120516-092304643", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAGS-11911" }, { "agency": "NASA", "grant_number": "NAGS-12788" }, { "agency": "NSF", "grant_number": "AST-0807990" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "NASA", "grant_number": "NNX11AB07G" }, { "agency": "NASA Graduate Student Research Fellowship" } ] }, "doi": "10.1088/0004-637X/749/2/114", "primary_object": { "basename": "Zemcov2012p18111Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/d9wkw-zvg05/files/Zemcov2012p18111Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Zemcov, M.; Aguirre, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/1n46b-6a898", "eprint_id": 31459, "eprint_status": "archive", "datestamp": "2023-08-22 05:15:19", "lastmod": "2024-02-24 00:16:25", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Hroner-P-F", "name": { "family": "Horner", "given": "P. F." } }, { "id": "Aguirre-J", "name": { "family": "Aguirre", "given": "J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Egami-Eichi", "name": { "family": "Egami", "given": "E." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Laurent-G-T", "name": { "family": "Laurent", "given": "G." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "name": { "family": "Sayers", "given": "J." } } ] }, "title": "A high signal-to-noise ratio map of the Sunyaev\u2013Zel'dovich increment at 1.1-mm wavelength in Abell 1835", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis; techniques: radial velocities; galaxies: clusters: individual: Abell 1835; cosmic background radiation; submillimetre: galaxies", "note": "\u00a9 2012 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2012 RAS. \n\nAccepted 2011 November 29. Received 2011 October 13; in original form 2011 July 7. Article first published online: 26 Jan 2012. \n\nThis work was supported by NSF grants AST-9980846 and AST-0206158 and by STFC grants XXX. We wish to acknowledge M. Zemcov for providing access to SCUBA archive data and for useful discussion, which improved the content of this paper significantly. We would also like to recognize and acknowledge the cultural role and reverence that the summit of Mauna Kea has within the Hawaiian community. We are fortunate and privileged to be able to conduct observations from this mountain.\n\nPublished - MNRAS-2012-Mauskopf-224-34.pdf
Published - Mauskopf2012p18075Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present an analysis of an 8-arcmin diameter map of the area around the galaxy cluster Abell 1835 from jiggle-map observations at a wavelength of 1.1 mm using the Bolometric Camera (Bolocam) mounted on the Caltech Submillimeter Observatory (CSO). The data are well described by a model including a extended Sunyaev\u2013Zel'dovich (SZ) emission from the cluster gas plus emission from the cluster central galaxy and two bright background submm galaxies magnified by the gravitational lensing of the cluster. We measure flux densities of the two bright point sources in the field: SMM J14011+0252 and SMM J14009+0252 to be 6.5 \u00b1 2.0 \u00b1 0.8 and 11.3 \u00b1 1.9 \u00b1 1.3 mJy, respectively. Fitting the map to a sky model consisting of the point sources and the SZ emission from the cluster gas with a beta model density profile with parameters, \u03b8_c= 33.6 arcsec and \u03b2= 0.69, we find the peak surface brightness of the SZ emission to be I_c= 3.73 \u00b1 0.45 \u00b1 0.60 \u00d7 10^(\u221221) W m^(\u22122)sr^(\u22121) Hz^(\u22121), where the first error is the statistical uncertainty in the fit and the second error represents the calibration uncertainty and additional systematics. Assuming zero cluster peculiar velocity and an X-ray temperature of T_e= 9 keV, this surface brightness corresponds to a central Comptonization of y_0= (4.41 \u00b1 0.53 \u00b1 0.70) \u00d7 10^(\u22124). The cluster image represents one of the highest significance SZ detections of a cluster in the positive region of the thermal SZ spectrum to date. We compare the measured central intensity at 1.1 mm to other SZ measurements of Abell 1835 at different wavelengths to obtain values for y_0= (3.58 \u00b1 0.28) \u00d7 10^(\u22124) and the cluster peculiar velocity v_z=\u2212538 \u00b1 414 km s^(\u22121).", "date": "2012-03-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "421", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "224-234", "id_number": "CaltechAUTHORS:20120515-072010829", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120515-072010829", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-9980846" }, { "agency": "NSF", "grant_number": "AST-0206158" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "doi": "10.1111/j.1365-2966.2011.20295.x", "primary_object": { "basename": "MNRAS-2012-Mauskopf-224-34.pdf", "url": "https://authors.library.caltech.edu/records/1n46b-6a898/files/MNRAS-2012-Mauskopf-224-34.pdf" }, "related_objects": [ { "basename": "Mauskopf2012p18075Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/1n46b-6a898/files/Mauskopf2012p18075Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Mauskopf, P. D.; Horner, P. F.; et el." }, { "id": "https://authors.library.caltech.edu/records/tn1ya-87q47", "eprint_id": 29873, "eprint_status": "archive", "datestamp": "2023-08-22 04:50:52", "lastmod": "2023-10-24 22:31:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Herschel Multi-tiered Extragalactic Survey: SPIRE\u2013mm photometric redshifts", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: statistics; submillimetre: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. \n\nAccepted 2011 September 12. Received 2011 September 12; in original form 2011 February 10. Article first published online: 15 Dec. 2011. \n\nWe thank the anonymous referee for suggestions which greatly enhanced this work. LW and SJO were supported by the Science and Technology Facilities Council (ST/F002858/1). JSD acknowledges the support of the Royal Society via a Wolfson Research Merit award, and the support of the European Research Council via the award of an Advanced Grant. AF, GM, LM and MV were supported by the Italian Space Agency (ASI Herschel Science Contract I/005/07/0). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (China), CEA, LAM(France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UK ATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES)\n\nPublished - Roseboom2012p17435Mon_Not_R_Astron_Soc.pdf
Accepted Version - 1109.2887.pdf
", "abstract": "We investigate the potential of submm\u2013mm and submm\u2013mm\u2013radio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500\u03bcm by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm sources with reliable radio identifications in the Great Observatories Origins Deep Survey North and Lockman Hole North fields, 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm sources are adequately described by a modified blackbody with constant optical depth \u03c4= (\u03bd/nu_0)^\u03b2, where \u03b2=+1.8 and \u03bd_0=c/100 \u03bcm. We find a tight correlation between dust temperature and IR luminosity. Using a single model of the dust temperature and IR luminosity relation, we derive photometric redshift estimates for the 46 SPIRE-detected mm sources. Testing against the 22 sources with known spectroscopic or good quality optical/near-IR photometric redshifts, we find submm/mm photometric redshifts offer a redshift accuracy of |\u0394z|/(1 +z) = 0.16 (\u3008|\u0394z|\u3009= 0.51). Including constraints from the radio\u2013far-IR correlation, the accuracy is improved to |\u0394z|/(1 +z) = 0.15 (\u3008|\u0394z|\u3009= 0.45). We estimate the redshift distribution of mm-selected sources finding a significant excess at z > 3 when compared to \u223c 850 \u03bcm selected samples.", "date": "2012-02", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "419", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2758-2773", "id_number": "CaltechAUTHORS:20120328-085250071", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120328-085250071", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/0" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2011.19827.x", "primary_object": { "basename": "Roseboom2012p17435Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/tn1ya-87q47/files/Roseboom2012p17435Mon_Not_R_Astron_Soc.pdf" }, "related_objects": [ { "basename": "1109.2887.pdf", "url": "https://authors.library.caltech.edu/records/tn1ya-87q47/files/1109.2887.pdf" } ], "resource_type": "article", "pub_year": "2012", "author_list": "Roseboom, I. G.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/jqwep-kbb08", "eprint_id": 29945, "eprint_status": "archive", "datestamp": "2023-08-22 04:45:13", "lastmod": "2023-10-24 22:36:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gong-Yan", "name": { "family": "Gong", "given": "Yan" } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Silva-M", "name": { "family": "Silva", "given": "Marta" } }, { "id": "Santos-M-G", "name": { "family": "Santos", "given": "Mario G." }, "orcid": "0000-0003-3892-3073" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. Matt" }, "orcid": "0000-0001-5261-7094" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "Michael" }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Intensity Mapping of the [C II] Fine Structure Line During the Epoch of Reionization", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: theory; diffuse radiation; intergalactic medium; large-scale structure of universe", "note": "\u00a9 2012 American Astronomical Society. Received 2011 July 18; accepted 2011 October 20; published 2011 December 28. We thank participants of the Keck Institute for Space Studies'\n(KISS) Billion Years workshop for helpful discussions.\nThis work was supported by NSF CAREER AST-0645427\nand NASA NNX10AD42G at UCI. M.G.S. and M.B.S. acknowledge\nsupport from FCT-Portugal under grant PTDC/FIS/\n100170/2008.\n\nPublished - Gong2012p17617Astrophys_J.pdf
", "abstract": "The atomic C II fine-structure line is one of the brightest lines in a typical star-forming galaxy spectrum with a luminosity ~0.1%-1% of the bolometric luminosity. It is potentially a reliable tracer of the dense gas distribution at high redshifts and could provide an additional probe to the era of reionization. By taking into account the spontaneous, stimulated, and collisional emission of the C II line, we calculate the spin temperature and the mean intensity as a function of the redshift. When averaged over a cosmologically large volume, we find that the C II emission from ionized carbon in individual galaxies is larger than the signal generated by carbon in the intergalactic medium. Assuming that the C II luminosity is proportional to the carbon mass in dark matter halos, we also compute the power spectrum of the C II line intensity at various redshifts. In order to avoid the contamination from CO rotational lines at low redshift when targeting a C II survey at high redshifts, we propose the cross-correlation of C II and 21 cm line emission from high redshifts. To explore the detectability of the C II signal from reionization, we also evaluate the expected errors on the C II power spectrum and C II-21 cm cross power spectrum based on the design of the future millimeter surveys. We note that the C II-21 cm cross power spectrum contains interesting features that capture physics during reionization, including the ionized bubble sizes and the mean ionization fraction, which are challenging to measure from 21 cm data alone. We propose an instrumental concept for the reionization C II experiment targeting the frequency range of ~200-300 GHz with 1, 3, and 10 m apertures and a bolometric spectrometer array with 64 independent spectral pixels with about 20,000 bolometers.", "date": "2012-01-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "745", "number": "1", "publisher": "American Astro745nomical Society", "pagerange": "Art. No. 49", "id_number": "CaltechAUTHORS:20120403-080450129", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120403-080450129", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "NASA", "grant_number": "NNX10AD42G" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)", "grant_number": "PTDC/FIS/100170/2008" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Keck-Institute-for-Space-Studies" } ] }, "doi": "10.1088/0004-637X/745/1/49", "primary_object": { "basename": "Gong2012p17617Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/jqwep-kbb08/files/Gong2012p17617Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Gong, Yan; Cooray, Asantha; et el." }, { "id": "https://authors.library.caltech.edu/records/2s1hr-z2m07", "eprint_id": 29000, "eprint_status": "archive", "datestamp": "2023-08-22 04:40:44", "lastmod": "2023-10-24 18:18:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hajian-A", "name": { "family": "Hajian", "given": "Amir" } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Correlations in the (Sub)millimeter Background from ACT \u00d7 BLAST", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; galaxies: evolution; infrared: galaxies; large-scale structure of universe; submillimeter: galaxies", "note": "\u00a9 2012 The American Astronomical Society. Received 2011 January 11; accepted 2011 September 9; published 2011 December 13. BLAST was made possible through the support of NASA through grant Nos. NAG5-12785, NAG5-13301, and NNGO-\n6GI11G, the NSF Office of Polar Programs, the Canadian Space\nAgency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology\nFacilities Council (STFC). C.B.N. acknowledges support from\nthe Canadian Institute for Advanced Research. ACT was supported by the U.S. National Science Foundation through awards AST-0408698 for the ACT project, and PHY-0355328, AST- 0707731, and PIRE-0507768. Funding was also provided by Princeton University and the University of Pennsylvania. Computations were performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund\u2013Research Excellence; and the University of Toronto. J.D. acknowledges support from an RCUK Fellowship. S.D., A.H., and T.M. were supported through NASA grant NNX08AH30G.\nA.K. was partially supported through NSF AST-0546035 and\nAST-0606975 for work on ACT. E.S. acknowledges support by\nNSF Physics Frontier Center grant PHY-0114422 to the Kavli\nInstitute of Cosmological Physics. S.D. acknowledges support\nfrom the Berkeley Center for Cosmological Physics. We thank\nCONICYT for overseeing the Chajnantor Science Preserve, enabling instruments like ACT to operate in Chile; and we thank AstroNorte for operating our scientific base station. Some of the results in this paper have been derived using the HEALPix (G\u03ccrski et al. 2005) package.\nThe authors thank Matthieu B\u00e9thermin and Guilaine Lagache\nfor their help.\n\nPublished - Hajian2012p16872Astrophys_J.pdf
", "abstract": "We present measurements of the auto- and cross-frequency correlation power spectra of the cosmic (sub)millimeter background at 250, 350, and 500 \u03bcm (1200, 860, and 600 GHz) from observations made with the Balloon-borne Large Aperture Submillimeter Telescope (BLAST); and at 1380 and 2030 \u03bcm (218 and 148 GHz) from observations made with the Atacama Cosmology Telescope (ACT). The overlapping observations cover 8.6 deg^2 in an area relatively free of Galactic dust near the south ecliptic pole. The ACT bands are sensitive to radiation from the cosmic microwave background, to the Sunyaev-Zel'dovich effect from galaxy clusters, and to emission by radio and dusty star-forming galaxies (DSFGs), while the dominant contribution to the BLAST bands is from DSFGs. We confirm and extend the BLAST analysis of clustering with an independent pipeline and also detect correlations between the ACT and BLAST maps at over 25\u03c3 significance, which we interpret as a detection of the DSFGs in the ACT maps. In addition to a Poisson component in the cross-frequency power spectra, we detect a clustered signal at 4\u03c3, and using a model for the DSFG evolution and number counts, we successfully fit all of our spectra with a linear clustering model and a bias that depends only on redshift and not on scale. Finally, the data are compared to, and generally agree with, phenomenological models for the DSFG population. This study demonstrates the constraining power of the cross-frequency correlation technique to constrain models for the DSFGs. Similar analyses with more data will impose tight constraints on future models.", "date": "2012-01-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "744", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 40", "id_number": "CaltechAUTHORS:20120127-111701766", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120127-111701766", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "NSF Office of Polar Programs" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Science and Technology Facilities Council (STFC) (UK)" }, { "agency": "Canadian Institute for Advanced Research" }, { "agency": "NSF", "grant_number": "AST-040698" }, { "agency": "NSF", "grant_number": "PHY-0355328" }, { "agency": "NSF", "grant_number": "AST-0707731" }, { "agency": "NSF", "grant_number": "PIRE-0507768" }, { "agency": "Princeton University" }, { "agency": "University of Pennsylvania" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Government of Ontario" }, { "agency": "Ontario Research Fund-Research Excellence" }, { "agency": "University of Toronto" }, { "agency": "RCUK fellowship" }, { "agency": "NASA", "grant_number": "NNX08AH30G" }, { "agency": "NSF", "grant_number": "AST-0546035" }, { "agency": "NSF Physics Frontier Center", "grant_number": "PHY-0114422" }, { "agency": "Berkeley Center for Cosmological Physics" }, { "agency": "NSF", "grant_number": "AST-0606975" } ] }, "doi": "10.1088/0004-637X/744/1/40", "primary_object": { "basename": "Hajian2012p16872Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/2s1hr-z2m07/files/Hajian2012p16872Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Hajian, Amir; Viero, Marco P.; et el." }, { "id": "https://authors.library.caltech.edu/records/kr9mf-kxr97", "eprint_id": 29469, "eprint_status": "archive", "datestamp": "2023-08-22 04:37:05", "lastmod": "2023-10-24 22:13:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Smith-A-J", "name": { "family": "Smith", "given": "A. J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: point source catalogues from deep Herschel-SPIRE\n observations", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis; catalogues; galaxies: photometry; submillimetre: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 August 25. Received 2011 August 25; in original form 2011 January 17. Article first published online: 6 Oct 2011. \nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation\nfrom NASA.\nSPIRE has been developed by a consortium of institutes led by\nCardiff University (UK) and including the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the University of Sussex (UK); Caltech, JPL, NHSC, the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES,\nCNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden);\nSTFC (UK) and NASA (USA). The released HerMES data are available through the HeDaM data base (http://hedam.oamp.fr), operated by CeSAM and hosted by the\nLaboratoire d'Astrophysique de Marseille. Data presented in this paper were analysed using HIPE, a joint\ndevelopment by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center and the HIFI, PACS and SPIRE consortia. (See http://herschel.esac.esa. int/DpHipeContributors.shtml.)\nWe acknowledge support from the Science and Technology Facilities Council (grant numbers ST/F002858/1 and ST/I000976/1. We are grateful to the anonymous referee for helpful and constructive comments.\n\nPublished - Smith2012p17267Mon_Not_R_Astron_Soc.pdf
", "abstract": "We describe the generation of single-band point source catalogues from submillimetre\u2002Herschel-SPIRE observations taken as part of the Science Demonstration Phase of the\u2002Herschel\u2002Multi-tiered Extragalactic Survey (HerMES). Flux densities are found by means of peak finding and the fitting of a Gaussian point-response function. With highly confused images, careful checks must be made on the completeness and flux-density accuracy of the detected sources. This is done by injecting artificial sources into the images and analysing the resulting catalogues. Measured flux densities at which 50 per cent of injected sources result in good detections at (250, 350 and 500) \u03bcm range from (11.6, 13.2 and 13.1) to (25.7, 27.1 and 35.8) mJy, depending on the depth of the observation (where a 'good' detection is taken to be one with positional offset less than one full-width half-maximum of the point-response function, and with the measured flux density within a factor of 2 of the flux density of the injected source). This paper acts as a reference for the 2010 July HerMES public data release.", "date": "2012-01", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "419", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "377-389", "id_number": "CaltechAUTHORS:20120224-154058470", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120224-154058470", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/I000976/1" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2011.19709.x", "primary_object": { "basename": "Smith2012p17267Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/kr9mf-kxr97/files/Smith2012p17267Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2012", "author_list": "Smith, A. J.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/726ev-70142", "eprint_id": 85229, "eprint_status": "archive", "datestamp": "2023-08-19 08:50:37", "lastmod": "2023-10-18 17:59:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Helou-G", "name": { "family": "Helou", "given": "G." }, "orcid": "0000-0003-3367-3415" }, { "id": "Hildebrant-S-R", "name": { "family": "Hildebrandt", "given": "S. R." } }, { "id": "Matsumura-Tomotake", "name": { "family": "Matsumura", "given": "Tomotake" } }, { "id": "Pearson-T-J", "name": { "family": "Pearson", "given": "T. J." }, "orcid": "0000-0001-5213-6231" }, { "id": "Pr\u00e9zeau-G", "name": { "family": "Pr\u00e9zeau", "given": "G." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "Ranga-Ram" }, "orcid": "0000-0001-7583-0621" }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "McGehee-P-M", "name": { "family": "McGehee", "given": "P." }, "orcid": "0000-0003-0948-6716" }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2011 ESO. \n\nReceived: 10 January 2011. Accepted: 29 June 2011. \n\nThe Planck HFI instrument (http://hfi.planck.fr/) was designed and built by an international consortium of laboratories, universities and institutes, with important contributions from the industry, under the leadership of the PI institute, IAS at Orsay, France. It was funded in particular by CNES, CNRS, NASA, STFC and ASI. The authors extend their gratitude to the numerous engineers and scientists, who have contributed to the design, development, construction or evaluation of the HFI instrument. A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.rssd.esa.int/index.php?project=PLANCK\\&page=Planck_Collaboration. The Planck Collaboration acknowledges financial support from: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC and MICINN (Spain); Tekes and AoF (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); Swiss Funding Agency (Switzerland); Norwegian Funding Agency (Norway); and FCT/MCTES (Portugal).\n\nPublished - aa16487-11.pdf
Submitted - 1101.2039.pdf
", "abstract": "The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ~30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10\u2032 (100 GHz), 7\u2032 (143 GHz), and 5\u2032 (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, theremoval of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6\u22122.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI.", "date": "2011-12", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "536", "number": "12", "publisher": "EDP Sciences", "pagerange": "Art. No. A4", "id_number": "CaltechAUTHORS:20180309-110837130", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180309-110837130", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "NASA" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "European Space Agency (ESA)" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Institut National de Physique Nucl\u00e9aire et de Physique des Particules (IN2P3)" }, { "agency": "Institut National du Patrimoine (INP)" }, { "agency": "Consiglio Nazionale delle Ricerche (CNR)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Department of Energy (DOE)" }, { "agency": "United Kingdom Space Agency (UKSA)" }, { "agency": "Consejo Superior de Investigaciones Cient\u00edficas (CSIC)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Finnish Funding Agency for Technology and Innovation" }, { "agency": "Academy of Finland" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Max Planck Society" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "DTU Space (Denmark)" }, { "agency": "Swiss Funding Agencies" }, { "agency": "Norwegian Funding Agency" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Minist\u00e9rio da Ci\u00eancia, Tecnologia e Ensino Superior (MCTES)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "corp_creators": { "items": [ "Planck HFI Core Team" ] }, "doi": "10.1051/0004-6361/201116487", "primary_object": { "basename": "1101.2039.pdf", "url": "https://authors.library.caltech.edu/records/726ev-70142/files/1101.2039.pdf" }, "related_objects": [ { "basename": "aa16487-11.pdf", "url": "https://authors.library.caltech.edu/records/726ev-70142/files/aa16487-11.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Ade, P. A. R.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/wyhr0-4yb78", "eprint_id": 28907, "eprint_status": "archive", "datestamp": "2023-08-22 04:09:00", "lastmod": "2023-10-24 18:13:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bierman-E-M", "name": { "family": "Bierman", "given": "E. M." } }, { "id": "Matsumura-T", "name": { "family": "Matsumura", "given": "T." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chiang-H-C", "name": { "family": "Chiang", "given": "H. C." } }, { "id": "Culverhouse-T-L", "name": { "family": "Culverhouse", "given": "T. L." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Kovac-J-M", "name": { "family": "Kovac", "given": "J. M." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Richter-S", "name": { "family": "Richter", "given": "S." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G. M." }, "orcid": "0000-0002-4150-8076" } ] }, "title": "A Millimeter-wave Galactic Plane Survey with the BICEP Polarimeter", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; Galaxy: structure; instrumentation: polarimeters; radio continuum: ISM; submillimeter: diffuse background; submillimeter: ISM", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 February 23; accepted 2011 August 3; published 2011 October 20. We especially recognize Andrew Lange whose passing has\ndeeply affected everyone on the team and who never saw the\nculmination of this project. Without his guidance and friendship this paper would not have been possible.\nBICEP is supported by NSF Grant OPP-0230438, Caltech\nDiscovery Fund, Caltech President's Fund PF-471, JPL Research and Technology Fund, and the late J. Robinson. We thank our colleagues in the ACBAR, Boomerang, QUaD, Bolocam,\nPOLARBEAR, and SPT collaborations for advice and helpful\ndiscussions, Kathy Deniston for logistical and administrative support, and the South Pole Station staff for their support. We gratefully acknowledge support by the NASA Graduate Fellowship program (E.M.B. and H.C.C.), the John B. and Nelly Kilroy Foundation (J.M.K.), the NSF PECASE Award AST-0548262 (B.G.K.), the US DOE contract to SLAC No. DEAC02-76SF00515 (C.L.K. and J.E.T.), KICP (C.P. and C.S.), and the NASA Science Mission Directorate via the US Planck Project (G.R.). We also thank the thorough and comprehensive work of the referee that has tremendously improved the quality of the final version of this paper.\n\nPublished - Bierman2011p16857Astrophys_J.pdf
", "abstract": "In order to study inflationary cosmology and the Milky Way Galaxy's composition and magnetic field structure, Stokes I, Q, and U maps of the Galactic plane covering the Galactic longitude range 260\u00b0 < \u2113 < 340\u00b0 in three atmospheric transmission windows centered on 100, 150, and 220 GHz are presented. The maps sample an optical depth 1 \u227e AV \u227e 30, and are consistent with previous characterizations of the Galactic millimeter-wave frequency spectrum and the large-scale magnetic field structure permeating the interstellar medium. The polarization angles in all three bands are generally perpendicular to those measured by starlight polarimetry as expected and show changes in the structure of the Galactic magnetic field on the scale of 60\u00b0. The frequency spectrum of degree-scale Galactic emission is plotted between 23 and 220 GHz (including WMAP data) and is fit to a two-component (synchrotron and dust) model showing that the higher frequency BICEP data are necessary to tightly constrain the amplitude and spectral index of Galactic dust. Polarized emission is detected over the entire region within two degrees of the Galactic plane, indicating the large-scale magnetic field is oriented parallel to the plane of the Galaxy. A trend of decreasing polarization fraction with increasing total intensity is observed, ruling out the simplest model of a constant Galactic magnetic field orientation along the line of sight in the Galactic plane. A generally increasing trend of polarization fraction with electromagnetic frequency is found, varying from 0.5%-1.5% at frequencies below 50 GHz to 2.5%-3.5% above 90 GHz. The effort to extend the capabilities of BICEP by installing 220 GHz band hardware is described along with analysis of the new band.", "date": "2011-11-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "741", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 81", "id_number": "CaltechAUTHORS:20120123-092043396", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120123-092043396", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0230438" }, { "agency": "Caltech Discovery Fund" }, { "agency": "Caltech President's Fund", "grant_number": "PF-471" }, { "agency": "JPL Research and Technology Fund" }, { "agency": "NASA Graduate Fellowship" }, { "agency": "John B. and Nelly Kilroy Foundation" }, { "agency": "NSF PECASE Award", "grant_number": "AST-0548262" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "KICP" }, { "agency": "NASA Science Mission Directorate via the US Planck Project" } ] }, "doi": "10.1088/0004-637X/741/2/81", "primary_object": { "basename": "Bierman2011p16857Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/wyhr0-4yb78/files/Bierman2011p16857Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Bierman, E. M.; Matsumura, T.; et el." }, { "id": "https://authors.library.caltech.edu/records/kgr1r-nsy06", "eprint_id": 28389, "eprint_status": "archive", "datestamp": "2023-08-22 04:08:28", "lastmod": "2023-10-24 17:51:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Bolatto-A-D", "name": { "family": "Bolatto", "given": "A. D." }, "orcid": "0000-0002-5480-5686" }, { "id": "Maloney-P-R", "name": { "family": "Maloney", "given": "P. R." } }, { "id": "Aguirre-J-E", "name": { "family": "Aguirre", "given": "J. E." }, "orcid": "0000-0002-4810-666X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Kamenetzky-J", "name": { "family": "Kamenetzky", "given": "J." } }, { "id": "Lupu-R-E", "name": { "family": "Lupu", "given": "R." } }, { "id": "Matsuhara-Hideo", "name": { "family": "Matsuhara", "given": "H." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Naylor-B-J", "name": { "family": "Naylor", "given": "B. J." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "The Water Vapor Spectrum of APM 08279+5255: X-Ray Heating and Infrared Pumping over Hundreds of Parsecs", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; instrumentation: spectrographs; ISM: molecules; quasars: emission lines", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2011 June 21; accepted 2011 July 13; published 2011 October 21.\n\nWe are indebted to the staff of the Caltech Submillimeter\nObservatory for their help in Z-Spec's commissioning and observing. We acknowledge the following grants and fellowships: NASA SARA grants NAGS-11911 and NAGS-12788, NSF\nAST grant 0807990, an NSF Career grant (AST-0239270) and\na Research Corporation Award (RI0928) to J. Glenn, a Caltech\nMillikan and JPL Director's fellowships to C.M.B., an NRAO\nJansky fellowship to J. E. Aguirre, NASAGSRP fellowship to L.\nEarle, and an NSF GSRP award to J. Kamenetzky. The research\ndescribed in this Letter, carried out at the Jet Propulsion Laboratory, California Institute of Technology, was done under a contract with the National Aeronautics and Space Administration.\n\nPublished - Bradford2011p16475Astrophys_J_Lett.pdf
", "abstract": "We present the rest-frame 200-320 \u03bcm spectrum of the z = 3.91 quasar APM 08279+5255, obtained with Z-Spec at the Caltech Submillimeter Observatory. In addition to the J = 8 \u2192 7 to J = 13 \u2192 12 CO rotational transitions which dominate the CO cooling, we find six transitions of water originating at energy levels ranging up to 643 K. Most are first detections at high redshift, and we have confirmed one transition with CARMA. The CO cooling is well described by our X-ray dominated region (XDR) model, assuming L_(1-100 keV) ~ 1 \u00d7 10^(46) erg s^(\u20131), and that the gas is distributed over a 550-pc size scale, as per the now-favored \u03bc = 4 lensing model. The total observed cooling in water corresponds to 6.5 \u00d7 109 L_\u2609, comparable to that of CO. We compare the water spectrum with that of Mrk 231, finding that the intensity ratios among the high-lying lines are similar, but with a total luminosity scaled up by a factor of ~50. Using this scaling, we estimate an average water abundance relative to H_2 of 1.4 \u00d7 10^(\u20137), a good match to the prediction of the chemical network in the XDR model. As with Mrk 231, the high-lying water transitions are excited radiatively via absorption in the rest-frame far-infrared, and we show that the powerful dust continuum in APM 08279+5255 is more than sufficient to pump this massive reservoir of warm water vapor.", "date": "2011-11-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "741", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L37", "id_number": "CaltechAUTHORS:20111209-094523752", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111209-094523752", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAGS-11911" }, { "agency": "NASA", "grant_number": "NAGS-12788" }, { "agency": "NSF", "grant_number": "AST-0807990" }, { "agency": "NSF", "grant_number": "AST-0239270" }, { "agency": "Research Corporation", "grant_number": "RI0928" }, { "agency": "Caltech Millikan Fellowship" }, { "agency": "JPL Director's fellowship" }, { "agency": "NRAO Jansky fellowship" }, { "agency": "NASA Graduate Student Research Fellowship" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "doi": "10.1088/2041-8205/741/2/L37", "primary_object": { "basename": "Bradford2011p16475Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/kgr1r-nsy06/files/Bradford2011p16475Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Bradford, C. M.; Bolatto, A. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/axc7y-53c26", "eprint_id": 28432, "eprint_status": "archive", "datestamp": "2023-08-22 04:03:10", "lastmod": "2023-10-24 17:53:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "Herschel/HerMES: the X-ray\u2013infrared correlation for star-forming galaxies at z ~ 1", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: general; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; X-rays: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS.\n\nAccepted 2011 July 6. Received 2011 June 7; in original form 2011 March 8. Article first published online: 1 Sep 2011. \n\nMS is grateful for MSSL/UCL support. The team is also extremely grateful to H\u00e9ctor Ot\u00ed-Floranes, Kazushi Iwasawa and Bret Lehmer, for useful discussions and for providing us with models and data\nessential for the various comparisons made in this paper. This paper uses data from Herschel's submm photometer SPIRE. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI\n(Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA\n(USA).\n\nPublished - Symeonidis2011p16459Mon_Not_R_Astron_Soc.pdf
Accepted Version - 1107.1373.pdf
", "abstract": "For the first time, we investigate the X-ray/infrared (IR) correlation for star-forming galaxies (SFGs) at z ~ 1, using SPIRE submm data from the recently launched Herschel Space Observatory and deep X-ray data from the 2-Ms Chandra Deep Field-North survey. We examine the X-ray/IR correlation in the soft X-ray (SX; 0.5\u20132 keV) and hard X-ray (HX; 2\u201310 keV) bands by comparing our z ~ 1 SPIRE-detected SFGs to equivalently IR-luminous (L_(IR) > 10^(10) L_\u2299) samples in the local/low-redshift Universe. Our results suggest that the X-ray/IR properties of the SPIRE SFGs are on average similar to those of their local counterparts, as we find no evidence for evolution in the L_(SX)/L_(IR) and L_(HX)/L_(IR) ratios with redshift. We note, however, that at all redshifts, both L_(SX)/L_(IR) and L_(HX)/L_(IR) are strongly dependent on IR luminosity, with luminous and ultraluminous IR galaxies (LIRGs and ULIRGs; L_(IR) > 10^(11) L_\u2299) having up to an order of magnitude lower values than normal IR galaxies (L_(IR) < 10^(11) L_\u2299). We derive a L_(SX)\u2013L_(IR) relation and confirm the applicability of an existing L_(HX)\u2013L_(IR) relation for both local and distant LIRGs and ULIRGs, consistent with a scenario where X-ray luminosity is correlated with the star formation rate.", "date": "2011-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "417", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "2239-2252", "id_number": "CaltechAUTHORS:20111213-074241845", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111213-074241845", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2011.19405.x", "primary_object": { "basename": "1107.1373.pdf", "url": "https://authors.library.caltech.edu/records/axc7y-53c26/files/1107.1373.pdf" }, "related_objects": [ { "basename": "Symeonidis2011p16459Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/axc7y-53c26/files/Symeonidis2011p16459Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2011", "author_list": "Symeonidis, M.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/b4b0d-akx18", "eprint_id": 25634, "eprint_status": "archive", "datestamp": "2023-08-22 03:40:35", "lastmod": "2023-10-24 15:58:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gavazzo-R", "name": { "family": "Gavazzi", "given": "R." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "H." }, "orcid": "0000-0001-9608-6395" }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Modeling of the HerMES Submillimeter Source Lensed by a Dark Matter Dominated Foreground Group of Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: elliptical and lenticular, cD; galaxies: groups: general; galaxies: halos; gravitational lensing: strong; submillimeter: galaxies", "note": "\u00a9 2011 The American Astronomical Society. \n\nReceived 2011 February 9; accepted 2011 June 7; published 2011 August 18. \n\nSome of the data presented herein were obtained at the W. M. Keck Observatory which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. R.G. and A.O. acknowledge support from the Centre National de Etudes Spatiales. S.G.D. and A.A.M. acknowledge partial support from SN grant AST-0909182 and the Ajax Foundation. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). The IRAM Plateau de Bure Interferometer is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).\n\nPublished - Gavazzi2011p15955Astrophys_J.pdf
", "abstract": "We present the results of a gravitational lensing analysis of the bright z_s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be \u03bc = 10.9 \u00b1 0.7. We measure the half-light radius R_(eff) of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R_(eff),* = [2.0 \u00b1 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (R_(eff,gas) = [1.1 \u00b1 0.5] kpc) by mapping back in the source plane the CO (J = 5 \u2192 4) transition line emission. The lens modeling yields a relatively large Einstein radius R_(Ein) = 4\".10 \u00b1 0\".02, corresponding to a deflector velocity dispersion of [483 \u00b1 16] km s^(\u20131). This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z_l ~ 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f_(dm)(< R_(Ein)) ~ 80%. This fraction reduces to f_(dm)(< R_(eff,G1) \u2243 4.5 kpc) ~ 47% within the effective radius of the main deflecting galaxy of stellar mass M_(*,G1) = [8.5 \u00b1 1.6] \u00d7 10^(11) M_\u2609. At this smaller scale the dark matter fraction is consistent with results already found for massive lensing ellipticals at z ~ 0.2 from the Sloan Lens ACS Survey.", "date": "2011-09-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "738", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 125", "id_number": "CaltechAUTHORS:20111004-113055775", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111004-113055775", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "NSF", "grant_number": "AST-0909182" }, { "agency": "Ajax Foundation" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/738/2/125", "primary_object": { "basename": "Gavazzi2011p15955Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/b4b0d-akx18/files/Gavazzi2011p15955Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Gavazzi, R.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/stkd9-dth76", "eprint_id": 25451, "eprint_status": "archive", "datestamp": "2023-08-22 03:21:04", "lastmod": "2023-10-24 15:52:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ikarashi-Soh", "name": { "family": "Ikarashi", "given": "S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Detection of an ultrabright submillimetre galaxy in the\n Subaru/XMM\u2013Newton Deep Field using AzTEC/ASTE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: ISM; galaxies: starburst; submillimetre: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 April 14. Received 2011 April 12; in original form 2010 September 7. \nArticle first published online: 22 Jul. 2011.\nWe would like to thank everyone who helped staff and support\nthe AzTEC/ASTE 2008 operations and data calibration, including N. Ukita, M. Tashiro, M. Uehara, S. Doyle, P. Horner, J. Cortes, J. Karakla, and G. Wallace. The ASTE project is driven by the Nobeyama Radio Observatory (NRO), a branch of the National Astronomical Observatory of Japan (NAOJ), in collaboration with the University of Chile and Japanese institutions including the University of Tokyo, Nagoya University, Osaka Prefecture University, Ibaraki University and Hokkaido University. Partial observations\nwith ASTE were carried out remotely from Japan using NTT's\nGEMnet2 and its partner R&E networks, which are based on the\nAccessNova collaboration of the University of Chile, NTT Laboratories and the NAOJ. This study was supported in part by the MEXT Grant-in-Aid for Specially Promoted Research (No. 20001003). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute\nof Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. The ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities.\n\nPublished - Ikarashi2011p15874Mon_Not_R_Astron_Soc.pdf
", "abstract": "We report on the detection of an extremely bright (\u223c37 mJy at 1100\u2002\u03bcm and \u223c91 mJy at 880\u2002\u03bcm) submillimetre galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi), discovered in the 1100\u2002\u03bcm observations of the Subaru/XMM\u2013Newton\u2002Deep Field\u2002using AzTEC on ASTE. Subsequent CARMA 1300-\u03bcm and SMA 880-\u03bcm observations successfully pinpoint the location of Orochi and suggest that it has two components, one extended [full width at half-maximum (FWHM) of \u223c4 arcsec] and one compact (unresolved). Z-Spec on CSO has also been used to obtain a wide-band spectrum from 190 to 308 GHz, although no significant emission/absorption lines were found. The derived upper limit to the line-to-continuum flux ratio is 0.1\u20130.3 (2\u03c3) across the Z-Spec band.\nBased on the analysis of the derived spectral energy distribution from optical to radio wavelengths of possible counterparts near the SMA/CARMA peak position, we suggest that Orochi is a lensed, optically dark SMG lying at\u2002z\u2002\u223c 3.4 behind a foreground, optically visible (but red) galaxy at\u2002z\u2002\u223c 1.4. The deduced apparent (i.e., no correction for magnification) infrared luminosity (L_(IR)) and star formation rate (SFR) are 6 \u00d7 10^(13) L_\u2299 and 11 000 M_\u2299 yr^(\u22121), respectively, assuming that the\u2002L_(IR) is dominated by star formation. These values suggest that Orochi will consume its gas reservoir within a short time-scale (3 \u00d7 10^7 yr), which is indeed comparable to those in extreme starbursts like the centres of local ultraluminous infrared galaxies (ULIRGs).", "date": "2011-08", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "415", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "3081-3096", "id_number": "CaltechAUTHORS:20110927-132054052", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110927-132054052", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)", "grant_number": "20001003" }, { "agency": "Smithsonian Institution" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Associates of the California Institute of Technology" }, { "agency": "University of Chicago" }, { "agency": "states of California, Illinois, and Maryland" }, { "agency": "NSF" }, { "agency": "Academica Sinica" } ] }, "doi": "10.1111/j.1365-2966.2011.18918.x", "primary_object": { "basename": "Ikarashi2011p15874Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/stkd9-dth76/files/Ikarashi2011p15874Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Ikarashi, S.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/5jw5c-hwh19", "eprint_id": 24622, "eprint_status": "archive", "datestamp": "2023-08-22 03:02:55", "lastmod": "2023-10-23 23:31:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The QUaD Galactic Plane Survey. II. A Compact Source Catalog", "ispublished": "pub", "full_text_status": "public", "keywords": "Galaxy: center; Galaxy: structure; H II regions; radio continuum: ISM; stars: formation; surveys", "note": "\u00a9 2011 The American Astronomical Society. Received 2010 May 20; accepted 2011 May 20; published 2011 June 29. \nThis paper is dedicated to the memory of Andrew Lange, who gave wisdom and guidance to so many members of the astrophysics and cosmology community. His presence is sorely missed. We thank our colleagues on the BICEP experiment for useful discussions. QUaD is funded by the National Science Foundation in the USA, through grants ANT-0338138, ANT-0338335, and ANT-0338238, by the Science and Technology Facilities Council (STFC) in the UK, and by the Science Foundation Ireland. We thank the staff of the Amundsen- Scott South Pole Station and all involved in the United States Antarctic Program for the superb support operation which makes the science presented here possible. Special thanks go to our intrepid winter scientist Robert Schwarz who spent three consecutive winter seasons tending the QUaD experiment. The BOOMERanG collaboration kindly allowed the use of their CMB maps for our calibration purposes. M.L.B. acknowledges the award of a PPARC Fellowship. S.E.C. acknowledges support from a Stanford Terman Fellowship. J.R.H. acknowledges the support of an NSF Graduate Research Fellowship and a Stanford Graduate Fellowship. C.P. acknowledges partial support from the Kavli Institute for Cosmological Physics through the grant NSF PHY-0114422. E.Y.W. acknowledges receipt of an NDSEG fellowship. J.M.K. acknowledges support from a John B. and Nelly L. Kilroy Foundation Fellowship.\n\nPublished - Culverhouse2011p15393Astrophys_J_Suppl_S.pdf
", "abstract": "We present a catalog of compact sources derived from the QUaD Galactic Plane Survey. The survey covers ~800 deg^2 of the inner galaxy (|b| < 4\u00b0) in Stokes I, Q, and U parameters at 100 and 150 GHz, with angular resolutions of 5 and 3.5 arcmin, respectively. Five hundred and twenty-six unique sources are identified in I, of which 239 are spatially matched between frequency bands, with 53 (234) detected at 100 (150) GHz alone; 170 sources are identified as ultracompact H II regions. Approximating the distribution of total intensity source fluxes as a power law, we find a slope of \u03b3_(S,100) = \u20131.8 \u00b1 0.4 at 100 GHz and \u03b3_(S,150) = \u20132.2 \u00b1 0.4 at 150 GHz. Similarly, the power-law index of the source two-point angular correlation function is \u03b3_(\u03b8,100) = \u20131.21 \u00b1 0.04 and \u03b3_(\u03b8,150) = \u20131.25 \u00b1 0.04. The total intensity spectral index distribution peaks at \u03b1_I ~ 0.25, indicating that dust emission is not the only source of radiation produced by these objects between 100 and 150 GHz; free-free radiation is likely significant in the 100 GHz band. Four sources are detected in polarized intensity P, of which three have matching counterparts in I. Three of the polarized sources lie close to the Galactic center, Sagittarius A^*, Sagittarius B2, and the Galactic Radio Arc, while the fourth is RCW 49, a bright H II region. An extended polarized source, undetected by the source extraction algorithm on account of its ~0\u00b05 size, is identified visually, and is an isolated example of large-scale polarized emission oriented distinctly from the bulk Galactic dust polarization.", "date": "2011-07", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "195", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 8", "id_number": "CaltechAUTHORS:20110802-081904943", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110802-081904943", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Science and Technology Facilities Council (STFC) (UK)" }, { "agency": "Science Foundation Ireland" }, { "agency": "PPARC Fellowship" }, { "agency": "Stanford Terman Fellowship" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Stanford Graduate Fellowship" }, { "agency": "Kavli Institute for Cosmological Physics", "grant_number": "NSF PHY-0114422" }, { "agency": "NDSEG Fellowship" }, { "agency": "John B. and Nelly L. Kilroy Foundation Fellowship" } ] }, "corp_creators": { "items": [ "QUaD Collaboration" ] }, "doi": "10.1088/0067-0049/195/1/8", "primary_object": { "basename": "Culverhouse2011p15393Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/5jw5c-hwh19/files/Culverhouse2011p15393Astrophys_J_Suppl_S.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Culverhouse, T.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/ehn5n-5ga96", "eprint_id": 25131, "eprint_status": "archive", "datestamp": "2023-08-22 02:55:27", "lastmod": "2023-10-24 15:38:55", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Burgarella-D", "name": { "family": "Burgarella", "given": "D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } } ] }, "title": "HerMES: Lyman Break Galaxies Individually Detected at 0.7 \u2264 z \u2264 2.0 in GOODS-N with Herschel/SPIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: high-redshift; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2011 January 31; accepted 2011 April 28; published 2011 May 19.\n\nSPIRE has been developed by a consortium of institutes\nled by Cardiff University (UK) and including University\nof Lethbridge (Canada); NAOC (China); CEA, OAMP\n(France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); and Caltech/ JPL, IPAC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM; http://hedam.oamp.fr/HerMES). This work makes use of TOPCAT \n(http://www.star.bristol.ac.uk/\u223cmbt/topcat/).\n\nPublished - Burgarella2011p15634Astrophys_J_Lett.pdf
", "abstract": "As part of the Herschel Multi-tiered Extragalactic Survey we have investigated the rest-frame far-infrared (FIR) properties of a sample of more than 4800 Lyman break galaxies (LBGs) in the Great Observatories Origins Deep Survey North field. Most LBGs are not detected individually, but we do detect a sub-sample of 12 objects at 0.7 < z < 1.6 and one object at z = 2.0. The ones detected by Herschel SPIRE have redder observed NUV \u2013 U and U \u2013 R colors than the others, while the undetected ones have colors consistent with average LBGs at z > 2.5. The UV-to-FIR spectral energy distributions of the objects detected in the rest-frame FIR are investigated using the code CIGALE to estimate physical parameters. We find that LBGs detected by SPIRE are high-mass, luminous infrared galaxies. It appears that LBGs are located in a triangle-shaped region in the A_(FUV) versus log L_(FUV) = 0 diagram limited by A_(FUV) = 0 at the bottom and by a diagonal following the temporal evolution of the most massive galaxies from the bottom right to the top left of the diagram. This upper envelop can be used as upper limits for the UV dust attenuation as a function of L_(FUV). The limits of this region are well explained using a closed-box model, where the chemical evolution of galaxies produces metals, which in turn lead to higher dust attenuation when the galaxies age.", "date": "2011-06-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "734", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L12", "id_number": "CaltechAUTHORS:20110826-141031886", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110826-141031886", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/2041-8205/734/1/L12", "primary_object": { "basename": "Burgarella2011p15634Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/ehn5n-5ga96/files/Burgarella2011p15634Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Burgarella, D.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/5yh3k-gh157", "eprint_id": 24446, "eprint_status": "archive", "datestamp": "2023-08-22 02:49:33", "lastmod": "2023-10-23 22:43:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wang-L", "name": { "family": "Wang", "given": "L." }, "orcid": "0000-0002-9803-166X" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "HerMES: detection of cosmic magnification of submillimetre galaxies using angular cross-correlation", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical; cosmology: observations; large-scale structure of Universe; infrared: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2011 January 25. Received 2011 January 24; in original form 2010 August 16. \nArticle first published online: 25 Mar. 2011.\nHerschel is a European Space Agency (ESA) space observatory with science instruments provided by European-led Principle Investigator consortia and with\nimportant participation from NASA.\n\nLWis supported by UK's Science and Technology Facilities Council\ngrant ST/F002858/1. LW thanks Antony Lewis for helpful\ndiscussions. We thank the GAMA team for providing the redshift\ndistribution of F1. The data presented in this paper will\nbe released through the Herschel database in Marseille HeDaM\n(hedam.oamp.fr/herMES). SPIRE has been developed by a consortium\nof institutes led by Cardiff University (UK) and including\nUniversity of Lethbridge (Canada), NAOC (China), CEA,\nLAM (France), IFSI, University of Padua (Italy), IAC (Spain),\nStockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA).\n\nPublished - Wang2011p14798Mon_Not_R_Astron_Soc.pdf
", "abstract": "Cosmic magnification is due to the weak gravitational lensing of sources in the distant Universe by foreground large-scale structure leading to coherent changes in the observed number density of the background sources. Depending on the slope of the background source number counts, cosmic magnification causes a correlation between the background and foreground galaxies, which is unexpected in the absence of lensing if the two populations are spatially disjoint. Previous attempts using submillimetre (submm) sources have been hampered by small number statistics. The large number of sources detected in the Herschel Multi-tiered Extra-galactic Survey (HerMES) Lockman-Spitzer Wide-area Infrared Extragalactic (SWIRE) field enables us to carry out the first robust study of the cross-correlation between submm sources and sources at lower redshifts. Using ancillary data, we compile two low-redshift samples from Sloan Digital Sky Survey (SDSS) and SWIRE with \u3008z\u3009\u223c 0.2 and 0.4, respectively, and cross-correlate with two submm samples based on flux density and colour criteria, selecting galaxies preferentially at z\u223c 2. We detect cross-correlation on angular scales between \u223c1 and 50 arcmin and find clear evidence that this is primarily due to cosmic magnification. A small, but non-negligible signal from intrinsic clustering is likely to be present due to the tails of the redshift distribution of the submm sources overlapping with those of the foreground samples.", "date": "2011-06", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "414", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "596-601", "id_number": "CaltechAUTHORS:20110718-105400386", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110718-105400386", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2011.18417.x", "primary_object": { "basename": "Wang2011p14798Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/5yh3k-gh157/files/Wang2011p14798Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Wang, L.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/x5c59-xw044", "eprint_id": 23980, "eprint_status": "archive", "datestamp": "2023-08-22 02:47:12", "lastmod": "2023-10-23 20:12:48", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Omont-A", "name": { "family": "Omont", "given": "A." }, "orcid": "0000-0002-4721-3922" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Observation of H_2O in a strongly lensed Herschel-ATLAS source at z = 2.3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; galaxies: active; infrared: galaxies; submillimeter: galaxies; radio lines: galaxies", "note": "\u00a9 2011 ESO. Received 18 March 2011. Accepted 11 April 2011. Published online 28 April 2011. \nHerschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA.\n\nBased on observations carried out with the IRAM Plateau de Bure interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The authors are grateful to the IRAM staff for\ntheir support. US participants in H-ATLAS acknowledge support from NASA through a contract from JPL. Italian participants in H-ATLAS acknowledge a financial contribution from the agreement ASI-INAF I/009/10/0. The SPIRE development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).We also thank the anonymous\nreferee for very helpful suggestions.\n\nPublished - Omont2011p14098Astron_Astrophys.pdf
", "abstract": "The Herschel survey, H-ATLAS, with its large areal coverage, has recently discovered a number of bright, strongly lensed high-z submillimeter galaxies. The strong magnification makes it possible to study molecular species other than CO, which are otherwise difficult to observe in high-z galaxies. Among the lensed galaxies already identified by H-ATLAS, the source J090302.9-014127B (SDP.17b) at z = 2.305 is remarkable because of its excitation conditions and a tentative detection of the H_2O 2_(02)-1_(11) emission line (Lupu et al. 2010, ApJ, submitted). We report observations of this line in SDP.17b using the IRAM interferometer equipped with its new 277\u2013371\u2009GHz receivers. The H_2O line is detected at a redshift of z = 2.3049 \u00b1 0.0006, with a flux of 7.8 \u00b1 0.5 Jy km s^(-1) and a FWHM of 250 \u00b1 60 \u2009 km \u2009 s^(-1). The new flux is 2.4 times weaker than the previous tentative detection, although both remain marginally consistent within 1.6\u03c3. The intrinsic line luminosity and ratio of H_2O(2_(02) \u2212 1_(11))/CO(8 \u2212 7) are comparable with those of the nearby starburst/enshrouded-AGN Mrk 231, and the ratio I(H_2O)/L_(FIR) is even higher, suggesting that SDP.17b could also host a luminous AGN. The detection of a strong H_2O 2_(02) \u2212 1_(11) line in SDP.17b implies an efficient excitation mechanism of the water levels that must occur in very dense and warm interstellar gas probably similar to Mrk 231.", "date": "2011-06", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "530", "publisher": "EDP Sciences", "pagerange": "Art. No. L3", "id_number": "CaltechAUTHORS:20110613-083728464", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110613-083728464", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max Planck Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "NASA/JPL" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/009/10/0" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "doi": "10.1051/0004-6361/201116921", "primary_object": { "basename": "Omont2011p14098Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/x5c59-xw044/files/Omont2011p14098Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Omont, A.; Murphy, E. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/ypne8-sxa15", "eprint_id": 25206, "eprint_status": "archive", "datestamp": "2023-08-22 02:45:37", "lastmod": "2023-10-24 15:41:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "Dominik A." }, "orcid": "0000-0001-9585-1462" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "J. M." }, "orcid": "0000-0003-2251-0602" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "Dynamical Structure of the Molecular Interstellar Medium in an Extremely Bright, Multiply Lensed z \u2243 3 Submillimeter Galaxy Discovered with Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; galaxies: formation; galaxies: high-redshift; galaxies: starburst; radio lines: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 February 18; accepted 2011 April 14; published 2011 May 3. We thank the referee for a detailed and helpful report. D.R.\nacknowledges support from NASA through Hubble Fellowship\ngrant HST-HF-51235.01 awarded by STScI, operated by AURA\nfor NASA, under contract NAS 5-26555. A.J.B. acknowledges\nsupport from NSF grant AST-0708653 to Rutgers University.\nIRAMis supported by INSU/CNRS(France),MPG (Germany),\nand IGN (Spain). Support for CARMA construction was derived\nfrom the Moore and Norris Foundations, the Associates of Caltech, the states of California, Illinois, and Maryland, and the NSF. Ongoing CARMA development and operations are supported by the NSF under a cooperative agreement, and by the CARMA partner universities. The National Radio Astronomy\nObservatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.\n\nPublished - Riechers2011p15622Astrophys_J_Lett.pdf
", "abstract": "We report the detection of CO(J = 5 \u2192 4), CO(J = 3 \u2192 2), and CO(J = 1 \u2192 0) emission in the strongly lensed, Herschel/SPIRE-selected submillimeter galaxy (SMG) HERMES J105751.1+573027 at z = 2.9574 \u00b1 0.0001, using the Plateau de Bure Interferometer, the Combined Array for Research in Millimeter-wave Astronomy, and the Green Bank Telescope. The observations spatially resolve the molecular gas into four lensed images with a maximum separation of ~9\" and reveal the internal gas dynamics in this system. We derive lensing-corrected CO line luminosities of L'_(CO(1-0)) = (4.17 \u00b1 0.41), L'_(CO(3-2)) = (3.96 \u00b1 0.20), and L'_(CO(5-4)) = (3.45 \u00b1 0.20) \u00d7 10^(10) (\u03bcL/10.9)^(\u20131) K km s^(\u20131) pc^2, corresponding to luminosity ratios of r_(31) = 0.95 \u00b1 0.10, r_(53) = 0.87 \u00b1 0.06, and r_(51) = 0.83 \u00b1 0.09. This suggests a total molecular gas mass of M_(gas) = 3.3\u00d710^(10) (\u03b1_(CO)/0.8) (\u03bc_L/10.9)^(\u20131) M_\u2609. The gas mass, gas mass fraction, gas depletion timescale, star formation efficiency, and specific star formation rate are typical for an SMG. The velocity structure of the gas reservoir suggests that the brightest two lensed images are dynamically resolved projections of the same dust-obscured region in the galaxy that are kinematically offset from the unresolved fainter images. The resolved kinematics appear consistent with the complex velocity structure observed in major, \"wet\" (i.e., gas-rich) mergers. Major mergers are commonly observed in SMGs and are likely to be responsible for fueling their intense starbursts at high gas consumption rates. This study demonstrates the level of detail to which galaxies in the early universe can be studied by utilizing the increase in effective spatial resolution and sensitivity provided by gravitational lensing.", "date": "2011-05-20", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "733", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. L12", "id_number": "CaltechAUTHORS:20110902-091027758", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110902-091027758", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Hubble Fellowship", "grant_number": "HST-HF-51235.01" }, { "agency": "NASA", "grant_number": "NAS 5-26555" }, { "agency": "NSF", "grant_number": "AST-0708653" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "Associates of the California Institute of Technology" }, { "agency": "States of California, Illinois, and Maryland" }, { "agency": "NSF" }, { "agency": "CARMA partner universities" }, { "agency": "Associated Universities, Inc." } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/2041-8205/733/1/L12", "primary_object": { "basename": "Riechers2011p15622Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/ypne8-sxa15/files/Riechers2011p15622Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Riechers, Dominik A.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/qz1tt-9kp38", "eprint_id": 23842, "eprint_status": "archive", "datestamp": "2023-08-22 02:45:04", "lastmod": "2023-10-23 20:04:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "J. M." }, "orcid": "0000-0003-2251-0602" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Redshift Determination and CO Line Excitation Modeling for the Multiply Lensed Galaxy HLSW-01", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: individual (HERMES J105751.1+573027); galaxies: starburst; submillimeter: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 February 14; accepted 2011 March 14; published 2011 April 29. We thank the anonymous referees for their suggestions,\nwhich improved the presentation of these results. We also thank the staff at CSO for support of the Z-Spec observations, and we appreciate the help of Robert Hanni and Jon Rodriguez with observing. J.E.A. acknowledges support by NSF grant AST-0807990 and by the CSO NSF Cooperative Agreement AST-0838261. J.K. acknowledges funding through an NSF graduate research fellowship. A.J.B. acknowledges support from NSF grant AST-0708653. Z-spec was constructed under NASA SARA grants NAGS-11911 and NAGS-12788 and an NSF Career grant (AST-0239270) and a Research Corporation Award (RI0928) to J.G., in collaboration with the Jet Propulsion Laboratory, California Institute of Technology, under a contract\nwith the National Aeronautics and Space Administration. We\nacknowledge Peter Ade and his group for their filters and Lionel Duband for the 3He/4He refrigerator in Z-Spec, and are grateful for their help in the early integration of the instrument. \nFacilities: CSO (Z-Spec), GBT (Zpectrometer), IRAM:\nInterferometer (PdBI), CARMA, SMA, Herschel (SPIRE)\n\nPublished - Scott2011p13973Astrophys_J.pdf
", "abstract": "We report on the redshift measurement and CO line excitation of HERMES J105751.1+573027 (HLSW-01), a strongly lensed submillimeter galaxy discovered in Herschel/SPIRE observations as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). HLSW-01 is an ultra-luminous galaxy with an intrinsic far-infrared luminosity of L _(FIR) = 1.4 \u00d7 10^(13) L _\u2299, and is lensed by a massive group of galaxies into at least four images with a total magnification of \u03bc = 10.9 \u00b1 0.7. With the 100 GHz instantaneous bandwidth of the Z-Spec instrument on the Caltech Submillimeter Observatory, we robustly identify a redshift of z = 2.958 \u00b1 0.007 for this source, using the simultaneous detection of four CO emission lines (J = 7 \u2192 6, J = 8 \u2192 7, J = 9 \u2192 8, and J = 10 \u2192 9). Combining the measured line fluxes for these high-J transitions with the J = 1 \u2192 0, J = 3 \u2192 2, and J = 5 \u2192 4 line fluxes measured with the Green Bank Telescope, the Combined Array for Research in Millimeter Astronomy, and the Plateau de Bure Interferometer, respectively, we model the physical properties of the molecular gas in this galaxy. We find that the full CO spectral line energy distribution is described well by warm, moderate-density gas with T _(kin) = 86-235 K and n_H_2 = (1.1-3.5)x10^3 cm^(\u20133). However, it is possible that the highest-J transitions are tracing a small fraction of very dense gas in molecular cloud cores, and two-component models that include a warm/dense molecular gas phase with T _(kin) ~ 200 K, n_H_2 ~ 10^5 cm^(\u20133) are also consistent with these data. Higher signal-to-noise measurements of the J _(up) \u2265 7 transitions with high spectral resolution, combined with high spatial resolution CO maps, are needed to improve our understanding of the gas excitation, morphology, and dynamics of this interesting high-redshift galaxy.", "date": "2011-05-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "733", "number": "1", "publisher": "American Astronomical Society", "pagerange": "Art. No. 29", "id_number": "CaltechAUTHORS:20110531-132533695", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110531-132533695", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0807990" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NSF", "grant_number": "AST-0708653" }, { "agency": "NASA", "grant_number": "NAGS-11911" }, { "agency": "NASA", "grant_number": "NAGS-12788" }, { "agency": "NSF", "grant_number": "AST-0239270" }, { "agency": "Research Corporation", "grant_number": "RI0928" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/733/1/29", "primary_object": { "basename": "Scott2011p13973Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/qz1tt-9kp38/files/Scott2011p13973Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Scott, K. S.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/2qa3f-jy958", "eprint_id": 25003, "eprint_status": "archive", "datestamp": "2023-08-22 02:44:24", "lastmod": "2023-10-24 15:32:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Conley-A", "name": { "family": "Conley", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Carpenter-J-M", "name": { "family": "Carpenter", "given": "J. M." }, "orcid": "0000-0003-2251-0602" }, { "id": "Djorgovski-S-G", "name": { "family": "Djorgovski", "given": "S. G." }, "orcid": "0000-0002-0603-3087" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Fu-Hai", "name": { "family": "Fu", "given": "H." }, "orcid": "0000-0001-9608-6395" }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Mahabal-A-A", "name": { "family": "Mahabal", "given": "A." }, "orcid": "0000-0003-2242-0244" }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E." }, "orcid": "0000-0001-7089-7325" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Riechers-D-A", "name": { "family": "Riechers", "given": "D." }, "orcid": "0000-0001-9585-1462" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Discovery of a Multiply Lensed Submillimeter Galaxy in Early HerMES Herschel/SPIRE Data", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; gravitational lensing: strong; submillimeter: galaxies", "note": "\u00a9 2011 The American Astronomical Society. Received 2011 February 1; accepted 2011 April 8; published 2011 April 21. \nHerschel is an ESA space observatory with science instruments provided by European-led principal Investigator consortia and with important participation from NASA. \n\nSPIRE has been developed by a consortium of institutes led\nby Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI,\nUniversity of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN\n(Spain); SNSB (Sweden); STFC (UK); and NASA (USA). The\nSubmillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics. The IRAM Plateau de Bure Interferometer is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National\nScience Foundation. Ongoing CARMA development and operations\nare supported by NSF grant ATI-0838178 to CARMA, and by the CARMA partner universities. The authors thank Elisabete\nda Cunha for running her models for us. The Herschel data\npresented in this Letter will be released through the Herschel Database in Marseille, HeDaM.\nFacilities: Herschel (SPIRE), CSO (Z-Spec), Subaru\n(SuprimeCam), SMA, Hale (SWIFT), Keck:II (NIRC2),\nIRAM:Interferometer, ING:Newton (WFC), Spitzer (IRAC; MIPS), CARMA, VLA, GBT (Zpectrometer)\n\nPublished - Conley2011p15553Astrophys_J_Lett.pdf
", "abstract": "We report the discovery of a bright (f(250 \u03bcm)>400 mJy), multiply lensed submillimeter galaxy HERMES J105751.1+573027 in Herschel/SPIRE Science Demonstration Phase data from the HerMES project. Interferometric 880 \u03bcm Submillimeter Array observations resolve at least four images with a large separation of ~9\". A high-resolution adaptive optics K_p image with Keck/NIRC2 clearly shows strong lensing arcs. Follow-up spectroscopy gives a redshift of z = 2.9575, and the lensing model gives a total magnification of \u03bc ~ 11 \u00b1 1. The large image separation allows us to study the multi-wavelength spectral energy distribution (SED) of the lensed source unobscured by the central lensing mass. The far-IR/millimeter-wave SED is well described by a modified blackbody fit with an unusually warm dust temperature, 88 \u00b1 3 K. We derive a lensing-corrected total IR luminosity of (1.43 \u00b1 0.09) \u00d7 10^(13) L_\u2609, implying a star formation rate of ~2500 M_\u2609 yr^(\u20131). However, models primarily developed from brighter galaxies selected at longer wavelengths are a poor fit to the full optical-to-millimeter SED. A number of other strongly lensed systems have already been discovered in early Herschel data, and many more are expected as additional data are collected.", "date": "2011-05-10", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "732", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. L35", "id_number": "CaltechAUTHORS:20110824-083050070", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110824-083050070", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Institut national des sciences de l'Univers (INSU)" }, { "agency": "Max-Planck-Gesellschaft" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "Gordon and Betty Moore Foundation" }, { "agency": "Kenneth T. and Eileen L. Norris Foundation" }, { "agency": "James S. McDonnell Foundation" }, { "agency": "Associates of the California Institute of Technology" }, { "agency": "States of California" }, { "agency": "State of Illinois" }, { "agency": "State of Maryland" }, { "agency": "NSF", "grant_number": "ATI-0838178" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/2041-8205/732/2/L35", "primary_object": { "basename": "Conley2011p15553Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/2qa3f-jy958/files/Conley2011p15553Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Conley, A.; Cooray, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/k5qvx-3ng62", "eprint_id": 23845, "eprint_status": "archive", "datestamp": "2023-08-22 02:40:05", "lastmod": "2023-10-23 20:04:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Seymour-N", "name": { "family": "Seymour", "given": "N." }, "orcid": "0000-0003-3506-5536" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: SPIRE emission from radio-selected active galactic nuclei", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; infrared: galaxies; radio continuum: galaxies", "note": "\u00a9 2011 The Authors. Monthly Notices of the Royal Astronomical Society \u00a9 2011 RAS. Accepted 2010 December 21. Received 2010 December 21; in original form 2010 September 24. Article first published online: 7 Mar 2011. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation\nfrom NASA.\nNS thanks Carlos De Breuck, Martin Hardcastle, Curtis Saxton and Clive Tadhunter for useful discussions. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies:\nCSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI\n(Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA\n(USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM hedam.oamp.fr/HerMES).\n\nPublished - Seymour2011p13960Mon_Not_R_Astron_Soc.pdf
", "abstract": "We examine the rest-frame far-infrared emission from powerful radio sources with 1.4-GHz luminosity densities of\u200225 \u2264 log(L_(1.4)/W Hz^(\u22121)) \u2264 26.5\u2002in the extragalactic\u2002Spitzer\u2002First Look Survey field. We combine\u2002Herschel/SPIRE flux densities with\u2002Spitzer/Infrared Array Camera and Multiband Imaging Photometer for\u2002Spitzer\u2002infrared data to obtain total (8-1000 \u00b5m) infrared luminosities for these radio sources. We separate our sources into a moderate,\u20020.4 <\u2002z\u2002< 0.9, and a high,\u20021.2 <\u2002z\u2002< 3.0, redshift sub-sample and we use\u2002Spitzer\u2002observations of a\u2002z\u2002< 0.1\u20023CRR sample as a local comparison. By comparison to numbers from the Square Kilometre Array (SKA) Simulated Skies, we find that our moderate-redshift sample is complete and our high-redshift sample is 14 per cent complete. We constrain the ranges of mean star formation rates (SFRs) to be 3.4\u20134.2, 18\u201341 and\u200280\u2013581 M_\u2299 yr^(\u22121)\u2002for the local, moderate- and high-redshift samples, respectively. Hence, we observe an increase in the mean SFR with increasing redshift which we can parametrize as\u2002\u223c(1 +\u2002z)^Q, where\u2002Q\u2002= 4.2 \u00b1 0.8. However, we observe no trends of mean SFR with radio luminosity within the moderate- or high-redshift bins. We estimate that radio-loud active galactic nuclei (AGN) in the high-redshift sample contribute 0.1\u20130.5 per cent to the total SFR density at that epoch. Hence, if all luminous starbursts host radio-loud AGN we infer a radio-loud phase duty cycle of 0.001\u20130.005.", "date": "2011-05", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "413", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1777-1786", "id_number": "CaltechAUTHORS:20110531-151240573", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110531-151240573", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2011.18253.x", "primary_object": { "basename": "Seymour2011p13960Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/k5qvx-3ng62/files/Seymour2011p13960Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Seymour, N.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/xs07x-yvw50", "eprint_id": 23715, "eprint_status": "archive", "datestamp": "2023-08-22 02:33:20", "lastmod": "2023-10-23 19:53:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kamenetzky-J", "name": { "family": "Kamenetzky", "given": "J." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Maloney-P-R", "name": { "family": "Maloney", "given": "P. R." } }, { "id": "Aguirre-J-E", "name": { "family": "Aguirre", "given": "J. E." }, "orcid": "0000-0002-4810-666X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Earle-L", "name": { "family": "Earle", "given": "L." } }, { "id": "Inami-Hanae", "name": { "family": "Inami", "given": "H." }, "orcid": "0000-0003-4268-0393" }, { "id": "Matsuhara-Hideo", "name": { "family": "Matsuhara", "given": "H." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Naylor-B-J", "name": { "family": "Naylor", "given": "B. J." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "The Dense Molecular Gas in the Circumnuclear Disk of NGC 1068", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 1068); galaxies: ISM; galaxies: Seyfert; ISM: molecules", "note": "\u00a9 2011 American Astronomical Society.\n\nReceived 2010 October 12; accepted 2011 February 17; published 2011 March 25.\n\nWe thank the anonymous referee for a thorough and constructive report, and we also express our gratitude to the staff at the Caltech Submillimeter Observatory. We acknowledge the following grants and fellowships in support of this work: NASA SARA grants NAGS-11911 and NAGS-12788, an NSF Career grant AST-0239270, and a Research Corporation Award RI0928 to J.G.; a Caltech Millikan fellowship and JPL Director's fellowship to C.M.B.; an NRAO Jansky fellowship and NSF grant AST-087990 to J.E.A.; a NASA GSRP fellowship to L.E.; and an NSF GRFP fellowship to J.K.\n\nPublished - Kamenetzky2011p13855Astrophys_J.pdf
", "abstract": "We present a 190-307 GHz broadband spectrum obtained with Z-Spec of NGC 1068 with new measurements of molecular rotational transitions. After combining our measurements with those previously published and considering the specific geometry of this Seyfert 2 galaxy, we conduct a multi-species Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+. We find that these molecules trace warm (T>100 K) gas of H_2 number densities 10^(4.2)-10^(4.9) cm^(\u20133). Our models also place strong constraints on the column densities and relative abundances of these molecules, as well as on the total mass in the circumnuclear disk. Using the uniform calibration afforded by the broad Z-Spec bandpass, we compare our line ratios to X-ray-dominated region (XDR) and photon-dominated region models. The majority of our line ratios are consistent with the XDR models at the densities indicated by the likelihood analysis, lending substantial support to the emerging interpretation that the energetics in the circumnuclear disk of NGC 1068 are dominated by accretion onto an active galactic nucleus.", "date": "2011-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "731", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 83", "id_number": "CaltechAUTHORS:20110518-111113979", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110518-111113979", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAGS-11911" }, { "agency": "NASA", "grant_number": "NAGS-12788" }, { "agency": "NSF", "grant_number": "AST-0239270" }, { "agency": "Research Corporation", "grant_number": "RI0928" }, { "agency": "Caltech Millikan Fellowship" }, { "agency": "JPL Director's Fellowship" }, { "agency": "NRAO Jansky Fellowship" }, { "agency": "NSF", "grant_number": "AST-087990" }, { "agency": "NASA Graduate Student Research Fellowship" } ] }, "doi": "10.1088/0004-637X/731/2/83", "primary_object": { "basename": "Kamenetzky2011p13855Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/xs07x-yvw50/files/Kamenetzky2011p13855Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Kamenetzky, J.; Glenn, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/qem3p-wg473", "eprint_id": 23390, "eprint_status": "archive", "datestamp": "2023-08-19 06:07:59", "lastmod": "2023-10-23 19:03:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roy-A", "name": { "family": "Roy", "given": "Arabindo" }, "orcid": "0000-0001-8127-5775" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } } ] }, "title": "Deconvolution of Images from BLAST 2005: Insight into the K3-50 and IC 5146 Star-forming Regions", "ispublished": "pub", "full_text_status": "public", "keywords": "stars: formation \u2013 submillimeter: general \u2013 techniques: image processing", "note": "\u00a9 2011 American Astronomical Society. Received 2010 October 22; accepted 2011 February 2; published 2011 March 15. The BLAST collaboration acknowledges the support of\nNASA through grant numbers NAG5-12785, NAG5-13301, and\nNNGO-6GI11G, the Canadian Space Agency (CSA), the UK\nParticle Physics & Astronomy Research Council (PPARC), and\nCanada's Natural Sciences and Engineering Research Council (NSERC). We also thank the Columbia Scientific Balloon\nFacility (CSBF) staff for their outstanding work.\n\nPublished - Roy2011p13406Astrophys_J.pdf
", "abstract": "We present an implementation of the iterative flux-conserving Lucy-Richardson (L-R) deconvolution method of image restoration for maps produced by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST). Compared to the direct Fourier transform method of deconvolution, the L-R operation restores images with better-controlled background noise and increases source detectability. Intermediate iterated images are useful for studying extended diffuse structures, while the later iterations truly enhance point sources to near the designed diffraction limit of the telescope. The L-R method of deconvolution is efficient in resolving compact sources in crowded regions while simultaneously conserving their respective flux densities. We have analyzed its performance and convergence extensively through simulations and cross-correlations of the deconvolved images with available high-resolution maps. We present new science results from two BLAST surveys, in the Galactic regions K3-50 and IC 5146, further demonstrating the benefits of performing this deconvolution. We have resolved three clumps within a radius of 4'.5 inside the star-forming molecular cloud containing K3-50. Combining the well-resolved dust emission map with available multi-wavelength data, we have constrained the spectral energy distributions (SEDs) of five clumps to obtain masses (M), bolometric luminosities (L), and dust temperatures (T). The L-M diagram has been used as a diagnostic tool to estimate the evolutionary stages of the clumps. There are close relationships between dust continuum emission and both 21 cm radio continuum and ^(12)CO molecular line emission. The restored extended large-scale structures in the Northern Streamer of IC 5146 have a strong spatial correlation with both SCUBA and high-resolution extinction images. A dust temperature of 12 K has been obtained for the central filament. We report physical properties of ten compact sources, including six associated protostars, by fitting SEDs to multi-wavelength data. All of these compact sources are still quite cold (typical temperature below ~ 16 K) and are above the critical Bonner-Ebert mass. They have associated low-power young stellar objects. Further evidence for starless clumps has also been found in the IC 5146 region.", "date": "2011-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "730", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 142", "id_number": "CaltechAUTHORS:20110420-092300527", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110420-092300527", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC) (UK)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "doi": "10.1088/0004-637X/730/2/142", "primary_object": { "basename": "Roy2011p13406Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/qem3p-wg473/files/Roy2011p13406Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Roy, Arabindo; Bock, James J.; et el." }, { "id": "https://authors.library.caltech.edu/records/gv0gy-paj42", "eprint_id": 22845, "eprint_status": "archive", "datestamp": "2023-08-19 05:39:00", "lastmod": "2023-10-23 17:15:31", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Amblard-A", "name": { "family": "Amblard", "given": "Alexandre" } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Submillimetre galaxies reside in dark matter haloes with masses greater than 3\u2009\u00d7\u200910^(11) solar masses", "ispublished": "pub", "full_text_status": "public", "keywords": "Astronomy", "note": "\u00a9 2011 Macmillan Publishers Limited. \n\nReceived 11 August; accepted 20 December 2010. Published online 16 February 2011. \n\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including the University of Lethbridge (Canada); NAOC (China); CEA and LAM (France); IFSI and the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC and the University of Sussex (UK); and Caltech/JPL, IPAC and the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES and CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). We thank M. Viero for comments. A.A., A. Cooray, P.S., A.A.K., K.M.-W. and other US co-authors are supported by NASA funds for US participants in Herschel through an award from JPL. \n\nAuthor Contributions: This paper represents the combined work of the HerMES collaboration, the SPIRE Instrument Team's Extragalactic Survey, and has been extensively internally reviewed. A. Cooray planned the study, supervised the research work of A.A. and P.S., and wrote the draft version of this paper. A.A. performed the power spectrum measurements and P.S. interpreted those measurements with the halo model. All other co-authors of this paper contributed extensively and equally by their varied contributions to the SPIRE instrument, Herschel mission, analysis of SPIRE and HerMES data, planning of HerMES observations and scientific support of HerMES, and by commenting on this manuscript as part of an internal review process.\n\nSupplemental Material - nature09771-s1.pdf
", "abstract": "The extragalactic background light at far-infrared wavelengths comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year. These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations. A previous attempt at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model. Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum\nof brightness fluctuations at 250, 350 and 500 \u00b5m. From this excess, we find that submillimetre galaxies are located in darkmatter haloes with a minimum mass, M_(min), such that log_(10)[M_(min)/M_\u2299] = 11.5^(+0.7)_(-0.2) at 350 \u00b5m, where M_\u2299 is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analytical models for galaxy formation.", "date": "2011-02-24", "date_type": "published", "publication": "Nature", "volume": "470", "number": "7335", "publisher": "Nature Publishing Group", "pagerange": "510-512", "id_number": "CaltechAUTHORS:20110314-094552984", "issn": "0028-0836", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110314-094552984", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1038/nature09771", "primary_object": { "basename": "nature09771-s1.pdf", "url": "https://authors.library.caltech.edu/records/gv0gy-paj42/files/nature09771-s1.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Amblard, Alexandre; Cooray, Asantha; et el." }, { "id": "https://authors.library.caltech.edu/records/tjkhy-2xg65", "eprint_id": 22812, "eprint_status": "archive", "datestamp": "2023-08-22 02:02:49", "lastmod": "2023-10-23 17:13:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roy-A", "name": { "family": "Roy", "given": "Arabindo" }, "orcid": "0000-0001-8127-5775" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Noriega-Crespo-A", "name": { "family": "Noriega-Crespo", "given": "Alberto" }, "orcid": "0000-0002-6296-8960" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } } ] }, "title": "The Balloon-Borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 10 deg^2 Survey of Star Formation in Cygnus X", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; ISM: clouds; stars: formation; stars: massive; submillimeter: general", "note": "\u00a9 2011 American Astronomical Society. Received 2010 September 10; accepted 2010 November 18; published 2011 January 11. The BLAST collaboration acknowledges the support of\nNASA through grant numbers NAG5-12785, NAG5-13301, and\nNNGO-6GI11G, the Canadian Space Agency (CSA), the UK\nParticle Physics & Astronomy Research Council (PPARC), and\nCanada's Natural Sciences and Engineering Research Council\n(NSERC). We would also thank the Columbia Scientific Balloon\nFacility (CSBF) staff for their outstanding work.\n\nPublished - Roy2011p12851Astrophys_J.pdf
", "abstract": "We present Cygnus X in a new multi-wavelength perspective based on an unbiased BLAST survey at 250, 350, and 500 \u03bcm, combined with rich data sets for this well-studied region. Our primary goal is to investigate the early stages of high-mass star formation. We have detected 184 compact sources in various stages of evolution across all three BLAST bands. From their well-constrained spectral energy distributions, we obtain the physical properties mass, surface density, bolometric luminosity, and dust temperature. Some of the bright sources reaching 40 K contain well-known compact H_(II) regions. We relate these to other sources at earlier stages of evolution via the energetics as deduced from their position in the luminosity-mass (L-M) diagram. The BLAST spectral coverage, near the peak of the spectral energy distribution of the dust, reveals fainter sources too cool (~10 K) to be seen by earlier shorter-wavelength surveys like IRAS. We detect thermal emission from infrared dark clouds and investigate the phenomenon of cold \"starless cores\" more generally. Spitzer images of these cold sources often show stellar nurseries, but these potential sites for massive star formation are \"starless\" in the sense that to date there is no massive protostar in a vigorous accretion phase. We discuss evolution in the context of the L-M diagram. Theory raises some interesting possibilities: some cold massive compact sources might never form a cluster containing massive stars, and clusters with massive stars might not have an identifiable compact cold massive precursor.", "date": "2011-02-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "727", "number": "2", "publisher": "American Astronomical Society", "pagerange": "Art. No. 114", "id_number": "CaltechAUTHORS:20110310-135511674", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110310-135511674", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC) (UK)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "doi": "10.1088/0004-637X/727/2/114", "primary_object": { "basename": "Roy2011p12851Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/tjkhy-2xg65/files/Roy2011p12851Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2011", "author_list": "Roy, Arabindo; Bock, James J.; et el." }, { "id": "https://authors.library.caltech.edu/records/e495a-5kk14", "eprint_id": 86107, "eprint_status": "archive", "datestamp": "2023-08-22 01:31:14", "lastmod": "2023-10-18 19:15:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Kim-Min-Gyu", "name": { "family": "Kim", "given": "M. G." } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "U. W." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Battle-J", "name": { "family": "Battle", "given": "J." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V." } }, { "id": "Renbarger-T", "name": { "family": "Renbarger", "given": "T." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Sullivan-I", "name": { "family": "Sullivan", "given": "I." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Mason-P", "name": { "family": "Mason", "given": "P." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Kim-G-H", "name": { "family": "Kim", "given": "G. H." } } ] }, "title": "Analysis of Dark Data of the PICNIC IR Arrays in the CIBER", "ispublished": "pub", "full_text_status": "public", "keywords": "instrument-CIBER; analysis-dark current; detector-PICNIC", "note": "\u00a9 2010 The Korean Space Science Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution Non-Commercial License (http://creativecommons.org/licenses/by-nc/3.0/) which permits unrestricted non-commercial use, distribution, and reproduction in any medium, provided the original work is properly cited. \n\nReceived Sep 11, 2010 Revised Oct 19, 2010 Accepted Oct 27, 2010. \n\nThis work was supported by the CIBER project (NASA APRA research grant) and the STSAT-3 MIRIS project of the Ministry of Education, Science and Technology (MEST) of Korea.\n\nPublished - OJOOBS_2010_v27n4_401.pdf
", "abstract": "We have measured and analyzed the dark data of two PICNIC IR arrays (P574 and P560) obtained through the Cosmic Infrared Background ExpeRiment (CIBER). First, we identified three types of bad pixels: the cold, the hot, and the transient, which are figured in total as 0.06% for P574 and 0.19% for P560. Then, after the bad pixels were masked, we determined the dark noise to be 20.5 \u00b1 0.05 e^- and 16.1 \u00b1 0.05 e^-, and the dark current to be 0.6 \u00b1 0.05 e^-/sec and 0.7 \u00b1 0.05 e^-/sec for P574 and P560, respectively. Finally, we discussed glitches and readout modes for a future mission.", "date": "2010-12", "date_type": "published", "publication": "Journal of Astronomy and Space Sciences", "volume": "27", "number": "4", "publisher": "Korean Space Science Society", "pagerange": "401-406", "id_number": "CaltechAUTHORS:20180427-155708301", "issn": "2093-5587", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180427-155708301", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Ministry of Education, Science and Technology (Korea)" } ] }, "doi": "10.5140/JASS.2010.27.4.401", "primary_object": { "basename": "OJOOBS_2010_v27n4_401.pdf", "url": "https://authors.library.caltech.edu/records/e495a-5kk14/files/OJOOBS_2010_v27n4_401.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Lee, D. H.; Kim, M. G.; et el." }, { "id": "https://authors.library.caltech.edu/records/3nfhh-yj671", "eprint_id": 22785, "eprint_status": "archive", "datestamp": "2023-08-22 01:30:06", "lastmod": "2023-10-23 17:12:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Valiante-E", "name": { "family": "Valiante", "given": "Elisabetta" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "BLAST Observations of the South Ecliptic Pole Field: Number Counts and Source Catalogs", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: statistics; methods: data analysis; submillimeter: galaxies", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2010 July 16; accepted 2010 October 15; published 2010 November 15.\n\nBLAST acknowledges the support of NASA through grant\nnumbers NAG5-12785, NAG5-13301, and NNGO-6GI11G, the\nNSF Office of Polar Programs, the Canadian Space Agency, the\nNatural Sciences and Engineering Research Council (NSERC)\nof Canada, and the UK Science and Technology Facilities\nCouncil (STFC). This research has been enabled by the use\nof WestGrid computing resources.\n\nPublished - Valiante2010p12829Astrophys_J_Suppl_S.pdf
", "abstract": "We present results from a survey carried out by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) on a 9 deg^2 field near the South Ecliptic Pole at 250, 350, and 500 \u03bcm. The median 1\u03c3 depths of the maps are 36.0, 26.4, and 18.4 mJy, respectively. We apply a statistical method to estimate submillimeter galaxy number counts and find that they are in agreement with other measurements made with the same instrument and with the more recent results from Herschel/SPIRE. Thanks to the large field observed, the new measurements give additional constraints on the bright end of the counts. We identify 132, 89, and 61 sources with S/N \u22654 at 250, 350, 500 \u03bcm, respectively and provide a multi-wavelength combined catalog of 232 sources with a significance \u22654\u03c3 in at least one BLAST band. The new BLAST maps and catalogs are available publicly at http://blastexperiment.info.", "date": "2010-12", "date_type": "published", "publication": "Astrophysical Journal Supplement Series", "volume": "191", "number": "2", "publisher": "American Astronomical Society", "pagerange": "222-231", "id_number": "CaltechAUTHORS:20110309-164356949", "issn": "0067-0049", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110309-164356949", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "NSF Office of Polar Programs" }, { "agency": "Canadian Space Agency" }, { "agency": "Natural Sciences and Engineering Research Council (NSERC) of Canada" }, { "agency": "UK Science and Technology Facilities Council (STFC)" } ] }, "doi": "10.1088/0067-0049/191/2/222", "primary_object": { "basename": "Valiante2010p12829Astrophys_J_Suppl_S.pdf", "url": "https://authors.library.caltech.edu/records/3nfhh-yj671/files/Valiante2010p12829Astrophys_J_Suppl_S.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Valiante, Elisabetta and Bock, James J." }, { "id": "https://authors.library.caltech.edu/records/t48e0-xhp71", "eprint_id": 101458, "eprint_status": "archive", "datestamp": "2023-08-19 04:22:38", "lastmod": "2023-10-19 22:45:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Negrello-M", "name": { "family": "Negrello", "given": "M." } }, { "name": { "family": "Hopwood", "given": "R." } }, { "name": { "family": "De Zotti", "given": "G." } }, { "name": { "family": "Cooray", "given": "A." } }, { "name": { "family": "Verma", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "name": { "family": "Frayer", "given": "D. T." } }, { "name": { "family": "Gurwell", "given": "M. A." } }, { "name": { "family": "Omont", "given": "A." } }, { "name": { "family": "Neri", "given": "R." } }, { "name": { "family": "Dannerbauer", "given": "H." } }, { "name": { "family": "Leeuw", "given": "L. L." } }, { "name": { "family": "Barton", "given": "E." } }, { "id": "Cooke-J", "name": { "family": "Cooke", "given": "J." }, "orcid": "0000-0001-5703-2108" }, { "name": { "family": "Kim", "given": "S." } }, { "name": { "family": "da Cunha", "given": "E." } }, { "name": { "family": "Rodighiero", "given": "G." } }, { "name": { "family": "Cox", "given": "P." } }, { "name": { "family": "Bonfield", "given": "D. G." } }, { "name": { "family": "Jarvis", "given": "M. J." } }, { "name": { "family": "Serjeant", "given": "S." } }, { "name": { "family": "Ivison", "given": "R. J." } }, { "name": { "family": "Dye", "given": "S." } }, { "name": { "family": "Aretxaga", "given": "I." } }, { "name": { "family": "Hughes", "given": "D. H." } }, { "name": { "family": "Ibar", "given": "E." } }, { "name": { "family": "Bertoldi", "given": "F." } }, { "name": { "family": "Valtchanov", "given": "I." } }, { "name": { "family": "Eales", "given": "S." } }, { "name": { "family": "Dunne", "given": "L." } }, { "name": { "family": "Driver", "given": "S. P." } }, { "name": { "family": "Auld", "given": "R." } }, { "name": { "family": "Buttiglione", "given": "S." } }, { "name": { "family": "Cava", "given": "A." } }, { "name": { "family": "Grady", "given": "C. A." } }, { "name": { "family": "Clements", "given": "D. L." } }, { "name": { "family": "Dariush", "given": "A." } }, { "name": { "family": "Fritz", "given": "J." } }, { "name": { "family": "Hill", "given": "D." } }, { "name": { "family": "Hornbeck", "given": "J. B." } }, { "name": { "family": "Kelvin", "given": "L." } }, { "name": { "family": "Lagache", "given": "G." } }, { "name": { "family": "Lopez-Caniego", "given": "M." } }, { "name": { "family": "Gonzalez-Nuevo", "given": "J." } }, { "name": { "family": "Maddox", "given": "S." } }, { "name": { "family": "Pascale", "given": "E." } }, { "name": { "family": "Pohlen", "given": "M." } }, { "name": { "family": "Rigby", "given": "E. E." } }, { "name": { "family": "Robotham", "given": "A." } }, { "name": { "family": "Simpson", "given": "C." } }, { "name": { "family": "Smith", "given": "D. J. B." } }, { "name": { "family": "Temi", "given": "P." } }, { "name": { "family": "Thompson", "given": "M. A." } }, { "name": { "family": "Woodgate", "given": "B. E." } }, { "name": { "family": "York", "given": "D. G." } }, { "name": { "family": "Aguirre", "given": "J. E." } }, { "name": { "family": "Beelen", "given": "A." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "name": { "family": "Baker", "given": "A. J." } }, { "name": { "family": "Birkinshaw", "given": "M." } }, { "name": { "family": "Blundell", "given": "R." } }, { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "name": { "family": "Burgarella", "given": "D." } }, { "name": { "family": "Danese", "given": "L." } }, { "name": { "family": "Dunlop", "given": "J. S." } }, { "name": { "family": "Fleuren", "given": "S." } }, { "name": { "family": "Glenn", "given": "J." } }, { "name": { "family": "Harris", "given": "A. I." } }, { "name": { "family": "Kamenetzky", "given": "J." } }, { "name": { "family": "Lupu", "given": "R. E." } }, { "name": { "family": "Maddalena", "given": "R. J." } }, { "name": { "family": "Madore", "given": "B. F." } }, { "name": { "family": "Maloney", "given": "P. R." } }, { "name": { "family": "Matsuhara", "given": "H." } }, { "name": { "family": "Michaowski", "given": "M. J." } }, { "id": "Murphy-E-J", "name": { "family": "Murphy", "given": "E. J." }, "orcid": "0000-0001-7089-7325" }, { "id": "Naylor-B-J", "name": { "family": "Naylor", "given": "B. J." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H." } }, { "name": { "family": "Popescu", "given": "C." } }, { "name": { "family": "Rawlings", "given": "S." } }, { "name": { "family": "Rigopoulou", "given": "D." } }, { "name": { "family": "Scott", "given": "D." } }, { "name": { "family": "Scott", "given": "K. S." } }, { "name": { "family": "Seibert", "given": "M." } }, { "name": { "family": "Smail", "given": "I." } }, { "name": { "family": "Tuffs", "given": "R. J." } }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "name": { "family": "van der Werf", "given": "P. P." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "Detection of a Population of Submillimeter-Bright, Strongly Lensed Galaxies", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 American Association for the Advancement of Science. \n\nReceived 8 June 2010; accepted 21 September 2010. \n\nHerschel is an ESA space observatory with science instruments provided by European-led principal investigator consortia and with important participation from NASA. U.S. participants in H-ATLAS acknowledge support from NASA through a contract from JPL. This work was supported by the Science and Technology Facilities Council (grants PP/D002400/1 and ST/G002533/1) and studentship SF/F005288/1. We thank Agenzia Spaziale Italiana (ASI) for funding through contract No. I/016/07/0 COFIS and ASI/Istituto Nazionale di Astrofisica agreement I/072/09/0 for the Planck Low-Frequency Instrument (LFI) Activity of Phase E2. Research supported in part by Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT) grants 39953-F and 39548-F. The W. M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. IRAM is supported by Institut National des Sciences de l'Univers (INSU)/CNRS (France), Max Planck Society (MPG) (Germany), and Instituto Geogr\u00e1fico Nacional (IGN) (Spain). Z-spec was supported by NSF grant AST-0807990 to J.A. and by the CSO NSF Cooperative Agreement AST-0838261. Support was provided to J.K. by an NSF Graduate Research Fellowship. Z-spec was constructed under NASA SARA grants NAGS-11911 and NAGS-12788 and an NSF Career grant (AST-0239270) and a Research Corporation Award (RI0928) to J.G., in collaboration with JPL, California Institute of Technology, under a contract with NASA. Construction of and observations with the Zpectrometer have been supported by NSF grants AST-0503946 and AST-0708653. NRAO is a facility of the NSF operated under cooperative agreement by Associated Universities. The optical spectroscopic redshift of ID130 was derived from observations obtained with the Apache Point Observatory 3.5-m telescope, which is owned and operated by the Astrophysical Research Consortium. The optical spectroscopic redshifts of ID9 and ID11 were obtained with the William Herschel Telescope, which is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof\u00edsica de Canarias. For the use of Keck, SMA, and CSO, the authors wish to recognize and acknowledge the very important cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nAccepted Version - 1011.1255.pdf
Supplemental Material - Negrello-SOM.pdf
", "abstract": "Gravitational lensing is a powerful astrophysical and cosmological probe and is particularly valuable at submillimeter wavelengths for the study of the statistical and individual properties of dusty star-forming galaxies. However, the identification of gravitational lenses is often time-intensive, involving the sifting of large volumes of imaging or spectroscopic data to find few candidates. We used early data from the Herschel Astrophysical Terahertz Large Area Survey to demonstrate that wide-area submillimeter surveys can simply and easily detect strong gravitational lensing events, with close to 100% efficiency.", "date": "2010-11-05", "date_type": "published", "publication": "Science", "volume": "330", "number": "6005", "publisher": "American Association for the Advancement of Science", "pagerange": "800-804", "id_number": "CaltechAUTHORS:20200221-111532581", "issn": "0036-8075", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200221-111532581", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "PP/D002400/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/G002533/1" }, { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "SF/F005288/1" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/016/07/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/072/09/0" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "39953-F" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "39548-F" }, { "agency": "W. M. Keck Foundation" }, { "agency": "Smithsonian Institution" }, { "agency": "Academia Sinica" }, { "agency": "Institut National des Sciences de l'Univers (INSU)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Max Planck Society" }, { "agency": "Instituto Geogr\u00e1fico Nacional (IGN)" }, { "agency": "NSF", "grant_number": "AST-0807990" }, { "agency": "NSF", "grant_number": "AST-0838261" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA", "grant_number": "NAGS-11911" }, { "agency": "NASA", "grant_number": "NAGS-12788" }, { "agency": "NSF", "grant_number": "AST-0239270" }, { "agency": "Research Corporation", "grant_number": "RI0928" }, { "agency": "NSF", "grant_number": "AST-0503946" }, { "agency": "NSF", "grant_number": "AST-0708653" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1126/science.1193420", "primary_object": { "basename": "1011.1255.pdf", "url": "https://authors.library.caltech.edu/records/t48e0-xhp71/files/1011.1255.pdf" }, "related_objects": [ { "basename": "Negrello-SOM.pdf", "url": "https://authors.library.caltech.edu/records/t48e0-xhp71/files/Negrello-SOM.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Negrello, M.; Hopwood, R.; et el." }, { "id": "https://authors.library.caltech.edu/records/0j381-6yj61", "eprint_id": 21418, "eprint_status": "archive", "datestamp": "2023-08-19 04:19:53", "lastmod": "2023-10-21 00:01:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rivera-Ingraham-A", "name": { "family": "Rivera-Ingraham", "given": "Alana" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "The blast view of the star-forming region in Aquila (\u2113 = 45\u00b0, b = 0\u00b0 )", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons \u2013 ISM: clouds \u2013 stars: formation \u2013 submillimeter: ISM", "note": "\u00a9 2010 American Astronomical Society. Received 2010 May 27; accepted 2010 September 6; published 2010 October 15. The BLAST collaboration acknowledges the support of\nNASA through grants NAG5-12785, NAG5-13301, and NNGO-\n6GI11G, the Canadian Space Agency (CSA), the UK Particle\nPhysics and Astronomy Research Council (PPARC), the\nCanada Foundation for Innovation (CFI), the Ontario Innovation Trust (OIT), and Canada's Natural Sciences and Engineering Research Council (NSERC). We also thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work. We also thank the referee for very useful suggestions and improvements to our paper, and Mubdi Rahman for useful discussions.\n\nPublished - RiveraIngraham2010p12054Astrophys_J.pdf
", "abstract": "We have carried out the first general submillimeter analysis of the field toward GRSMC 45.46+0.05, a massive\nstar-forming region in Aquila. The deconvolved 6 deg^2 (3\u00b0 \u00d7 2\u00b0) maps provided by BLAST in 2005 at 250, 350,\nand 500 \u03bcm were used to perform a preliminary characterization of the clump population previously investigated in the infrared, radio, and molecular maps. Interferometric CORNISH data at 4.8 GHz have also been used to characterize the Ultracompact H_II regions (UCH_(II)Rs) within the main clumps. By means of the BLAST maps,\nwe have produced an initial census of the submillimeter structures that will be observed by Herschel, several of\nwhich are known Infrared Dark Clouds. Our spectral energy distributions of the main clumps in the field, located\nat ~7 kpc, reveal an active population with temperatures of T ~ 35\u201340 K and masses of ~10^3 M_\u2299 for a dust emissivity index \u03b2 = 1.5. The clump evolutionary stages range from evolved sources, with extended H_II regions and prominent IR stellar population, to massive young stellar objects, prior to the formation of an UCH_(II)R. The CORNISH data have revealed the details of the stellar content and structure of the UCH_(II)Rs. In most cases, the ionizing stars corresponding to the brightest radio detections are capable of accounting for the clump bolometric luminosity, in most cases powered by embedded OB stellar clusters.", "date": "2010-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "723", "number": "1", "publisher": "American Astronomical Society", "pagerange": "915-934", "id_number": "CaltechAUTHORS:20101217-091654208", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101217-091654208", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Canada Foundation for Innovation (CFI)" }, { "agency": "Ontario Innovation Trust (OIT)" }, { "agency": "Natural Sciences and Engineering Research Council (NSERC)" } ] }, "doi": "10.1088/0004-637X/723/1/915", "primary_object": { "basename": "RiveraIngraham2010p12054Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/0j381-6yj61/files/RiveraIngraham2010p12054Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Rivera-Ingraham, Alana and Bock, James J." }, { "id": "https://authors.library.caltech.edu/records/kmktn-cr612", "eprint_id": 100994, "eprint_status": "archive", "datestamp": "2023-08-19 04:18:34", "lastmod": "2023-10-19 22:19:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Natoli-P", "name": { "family": "Natoli", "given": "P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } } ] }, "title": "BOOMERanG constraints on primordial non-Gaussianity from analytical Minkowski functionals", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: analytical, methods: statistical, early Universe, cosmic background radiation, cosmology: observations", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 June 21. Received 2010 May 18; in original form 2009 June 2. Published: 19 October 2010. \n\nThe BOOMERanG team gratefully acknowledges support from the CIAR, CSA and NSERC in Canada; Agenzia Spaziale Italiana, University La Sapienza and Programma Nazionale Ricerche in Antartide in Italy; PPARC and the Leverhulme Trust in the UK and NASA (awards NAG5-9251 and NAG5-12723) and NSF (awards OPP-9980654 and OPP-0407592) in the USA. Additional support for detector development was provided by CIT and JPL. Field, logistical and flight support were supplied by USAP and NSBF. This research used resources at NERSC, supported by the DOE under Contract No. DE-AC03-76SF00098, and CASPUR (Rome, Italy; special thanks are due to M. Botti and F. Massaioli). We also acknowledge partial support from ASI Contract I/016/07/0 'COFIS' and ASI Contract Planck LFI activity of Phase E2. Some of the results in this paper have been derived using the HEALPIX package (G\u00f3rski et al. 2005). CH acknowledges support from the Particle Physics and Astronomy Research Council grant number PP/C501692/1 and a JSPS (Japan Society for the Promotion of Science) fellowship. We thank an anonymous referee for useful suggestions.\n\nPublished - mnras0408-1658.pdf
Submitted - 0905.4301.pdf
", "abstract": "We use Minkowski functionals (MFs) to constrain a primordial non-Gaussian contribution to the cosmic microwave background intensity field as observed in the 150- and 145-GHz BOOMERanG maps from the 1998 and 2003 flights, respectively, performing for the first time a joint analysis of the two data sets. A perturbative expansion of the MF formulae in the limit of a weakly non-Gaussian field yields analytical formulae, derived by Hikage et al., which can be used to constrain the coupling parameter f_(NL) without the need for non-Gaussian simulations. We find \u2212770 < f_(NL) < 500 at 95 per cent CL, significantly improving the previous constraints by De Troia et al. on the BOOMERanG 2003 data set. These are the best f_(NL) limits to date for suborbital probes.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "408", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1658-1665", "id_number": "CaltechAUTHORS:20200129-140653790", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200129-140653790", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/016/07/0" }, { "agency": "University La Sapienza" }, { "agency": "Programma Nazionale Ricerche in Antartide (PNRA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)", "grant_number": "PP/C501692/1" }, { "agency": "Leverhulme Trust" }, { "agency": "NASA", "grant_number": "NAG5-9251" }, { "agency": "NASA", "grant_number": "NAG5-12723" }, { "agency": "NSF", "grant_number": "OPP-9980654" }, { "agency": "NSF", "grant_number": "OPP-0407592" }, { "agency": "Caltech" }, { "agency": "JPL" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC03-76SF00098" }, { "agency": "Japan Society for the Promotion of Science (JSPS)" } ] }, "doi": "10.1111/j.1365-2966.2010.17228.x", "primary_object": { "basename": "0905.4301.pdf", "url": "https://authors.library.caltech.edu/records/kmktn-cr612/files/0905.4301.pdf" }, "related_objects": [ { "basename": "mnras0408-1658.pdf", "url": "https://authors.library.caltech.edu/records/kmktn-cr612/files/mnras0408-1658.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Natoli, P.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/8007b-r9t74", "eprint_id": 21411, "eprint_status": "archive", "datestamp": "2023-08-22 01:15:48", "lastmod": "2023-10-21 00:01:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rowan-Robinson-M", "name": { "family": "Rowan-Robinson", "given": "M." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N. Y." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Cold dust and young starbursts: spectral energy distributions of Herschel SPIRE sources from the HerMES survey", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: starburst; galaxies: star formation; cosmology: observations; infrared: galaxies", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 May 17. Received 2010 May 17; in original form 2010 April 30. Article first published online: 25 Aug. 2010. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies:\nCSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI\n(Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA\n(USA). \n\nThe data presented in this paper will be released through the Herschel data base in Marseille HeDaM.\n\nPublished - RowanRobinson2010p12106Mon_Not_R_Astron_Soc.pdf
Accepted Version - 1006.0120.pdf
", "abstract": "We present spectral energy distributions (SEDs) for 68 Herschel sources detected at 5\u03c3 at 250, 350 and 500 \u03bcm in the HerMES SWIRE-Lockman field. We explore whether existing models for starbursts, quiescent star-forming galaxies and active galactic nucleus dust tori are able to model the full range of SEDs measured with Herschel. We find that while many galaxies (~56 per cent) are well fitted with the templates used to fit IRAS, Infrared Space Observatory (ISO) and Spitzer sources, for about half the galaxies two new templates are required: quiescent ('cirrus') models with colder (10\u201320 K) dust and a young starburst model with higher optical depth than Arp 220. Predictions of submillimetre fluxes based on model fits to 4.5\u201324 \u03bcm data agree rather poorly with the observed fluxes, but the agreement is better for fits to 4.5\u201370 \u03bcm data. Herschel galaxies detected at 500 \u03bcm tend to be those with the highest dust masses.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "2-11", "id_number": "CaltechAUTHORS:20101216-153515222", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101216-153515222", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2010.17041.x", "primary_object": { "basename": "1006.0120.pdf", "url": "https://authors.library.caltech.edu/records/8007b-r9t74/files/1006.0120.pdf" }, "related_objects": [ { "basename": "RowanRobinson2010p12106Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/8007b-r9t74/files/RowanRobinson2010p12106Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Rowan-Robinson, M.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/cexj5-d5d95", "eprint_id": 21541, "eprint_status": "archive", "datestamp": "2023-08-22 01:16:18", "lastmod": "2023-10-21 00:07:13", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hwang-H-S", "name": { "family": "Hwang", "given": "H. S." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Evolution of dust temperature of galaxies through cosmic time as seen by Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: formation; galaxies: general; galaxies: highredshift; galaxies: starburst; infrared: galaxies", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 September 3. Received 2010 July 26. Article first published online: 25 Oct. 2010. \n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. \n\nPACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy) and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); SNSB (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK) and NASA (USA). The HerMES data were accessed through the HeDaM data base (http://hedam.oamp.fr) operated by CeSAM and hosted by the Laboratoire d'Astrophysique de Marseille. This research is based on observations with AKARI, a JAXA project with the participation of ESA. MGL was supported by a National Research Foundation of Korea (NRF) grant funded by the Korea Government (MEST) (grant no. R01-2007-000-20336-0).\n\nPublished - Hwang2010p12112Mon_Not_R_Astron_Soc.pdf
Submitted - 1009.1058.pdf
", "abstract": "We study the dust properties of galaxies in the redshift range 0.1 \u2272 z \u2272 2.8 observed by the Herschel Space Observatory in the field of the Great Observatories Origins Deep Survey-North as part of the PACS Extragalactic Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) key programmes. Infrared (IR) luminosity (L_(IR)) and dust temperature (T_dust) of galaxies are derived from the spectral energy distribution fit of the far-IR (FIR) flux densities obtained with the PACS and SPIRE instruments onboard Herschel. As a reference sample, we also obtain IR luminosities and dust temperatures of local galaxies at z < 0.1 using AKARI and IRAS data in the field of the Sloan Digital Sky Survey. We compare the L_(IR)\u2013T_dust relation between the two samples and find that the median Tdust of Herschel-selected galaxies at z \u2273 0.5 with L_(IR) \u2273 5 \u00d7 10^(10) L_\u2299 appears to be 2\u20135 K colder than that of AKARI-selected local galaxies with similar luminosities, and the dispersion in T_dust for high-z galaxies increases with L_(IR) due to the existence of cold galaxies that are not seen among local galaxies. We show that this large dispersion of the L_(IR)\u2212T_dust relation can bridge the gap between local star-forming galaxies and high-z submillimetre galaxies (SMGs). We also find that three SMGs with very low T_dust\u2002(\u227220 K) covered in this study have close neighbouring sources with similar 24-\u03bcm brightness, which could lead to an overestimation of FIR/(sub)millimetre fluxes of the SMGs.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "75-82", "id_number": "CaltechAUTHORS:20110103-110253076", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110103-110253076", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency (ESA) PROgramme for the Development of scientific Experiments (PRODEX) (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Laboratoire d'Astrophysique de Marseille (LAM)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "National Research Foundation of Korea", "grant_number": "R01-2007-000-20336-0" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2010.17645.x", "primary_object": { "basename": "1009.1058.pdf", "url": "https://authors.library.caltech.edu/records/cexj5-d5d95/files/1009.1058.pdf" }, "related_objects": [ { "basename": "Hwang2010p12112Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/cexj5-d5d95/files/Hwang2010p12112Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Hwang, H. S.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/75c17-eas67", "eprint_id": 23605, "eprint_status": "archive", "datestamp": "2023-08-22 01:17:54", "lastmod": "2023-10-23 19:47:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rigopoulou-D", "name": { "family": "Rigopoulou", "given": "D." }, "orcid": "0000-0001-6854-7545" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: Herschel-SPIRE observations of Lyman break galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; submillimetre: galaxies", "note": "\u00a9 2010 The Authors. \nJournal compilation \u00a9 2010 RAS.\nAccepted 2010 September 10. Received 2010 September 2; in original form 2010 June 20.\nArticle first published online: 12 Oct. 2010.\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM(France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). The data presented in this Letter will be released through the\nHerschel data base in Marseille HeDaM (hedam.oamp.fr/HerMES).\n\nPublished - Rigopoulou2010p13726Mon_Not_R_Astron_Soc.pdf
", "abstract": "We present first results of a study of the submillimetre (submm) (rest-frame far-infrared) properties of z ~ 3 Lyman break galaxies (LBGs) and their lower redshift counterparts BX/BM galaxies, based on Herschel-SPIRE observations of the Northern field of the Great Observatories Origins Deep Survey (GOODS-N). We use stacking analysis to determine the properties of LBGs well below the current limit of the survey. Although LBGs are not detected individually, stacking the infrared luminous LBGs (those detected with Spitzer at 24 \u03bcm) yields a statistically significant submm detection with mean flux \u3008S_(250)\u3009= 5.9 \u00b1 1.4 mJy confirming the power of SPIRE in detecting UV-selected high-redshift galaxies at submm wavelengths. In comparison, the Spitzer 24 \u03bcm detected BX/BM galaxies appear fainter with a stacked value of\u3008S_(250)\u3009= 2.7 \u00b1 0.8 mJy. By fitting the spectral energy distributions (SEDs) we derive median infrared luminosities, L_(IR), of 2.8 \u00d7 10^(12) L_\u2299 and 1.5 \u00d7 10^(11) L_\u2299 for z ~ 3 LBGs and BX/BMs, respectively. We find that LIR estimates derived from present measurements are in good agreement with those based on UV data for z ~ 2 BX/BM galaxies, unlike the case for z ~ 3 infrared luminous LBGs where the UV underestimates the true L_(IR). Although sample selection effects may influence this result we suggest that differences in physical properties (such as morphologies, dust distribution and extent of star-forming regions) between z ~ 3 LBGs and z ~ 2 BX/BMs may also play a significant role.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "L7-L12", "id_number": "CaltechAUTHORS:20110509-110943988", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110509-110943988", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1745-3933.2010.00950.x", "primary_object": { "basename": "Rigopoulou2010p13726Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/75c17-eas67/files/Rigopoulou2010p13726Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Rigopoulou, D.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/j60ta-t8a10", "eprint_id": 21323, "eprint_status": "archive", "datestamp": "2023-08-22 01:15:33", "lastmod": "2023-10-20 23:56:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" } ] }, "title": "HerMES: SPIRE Science Demonstration Phase maps", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; diffuse radiation; infrared: general; submillimetre: general", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS.\nAccepted 2010 September 24. Received 2010 September 24; in original form 2010 September 13.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nSPIRE has been developed by a consortium of institutes\nled by Cardiff Univ. (UK) and including Univ. Lethbridge\n(Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. \nPadua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). The authors thank Dave Clements and Mattia Vaccari for useful comments.\n\nPublished - Levenson2010p12116Mon_Not_R_Astron_Soc.pdf
", "abstract": "We describe the production and verification of sky maps of the five Spectral and Photometric Imaging Receiver (SPIRE) fields observed as part of the Herschel Multi-tiered Extragalactic Survey (HerMES) during the Science Demonstration Phase (SDP) of the Herschel mission. We have implemented an iterative map-making algorithm [The SPIRE-HerMES Iterative Mapper (SHIM)] to produce high fidelity maps that preserve extended diffuse emission on the sky while exploiting the repeated observations of the same region of the sky with many detectors in multiple scan directions to minimize residual instrument noise. We specify here the SHIM algorithm and outline the various tests that were performed to determine and characterize the quality of the maps and verify that the astrometry, point source flux and power on all relevant angular scales meet the needs of the HerMES science goals. These include multiple jackknife tests, determination of the map transfer function and detailed examination of the power spectra of both sky and jackknife maps. The map transfer function is approximately unity on scales from 1 arcmin to 1\u00b0. Final maps (v1.0), including multiple jackknives, as well as the SHIM pipeline, have been used by the HerMES team for the production of SDP papers.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "83-91", "id_number": "CaltechAUTHORS:20101213-112923482", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101213-112923482", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2010.17771.x", "primary_object": { "basename": "Levenson2010p12116Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/j60ta-t8a10/files/Levenson2010p12116Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Levenson, L.; Zemcov, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/mt0mr-jty20", "eprint_id": 23630, "eprint_status": "archive", "datestamp": "2023-08-22 01:18:04", "lastmod": "2023-10-23 19:48:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cava-A", "name": { "family": "Cava", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "HerMES: SPIRE detection of high-redshift massive compact galaxies in GOODS-N field", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: high-redshift; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2010 The Authors. \nJournal compilation \u00a9 2010 RAS.\nAccepted 2010 October 1. Received 2010 August 22; in original form 2010 July 16. Article first published online: 25 Oct 2010. Special thanks to E. Ricciardelli, J. Fritz and J.M. Varela-Lopez for useful discussions and technical support. The data presented in this Letter will be released through the Herschel data base in Marseille HeDaM (hedam.oamp.fr/herMES). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory\n(Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, University of Sussex (UK); Caltech, JPL, NHSC,\nUniversity Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). AC acknowledges a grant from the Spanish MCINN: ESP2007-65812-C02-02.\n\nPublished - Cava2010p13724Mon_Not_R_Astron_Soc.pdf
", "abstract": "We have analysed the rest-frame far-infrared properties of a sample of massive (M_\u2605 > 10^(11) M_\u2299) galaxies at 2 \u2272 z \u2272 3 in the Great Observatories Origins Deep Survey-North (GOODS-N) field using the Spectral and Photometric Imaging Receiver (SPIRE) instrument aboard the Herschel Space Observatory. To conduct this analysis we take advantage of the data from the Herschel Multi-tiered Extragalactic Survey (HerMES) key programme. The sample comprises 45 massive galaxies with structural parameters characterized with HST NICMOS-3. We study detections at submm Herschel bands, together with Spitzer 24-\u03bcm data, as a function of the morphological type, mass and size. We find that 26/45 sources are detected at MIPS 24 \u03bcm and 15/45 (all MIPS 24-\u03bcm detections) are detected at SPIRE 250 \u03bcm, with disc-like galaxies more easily detected. We derive star formation rates (SFRs) and specific star formation rates (sSFRs) by fitting the spectral energy distribution of our sources, taking into account non-detections for SPIRE and systematic effects for MIPS derived quantities. We find that the mean SFR for the spheroidal galaxies (~50\u2013100 M_\u2299 yr^(\u22121)) is substantially (a factor ~3) lower than the mean value presented by disc-like galaxies (~250\u2013300 M_\u2299 yr^(\u22121)).", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "L19-L24", "id_number": "CaltechAUTHORS:20110511-082509908", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110511-082509908", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)", "grant_number": "ESP2007-65812-C02-02" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1745-3933.2010.00964.x", "primary_object": { "basename": "Cava2010p13724Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/mt0mr-jty20/files/Cava2010p13724Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Cava, A.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/2qmem-vh395", "eprint_id": 21417, "eprint_status": "archive", "datestamp": "2023-08-22 01:15:54", "lastmod": "2023-10-21 00:01:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: deep galaxy number counts from a P(D) fluctuation analysis of SPIRE Science Demonstration Phase observations", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; submillimetre: diffuse background; submillimetre: galaxies", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS.\nAccepted 2010 September 27. Received 2010 September 25; in original form 2010 June 25.\nArticle first published online: 29 Oct. 2010.\n\n\n\nThe authors would like to thank Guillaume Patanchon and Phil Maloney\nfor many useful discussions. JG and AC acknowledge support\nfrom NASA Herschel GTO grant 1394366, sponsored by the Jet\nPropulsion Laboratory. SPIRE has been developed by a consortium\nof institutes led by Cardiff University (UK) and including University\nof Lethbridge (Canada); NAOC (China); CEA, LAM (France);\nIFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory\n(Sweden); Imperial College London, RAL, UCL-MSSL,\nUKATC, University of Sussex (UK); Caltech, JPL, NHSC, University\nof Colorado (USA). This development has been supported\nby national funding agencies: CSA (Canada); NAOC (China);\nCEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB\n(Sweden); STFC (UK) and NASA (USA). The data presented in this\npaper will be released through the Herschel Database in Marseille,\nHeDaM (http://hedam.oamp.fr/HerMES).\n\nPublished - Glenn2010p12115Mon_Not_R_Astron_Soc.pdf
", "abstract": "Dusty, star-forming galaxies contribute to a bright, currently unresolved cosmic far-infrared background. Deep Herschel-Spectral and Photometric Imaging Receiver (SPIRE) images designed to detect and characterize the galaxies that comprise this background are highly confused, such that the bulk lies below the classical confusion limit. We analyse three fields from the Herschel Multi-tiered Extragalactic Survey (HerMES) programme in all three SPIRE bands (250, 350 and 500 \u03bcm); parametrized galaxy number count models are derived to a depth of ~2 mJy beam^(\u22121), approximately four times the depth of previous analyses at these wavelengths, using a probability of deflection [P(D)] approach for comparison to theoretical number count models. Our fits account for 64, 60 and 43 per cent of the far-infrared background in the three bands. The number counts are consistent with those based on individually detected SPIRE sources, but generally inconsistent with most galaxy number count models, which generically overpredict the number of bright galaxies and are not as steep as the P(D)-derived number counts. Clear evidence is found for a break in the slope of the differential number counts at low flux densities. Systematic effects in the P(D) analysis are explored. We find that the effects of clustering have a small impact on the data, and the largest identified systematic error arises from uncertainties in the SPIRE beam.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "109-121", "id_number": "CaltechAUTHORS:20101217-091446952", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101217-091446952", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1394366" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2010.17781.x", "primary_object": { "basename": "Glenn2010p12115Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/2qmem-vh395/files/Glenn2010p12115Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Glenn, J.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/ny3sn-gcj60", "eprint_id": 21737, "eprint_status": "archive", "datestamp": "2023-08-19 04:15:08", "lastmod": "2023-10-21 00:17:03", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Magdis-G-E", "name": { "family": "Magdis", "given": "G. E." }, "orcid": "0000-0002-4872-2294" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Herschel reveals a T_(dust)-unbiased selection of z ~ 2 ultraluminous infrared galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution \u2013 galaxies: high-redshift \u2013 galaxies: starburst \u2013 cosmology:\nobservations \u2013 infrared: galaxies \u2013 submillimetre: galaxies.", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. Accepted 2010 July 27. Received 2010 July 15; in original form 2010 May 31. \n\nArticle first published online: 29 Oct. 2010.\nSPIRE has been developed by a consortium of institutes led by\nCardiff University (UK) and including Univ. Lethbridge (Canada);\nNAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);\nIAC (Spain); Stockholm Observatory (Sweden); Imperial College\nLondon, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK)\nand Caltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA\n(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI\n(Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA\n(USA). HIPE is a joint development by the Herschel Science\nGround Segment Consortium, consisting of ESA, the NASA\nHerschel Science Center and the HIFI, PACS and SPIRE consortia.\nThe data presented in this paper will be released through the\nHerschel Data base in Marseille, HeDaM (hedam.oamp.fr/\nHerMES).\n\nPublished - Magdis2010p12111Mon_Not_R_Astron_Soc.pdf
", "abstract": "Using Herschel Photodetector Array Camera (PACS) and Spectral and Photometric Imaging\nReceiver (SPIRE) observations of Lockman Hole-North and Great Observatories Origins\nDeep Survey-North (GOODS-N) as part of the Herschel Multi-tiered Extragalactic Survey\n(HerMES) project, we explore the far-infrared (IR) properties of a sample of mid-IR-selected\nstarburst-dominated ultraluminous infrared galaxies (ULIRGs) at z ~ 2. The selection of the\nsample is based on the detection of the stellar bump that appears in the spectral energy distribution\nof star-forming galaxies at 1.6 \u03bcm. We derive robust estimates of infrared luminosities\n(L_(IR)) and dust temperatures (T_d) of the population and find that while the luminosities in our\nsample span less than an order of magnitude (12.24 \u2264 log(L_(IR)/L_\u2299) \u2264 12.94), they cover\na wide range of dust temperatures (25 \u2264 T_d \u2264 62 K). Galaxies in our sample range from\nthose that are as cold as high-z submillimetre galaxies (SMGs) to those that are as warm\nas optically faint radio galaxies (OFRGs) and local ULIRGs. Nevertheless, our sample has\nmedian T_d = 42.3 K, filling the gap between SMGs and OFRGs, bridging the two populations.\nWe demonstrate that a significant fraction of our sample would be missed from ground-based\n(sub)mm surveys (850\u20131200 \u03bcm), showing that the latter introduce a bias towards the detection\nof colder sources. We conclude that Herschel observations confirm the existence of\nhigh-z ULIRGs warmer than SMGs, show that the mid-IR selection of high-z ULIRGs is\nnot T_d dependent, reveal a large dispersion in T_d of high-z ULIRGs and provide the means\nto characterize the bulk of the ULIRG population, free from selection biases introduced by\nground-based (sub)mm surveys.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "22-28", "id_number": "CaltechAUTHORS:20110112-141736463", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110112-141736463", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2010.17551.x", "primary_object": { "basename": "Magdis2010p12111Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/ny3sn-gcj60/files/Magdis2010p12111Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Magdis, G. E.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/swxa9-fye69", "eprint_id": 23634, "eprint_status": "archive", "datestamp": "2023-08-19 04:16:57", "lastmod": "2023-10-23 19:49:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chapman-S-C", "name": { "family": "Chapman", "given": "S. C." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } } ] }, "title": "Herschel-SPIRE, far-infrared properties of millimetre-bright and -faint radio galaxies", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 The Authors. \nJournal compilation \u00a9 2010 RAS.\nAccepted 2010 September 14. Received 2010 September 11; in original form 2010 July 20. Article first published online: 2 Nov 2010. The data presented in this Letter will be released through the Herschel data base in Marseille HeDaM (hedam.oamp.fr/HerMES). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge\n(Canada), NAOC (China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). Data presented herein were obtained using the W. M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California and NASA. The Observatory was made possible by the generous financial support of the W. M.\nKeck Foundation.\n\nPublished - Chapman2010p13721Mon_Not_R_Astron_Soc.pdf
Supplemental Material - MNL2_956_sm_TableS1.doc
", "abstract": "We present the first study of the far-infrared (FIR) properties of high-redshift, radio-selected ultraluminous infrared galaxies (ULIRGs) using deep observations obtained with the Spectral and Photometric Imaging Receiver (SPIRE) from the Herschel Multi-tiered Extragalactic Survey (HerMES). These galaxies span a large range of 850-\u03bcm fluxes from submillimetre-luminous \u223c10 mJy sources (SCUBA galaxies) to \u223c1.5 mJy from stacked SCUBA non-detections, thus likely representing a complete distribution of ULIRG spectral energy distributions (SEDs). From Keck spectroscopic surveys in the Lockman-North field we identified a sample of 31 submillimetre galaxies (SMGs) and 37 submillimetre-faint, optically faint radio galaxies (OFRGs), all with radio-inferred IR luminosities >10^(12) L_\u2299. These galaxies were cross-identified with SPIRE 250-, 350- and 500-\u03bcm catalogues based on fluxes extracted at 24-\u03bcm positions in the SWIRE survey, yielding a sample of more than half of the galaxies well detected in at least two of the SPIRE bandpasses. By fitting greybody dust models to the SPIRE photometry together with SCUBA 850-\u03bcm measurements (for OFRGs, only 850-inline image upper limits), we infer dust temperatures and FIR luminosities. The OFRGs detected by SPIRE have median \u3008T_d\u3009= 41 \u00b1 5 K and the SMGs have \u3008T_d\u3009= 34 \u00b1 5 K, both in reasonable agreement with previous (pre-Herschel) estimates, reaffirming that the local FIR/radio correlation holds (at least for this subset of high-z ULIRGs) at high redshift (we measure \u3008q_(IR)\u3009= 2.43 \u00b1 0.21 using S_(IR) derived from greybody fit coupled with a power-law extrapolation to the 24 \u03bcm). Our observations first confirm that a substantial fraction of OFRGs exhibits large infrared luminosities corresponding to SFRs of \u223c400 M_\u2299 yr^\u22121. The SPIRE observations secondly confirm the higher dust temperatures for these OFRGs than similarly selected SMGs, consistent with early predictions of the submillimetre-faint radio populations. Our observations also clearly confirm the large infrared luminosities of most SMGs selected with S_(850 \u03bcm) > 5 mJy and radio and strong 24-\u03bcm detections, corresponding to SFRs of \u223c700 M_\u2299 yr^(\u22121).", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "L13-L18", "id_number": "CaltechAUTHORS:20110511-094831977", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110511-094831977", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1111/j.1745-3933.2010.00956.x", "primary_object": { "basename": "MNL2_956_sm_TableS1.doc", "url": "https://authors.library.caltech.edu/records/swxa9-fye69/files/MNL2_956_sm_TableS1.doc" }, "related_objects": [ { "basename": "Chapman2010p13721Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/swxa9-fye69/files/Chapman2010p13721Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Chapman, S. C.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/cjgcb-d3a60", "eprint_id": 23585, "eprint_status": "archive", "datestamp": "2023-08-22 01:17:49", "lastmod": "2023-10-23 19:46:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Measures of star formation rates from infrared (Herschel) and UV (GALEX) emissions of galaxies in the HerMES fields", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; galaxies: stellar content; infrared: galaxies; ultraviolet: galaxies", "note": "\u00a9 2010 The Authors. \nJournal compilation \u00a9 2010 RAS.\nAccepted 2010 July 6. Received 2010 July 6; in original form 2010 May 20. Article first published online: 19 Aug 2010. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, OAMP (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK) and Caltech/JPL, IPAC, University of\nColorado (USA). This development has been supported by national funding agencies CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK) and NASA (USA). The data presented in this Letter will be released through the Herschel Database in Marseille HeDaM (http://hedam.oamp.fr/HerMES). This Letter makes use of TOPCAT, http://www.star.bristol.ac.uk/mbt/topcat/.\n\nPublished - Buat2010p13729Mon_Not_R_Astron_Soc.pdf
", "abstract": "The reliability of infrared (IR) and ultraviolet (UV) emissions to measure star formation rates (SFRs) in galaxies is investigated for a large sample of galaxies observed with the Spectral and Photometric Imaging Receiver (SPIRE) and the Photodetector Array Camera and Spectrometer (PACS) instruments on\u2002Herschel\u2002as part of the\u2002Herschel\u2002Multi-Tiered Extragalactic Survey (HerMES) project. We build flux-limited 250-\u03bcm samples of sources at redshift\u2002z\u2002< 1, cross-matched with the\u2002Spitzer/MIPS and\u2002GALEX\u2002catalogues. About 60 per cent of the\u2002Herschel\u2002sources are detected in UV. The total IR luminosities,\u2002L_(IR), of the sources are estimated using a spectral energy distribution (SED) fitting code that fits to fluxes between 24 and 500 \u03bcm. Dust attenuation is discussed on the basis of commonly used diagnostics: the\u2002L_(IR)/L_(UV)\u2002ratio and the slope, \u03b2, of the UV continuum. A mean dust attenuation\u2002A_(UV)\u2002of\u2002\u2243\u20023 mag is measured in the samples.\u2002L_(IR)/L_(UV)\u2002is found to correlate with\u2002L_(IR). Galaxies with\u2002L_(IR) \u2002> 10^(11) L_\u2299 and\u20020.5 <\u2002z\u2002< 1\u2002exhibit a mean dust attenuation\u2002A_(UV)\u2002of about 0.7 mag lower than that found for their local counterparts, although with a large dispersion. Our galaxy samples span a large range of \u03b2 and\u2002L_(IR)/L_(UV)\u2002values which, for the most part, are distributed between the ranges defined by the relations found locally for starburst and normal star-forming galaxies. As a consequence the recipe commonly applied to local starbursts is found to overestimate the dust attenuation correction in our galaxy sample by a factor of ~2\u20133. The SFRs deduced from\u2002L_(IR)\u2002are found to account for about 90 per cent of the total SFR; this percentage drops to 71 per cent for galaxies with\u2002SFR < 1 M_\u2299\u2002yr^(-1) (or\u2002L_(RI) < 10^(10) L_\u2299). For these faint objects, one needs to combine UV and IR emissions to obtain an accurate measure of the SFR.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "L1-L6", "id_number": "CaltechAUTHORS:20110506-141700003", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110506-141700003", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1745-3933.2010.00916.x", "primary_object": { "basename": "Buat2010p13729Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/cjgcb-d3a60/files/Buat2010p13729Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Buat, V.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/rvzqv-0v929", "eprint_id": 21443, "eprint_status": "archive", "datestamp": "2023-08-22 01:16:05", "lastmod": "2023-10-21 00:02:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Davies-J-I", "name": { "family": "Davies", "given": "J. I." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "On the origin of M81 group extended dust emission", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; galaxies: evolution; galaxies: individual: M81", "note": "\u00a9 2010 The Authors. \u00a9 2010 RAS.\nAccepted 2010 September 27. Received 2010 September 25; in original form 2010 August 16.\nArticle first published online: 4 Nov. 2010.\n\n\nPACS has been developed by a consortium of institutes led \nby MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies \nBMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univeristy of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK) and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI\n(Italy); MCINN (Spain); Stockholm Observatory (Sweden);\nSTFC (UK) and NASA (USA). GALEX is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA's support for construction, operation and science analysis for the GALEX mission. We thank Katie Chynoweth for reprocessing her M81 HI data for us and the THINGS team for providing us with their HI data cube.\n\nPublished - Davies2010p12117Mon_Not_R_Astron_Soc.pdf
", "abstract": "Galactic cirrus emission at far-infrared wavelengths affects many extragalactic observations. Separating this emission from that associated with extragalactic objects is both important and difficult. In this paper we discuss a particular case, the M81 group, and the identification of diffuse structures prominent in the infrared, but also detected at optical wavelengths. The origin of these structures has previously been controversial, ranging from them being the result of a past interaction between M81 and M82 or due to more local Galactic emission. We show that over an order of a few arcmin scales, the far-infrared (Herschel 250 \u03bcm) emission correlates spatially very well with a particular narrow-velocity (2\u20133 km s^(\u22121)) component of the Galactic H i. We find no evidence that any of the far-infrared emission associated with these features actually originates in the M81 group. Thus we infer that the associated diffuse optical emission must be due to galactic light-back scattered off dust in our galaxy. Ultraviolet observations pick out young stellar associations around M81, but no detectable far-infrared emission. We consider in detail one of the Galactic cirrus features, finding that the far-infrared H i relation breaks down below arcmin scales and that at smaller scales there can be quite large dust-temperature variations.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "102-108", "id_number": "CaltechAUTHORS:20101220-114124533", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101220-114124533", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency (ESA) PROgramme for the Development of scientific Experiments (PRODEX) (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Ministerio de Ciencia y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2010.17774.x", "primary_object": { "basename": "Davies2010p12117Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/rvzqv-0v929/files/Davies2010p12117Mon_Not_R_Astron_Soc.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Davies, J. I.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/b1k0a-fpq91", "eprint_id": 100992, "eprint_status": "archive", "datestamp": "2023-08-19 04:18:27", "lastmod": "2023-10-19 22:18:57", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Dunlop-J-S", "name": { "family": "Dunlop", "given": "J. S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "The BLAST 250 \u03bcm-selected galaxy population in GOODS-South", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active, galaxies: fundamental parameters, galaxies: photometry, galaxies: starburst, infrared: galaxies", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 June 30. Received 2010 June 2; in original form 2009 October 23. Published: 28 October 2010. \n\nJSD acknowledges the support of the Royal Society through a Wolfson Research Merit Award, and the support of the European Research Council through the award of an Advanced Grant. We acknowledge the support of NASA through grant numbers NAG5-12785, NAG5-13301 and NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology Facilities Council (STFC). This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. APEX is operated by the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory and the Onsala Space Observatory. This work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. MC acknowledges the award of a STFC Advanced Fellowship. IRS acknowledges support from STFC. JLW acknowledges the support of an STFC Studentship.\n\nPublished - mnras0408-2022.pdf
Submitted - 0910.3642.pdf
", "abstract": "We identify and investigate the nature of the 20 brightest 250 \u03bcm sources detected by the Balloon-borne Large Aperture Submillimetre Telescope (BLAST) within the central 150 arcmin\u00b2 of the Great Observatories Origins Deep Survey (GOODS)-South field. Aided by the available deep VLA 1.4 GHz radio imaging, reaching S_(1.4)\u224340 \u03bcJy (4\u03c3), we have identified radio counterparts for 17/20 of the 250 \u03bcm sources. The resulting enhanced positional accuracy of \u22431 arcsec has then allowed us to exploit the deep optical (Hubble Space Telescope), near-infrared (VLT) and mid-infrared (Spitzer) imaging of GOODS-South to establish secure galaxy counterparts for the 17 radio-identified sources, and plausible galaxy candidates for the three radio-unidentified sources. Confusion is a serious issue for this deep BLAST 250 \u03bcm survey, due to the large size of the beam. Nevertheless, we argue that our chosen counterparts are significant, and often dominant contributors to the measured BLAST flux densities. For all of these 20 galaxies we have been able to determine spectroscopic (eight) or photometric (12) redshifts. The result is the first near-complete redshift distribution for a deep 250 \u03bcm-selected galaxy sample. This reveals that 250 \u03bcm surveys reaching detection limits of \u224340 mJy have a median redshift z\u2243 1, and contain not only low-redshift spirals/LIRGs, but also the extreme z\u22432 dust-enshrouded starburst galaxies previously discovered at sub-millimetre wavelengths. Inspection of the LABOCA 870 \u03bcm imaging of GOODS-South yields detections of \u22431/3 of the proposed BLAST sources (all at z > 1.5), and reveals 250/870 \u03bcm flux-density ratios consistent with a standard 40 K modified blackbody fit with a dust emissivity index \u03b2= 1.5. Based on their Infrared Array Camera (IRAC) colours, we find that virtually all of the BLAST galaxy identifications appear better described as analogues of the M82 starburst galaxy, or Sc star-forming discs rather than highly obscured ULIRGs. This is perhaps as expected at low redshift, where the 250 \u03bcm BLAST selection function is biased towards spectral energy distributions which peak longward of \u03bb_(rest)= 100 \u03bcm. However, it also appears largely true at z\u22432.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "408", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2022-2050", "id_number": "CaltechAUTHORS:20200129-135112537", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200129-135112537", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Royal Society" }, { "agency": "European Research Council (ERC)" }, { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "NSF" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "NASA", "grant_number": "NAS 5-26555" } ] }, "doi": "10.1111/j.1365-2966.2010.17278.x", "primary_object": { "basename": "0910.3642.pdf", "url": "https://authors.library.caltech.edu/records/b1k0a-fpq91/files/0910.3642.pdf" }, "related_objects": [ { "basename": "mnras0408-2022.pdf", "url": "https://authors.library.caltech.edu/records/b1k0a-fpq91/files/mnras0408-2022.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Dunlop, J. S. and Bock, J. J." }, { "id": "https://authors.library.caltech.edu/records/fweya-62524", "eprint_id": 21321, "eprint_status": "archive", "datestamp": "2023-08-22 01:15:27", "lastmod": "2023-10-20 23:56:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brisbin-D", "name": { "family": "Brisbin", "given": "D." }, "orcid": "0000-0002-4795-419X" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Deep SPIRE HerMES Survey: spectral energy distributions and their astrophysical indications at high redshift", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: high-redshift; galaxies: starburst; galaxies: star formation; infrared: galaxies", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 September 3. Received 2010 September 2; in original form 2010 June 11. Article first published online: 25 Oct. 2010. \n\nHerschel is an ESA space observatory with science instruments provided by the European-led Principal Investigator consortia and with important participation from the NASA. \n\nThis work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by the NASA. Support for this work was provided by the NASA through an award issued by JPL/Caltech. The SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC(China); CEA, OAMP(France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). We thank the referee of this paper, Stephen J. Messenger, for his incisive comments and helpful recommendations.\n\nPublished - Brisbin2010p12119Mon_Not_R_Astron_Soc.pdf
Accepted Version - 1009.1371.pdf
", "abstract": "The Spectral and Photometric Imaging Receiver on-board Herschel has been carrying out deep extragalactic surveys, one of the aims of which is to establish spectral energy distributions of individual galaxies spanning the infrared/submillimetre (IR/SMM) wavelength region. We report observations of the IR/SMM emission from the Lockman North field and Great Observatories Origins Deep Survey Field-North. Because galaxy images in the wavelength range covered by Herschel generally represent a blend with contributions from neighbouring galaxies, we present sets of galaxies in each field, especially free of blending at 250, 350 and 500 \u03bcm. We identify the cumulative emission of these galaxies and the fraction of the FIR cosmic background radiation they contribute. Our surveys reveal a number of highly luminous galaxies at redshift z \u2272 3 and a novel relationship between IR and visible emission that shows a dependence on luminosity and redshift.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "66-74", "id_number": "CaltechAUTHORS:20101213-112741295", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101213-112741295", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2010.17643.x", "primary_object": { "basename": "1009.1371.pdf", "url": "https://authors.library.caltech.edu/records/fweya-62524/files/1009.1371.pdf" }, "related_objects": [ { "basename": "Brisbin2010p12119Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/fweya-62524/files/Brisbin2010p12119Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Brisbin, D.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/w46bb-y4x92", "eprint_id": 21611, "eprint_status": "archive", "datestamp": "2023-08-22 01:16:57", "lastmod": "2023-10-21 00:10:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roseboom-I-G", "name": { "family": "Roseboom", "given": "I. G." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The Herschel Multi-Tiered Extragalactic Survey: source extraction and cross-identifications in confusion-dominated SPIRE images", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical; galaxies: statistics; infrared: galaxies", "note": "\u00a9 2010 The Authors. Journal compilation \u00a9 2010 RAS. \n\nAccepted 2010 September 3. Received 2010 September 2; in original form 2010 June 1. Article first published online: 21 Oct. 2010. \n\nWe thank the anonymous referee for many suggestions, which greatly enhanced the clarity of this paper. IGR and LW were supported by the Science and Technology Facilities Council (grant number ST/F002858/1). \n\nThe SPIRE Consortium includes participants from eight countries (Canada, China, France, Italy, Spain, Sweden, UK, USA). The following institutes have provided hardware and software elements to the instrument programme: Cardiff University, UK; Commissariat l'nergie Atomique (CEA), Saclay, France; CEA, Grenoble, France; Imperial College, London, UK; Instituto de Astrofisica de Canarias (IAC), Tenerife, Spain; Infrared Processing and Analysis Centre (IPAC), Pasadena, USA; Istituto di Fisica dello Spazio Interplanetario (IFSI), Rome, Italy; University College London's Mullard Space Science Laboratory (MSSL), Surrey, UK; NASA Goddard Space Flight Centre (GSFC), Maryland, USA; NASA Jet Propulsion Laboratory (JPL) and Caltech, Pasadena, USA; National Astronomical Observatories, Chinese Academy of Sciences (NAOC), Beijing, China; Observatoire Astronomique de Marseille Provence (OAMP), France; Rutherford Appleton Laboratory (RAL), Oxfordshire, UK; Stockholm Observatory, Sweden; UK Astronomy Technology Centre (UK ATC) Edinburgh; University of Colorado, USA; University of Lethbridge, Canada; University of Padua, Italy; and the University of Sussex, UK. Funding for SPIRE has been provided by the national agencies of the participating countries and by internal institute funding: the Canadian Space Agency (CSA); NAOC in China; Centre National d'tudes Spatiales (CNES), Centre National de la Recherche Scientifique (CNRS), and CEA in France; Agenzia Spaziale Italiana (ASI) in Italy; Ministerio de Educacin y Ciencia (MEC) in Spain, Stockholm Observatory in Sweden; the Science and Technology Facilities Council (STFC) in the UK; and NASA in the USA. Additional funding support for some instrument activities has been provided by ESA.\n\nPublished - Roseboom2010p12118Mon_Not_R_Astron_Soc.pdf
Accepted Version - 1009.1658.pdf
", "abstract": "We present the cross-identification and source photometry techniques used to process Herschel SPIRE imaging taken as part of the Herschel Multi-Tiered Extragalactic Survey (HerMES). Cross-identifications are performed in map-space so as to minimize source-blending effects. We make use of a combination of linear inversion and model selection techniques to produce reliable cross-identification catalogues based on Spitzer MIPS 24-\u03bcm source positions. Testing on simulations and real Herschel observations shows that this approach gives robust results for even the faintest sources (S_(250) ~10 mJy). We apply our new technique to HerMES SPIRE observations taken as part of the science demonstration phase of Herschel. For our real SPIRE observations, we show that, for bright unconfused sources, our flux density estimates are in good agreement with those produced via more traditional point source detection methods (SUSSEXtractor) by Smith et al. When compared to the measured number density of sources in the SPIRE bands, we show that our method allows the recovery of a larger fraction of faint sources than these traditional methods. However, this completeness is heavily dependent on the relative depth of the existing 24-\u03bcm catalogues and SPIRE imaging. Using our deepest multiwavelength data set in the GOODS-N, we estimate that the use of shallow 24-\u03bcm catalogues in our other fields introduces an incompleteness at faint levels of between 20\u201340 per cent at 250 \u03bcm.", "date": "2010-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "409", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "48-65", "id_number": "CaltechAUTHORS:20110105-153945195", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110105-153945195", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" } ] }, "doi": "10.1111/j.1365-2966.2010.17634.x", "primary_object": { "basename": "1009.1658.pdf", "url": "https://authors.library.caltech.edu/records/w46bb-y4x92/files/1009.1658.pdf" }, "related_objects": [ { "basename": "Roseboom2010p12118Mon_Not_R_Astron_Soc.pdf", "url": "https://authors.library.caltech.edu/records/w46bb-y4x92/files/Roseboom2010p12118Mon_Not_R_Astron_Soc.pdf" } ], "resource_type": "article", "pub_year": "2010", "author_list": "Roseboom, I. G.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/7a3qz-8bh57", "eprint_id": 21269, "eprint_status": "archive", "datestamp": "2023-08-19 04:08:28", "lastmod": "2023-10-20 23:53:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The QUaD galactic plane survey. I. Maps and analysis of diffuse emission", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations \u2013 diffuse radiation \u2013 Galaxy: structure \u2013 polarization \u2013 submillimeter: diffuse\nbackground \u2013 surveys", "note": "\u00a9 2010 American Astronomical Society. Received 2009 December 16; accepted 2010 June 23; published 2010 September 27. This paper is dedicated to the memory of Andrew Lange,\nwho gave wisdom and guidance to so many members of the\nastrophysics and cosmology community. His presence is sorely\nmissed. We thank our colleagues on the BICEP experiment\nand Dan Marrone for useful discussions. QUaD is funded\nby the National Science Foundation in the USA, through\ngrants ANT-0338138, ANT-0338335, and ANT-0338238, by\nthe Science and Technology Facilities Council (STFC) in the\nUK and by the Science Foundation Ireland. The BOOMERanG\ncollaboration kindly allowed the use of their CMB maps for our\ncalibration purposes. M.Z. acknowledges support from a NASA\nPostdoctoral Fellowship. P.G.C. acknowledges funding from the\nPortuguese FCT. S.E.C. acknowledges support from a Stanford\nTerman Fellowship. J.R.H. acknowledges the support of an NSF\nGraduate Research Fellowship, a Stanford Graduate Fellowship,\nand a NASA Postdoctoral Fellowship. Y.M. acknowledges\nsupport from a SUPA Prize studentship. C.P. acknowledges\npartial support from the Kavli Institute for Cosmological Physics\nthrough the grant NSF PHY-0114422. E.Y.W. acknowledges\nreceipt of an NDSEG fellowship. We acknowledge the use of\nthe Legacy Archive for Microwave Background Data Analysis\n(LAMBDA). Support for LAMBDA is provided by the NASA\nOffice of Space Science.\n\nPublished - Culverhouse2010p12040Astrophys_J.pdf
", "abstract": "We present a survey of ~800 deg^2 of the galactic plane observed with the QUaD telescope. The primary products\nof the survey are maps of Stokes I, Q, and U parameters at 100 and 150 GHz, with spatial resolution of 5' and 3'.5,\nrespectively. Two regions are covered, spanning approximately 245\u00b0\u2013295\u00b0 and 315\u00b0\u20135\u00b0 in the galactic longitude l and \u22124\u00b0 < b < +4\u00b0 in the galactic latitude b. At 0\u00b0.02 square pixel size, the median sensitivity is 74 and 107 kJy sr^(\u22121) at 100 GHz and 150 GHz respectively in I, and 98 and 120 kJy sr^(\u22121) for Q and U. In total intensity, we find an average spectral index of \u03b1 = 2.35 \u00b1 0.01 (stat) \u00b1 0.02 (sys) for |b| \u2264 1\u00b0, indicative of emission components other than thermal dust. A comparison to published dust, synchrotron, and free\u2013free models implies an excess of emission in the 100 GHz QUaD band, while better agreement is found at 150 GHz. A smaller excess is observed when comparing QUaD 100 GHz data to the WMAP five-year W band; in this case, the excess is likely due to the wider bandwidth of QUaD. Combining the QUaD and WMAP data, a two-component spectral fit to the inner galactic plane (|b| \u2264 1\u00b0) yields mean spectral indices of \u03b1_s = \u22120.32 \u00b1 0.03 and \u03b1_d = 2.84 \u00b1 0.03; the former is\ninterpreted as a combination of the spectral indices of synchrotron, free\u2013free, and dust, while the second is largely attributed to the thermal dust continuum. In the same galactic latitude range, the polarization data show a high degree of alignment perpendicular to the expected galactic magnetic field direction, and exhibit mean polarization fraction 1.38 \u00b1 0.08 (stat) \u00b1 0.1 (sys)% at 100 GHz and 1.70 \u00b1 0.06 (stat) \u00b1 0.1 (sys)% at 150 GHz. We find agreement in polarization fraction between QUaD 100 GHz and the WMAP W band, the latter giving 1.1% \u00b1 0.4%.", "date": "2010-10-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "722", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1057-1077", "id_number": "CaltechAUTHORS:20101209-111943762", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101209-111943762", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Science and Technology Facilities Council (STFC) (UK)" }, { "agency": "Science Foundation Ireland (SFI)" }, { "agency": "NASA" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT) (Portugal)" }, { "agency": "Stanford Terman Fellowship" }, { "agency": "Stanford Graduate Fellowship" }, { "agency": "Scottish Universities Physics Alliance (SUPA)" }, { "agency": "Kavli Institute for Cosmological Physics/NSF", "grant_number": "PHY-0114422" }, { "agency": "National Defense Science and Engineering Graduate (NDSEG)" } ] }, "corp_creators": { "items": [ "QUaD Collaboration" ] }, "doi": "10.1088/0004-637X/722/2/1057", "primary_object": { "basename": "Culverhouse2010p12040Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/7a3qz-8bh57/files/Culverhouse2010p12040Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Culverhouse, T.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/5cf6h-1r516", "eprint_id": 20761, "eprint_status": "archive", "datestamp": "2023-08-22 00:44:40", "lastmod": "2023-10-20 23:25:05", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Lamarre-J-M", "name": { "family": "Lamarre", "given": "J.-M" } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" } ] }, "title": "Planck pre-launch status: The HFI instrument, from specification to actual performance", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; space vehicles: instruments; submillimeter: general; techniques: photometric; techniques: polarimetric", "note": "\u00a9 2010 ESO.\n\nReceived 24 July 2009; accepted 27 January 2010.\nPublished online 15 September 2010.\n\nThe Planck-HFI instrument (http://hfi.planck.fr/) was designed and built by an international consortium of laboratories, universities and institutes, with important contributions from the industry, under the leadership of the PI institute, IAS at Orsay, France. It was funded in particular by CNES, CNRS, NASA, STFC and ASI. The authors extend their gratitude to the numerous engineers and scientists, who have contributed to the design, development, construction or evaluation of the HFI instrument. The authors are pleased to thank the referee for his/her very useful remarks.\n\nPublished - Lamarre2010p11793Astron_Astrophys.pdf
", "abstract": "Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six\nbands in the 100 GHz\u22121 THz range.\nAims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental\nsources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide\nfull maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels\nor accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests\nand calibration.\nMethods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly:\n(i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions;\n(iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques.\nResults. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based\ncalibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification.", "date": "2010-09", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "520", "publisher": "EDP Sciences", "pagerange": "A9", "id_number": "CaltechAUTHORS:20101111-100415286", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101111-100415286", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'Etudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "NASA" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" } ] }, "doi": "10.1051/0004-6361/200912975", "primary_object": { "basename": "Lamarre2010p11793Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/5cf6h-1r516/files/Lamarre2010p11793Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Lamarre, J.-M; Lange, A. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/7bw2k-4mt80", "eprint_id": 19752, "eprint_status": "archive", "datestamp": "2023-09-15 23:16:31", "lastmod": "2023-10-23 21:40:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sibthorpe-", "name": { "family": "Sibthorpe", "given": "B." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "AKARI and BLAST Observations of the Cassiopeia A Supernova Remnant and Surrounding Interstellar Medium", "ispublished": "pub", "full_text_status": "public", "keywords": "early universe; ISM: supernova remnants", "note": "\u00a9 2010 \n\nReceived 2009 October 5; accepted 2010 April 20; published 2010 August 2.\n\nWe acknowledge the support of NASA through grant numbers\nNAG5-12785, NAG5-13301, and NNGO-6GI11G, the NSF\nOffice of Polar Programs, the Canadian Space Agency, the\nNatural Sciences and Engineering Research Council (NSERC)\nof Canada, the UK Science and Technology Facilities Council\n(STFC), and Korea Science and Engineering Foundation (R01-\n2007-000-20336-0, F01-2007-000-10048-0). This work is also\nbased on observations with AKARI, a JAXA project with the\nparticipation of ESA. Finally, we acknowledge M. Wright for\nthe use of his 83 GHz radio map of Cas A.\n\nPublished - Sibthorpe2010p11210Astrophys_J.pdf
", "abstract": "We use new large area far infrared maps ranging from 65 to 500 \u03bcm obtained with the AKARI and the Balloon-borne Large Aperture Submillimeter Telescope missions to characterize the dust emission toward the Cassiopeia A supernova remnant (SNR). Using the AKARI high-resolution data we find a new \"tepid\" dust grain population at a temperature of ~35 K and with an estimated mass of 0.06 M_\u2609. This component is confined to the central area of the SNR and may represent newly formed dust in the unshocked supernova ejecta. While the mass of tepid dust that we measure is insufficient by itself to account for the dust observed at high redshift, it does constitute an additional dust population to contribute to those previously reported. We fit our maps at 65, 90, 140, 250, 350, and 500 \u03bcm to obtain maps of the column density and temperature of \"cold\" dust (near 16 K) distributed throughout the region. The large column density of cold dust associated with clouds seen in molecular emission extends continuously from the surrounding interstellar medium to project on the SNR, where the foreground component of the clouds is also detectable through optical, X-ray, and molecular extinction. At the resolution available here, there is no morphological signature to isolate any cold dust associated only with the SNR from this confusing interstellar emission. Our fit also recovers the previously detected \"hot\" dust in the remnant, with characteristic temperature 100 K.", "date": "2010-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "719", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1553-1564", "id_number": "CaltechAUTHORS:20100831-152351185", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100831-152351185", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "NSF" }, { "agency": "Canadian Space Agency" }, { "agency": "Natural Sciences and Engineering Research Council (NSERC) of Canada" }, { "agency": "UK Science and Technology Facilities Council" }, { "agency": "Korea Science and Engineering Foundation", "grant_number": "R01-2007-000-20336-0" }, { "agency": "Korea Science and Engineering Foundation", "grant_number": "F01-2007-000-10048-0" } ] }, "doi": "10.1088/0004-637X/719/2/1553", "primary_object": { "basename": "Sibthorpe2010p11210Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/7bw2k-4mt80/files/Sibthorpe2010p11210Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Sibthorpe, B. and Bock, J. J." }, { "id": "https://authors.library.caltech.edu/records/rqh79-ppw08", "eprint_id": 19598, "eprint_status": "archive", "datestamp": "2023-08-22 00:33:52", "lastmod": "2023-10-20 21:11:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "K." } }, { "id": "Battle-J", "name": { "family": "Battle", "given": "J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V." } }, { "id": "Keating-B", "name": { "family": "Keating", "given": "B." } }, { "id": "Lee-D-H", "name": { "family": "Lee", "given": "D. H." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Mason-P", "name": { "family": "Mason", "given": "P." } }, { "id": "Matsumoto-T", "name": { "family": "Matsumoto", "given": "T." } }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "S." }, "orcid": "0000-0002-5698-9634" }, { "id": "Nam-Uk-Won", "name": { "family": "Nam", "given": "U. W." } }, { "id": "Renbarger-T", "name": { "family": "Renbarger", "given": "T." } }, { "id": "Sullivan-I", "name": { "family": "Sullivan", "given": "I." } }, { "id": "Suzuki-K", "name": { "family": "Suzuki", "given": "K." } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "T." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Observations of the Near-infrared Spectrum of the Zodiacal Light with CIBER", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: diffuse background; interplanetary medium; zodiacal dust", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2010 April 27; accepted 2010 June 14; published 2010 July 20.\n\nThis work was supported by KAKENHI (20\u00b734, 18204018,\n19540250, 21111004, and 21340047) from Japan Society for\nthe Promotion of Science (JSPS) and the Ministry of Education,\nCulture, Sports, Science and Technology (MEXT), and\nNASA APRA research grants (NNX07AI54G, NNG05WC18G,\nNNX07AG43G, and NNX07AJ24G).We acknowledge the dedicated\nefforts of the sounding rocket staff at NASA Wallops\nFlight Facility and White Sands Missile Range. We also acknowledge\nthe engineers at the Genesia Corporation for the\ntechnical support of the CIBER optics. We thank Dr. Allan\nSmith, Dr. Keith Lykke, and Dr. Steven Brown (the National\nInstitute of Standards and Technology) for the laboratory calibration\nof LRS. We also thank Dr. Hasegawa Sunao (ISAS/\nJAXA), Dr. Ishiguro Masateru (Seoul National University), Dr.\nOotsubo Takafumi (Tohoku University), Dr. Noguchi Takaaki\n(Ibaraki University), Dr. Pyo Jeonghyun (KASI), and Dr. Carey\nLisse (Johns Hopkins University) for discussions and comments\nabout IPD, and Dr. Martin Cohen (UC Berkeley) and Dr.\nYamamura Issei (ISAS/JAXA) for comments about stellar \nspectrum. K.T. acknowledges support from the JSPS Research\nFellowship for theYoung Scientists,M.Z. acknowledges support\nfrom a NASA Postdoctoral Fellowship, and A.C. acknowledges\nsupport from an NSF CARRER award.\n\nPublished - Tsumura2010p11124Astrophys_J.pdf
", "abstract": "Interplanetary dust (IPD) scatters solar radiation which results in the zodiacal light that dominates the celestial diffuse brightness at optical and near-infrared wavelengths. Both asteroid collisions and cometary ejections produce the IPD, but the relative contribution from these two sources is still unknown. The low resolution spectrometer (LRS) onboard the Cosmic Infrared Background ExpeRiment (CIBER) observed the astrophysical sky spectrum between 0.75 and 2.1 \u03bcm over a wide range of ecliptic latitude. The resulting zodiacal light spectrum is redder than the solar spectrum, and shows a broad absorption feature, previously unreported, at approximately 0.9 \u03bcm, suggesting the existence of silicates in the IPD material. The spectral shape of the zodiacal light is isotropic at all ecliptic latitudes within the measurement error. The zodiacal light spectrum, including the extended wavelength range to 2.5 \u03bcm using Infrared Telescope in Space (IRTS) data, is qualitatively similar to the reflectance of S-type asteroids. This result can be explained by the proximity of S-type asteroidal dust to Earth's orbit, and the relatively high albedo of asteroidal dust compared with cometary dust.", "date": "2010-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "719", "number": "1", "publisher": "American Astronomical Society", "pagerange": "394-402", "id_number": "CaltechAUTHORS:20100823-131524312", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100823-131524312", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "20\u00b734" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "18204018" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "19540250" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21111004" }, { "agency": "Japan Society for the Promotion of Science (JSPS)", "grant_number": "21340047" }, { "agency": "NASA", "grant_number": "NNX07AI54G" }, { "agency": "NASA", "grant_number": "NNG05WC18G" }, { "agency": "NASA", "grant_number": "NNX07AG43G" }, { "agency": "NASA", "grant_number": "NNX07AJ24G" }, { "agency": "Ministry of Education, Culture, Sports, Science and Technology (MEXT)" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/719/1/394", "primary_object": { "basename": "Tsumura2010p11124Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/rqh79-ppw08/files/Tsumura2010p11124Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Tsumura, K.; Battle, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/pqp6y-b2w73", "eprint_id": 20974, "eprint_status": "archive", "datestamp": "2023-08-22 00:23:11", "lastmod": "2023-10-20 23:38:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rawle-T-D", "name": { "family": "Rawle", "given": "T. D." } }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Appleton-P-N", "name": { "family": "Appleton", "given": "P. N." }, "orcid": "0000-0002-7607-8766" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } } ] }, "title": "Deep Herschel view of obscured star formation in the Bullet cluster", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual: Bullet cluster; galaxies: star formation; infrared: galaxies; submillimeter: galaxies", "note": "\u00a9 2010 ESO.\n\nReceived 31 March 2010; Accepted 11 May 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Data presented in this paper were analyzed using \"The Herschel Interactive Processing Environment (HIPE)\", a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia.\n\nThis work is based in part on observations made with\nHerschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.\n\nPublished - Rawle2010p11849Astron_Astrophys.pdf
", "abstract": "We use deep, five band (100\u2013500 \u03bcm) data from the Herschel Lensing Survey (HLS) to fully constrain the obscured star formation rate, SFR_(FIR), of galaxies in the Bullet cluster (z = 0.296), and a smaller background system (z = 0.35) in the same field. Herschel detects 23 Bullet cluster members with a total SFRFIR = 144\u00b114 M_\u2609 yr^(-1). On average, the background system contains brighter far-infrared (FIR) galaxies, with ~50% higher SFRFIR (21 galaxies; 207 \u00b1 9 M_\u2609 yr^(-1)). SFRs extrapolated from 24 \u03bcm flux via recent templates (SFR_(24 \u00b5m)) agree well with SFRFIR for ~60% of the cluster galaxies. In the remaining ~40%, SFR24 \u00b5m underestimates SFR_(FIR) due to a significant excess in observed S_(100)/S_(24) (rest frame S_(75)/S_(18)) compared to templates of the same FIR luminosity.", "date": "2010-07-16", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L14", "id_number": "CaltechAUTHORS:20101123-094918178", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101123-094918178", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "JPL/Caltech" } ] }, "doi": "10.1051/0004-6361/201014681", "primary_object": { "basename": "Rawle2010p11849Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/pqp6y-b2w73/files/Rawle2010p11849Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Rawle, T. D.; Fadda, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/0zjsr-4dd25", "eprint_id": 21079, "eprint_status": "archive", "datestamp": "2023-08-19 03:01:07", "lastmod": "2023-10-20 23:44:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Wright-G", "name": { "family": "Wright", "given": "G." } } ] }, "title": "FIR colours and SEDs of nearby galaxies observed with Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM, galaxies: spiral, galaxies: elliptical and lenticular, cD, infrared: galaxies", "note": "\u00a9 2010 ESO. Received 29 March 2010, Accepted 9 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by Principal Investigator consortia. It is open for proposals\nfor observing time from the worldwide astronomical community. SPIRE has been developed by a consortium of institutes\nled by Cardiff University (UK) and including Univ. Lethbridge (Canada);\nNAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain);\nStockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado\n(USA). This development has been supported by national funding agencies: CSA\n(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN\n(Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).\n\nPublished - Boselli2010p11877Astron_Astrophys.pdf
", "abstract": "We present infrared colours (in the 25\u2212500 \u03bcm spectral range) and UV to radio continuum spectral energy distributions of a sample of 51 nearby galaxies observed with SPIRE on Herschel. The observed sample includes all morphological classes, from quiescent ellipticals to active starbursts. Active galaxies have warmer colour temperatures than normal spirals. In ellipticals hosting a radio galaxy, the far-infrared (FIR) emission is dominated by the synchrotron nuclear emission. The colour temperature of the cold dust is higher in quiescent E-S0a than in star-forming systems probably because of the different nature of their dust heating sources (evolved stellar populations, X-ray, fast electrons) and dust grain properties. In contrast to the colour temperature of the warm dust, the f350/ f500 index sensitive to the cold dust decreases with star formation and increases with metallicity, suggesting an overabundance of cold dust or an emissivity parameter \u03b2 <2 in low metallicity, active systems.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L61", "id_number": "CaltechAUTHORS:20101130-162459328", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101130-162459328", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014534", "primary_object": { "basename": "Boselli2010p11877Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/0zjsr-4dd25/files/Boselli2010p11877Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Boselli, A.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/6b71g-an727", "eprint_id": 20801, "eprint_status": "archive", "datestamp": "2023-08-22 00:12:56", "lastmod": "2023-10-20 23:27:58", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" } ] }, "title": "First detection of the Sunyaev Zel'dovich effect increment at \u03bb < 650 \u03bcm", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; galaxies: clusters: individual: 1E0657\u221256", "note": "\u00a9 2010 ESO.\n\nReceived 31 March 2010; Accepted 10 May 2010.\nPublished online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. It is open for proposals for observing time from the worldwide astronomical community. Data presented in this paper were analyzed using \"The Herschel interactive processing environment (HIPE)\", a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. \n\nThis work is based in part on observations made with\nHerschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.\n\nPublished - Zemcov2010p11847Astron_Astrophys.pdf
", "abstract": "The Sunyaev-Zel'dovich (SZ) effect is a spectral distortion of the cosmic microwave background as observed through the hot plasma in galaxy clusters. This distortion is a decrement in the CMB intensity for \u03bb > 1.3 mm, an increment at shorter wavelengths, and small again by \u03bb ~ 250 \u03bcm. As part of the Herschel Lensing Survey (HLS) we have mapped 1E0657\u201356 (the Bullet cluster) with SPIRE with bands centered at 250, 350 and 500 \u03bcm and have detected the SZ effect at the two longest wavelengths. The measured SZ effect increment central intensities are \u0394I_0 = 0.097 \u00b1 0.019 MJy\u2009sr^(-1) at 350 \u03bcm and \u0394I_0 = 0.268 \u00b1 0.031 MJy\u2009sr^(-1) at 500 \u03bcm, consistent with the SZ effect spectrum derived from previous measurements at 2 mm. No other diffuse emission is detected. The presence of the finite temperature SZ effect correction is preferred by the SPIRE data at a significance of 2.1\u03c3, opening the possibility that the relativistic SZ effect correction can be constrained by SPIRE in a sample of clusters. The results presented here have important ramifications for both sub-mm measurements of galaxy clusters and blank field surveys with SPIRE.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L16", "id_number": "CaltechAUTHORS:20101115-102053323", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101115-102053323", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1051/0004-6361/201014685", "primary_object": { "basename": "Zemcov2010p11847Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/6b71g-an727/files/Zemcov2010p11847Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Zemcov, M.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/ptb0m-cd375", "eprint_id": 21098, "eprint_status": "archive", "datestamp": "2023-08-19 03:01:33", "lastmod": "2023-10-20 23:45:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Eales-S-A", "name": { "family": "Eales", "given": "S. A." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "First results from HerMES on the evolution of the submillimetre luminosity function", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evoluton, galaxies: formation, galaxies: high-redshift, submillimeter: galaxies", "note": "\u00a9 2010 ESO. Received 31 March 2010, Accepted 5 May 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. SPIRE has been developed by a consortium of institutes led\nby Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC\n(China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm\nObservatory (Sweden); STFC (UK); and NASA (USA).\n\nPublished - Eales2010p11855Astron_Astrophys.pdf
", "abstract": "We have carried out two extremely deep surveys with SPIRE, one of the two cameras on Herschel, at 250 \u03bcm, close to the peak of the far-infrared background. We have used the results to investigate the evolution of the rest-frame 250-\u03bcm luminosity function out to z = 2. We find evidence for strong evolution out to z \u2243 1 but evidence for at most weak evolution beyond this redshift. Our results suggest that a significant part of the stars and metals in the universe today were formed at z \u2264 1.4 in spiral galaxies.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L23", "id_number": "CaltechAUTHORS:20101201-111403706", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-111403706", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014675", "primary_object": { "basename": "Eales2010p11855Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/ptb0m-cd375/files/Eales2010p11855Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Eales, S. A.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/54sf3-dwk05", "eprint_id": 20802, "eprint_status": "archive", "datestamp": "2023-08-22 00:13:02", "lastmod": "2023-10-20 23:28:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hatziminaoglou-E", "name": { "family": "Hatziminaoglou", "given": "E." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: Far infrared properties of known AGN in the HerMES fields", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: active; galaxies: Seyfert; galaxies: star formation; infrared: general; quasars: general", "note": "\u00a9 2010 ESO.\n\nReceived 31 March 2010; Accepted 19 April 2010.\nPublished online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nSPIRE has been developed by a consortium of institutes\nled by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille HeDaM2. This work makes use of data taken with the Spitzer Space Telescope, the Sloan Digital Sky Survey (http://www.sdss.org) and the Two Micron All Sky Survey \n(http://www.ipac.caltech.edu/2mass/overview/access.html). This work made use of Virtual Observatory tools and services for catalogue searches, crosscorrelation and plotting namely TOPCAT \n(http://www.star.bris.ac.uk/~mbt/topcat/), and VizieR (http://vizier.u-strasbg.fr/cgi-bin/VizieR). E.H. would like to thank Kambiz Fathi and Jacopo Fritz for the very\nuseful discussions. We thank the anonymous referee for the very insightful comments.\n\nPublished - Hatziminaoglou2010p11864Astron_Astrophys.pdf
", "abstract": "Nuclear and starburst activity are known to often occur concomitantly. Herschel-SPIRE provides sampling of the far-infrared (FIR) spectral energy distributions (SEDs) of type 1 and type 2 AGN, allowing for the separation between the hot dust (torus) and cold dust (starburst) emission. We study large samples of spectroscopically confirmed type 1 and type 2 AGN lying within the Herschel Multi-tiered Extragalactic Survey (HerMES) fields observed during the science demonstration phase, aiming to understand their FIR colour distributions and constrain their starburst contributions. We find that one third of the spectroscopically confirmed AGN in the HerMES fields have 5\u03c3 detections at 250\u2009\u03bcm, in agreement with previous (sub)mm AGN studies. Their combined Spitzer-MIPS and Herschel-SPIRE colours (specifically S_(250)/S_(70) vs S_(70)/S_(24)) quite clearly separate them from the non-AGN, star forming galaxy population, as their 24 \u03bcm flux is dominated by the hot torus emission. However, their SPIRE colours alone do not differ from those of non-AGN galaxies. SED fitting shows that all those AGN need a starburst component to fully account for their FIR emission. For objects at z > 2 we find a correlation between the infrared luminosity attributed to the starburst component, LSB, and the AGN accretion luminosity, L_(acc), with L_(SB) \u221d L_(acc)^(0.35). Type 2 AGN detected at 250\u2009\u03bcm show on average higher LSB than type 1 objects but their number is still too low to establish whether this trend indicates stronger star formation activity.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L33", "id_number": "CaltechAUTHORS:20101115-102122698", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101115-102122698", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014679", "primary_object": { "basename": "Hatziminaoglou2010p11864Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/54sf3-dwk05/files/Hatziminaoglou2010p11864Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Hatziminaoglou, E.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/vfyg7-a2f51", "eprint_id": 21083, "eprint_status": "archive", "datestamp": "2023-08-19 03:01:17", "lastmod": "2023-10-20 23:45:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: Halo occupation number and bias properties of dusty galaxies from angular clustering measurements", "ispublished": "pub", "full_text_status": "public", "keywords": "submillimeter: galaxies, large-scale structure of Universe, cosmology: observations, galaxies: evolution, galaxies: high-redshift", "note": "\u00a9 2010 ESO. Received 31 March 2010, Accepted 19 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. Cooray, Amblard, Serra, Khostovan, and Mitchell-Wynne\nare supported by NASA funds for US participants in Herschel through an award\nfrom JPL. SPIRE has been developed by a consortium of institutes led by Cardiff\nUniversity (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada);\nNAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain);\nSNSB (Sweden); STFC (UK); and NASA (USA). The data presented in this\npaper will be released through the HeDaM Database in Marseille.\n\nPublished - Cooray2010p11852Astron_Astrophys.pdf
", "abstract": "We measure the angular correlation function, w(\u03b8), from 0.5 to 30 arcmin of detected sources in two wide fields of the Herschel Multi-tiered Extragalactic Survey (HerMES). Our measurements are consistent with the expected clustering shape from a population of sources that trace the\ndark matter density field, including non-linear clustering at arcminute angular scales arising from multiple sources that occupy the same dark matter halos. By making use of the halo model to connect the spatial clustering of sources to the dark matter halo distribution, we estimate source\nbias and halo occupation number for dusty sub-mm galaxies at z ~ 2. We find that sub-mm galaxies with 250 \u03bcm flux densities above 30 mJy reside in dark matter halos with mass above (5 \u00b1 4) \u00d7 10^(12) M_\u2299 while (14 \u00b1 8)% of such sources appear as satellites in more massive halos.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L22", "id_number": "CaltechAUTHORS:20101201-081855281", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-081855281", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014597", "primary_object": { "basename": "Cooray2010p11852Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/vfyg7-a2f51/files/Cooray2010p11852Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Cooray, A.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/4d2ya-ktq05", "eprint_id": 20943, "eprint_status": "archive", "datestamp": "2023-08-22 00:15:11", "lastmod": "2023-10-20 23:36:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S. J." }, "orcid": "0000-0001-7862-1032" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J. D." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: SPIRE galaxy number counts at 250, 350, and 500 \u03bcm", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; submillimeter: galaxies; surveys", "note": "\u00a9 2010 ESO.\n\nReceived 1 April 2010; Accepted 12 May 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nOliver, Wang and Smith were supported by UK's Science\nand Technology Facilities Council grant ST/F002858/1. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France);\nASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). HIPE is a joint development (are joint developments) by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science\nCenter, and the HIFI, PACS and SPIRE consortia\". The data presented in this paper will be released through the Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES).\n\nPublished - Oliver2010p11848Astron_Astrophys.pdf
", "abstract": "Emission at far-infrared wavelengths makes up a significant fraction of the total light detected from galaxies over the age of Universe. Herschel provides an opportunity for studying galaxies at the peak wavelength of their emission. Our aim is to provide a benchmark for models of galaxy population evolution and to test pre-existing models of galaxies. With the Herschel Multi-tiered Extra-galactic survey, HerMES, we have observed a number of fields of different areas and sensitivity using the SPIRE instrument on Herschel. We have determined the number counts of galaxies down to ~20 mJy. Our constraints from directly counting galaxies are consistent with, though more precise than, estimates from the BLAST fluctuation analysis. We have found a steep rise in the Euclidean normalised counts <100 mJy. We have directly resolved ~15% of the infrared extra-galactic background at the wavelength near where it peaks.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L21", "id_number": "CaltechAUTHORS:20101122-111936760", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101122-111936760", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)", "grant_number": "ST/F002858/1" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014697", "primary_object": { "basename": "Oliver2010p11848Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/4d2ya-ktq05/files/Oliver2010p11848Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Oliver, S. J.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/wtvng-g8j47", "eprint_id": 21132, "eprint_status": "archive", "datestamp": "2023-08-19 03:02:32", "lastmod": "2023-10-20 23:46:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Marshall-J", "name": { "family": "Marshall", "given": "J." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: The SPIRE confusion limit", "ispublished": "pub", "full_text_status": "public", "keywords": "space vehicules: instruments, surveys, submillimeter: diffuse background, submillimiter: galaxies", "note": "\u00a9 2010 ESO. Received 31 March 2010, Accepted 20 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. SPIRE has been developed by a consortium of institutes led\nby Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC\n(China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB\n(Sweden); STFC (UK); and NASA (USA).\n\nPublished - Nguyen2010p11837Astron_Astrophys.pdf
", "abstract": "We report on the sensitivity of SPIRE photometers on the Herschel Space Observatory. Specifically, we measure the confusion noise from observations taken during the science demonstration phase of the Herschel Multi-tiered Extragalactic Survey. Confusion noise is defined to be the\nspatial variation of the sky intensity in the limit of infinite integration time, and is found to be consistent among the different fields in our survey at the level of 5.8, 6.3 and 6.8 mJy/beam at 250, 350 and 500 \u03bcm, respectively. These results, together with the measured instrument noise, may be used to estimate the integration time required for confusion limited maps, and provide a noise estimate for maps obtained by SPIRE.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L5", "id_number": "CaltechAUTHORS:20101202-143136718", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101202-143136718", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014680", "primary_object": { "basename": "Nguyen2010p11837Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/wtvng-g8j47/files/Nguyen2010p11837Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Nguyen, H. T.; Schulz, B.; et el." }, { "id": "https://authors.library.caltech.edu/records/xp4jn-t7g17", "eprint_id": 21141, "eprint_status": "archive", "datestamp": "2023-08-19 03:02:53", "lastmod": "2023-10-20 23:47:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "HerMES: The submillimeter spectral energy distributions of Herschel/SPIRE-detected galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "submillimeter: galaxies, galaxies: evolution, galaxies: high-redshift", "note": "\u00a9 2010 ESO. Received 31 March 2010, Accepted 13 May 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. SPIRE has been developed by a consortium of institutes led\nby Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC\n(China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB\n(Sweden); STFC (UK); and NASA (USA). Support for this work was provided\nby NASA through an award issued by JPL, Caltech. Data presented in this paper\nwere analyzed using The Herschel interactive processing environment (HIPE),\na joint development by the Herschel Science Ground Segment Consortium, consisting\nof ESA, the NASA Herschel Science Center, and the HIFI, PACS and\nSPIRE consortia. The data presented in this paper will be released through the\nHerschel Database in Marseille HeDaM2. This work made substantial use of\nTOPCAT written by Mark Taylor3. We thank Mattia Negrello for predictions of lensed counts. Many thanks also to George Helou and an anonymous referee for\nhelpful comments.\n\nPublished - Schulz2010p11860Astron_Astrophys.pdf
", "abstract": "We present colours of sources detected with the Herschel/SPIRE instrument in deep extragalactic surveys of the Lockman Hole, Spitzer-FLS, and GOODS-N fields in three photometric bands at 250, 350 and 500 \u03bcm. We compare these with expectations from the literature and discuss\nassociated uncertainties and biases in the SPIRE data. We identify a 500 \u03bcm flux limited selection of sources from the HerMES point source catalogue that appears free from neighbouring/blended sources in all three SPIRE bands. We compare the colours with redshift tracks of various\ncontemporary models. Based on these spectral templates we show that regions corresponding to specific population types and redshifts can be identified better in colour-flux space. The redshift tracks as well as the colour-flux plots imply a majority of detected objects with redshifts at\n1 < z < 3.5, somewhat depending on the group of model SEDs used. We also find that a population of sources with S_(250)/S_(350) < 0.8 at fluxes above 50 mJy as observed by SPIRE are not well represented by contemporary models and could consist of a mix of cold and lensed galaxies.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L32", "id_number": "CaltechAUTHORS:20101203-082006802", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101203-082006802", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014673", "primary_object": { "basename": "Schulz2010p11860Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/xp4jn-t7g17/files/Schulz2010p11860Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Schulz, B.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/wvgec-c7590", "eprint_id": 20916, "eprint_status": "archive", "datestamp": "2023-08-22 00:14:50", "lastmod": "2023-10-20 23:35:17", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" } ] }, "title": "Herschel and SCUBA-2 imaging and spectroscopy of a bright, lensed submillimetre galaxy at z = 2.3", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution; infrared: galaxies; infrared: ISM; radio continuum: galaxies; submillimeter: galaxies", "note": "\u00a9 2010 ESO.\n\nReceived 30 March 2010; Accepted 20 April 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nWe thank Steve Hailey-Dunsheath for useful discussion. We thank Fred Lo for granting DDT observations, and Wayne Holland for observing SMMJ2135 during SCUBA-2 commissioning. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). SCUBA-2 is funded by STFC, the JCMT Development Fund and the Canadian Foundation for Innovation.\n\nPublished - Ivison2010p11859Astron_Astrophys.pdf
", "abstract": "We present a detailed analysis of the far-infrared (-IR) properties of the bright, lensed, z = 2.3, submillimetre-selected galaxy (SMG), SMM\u2009J2135-0102 (hereafter SMM\u2009J2135), using new observations with Herschel, SCUBA-2 and the Very Large Array (VLA). These data allow us to constrain the galaxy's spectral energy distribution (SED) and show that it has an intrinsic rest-frame 8-1000-\u03bcm luminosity, L_(bol), of (2.3\u00b10.2) \u00d7 10^(12) L_\u2609 and a likely star-formation rate (SFR) of ~400 yr-1. The galaxy sits on the far-IR/radio correlation for far-IR-selected galaxies. At \u227370 \u03bcm, the SED can be described adequately by dust components with dust temperatures, T_d ~ 30 and 60 k. Using SPIRE's Fourier- transform spectrometer (FTS) we report a detection of the [C ii]\u2009158 \u03bcm cooling line. If the [C ii], CO and far-IR continuum arise in photo-dissociation regions (PDRs), we derive a characteristic gas density, n ~ 10^3 cm^(-3), and a far-ultraviolet (-UV) radiation field, G_0, 10^(3)\u00d7 stronger than the Milky Way. L_[CII]/L_(bol) is significantly higher than in local ultra-luminous IR galaxies (ULIRGs) but similar to the values found in local star-forming galaxies and starburst nuclei. This is consistent with SMM\u2009J2135 being powered by starburst clumps distributed across ~2 kpc, evidence that SMGs are not simply scaled-up ULIRGs. Our results show that SPIRE's FTS has the ability to measure the redshifts of distant, obscured galaxies via the blind detection of atomic cooling lines, but it will not be competitive with ground-based CO-line searches. It will, however, allow detailed study of the integrated properties of high-redshift galaxies, as well as the chemistry of their interstellar medium (ISM), once more suitably bright candidates have been found.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L35", "id_number": "CaltechAUTHORS:20101119-104348447", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101119-104348447", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'\u00c9nergie Atomique (CEA) (France)" }, { "agency": "Centre National d'Etudes Spatiales (CNES) (France)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS) (France)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MICIIN) (Spain)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "doi": "10.1051/0004-6361/201014548", "primary_object": { "basename": "Ivison2010p11859Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/wvgec-c7590/files/Ivison2010p11859Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Ivison, R. J.; Blain, A. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/qvba8-qwn76", "eprint_id": 21022, "eprint_status": "archive", "datestamp": "2023-08-22 00:15:56", "lastmod": "2023-10-20 23:41:41", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "O'Halloran-B", "name": { "family": "O'Halloran", "given": "B." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "Herschel photometric observations of the low metallicity dwarf galaxy NGC 1705", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: dwarf; dust, extinction; evolution", "note": "\u00a9 2010 ESO.\n\nReceived 30 March 2010; Accepted 11 May 2010; Published online 16 July 2010.\n\nSPIRE has been developed by a consortium of institutes\nled by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, OAMP (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies\nBMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain).\n\nPublished - OHalloran2010p11879Astron_Astrophys.pdf
", "abstract": "We present Herschel SPIRE and PACS photometeric observations of the low metallicity (Z ~ 0.35 Z_\u2609) nearby dwarf galaxy, NGC 1705, in six wavelength bands as part of the Dwarf Galaxy Survey guaranteed time Herschel key program. We confirm the presence of two dominant circumnuclear IR-bright regions surrounding the central super star cluster that had been previously noted at mid-IR wavelengths and in the sub-mm by LABOCA. On constructing a global spectral energy distribution using the SPIRE and PACS photometry, in conjunction with archival IR measurements, we note the presence of an excess at sub-mm wavelengths. This excess suggests the presence of a significant cold dust component within NGC 1705 and was modeled as an additional cold component in the SED. Although alternative explanations for the sub-mm excess beyond 350 \u03bcm, such as changes to the dust emissivity cannot be ruled out, the most likely explanation for the observed submillimetre excess is that of an additional cold dust component.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L58", "id_number": "CaltechAUTHORS:20101124-111335303", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101124-111335303", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'\u00c9nergie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MICIIN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency-PROgramme for the Development of scientific EXperiments (ESA-PRODEX) (Belgium)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014580", "primary_object": { "basename": "OHalloran2010p11879Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/qvba8-qwn76/files/OHalloran2010p11879Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "O'Halloran, B.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/n16ep-66892", "eprint_id": 20917, "eprint_status": "archive", "datestamp": "2023-08-22 00:14:55", "lastmod": "2023-10-20 23:35:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Galametz-M", "name": { "family": "Galametz", "given": "M." }, "orcid": "0000-0002-0283-8689" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "Herschel photometric observations of the nearby low metallicity irregular galaxy NGC 6822", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; galaxies: dwarf; galaxies: photometry", "note": "\u00a9 2010 ESO.\n\nReceived 31 March 2010; Accepted 21 April 2010; Published online 16 July 2010.\n\nHerschel\u2002is an ESA space observatory with science instruments provided by Principal Investigator consortia. It is open for proposals for observing time from the worldwide astronomical community.\n\nWe thank the referee for his comments that help to improve\nthe quality of this paper. We also thank Erwin de Blok for the integrated H i map of NGC 6822. PACS has been developed by MPE (Germany); UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by BMVIT (Austria), ESAPRODEX\n(Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by Cardiff University (UK); Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); SNSB (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK) and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).\n\nPublished - Galametz2010p11869Astron_Astrophys.pdf
", "abstract": "We present the first Herschel PACS and SPIRE images of the low-metallicity galaxy NGC 6822 observed from 70 to 500 \u03bcm and clearly resolve the H ii regions with PACS and SPIRE. We find that the ratio 250/500 is dependent on the 24 \u03bcm surface brightness in NGC 6822, which would locally link the heating processes of the coldest phases of dust in the ISM to the star formation activity. We model the SEDs of some regions H ii regions and less active regions across the galaxy and find that the SEDs of H ii regions show warmer ranges of dust temperatures. We derive very high dust masses when graphite is used in our model to describe carbon dust. Using amorphous carbon, instead, requires less dust mass to account for submm emission due to its lower emissivity properties. This indicates that SED models including Herschel constraints may require different dust properties than commonly used. The global G/D of NGC 6822 is finally estimated to be 186, using amorphous carbon.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L55", "id_number": "CaltechAUTHORS:20101119-104442883", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101119-104442883", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency-PROgramme for the Development of scientific EXperiments (ESA-PRODEX) (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutschland f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MICIIN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Ministerio de Ciencia y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014604", "primary_object": { "basename": "Galametz2010p11869Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/n16ep-66892/files/Galametz2010p11869Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Galametz, M.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/rrfsc-srz18", "eprint_id": 21109, "eprint_status": "archive", "datestamp": "2023-08-19 03:01:48", "lastmod": "2023-10-20 23:46:08", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "D." }, "orcid": "0000-0002-7631-647X" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chary-R-R", "name": { "family": "Chary", "given": "R.-R." }, "orcid": "0000-0001-7583-0621" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Herschel unveils a puzzling uniformity of distant dusty galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: active, galaxies: starburst, infrared: galaxies", "note": "\u00a9 2010 ESO. Received 31 March 2010, Accepted 23 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. PACS has been developed by a consortium of institutes\nled by MPE (Germany) and including UVIE (Austria); KU Leuven,\nCSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/\nOAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been\nsupported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium),\nCEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT\n(Spain). SPIRE has been developed by a consortium of institutes led by Cardiff\nUniversity (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC\n(China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm\nObservatory (Sweden); STFC (UK); and NASA (USA).\n\nPublished - Elbaz2010p11858Astron_Astrophys.pdf
", "abstract": "The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved over the last 80% of the age of the Universe. We discuss possible consequences for the determination of starformation\nrates (SFR) and any evidence for a major change in their star-formation properties. We use Herschel deep extragalactic surveys from 100 to 500 \u03bcm to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and\nHerMES key programs). An extension to fainter luminosities is done by stacking images on 24 \u03bcm prior positions. We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used, e.g. at 24 \u03bcm, to identify\n\"isolated\" galaxies whose flux is not boosted by bright neighbors. Below z ~ 1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15 dex), therefore similar to z ~ 0 galaxies, over three decades in luminosity below the regime of ultra-luminous IR galaxies (ULIRGs, L_(IR) \u2265 10^(12) L_\u2299). This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160 \u03bcm, 250 \u03bcm or 350 \u03bcm bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ~150 \u03bcm (rest-frame) before Herschel on those templates. We also note that the dust temperature of luminous IR galaxies (LIRGs, L_(IR) \u2265 10^(11) L_\u2299) around z ~ 1 is mildly colder by 10\u201315% than their local analogs and up to 20% for ULIRGs at z ~ 1.6 (using a single modified blackbody-fit to the peak far-IR emission with an emissivity index of \u03b2 = 1.5). Above z = 1.5, distant galaxies are found to exhibit a substantially larger mid- over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor coeval star formation at very high SFR and in conditions similar to purely star-forming galaxies.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L29", "id_number": "CaltechAUTHORS:20101202-085141496", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101202-085141496", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency (ESA) PROgramme for the Development of scientific EXperiments (PRODEX) (Belgium)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Istituto Nazionale di Astrofisica (INAF)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014687", "primary_object": { "basename": "Elbaz2010p11858Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/rrfsc-srz18/files/Elbaz2010p11858Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Elbaz, D.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/nt43b-mhc81", "eprint_id": 21024, "eprint_status": "archive", "datestamp": "2023-08-19 03:00:28", "lastmod": "2023-10-20 23:41:47", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Amblard-A", "name": { "family": "Amblard", "given": "A." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D." }, "orcid": "0000-0003-1924-1122" }, { "id": "Vieira-J-D", "name": { "family": "Vieira", "given": "J." } } ] }, "title": "Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours", "ispublished": "pub", "full_text_status": "public", "keywords": "submillimeter: galaxies, Galaxy: evolution, galaxies: high-redshift", "note": "\u00a9 2010 ESO. Received 30 March 2010, Accepted 26 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Amblard, Barton, Cooray, Leeuw, Serra and Temi acknowledge\nsupport from NASA funds for US participants in Herschel through JPL.\nFunding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan\nFoundation, the Participating Institutions, the National Science Foundation, the\nUS Department of Energy, the National Aeronautics and Space Administration,\nthe Japanese Monbukagakusho, the Max Planck Society, and the Higher\nEducation Funding Council for England. The SDSS Web Site is http://www.\nsdss.org/. The SDSS is managed by the Astrophysical Research Consortium\nfor the Participating Institutions.\nThe UKIDSS project is defined in Lawrence et al. (2007).\n\nPublished - Amblard2010p11844Astron_Astrophys.pdf
", "abstract": "We present colour\u2013colour diagrams of detected sources in the Herschel-ATLAS science demonstration field from 100 to 500 \u03bcm using both PACS and SPIRE. We fit isothermal modified black bodies to the spectral energy distribution (SED) to extract the dust temperature of sources with counterparts in Galaxy And Mass Assembly (GAMA) or SDSS surveys with either a spectroscopic or a photometric redshift. For a subsample of 330 sources detected in at least three FIR bands with a significance greater than 3\u03c3, we find an average dust temperature of (28\u00b18) K. For sources with no known redshift, we populate the colour\u2013colour diagram with a large number of SEDs generated with a broad range of dust temperatures and emissivity parameters, and compare to colours of observed sources to establish the redshift distribution of this sample. For another subsample of 1686 sources with fluxes above 35 mJy at 350 \u03bcm and detected at 250 and 500 \u03bcm with a significance greater than 3\u03c3, we find an average redshift of 2.2 \u00b1 0.6.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L9", "id_number": "CaltechAUTHORS:20101124-113357521", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101124-113357521", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NSF" }, { "agency": "Department of Energy (DOE)" }, { "agency": "Japanese Monbukagakusho" }, { "agency": "Max Planck Society" }, { "agency": "England Higher Education Funding Council" } ] }, "doi": "10.1051/0004-6361/201014586", "primary_object": { "basename": "Amblard2010p11844Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/nt43b-mhc81/files/Amblard2010p11844Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Amblard, A.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/beayn-mn196", "eprint_id": 21093, "eprint_status": "archive", "datestamp": "2023-08-19 03:01:23", "lastmod": "2023-10-20 23:45:33", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Cortese-L", "name": { "family": "Cortese", "given": "L." }, "orcid": "0000-0002-7422-9823" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M-C", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "Herschel-SPIRE observations of the disturbed galaxy NGC4438", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: individual: NGC4438, infrared: galaxies, dust, extinction", "note": "\u00a9 2010 ESO. Received 30 March 2010, Accepted 15 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. We thank Ananda Hota, Jeff Kenney and Bernd Vollmer\nfor providing us with an electronic version of their data. SPIRE has been developed\nby a consortium of institutes led by Cardiff University (UK) and including\nUniv. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI,\nUniv. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial\nCollege London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech,\nJPL, NHSC, Univ. Colorado (USA). This development has been supported by\nnational funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS\n(France); ASI (Italy);MCINN (Spain); Stockholm Observatory (Sweden); STFC\n(UK); and NASA (USA).\n\nPublished - Cortese2010p11875Astron_Astrophys.pdf
", "abstract": "We present Herschel-SPIRE observations of the perturbed galaxy NGC4438 in the Virgo cluster. These images reveal the presence of extra-planar dust up to ~4\u20135 kpc away from the galaxy's disk. The dust closely follows the distribution of the stripped atomic and molecular hydrogen, supporting the idea that gas and dust are perturbed in a similar fashion by the cluster environment. Interestingly, the extra-planar dust lacks a warm temperature component when compared to the material still present in the disk, explaining why it was missed by previous far-infrared investigations. Our study provides evidence for dust stripping in clusters of galaxies and illustrates the potential of Herschel data for our understanding of\nenvironmental effects on galaxy evolution.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "number": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L63", "id_number": "CaltechAUTHORS:20101201-100958345", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-100958345", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES) (France)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014547", "primary_object": { "basename": "Cortese2010p11875Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/beayn-mn196/files/Cortese2010p11875Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Cortese, L.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/daxbh-8df73", "eprint_id": 21089, "eprint_status": "archive", "datestamp": "2023-08-22 00:16:39", "lastmod": "2023-10-20 23:45:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "P\u00e9rez-Gonz\u00e1lez-P-G", "name": { "family": "P\u00e9rez-Gonz\u00e1lez", "given": "P. G." }, "orcid": "0000-0003-4528-5639" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Improving the identification of high-z Herschel sources with position priors and optical/NIR and FIR/mm photometric redshifts", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies; submillimeter: galaxies; galaxies: evolution; galaxies: high-redshift; gravitational lensing: strong; galaxies: photometry", "note": "\u00a9 2010 ESO.\n\nReceived 31 March 2010; Accepted 6 May 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nThis work is based in part on observations made with\nSpitzer, operated by JPL/Caltech. We thank the AzTEC Team for letting us use their data. P.G.P.-G. acknowledges support from grants AYA 2006\u201302358, AYA 2006\u201315698\u2013C02\u201302, and CSD2006-00070, and the Ram\u00f3n y Cajal Program, all financed by the Spanish Government and/or the European Union.\n\nPublished - PerezGonzalez2010p11851Astron_Astrophys.pdf
", "abstract": "We present preliminary results about the detection of high redshift (U)LIRGs in the Bullet cluster field by the PACS and SPIRE instruments within the Herschel Lensing Survey (HLS) Program. We describe in detail a photometric procedure designed to recover robust fluxes and deblend faint Herschel sources near the confusion noise. The method is based on the use of the positions of Spitzer/MIPS 24 \u03bcm sources as priors. Our catalogs are able to reliably (5\u03c3) recover galaxies with fluxes above 6 and 10 mJy in the PACS 100 and 160 \u03bcm channels, respectively, and 12 to 18 mJy in the SPIRE bands. We also obtain spectral energy distributions covering the optical through the far-infrared/millimeter spectral ranges of all the Herschel detected sources, and analyze them to obtain independent estimations of the photometric redshift based on either stellar population or dust emission models. We exemplify the potential of the combined use of Spitzer position priors plus independent optical and IR photometric redshifts to robustly assign optical/NIR counterparts to the sources detected by Herschel and other (sub-)mm instruments.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L15", "id_number": "CaltechAUTHORS:20101201-100758912", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-100758912", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Spanish Government", "grant_number": "AYA 2006\u201302358" }, { "agency": "Spanish Government", "grant_number": "AYA 2006\u201315698\u2013C02\u201302" }, { "agency": "Spanish Government", "grant_number": "CSD2006-00070" }, { "agency": "European Union" } ] }, "doi": "10.1051/0004-6361/201014593", "primary_object": { "basename": "PerezGonzalez2010p11851Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/daxbh-8df73/files/PerezGonzalez2010p11851Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "P\u00e9rez-Gonz\u00e1lez, P. G.; Blain, A. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/q0qee-n6140", "eprint_id": 21100, "eprint_status": "archive", "datestamp": "2023-08-19 03:01:38", "lastmod": "2023-10-20 23:45:52", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Eales-S-A", "name": { "family": "Eales", "given": "S. A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "Mapping the interstellar medium in galaxies with Herschel/SPIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM, galaxies: spiral, dust, extinction, ISM: abundances", "note": "\u00a9 2010 ESO. Received 29 March 2010, Accepted 19 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. SPIRE has been developed by a consortium of institutes led\nby Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China);\nCEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm\nObservatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development\nhas been supported by national funding agencies: CSA (Canada); NAOC\n(China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm\nObservatory (Sweden); STFC (UK); and NASA (USA).\n\nPublished - Eales2010p11880Astron_Astrophys.pdf
", "abstract": "The standard method of mapping the interstellar medium in a galaxy, by observing the molecular gas in the CO 1-0 line and the atomic gas in the 21-cm line, is largely limited with current telescopes to galaxies in the nearby universe. In this letter, we use SPIRE observations of the galaxies\nM99 and M100 to explore the alternative approach of mapping the interstellar medium using the continuum emission from the dust. We have compared the methods by measuring the relationship between the star-formation rate and the surface density of gas in the galaxies using both\nmethods. We find the two methods give relationships with a similar dispersion, confirming that observing the continuum emission from the dust is a promising method of mapping the interstellar medium in galaxies.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L62", "id_number": "CaltechAUTHORS:20101201-114052474", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-114052474", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA) (France)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN) (Spain)" }, { "agency": "Stockholm Observatory (Sweden)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES) (France)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS) (France)" } ] }, "doi": "10.1051/0004-6361/201014536", "primary_object": { "basename": "Eales2010p11880Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/q0qee-n6140/files/Eales2010p11880Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Eales, S. A.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/h1wy5-v7t87", "eprint_id": 20946, "eprint_status": "archive", "datestamp": "2023-08-22 00:15:22", "lastmod": "2023-10-20 23:36:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Panuzzo-P", "name": { "family": "Panuzzo", "given": "P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "Probing the molecular interstellar medium of M82 with Herschel-SPIRE spectroscopy", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM \u2013 galaxies: starburst; galaxies: individual: M82; ISM: molecules; submillimeter: galaxies", "note": "\u00a9 2010 ESO.\n\nReceived 30 March 2010; Accepted 28 April 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nWe are grateful to P. Maloney for his advices on radiative\ntransfer modeling, and to the SPIRE FTS team for assistance with data reduction. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, OAMP (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada);\nNAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). Additional funding support for some instrument activities has been provided by ESA.\n\nPublished - Panuzzo2010p11856Astron_Astrophys.pdf
", "abstract": "We present the observations of the starburst galaxy M82 taken with the Herschel SPIRE Fourier-transform spectrometer. The spectrum (194\u2013671 \u03bcm) shows a prominent CO rotational ladder from J = 4\u20133 to 13\u201312 emitted by the central region of M82. The fundamental properties of the gas are well constrained by the high J lines observed for the first time. Radiative transfer modeling of these high-S/N ^(12)CO and ^(13)CO lines strongly indicates a very warm molecular gas component at ~500 K and pressure of ~3\u00d710^6 K cm^(-3), in good agreement with the H_2 rotational lines measurements from Spitzer and ISO. We suggest that this warm gas is heated by dissipation of turbulence in the interstellar medium (ISM) rather than X-rays or UV flux from the straburst. This paper illustrates the promise of the SPIRE FTS for the study of the ISM of nearby galaxies.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L37", "id_number": "CaltechAUTHORS:20101122-112239522", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101122-112239522", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014558", "primary_object": { "basename": "Panuzzo2010p11856Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/h1wy5-v7t87/files/Panuzzo2010p11856Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Panuzzo, P.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/hpr30-86p28", "eprint_id": 20976, "eprint_status": "archive", "datestamp": "2023-08-22 00:15:33", "lastmod": "2023-10-20 23:38:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pohlen-M", "name": { "family": "Pohlen", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "Radial distribution of gas and dust in spiral galaxies: The case of M\u200999 (NGC\u20094254) and M\u2009100 (NGC\u20094321)", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: structure; galaxies: individual: M99; galaxies: individual: M100; infrared: galaxies; ISM: dust, extinction; submillimetre: galaxies", "note": "\u00a9 2010 ESO.\n\nReceived 30 March 2010; Accepted 19 April 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nSPIRE has been developed by a consortium of institutes led\nby Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). Thanks to Tom Hughes for providing\nthe recalibrated metallicities. The SDSS jpg was taken from http://www.sdss.org using the Finding Chart tool.\n\nPublished - Pohlen2010p11892Astron_Astrophys.pdf
", "abstract": "By combining Herschel-SPIRE data with archival Spitzer, H\u2009i\u2009, and CO maps, we investigate the spatial distribution of gas and dust in the two famous grand-design spirals M\u200999 and M\u2009100 in the Virgo cluster. Thanks to the unique resolution and sensitivity of the Herschel-SPIRE photometer, we are for the first time able to measure the distribution and extent of cool, submillimetre (submm)-emitting dust inside and beyond the optical radius. We compare this with the radial variation in both the gas mass and the metallicity. Although we adopt a model-independent, phenomenological approach, our analysis provides important insights. We find the dust extending to at least the optical radius of the galaxy and showing breaks in its radial profiles at similar positions as the stellar distribution. The colour indices f350/f500 and f250/f350 decrease radially consistent with the temperature decreasing with radius. We also find evidence of an increasing gas to dust ratio with radius in the outer regions of both galaxies.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L72", "id_number": "CaltechAUTHORS:20101123-094951990", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101123-094951990", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014554", "primary_object": { "basename": "Pohlen2010p11892Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/hpr30-86p28/files/Pohlen2010p11892Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Pohlen, M.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/y5wqt-rn406", "eprint_id": 21087, "eprint_status": "archive", "datestamp": "2023-08-22 00:16:28", "lastmod": "2023-10-20 23:45:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "SPIRE imaging of M\u200982: Cool dust in the wind and tidal streams", "ispublished": "pub", "full_text_status": "public", "keywords": "dust, extinction; evolution; galaxies: interactions; galaxies: starburst; infrared: ISM", "note": "\u00a9 2010 ESO.\n\nReceived 30 March 2010; Accepted 13 April 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia, and with important participation from NASA.\n\nWe thank the referee for suggesting useful clarifications,\nL. Leeuw and I. Robson for providing their SCUBA images. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK): Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);\nIAC (Spain); Stockholm Obs. (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA\n(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Obs. (Sweden); STFC (UK); and NASA (USA).\n\nPublished - Roussel2010p11882Astron_Astrophys.pdf
", "abstract": "M\u200982 is a unique representative of a whole class of galaxies, starbursts with superwinds, in the Very Nearby Galaxy Survey with Herschel. In addition, its interaction with the M\u200981 group has stripped a significant portion of its interstellar medium from its disk. SPIRE maps now afford better characterization of the far-infrared emission from cool dust outside the disk, and sketch a far more complete picture of its mass distribution and energetics than previously possible. They show emission coincident in projection with the starburst wind and in a large halo, much more extended than the PAH band emission seen with Spitzer. Some complex substructures coincide with the brightest PAH filaments, and others with tidal streams seen in atomic hydrogen. We subtract the far-infrared emission of the starburst and underlying disk from the maps, and derive spatially-resolved far-infrared colors for the wind and halo. We interpret the results in terms of dust mass, dust temperature, and global physical conditions. In particular, we examine variations in the dust physical properties as a function of distance from the center and the wind polar axis, and conclude that more than two thirds of the extraplanar dust has been removed by tidal interaction, and not entrained by the starburst wind.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L66", "id_number": "CaltechAUTHORS:20101201-100641662", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-100641662", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014567", "primary_object": { "basename": "Roussel2010p11882Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/y5wqt-rn406/files/Roussel2010p11882Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Roussel, H.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/rbr1c-6te72", "eprint_id": 20804, "eprint_status": "archive", "datestamp": "2023-08-22 00:13:08", "lastmod": "2023-10-20 23:28:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The HerMES SPIRE submillimeter local luminosity function", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: luminosity function, mass functions; galaxies: evolution; galaxies: statistics; submillimeter: galaxies", "note": "\u00a9 2010 ESO.\n\nReceived 1 April 2010; Accepted 27 April 2010.\nPublished online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nM.V. acknowledges support from a University of Padova\n\"Herschel & ALMA\" Fellowship and ASI \"Herschel Science\" Contract I/005/07/0. Micol Bolzonella kindly provided advice on the use of hyperz and Mattia Negrello swiftly produced additional predictions based on his models.\nSPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC,\nUniv. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm\nObservatory (Sweden); STFC (UK); and NASA (USA). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM, \nhttp://hedam.oamp.fr/HerMES).\n\nPublished - Vaccari2010p11845Astron_Astrophys.pdf
", "abstract": "Local luminosity functions are fundamental benchmarks for high-redshift galaxy formation and evolution studies as well as for models describing these processes. Determining the local luminosity function in the submillimeter range can help to better constrain in particular the bolometric luminosity density in the local Universe, and Herschel offers the first opportunity to do so in an unbiased way by imaging large sky areas at several submillimeter wavelengths. We present the first Herschel measurement of the submillimeter 0 < z < 0.2 local luminosity function and infrared bolometric (8\u20131000 \u03bcm) local luminosity density based on SPIRE data from the HerMES Herschel key program over 14.7 deg^2. Flux measurements in the three SPIRE channels at 250, 350 and 500 \u03bcm are combined with Spitzer photometry and archival data. We fit the observed optical-to-submillimeter spectral energy distribution of SPIRE sources and use the 1/V_(max) estimator to provide the first constraints on the monochromatic 250, 350 and 500 \u03bcm as well as on the infrared bolometric (8\u20131000 \u03bcm) local luminosity function based on Herschel data. We compare our results with modeling predictions and find a slightly more abundant local submillimeter population than predicted by a number of models. Our measurement of the infrared bolometric (8\u20131000 \u03bcm) local luminosity function suggests a flat slope at low luminosity, and the inferred local luminosity density, 1.31_(-0.21)^(+0.24)\u2009 \u00d7\u200910^8\u2009L_\u2609 Mpc^(-3), is consistent with the range of values reported in recent literature.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L20", "id_number": "CaltechAUTHORS:20101115-102412434", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101115-102412434", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Padova" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/005/07/0" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014694", "primary_object": { "basename": "Vaccari2010p11845Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/rbr1c-6te72/files/Vaccari2010p11845Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Vaccari, M.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/sdd7g-wxj62", "eprint_id": 21101, "eprint_status": "archive", "datestamp": "2023-08-19 03:01:42", "lastmod": "2023-10-20 23:45:54", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Egami-Eichi", "name": { "family": "Egami", "given": "E." } }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } } ] }, "title": "The Herschel Lensing Survey (HLS): Overview", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies, submillimeter: galaxies, galaxies: evolution, galaxies: high-redshift, galaxies: clusters: general", "note": "\u00a9 2010 ESO. Received 1 April 2010, Accepted 19 May 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with\nimportant participation from NASA. Data presented in this paper\nwere analyzed using \"The Herschel interactive processing environment\n(HIPE)\", a joint development by the Herschel Science Ground Segment\nConsortium, consisting of ESA, the NASA Herschel Science Center,\nand the HIFI, PACS and SPIRE consortia. \n\nWe thank the following people for providing various data\nsets/information to us: D. Clowe (Magellan/IMACS images), S. M. Chung and\nA. H. Gonzalez (IMACS spectroscopic redshifts), J.-G. Cuby (VLT/HAWKI images),\nD. Johansson, C. Horellou, and the LABOCA team (LABOCA map), and\nD. Hughes, I. Aretxaga, and the AzTEC team (AzTEC map and far-infrared photometric\nredshifts). We thank the NASA Herschel Science Center for its excellent\nuser support, and the International Space Science Institute in Berne for their\nsupport through the International team 181. EE would like to thank D. Elbaz for\ncommunicating his results before publication.\nThis work is based in part on observations made with Herschel, a European\nSpace Agency Cornerstone Mission with significant participation by NASA.\nSupport for this work was provided by NASA through an award issued by\nJPL/Caltech.\n\nPublished - Egami2010p11854Astron_Astrophys.pdf
", "abstract": "The Herschel Lensing Survey (HLS) will conduct deep PACS and SPIRE imaging of \u223c40 massive clusters of galaxies. The strong gravitational lensing power of these clusters will enable us to penetrate through the confusion noise, which sets the ultimate limit on our ability to probe the\nUniverse with Herschel. Here we present an overview of our survey and a summary of the major results from our science demonstration phase (SDP) observations of the Bullet cluster (z = 0.297). The SDP data are rich and allow us to study not only the background high-redshift galaxies\n(e.g., strongly lensed and distorted galaxies at z = 2.8 and 3.2) but also the properties of cluster-member galaxies. Our preliminary analysis shows a great diversity of far-infrared/submillimeter spectral energy distributions (SEDs), indicating that we have much to learn with Herschel about the properties of galaxy SEDs. We have also detected the Sunyaev-Zel'dovich (SZ) effect increment with the SPIRE data. The success of this SDP program demonstrates the great potential of the Herschel Lensing Survey to produce exciting results in a variety of science areas.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L12", "id_number": "CaltechAUTHORS:20101201-114942947", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101201-114942947", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Berne International Space Science Institute" }, { "agency": "NASA" } ] }, "doi": "10.1051/0004-6361/201014696", "primary_object": { "basename": "Egami2010p11854Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/sdd7g-wxj62/files/Egami2010p11854Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Egami, E.; Blain, A. W.; et el." }, { "id": "https://authors.library.caltech.edu/records/hhsam-grp11", "eprint_id": 21010, "eprint_status": "archive", "datestamp": "2023-08-19 02:59:49", "lastmod": "2023-10-20 23:40:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G. J." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "The Herschel Space Observatory view of dust in M81", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM, galaxies: spiral, galaxies: individual: M81", "note": "\u00a9 2010 ESO. Received 30 March 2010, Accepted 20 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by Principal Investigator consortia. It is open for proposals for\nobserving time from the worldwide astronomical community. We thank A. Fraceschini and E. Murphy for comments on this paper. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain).\n\nPublished - Bendo2010p11878Astron_Astrophys.pdf
", "abstract": "We use Herschel Space Observatory data to place observational constraints on the peak and Rayleigh-Jeans slope of dust emission observed at 70\u2212500 \u03bcm in the nearby spiral galaxy M81. We find that the ratios of wave bands between 160 and 500 \u03bcm are primarily dependent on radius but that the ratio of 70 to 160 \u03bcm emission shows no clear dependence on surface brightness or radius. These\nresults along with analyses of the spectral energy distributions imply that the 160\u2212500 \u03bcm emission traces 15\u221230 K dust heated by evolved stars in the bulge and disc whereas the 70 \u03bcm emission includes dust heated by the active galactic nucleus and young stars in star forming regions.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L65", "id_number": "CaltechAUTHORS:20101124-083351080", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101124-083351080", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency (ESA) PROgramme for the Development of scientific Experiments (PRODEX) (Belgium)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICT)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014568", "primary_object": { "basename": "Bendo2010p11878Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/hhsam-grp11/files/Bendo2010p11878Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Bendo, G. J.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/r472y-3v982", "eprint_id": 21138, "eprint_status": "archive", "datestamp": "2023-08-19 03:02:48", "lastmod": "2023-10-20 23:47:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Sauvage-M", "name": { "family": "Sauvage", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "The central region of spiral galaxies as seen by Herschel: M 81, M 99, and M 100", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies, submillimeter: galaxies, galaxies: spiral, galaxies: nuclei, galaxies: fundamental parameters", "note": "\u00a9 2010 ESO. Received 30 March 2010, Accepted 20 April 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with significant\nparticipation from NASA. SPIRE has been developed by a consortium of institutes\nled by Cardiff University (UK) and including Univ. Lethbridge (Canada);\nNAOC (China); CEA, OAMP (France); IFSI, Univ. Padua (Italy); IAC (Spain);\nStockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL,\nUKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado\n(USA). This development has been supported by national funding agencies: CSA\n(Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN\n(Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).\nPACS has been developed by a consortium of institutes led by MPE (Germany)\nand including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP\n(France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA\n(Italy); IAC (Spain). This development has been supported by the funding agencies\nBMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR\n(Germany), ASI (Italy), and CICT/MCT (Spain).\nThis research has made use of HIPE, a joint development by the Herschel\nScience Ground Segment Consortium, consisting of ESA, the NASA Herschel\nScience Center, and the HIFI, PACS and SPIRE consortia, and of the\nNASA/IPAC Extragalactic Database (NED) which is operated by the Jet\nPropulsion Laboratory, Caltech, under contract with NASA.\n\nPublished - Sauvage2010p11881Astron_Astrophys.pdf
", "abstract": "With appropriate spatial resolution, images of spiral galaxies in thermal infrared (~10 \u03bcm and beyond) often reveal a bright central component, distinct from the stellar bulge, superimposed on a disk with prominent spiral arms. ISO and Spitzer studies have shown that much of the scatter in the mid-infrared colors of spiral galaxies is related to changes in the relative importance of these two components, rather than to other modifications, such as the morphological type or star formation rate, that affect the properties of the galaxy as a whole. With the Herschel imaging capability from 70 to 500 \u03bcm, we revisit this two-component approach at longer wavelengths, to see if it still provides a working description of the brightness\ndistribution of galaxies, and to determine its implications on the interpretation of global far-infrared properties of galaxies. We quantify the luminosity of the central component by both a decomposition of the radial surface brightness profile and a direct extraction in 2D.\nWe find the central component contribution is variable within the three galaxies in our sample, possibly connected more directly to the presence of a bar than to the morphological type. The central component's relative contribution is at its maximum in the mid-infrared range and drops around 160 \u03bcm to reach a constant value beyond 200 \u03bcm. The central component contains a greater fraction of hot dust than the disk component, and while the colors of the central components are scattered, colors of the disk components are more homogenous from one galaxy to the next.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L64", "id_number": "CaltechAUTHORS:20101202-162451019", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101202-162451019", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory (Sweden)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency (ESA) PROgramme for the Development of scientific EXperiments (PRODEX) (Belgium)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Ministerio de Ciencia Y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014588", "primary_object": { "basename": "Sauvage2010p11881Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/r472y-3v982/files/Sauvage2010p11881Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Sauvage, M.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/hfhak-69032", "eprint_id": 20838, "eprint_status": "archive", "datestamp": "2023-08-22 00:13:52", "lastmod": "2023-10-20 23:30:20", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gomez-H-L", "name": { "family": "Gomez", "given": "H. L." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M", "name": { "family": "Bradford", "given": "M." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L. R." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } } ] }, "title": "The dust morphology of the elliptical Galaxy M86 with SPIRE", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ellipticals and lenticular, cD; galaxies: individual: M86; submillimeter: ISM; dust, extinction", "note": "\u00a9 2010 ESO.\n\nReceived 29 March 2010; Accepted 25 April 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.\n\nWe thank Jeff Kenney & Jacqueline van Gorkom for providing\nelectronic versions of their data. The images were produced with APLpy, thanks to Edward Gomez & Eli Bressart. We thank the referee for their constructive comments. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada);\nNAOC (China); CEA, OAMP (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).\n\nPublished - Gomez2010p11873Astron_Astrophys.pdf
", "abstract": "We present Herschel-SPIRE observations at 250\u2013500\u2009\u03bcm of the giant elliptical galaxy M\u200986 and examine the distribution of the resolved cold dust emission and its relation with other galactic tracers. The SPIRE images reveal three dust components: emission from the central region; a dust lane extending north-south; and a bright emission feature 10\u2009kpc to the south-east. We estimate that ~10^6\u2009M_\u2609 of dust is spatially coincident with atomic and ionized hydrogen, originating from stripped material from the nearby spiral NGC 4438 due to recent tidal interactions with M\u200986. The gas-to-dust ratio of the cold gas component ranges from ~20\u201380. We discuss the different heating mechanisms for the dust features.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L45", "id_number": "CaltechAUTHORS:20101116-142023824", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101116-142023824", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA) (Canada)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC) (China)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Stockholm Observatory" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014530", "primary_object": { "basename": "Gomez2010p11873Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/hfhak-69032/files/Gomez2010p11873Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Gomez, H. L.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/q0t58-eeb38", "eprint_id": 21120, "eprint_status": "archive", "datestamp": "2023-08-19 03:02:03", "lastmod": "2023-10-20 23:46:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Levenson-L", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Shupe-David-L", "name": { "family": "Shupe", "given": "D. L." }, "orcid": "0000-0003-4401-0430" }, { "id": "Vieira-J", "name": { "family": "Vieira", "given": "J." } }, { "id": "Xu-C-Kevin", "name": { "family": "Xu", "given": "C. K." }, "orcid": "0000-0002-1588-6700" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "The far-infrared/radio correlation as probed by Herschel", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: evolution, galaxies: starburst, infrared: galaxies, submillimeter: galaxies, radio continuum: galaxies", "note": "\u00a9 2010 ESO. Received 30 March 2010, Accepted 23 April 2010, Published Online 16 July 2010. Herschel is an ESA space observatory with science instruments\nprovided by European-led Principal Investigator consortia and with important\nparticipation from NASA. The data presented in this paper will be released through\nthe Herschel Database in Marseille HeDaM (hedam.oamp.fr/HerMES). SPIRE\nhas been developed by a consortium of institutes led by Cardiff Univ. (UK) and\nincluding Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France);\nIFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden);\nImperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK);\nCaltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported\nby national funding agencies: CSA (Canada); NAOC (China); CEA,\nCNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC\n(UK); and NASA (USA). PACS has been developed by a consortium of institutes\nled by MPE (Germany) and including UVIE (Austria); KUL, CSL,\nIMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT,\nOAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been\nsupported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium),\nCEA/CNES (France), DLR (Germany), ASI (Italy), and CICYT/MCYT (Spain).\n\nPublished - Ivison2010p11861Astron_Astrophys.pdf
", "abstract": "We set out to determine the ratio, q_(IR), of rest-frame 8\u20131000-\u03bcm flux, S_(IR), to monochromatic radio flux, S_(1.4 GHz), for galaxies selected at far-infrared (IR) and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, T_d, and to identify any far-IR-bright outliers \u2013 useful laboratories for exploring why the far-IR/radio correlation (FIRRC) is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-\u03bcm and 1.4-GHz samples, obtained using Herschel and the Very Large Array (VLA) in GOODS-North (-N). We determine bolometric IR output using ten bands spanning \u03bb_(obs) = 24\u22121250 \u03bcm, exploiting data from PACS and SPIRE (PEP; HerMES), as well as Spitzer, SCUBA, AzTEC and MAMBO. We also explore the properties of an L_(IR)-matched sample, designed to reveal evolution of q_(IR) with redshift, spanning log L_(IR) = 11\u201312 L_\u2299 and z = 0\u22122, by stacking into the radio and far-IR images. For 1.4-GHz-selected galaxies in GOODS-N, we see tentative evidence of a break in the flux ratio, q_(IR), at L_(1.4 GHz) ~ 10^(22.7) WHz^(\u22121) where active galactic nuclei (AGN) are starting to dominate the radio power density, and of weaker correlations with redshift and T_d. From our 250-\u03bcm-selected sample we identify a small number of far-IR-bright outliers, and see trends of q_(IR) with L_(1.4 GHz), L_(IR), T_d and redshift, noting that some of these are inter-related. For our L_(IR-)matched sample, there is no evidence that q_(IR) changes significantly as we move back into the epoch of galaxy formation: we find q_(IR) \u221d (1+z)^\u03b3, where \u03b3 = \u22120.04 \u00b1 0.03 at z = 0 \u2212 2; however, discounting the least reliable data at z < 0.5 we find \u03b3 = \u22120.26 \u00b1 0.07, modest evolution which may be related to the radio background seen by ARCADE 2, perhaps driven by <10-\u03bcJy radio activity amongst ordinary star-forming galaxies at z > 1.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "Art. No. L31", "id_number": "CaltechAUTHORS:20101202-100221983", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101202-100221983", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Space Agency (CSA)" }, { "agency": "National Astronomical Observatories, Chinese Academy of Sciences (NAOC)" }, { "agency": "Commissariat \u00e0 l'Energie Atomique (CEA)" }, { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Centre National de la Recherche Scientifique (CNRS)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Ministerio de Ciencia e Innovaci\u00f3n (MCINN)" }, { "agency": "Swedish National Space Board (SNSB)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "NASA" }, { "agency": "Bundesministerium f\u00fcr Verkehr, Innovation und Technologie (BMVIT)" }, { "agency": "European Space Agency (ESA) PROgramme for the Development of scientific EXperiments (PRODEX) (Belgium)" }, { "agency": "Deutsches Zentrum f\u00fcr Luft- und Raumfahrt (DLR)" }, { "agency": "Comisi\u00f3n Interministerial de Ciencia y Tecnolog\u00eda (CICYT)" }, { "agency": "Ministerio de Ciencia y Tecnologia (MCYT)" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1051/0004-6361/201014552", "primary_object": { "basename": "Ivison2010p11861Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/q0t58-eeb38/files/Ivison2010p11861Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Ivison, R. J.; Blain, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/3kmgg-b9731", "eprint_id": 20892, "eprint_status": "archive", "datestamp": "2023-08-22 00:14:32", "lastmod": "2023-10-20 23:34:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rex-M", "name": { "family": "Rex", "given": "M." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Fadda-D", "name": { "family": "Fadda", "given": "D." }, "orcid": "0000-0002-3698-7076" }, { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C-R", "name": { "family": "Bridge", "given": "C. R." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } } ] }, "title": "The far-infrared/submillimeter properties of galaxies located behind the Bullet cluster", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies \u2013 submillimeter: galaxies \u2013 galaxies: evolution; galaxies: high-redshift; galaxies: clusters: general; gravitational lensing: strong", "note": "\u00a9 2010 ESO.\n\nReceived 1 April 2010; Accepted 18 May 2010; Published online 16 July 2010.\n\nHerschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Data presented in this paper were analyzed using \"The Herschel interactive processing environment (HIPE)\", a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia.\n\nWe thank Ben Weiner and David Elbaz for their valuable\ncomments and help with our computations. This work is based in part on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by\nNASA through an award issued by JPL/Caltech.\n\nPublished - Rex2010p11853Astron_Astrophys.pdf
", "abstract": "The Herschel Lensing Survey (HLS) takes advantage of gravitational lensing by massive galaxy clusters to sample a population of high-redshift galaxies which are too faint to be detected above the confusion limit of current far-infrared/submillimeter telescopes. Measurements from 100\u2013500 \u03bcm bracket the peaks of the far-infrared spectral energy distributions of these galaxies, characterizing their infrared luminosities and star formation rates. We introduce initial results from our science demonstration phase observations, directed toward the Bullet cluster (1E0657-56). By combining our observations with LABOCA 870 \u03bcm and AzTEC 1.1 mm data we fully constrain the spectral energy distributions of 19 MIPS 24 \u03bcm-selected galaxies which are located behind the cluster. We find that their colors are best fit using templates based on local galaxies with systematically lower infrared luminosities. This suggests that our sources are not like local ultra-luminous infrared galaxies in which vigorous star formation is contained in a compact highly dust-obscured region. Instead, they appear to be scaled up versions of lower luminosity local galaxies with star formation occurring on larger physical scales.", "date": "2010-07", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "518", "publisher": "EDP Sciences", "pagerange": "L13", "id_number": "CaltechAUTHORS:20101118-114636998", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101118-114636998", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "doi": "10.1051/0004-6361/201014693", "primary_object": { "basename": "Rex2010p11853Astron_Astrophys.pdf", "url": "https://authors.library.caltech.edu/records/3kmgg-b9731/files/Rex2010p11853Astron_Astrophys.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Rex, M.; Zemcov, M.; et el." }, { "id": "https://authors.library.caltech.edu/records/es1m4-88b21", "eprint_id": 18857, "eprint_status": "archive", "datestamp": "2023-08-22 00:08:26", "lastmod": "2023-10-20 19:07:46", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Gupta-S", "name": { "family": "Gupta", "given": "S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Parameter Estimation from Improved Measurements of the Cosmic Microwave Background from QUaD", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmological parameters", "note": "\u00a9 2010 The American Astronomical Society.\nReceived 2009 September 9; accepted 2010 April 29; published 2010 May 26. QUaD is funded by the National Science Foundation in the\nUSA, through grants ANT-0338138, ANT-0338335, & ANT-\n0338238, by the Science and Technology Facilities Council\n(STFC) in the UK, and by the Science Foundation Ireland.\nP.G.C. acknowledges funding from the Portuguese FCT. S.E.C.\nacknowledges support from a Stanford Terman Fellowship.\nJ.R.H. acknowledges the support of an NSF Graduate Research\nFellowship, a Stanford Graduate Fellowship, and a NASA\nPostdoctoral Fellowship. Y.M. acknowledges support from a\nSUPA Prize studentship. C.P. acknowledges partial support\nfrom the Kavli Institute for Cosmological Physics through the\ngrant NSF PHY-0114422. E.Y.W. acknowledges receipt of an\nNDSEG fellowship. M.Z. acknowledges support from a NASA\nPostdoctoral Fellowship.We acknowledge the use of the CAMB\n(Lewis et al. 2000), CosmoMC (Lewis & Bridle 2002), and\nHEALPix (G\u00b4orski et al. 2005) packages. We acknowledge the\nuse of the Legacy Archive for Microwave Background Data\nAnalysis (LAMBDA). Support for LAMBDA is provided by\nthe NASA Office of Space Science. This work was performed\nusing the computational facilities of the Advanced Research\nComputing @ Cardiff (ARCCA) Division, Cardiff University.\n\nPublished - Gupta2010p10454Astrophys_J.pdf
", "abstract": "We evaluate the contribution of cosmic microwave background (CMB) polarization spectra to cosmological parameter constraints. We produce cosmological parameters using high-quality CMB polarization data from the ground-based QUaD experiment and demonstrate for the majority of parameters that there is significant improvement on the constraints obtained from satellite CMB polarization data. We split a multi-experiment CMB data set into temperature and polarization subsets and show that the best-fit confidence regions for the \u039bCDM six-parameter cosmological model are consistent with each other, and that polarization data reduces the confidence regions on all parameters. We provide the best limits on parameters from QUaD EE/BB polarization data and we find best-fit parameters from the multi-experiment CMB data set using the optimal pivot scale of k_p = 0.013 Mpc^(\u20131) to be {h^2\u03a9_c, h^2\u03a9_b, H_0, A_s, n_s, \u03c4} = {0.113, 0.0224, 70.6, 2.29 \u00d7 10^(\u20139), 0.960, 0.086}.", "date": "2010-06-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "716", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1040-1046", "id_number": "CaltechAUTHORS:20100629-134623858", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100629-134623858", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Science Foundation Ireland" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Stanford Terman Fellowship" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Stanford Graduate Fellowship" }, { "agency": "NASA Postdoctoral Fellowship" }, { "agency": "State University Presidents Association (SUPA) Prize studentship" }, { "agency": "NSF Kavli Institute for Cosmological Physics", "grant_number": "PHY-0114422" }, { "agency": "National Defense Science and Engineering Graduate Fellowship (NDSEG)" }, { "agency": "NASA Postdoctoral Fellowship" } ] }, "doi": "10.1088/0004-637X/716/2/1040", "primary_object": { "basename": "Gupta2010p10454Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/es1m4-88b21/files/Gupta2010p10454Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Gupta, S.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/wes6t-cpc94", "eprint_id": 18755, "eprint_status": "archive", "datestamp": "2023-08-22 00:06:34", "lastmod": "2023-10-20 16:44:18", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Kozlowski-S", "name": { "family": "Kozlowski", "given": "Szymon" } }, { "id": "Stern-D", "name": { "family": "Stern", "given": "Daniel" }, "orcid": "0000-0003-2686-9241" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Borys-C-J-K", "name": { "family": "Borys", "given": "C." } }, { "id": "Eisenhardt-P-R-M", "name": { "family": "Eisenhardt", "given": "P. R." } }, { "id": "Gorjian-V", "name": { "family": "Gorjian", "given": "V." } }, { "id": "Griffith-R", "name": { "family": "Griffith", "given": "R." } }, { "id": "Jacob-J-C", "name": { "family": "Jacob", "given": "J." } }, { "id": "Mainzer-A-K", "name": { "family": "Mainzer", "given": "A." } }, { "id": "Moustakas-L-A", "name": { "family": "Moustakas", "given": "L." }, "orcid": "0000-0003-3030-2360" }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "J. R." }, "orcid": "0000-0003-3595-7382" } ] }, "title": "Mid-infrared Variability from the Spitzer Deep Wide-field Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; galaxies: active; infrared: galaxies; quasars: general", "note": "\u00a9 2010 The American Astronomical Society. Received 2010 February 5; accepted 2010 April 8; published 2010 May 20. This work is based on observations made with the Spitzer\nSpace Telescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of the Technology under contract with\nthe National Aeronautics and Space Administration (NASA).\nSupport for this work was provided by NASA through award\nnumbers 1310744 (C.S.K. and S.K.), 1314516 (M.L.N.A.), and\n1317692 (H.A.S.) issued by JPL/CalTech. C.S.K. and S.K. are\nalso supported by NSF grant AST-0708082. The NDWFS and\nthe research of A.D. and B.T.J. are supported by the National\nOptical Astronomy Observatory, which is operated by the Association\nof Universities for Research in Astronomy (AURA)\nunder cooperative agreement with the National Science Foundation.\nSupport for M.B. was provided by the W. M. Keck\nFoundation.\n\nPublished - Kozlowski2010p10355Astrophys_J.pdf
", "abstract": "We use the multi-epoch, mid-infrared Spitzer Deep Wide-Field Survey to investigate the variability of objects in 8.1 deg^2 of the NOAO Deep Wide Field Survey Bo\u00f6tes field. We perform a Difference Image Analysis of the four available epochs between 2004 and 2008, focusing on the deeper 3.6 and 4.5 \u03bcm bands. Out of 474, 179 analyzed sources, 1.1% meet our standard variability selection criteria that the two light curves are strongly correlated (r > 0.8) and that their joint variance (\u03c3_(12)) exceeds that for all sources with the same magnitude by 2\u03c3. We then examine the mid-IR colors of the variable sources and match them with X-ray sources from the XBo\u00f6tes survey, radio catalogs, 24 \u03bcm selected active galactic nucleus (AGN) candidates, and spectroscopically identified AGNs from the AGN and Galaxy Evolution Survey (AGES). Based on their mid-IR colors, most of the variable sources are AGNs (76%), with smaller contributions from stars (11%), galaxies (6%), and unclassified objects, although most of the stellar, galaxy, and unclassified sources are false positives. For our standard selection criteria, 11%-12% of the mid-IR counterparts to X-ray sources, 24 \u03bcm AGN candidates, and spectroscopically identified AGNs show variability. The exact fractions depend on both the search depth and the selection criteria. For example, 12% of the 1131 known z>1 AGNs in the field and 14%-17% of the known AGNs with well-measured fluxes in all four Infrared Array Camera bands meet our standard selection criteria. The mid-IR AGN variability can be well described by a single power-law structure function with an index of \u03b3 \u2248 0.5 at both 3.6 and 4.5 \u03bcm, and an amplitude of S _0 \u2243 0.1 mag on rest-frame timescales of 2 yr. The variability amplitude is higher for shorter rest-frame wavelengths and lower luminosities.", "date": "2010-06-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "716", "number": "1", "publisher": "American Astronomical Society", "pagerange": "530-543", "id_number": "CaltechAUTHORS:20100621-142204054", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100621-142204054", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "AST-1310744" }, { "agency": "NASA", "grant_number": "AST-1314516" }, { "agency": "NASA", "grant_number": "AST-1317692" }, { "agency": "NSF", "grant_number": "AST-0708082" }, { "agency": "National Optical Astronomy Observatory (NOAO)" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/716/1/530", "primary_object": { "basename": "Kozlowski2010p10355Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/wes6t-cpc94/files/Kozlowski2010p10355Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Kozlowski, Szymon; Stern, Daniel; et el." }, { "id": "https://authors.library.caltech.edu/records/c8q1b-mwj60", "eprint_id": 18432, "eprint_status": "archive", "datestamp": "2023-08-19 02:19:25", "lastmod": "2023-10-20 16:22:27", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Eales-S-A", "name": { "family": "Eales", "given": "S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bridge-C", "name": { "family": "Bridge", "given": "C." } }, { "id": "Frayer-D", "name": { "family": "Frayer", "given": "D." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Vieria-J", "name": { "family": "Vieria", "given": "J." } } ] }, "title": "The Herschel ATLAS", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010 The Astronomical Society of the Pacific. Received 2009 October 19; accepted 2010 March 29; published 2010 April 22. We thank the UK Science and Technology Facilities Council\nand the Italian Space Agency (ASI contract I/016/07/0\nCOFIS) for funding. This research has made use of the\nNASA/IPAC Extragalactic Database (NED), which is operated\nby the Jet Propulsion Laboratory, California Institute of Technology,\nunder contract with the National Aeronautics and\nSpace Administration.\n\nPublished - Eales2010p10038Publ_Astron_Soc_Pac.pdf
", "abstract": "The Herschel ATLAS is the largest open-time key project that will be carried out on the Herschel\nSpace Observatory. It will survey 570 deg2 of the extragalactic sky, 4 times larger than all the other Herschel extragalactic\nsurveys combined, in five far-infrared and submillimeter bands. We describe the survey, the complementary\nmultiwavelength data sets that will be combined with the Herschel data, and the six major science\nprograms we are undertaking. Using new models based on a previous submillimeter survey of galaxies, we present\npredictions of the properties of the ATLAS sources in other wave bands.", "date": "2010-05", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "122", "number": "891", "publisher": "Astronomical Society of the Pacific", "pagerange": "499-515", "id_number": "CaltechAUTHORS:20100525-115457996", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100525-115457996", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/016/07/0 COFIS" }, { "agency": "NASA/JPL/Caltech" } ] }, "collection": "CaltechAUTHORS", "doi": "10.1086/653086", "primary_object": { "basename": "Eales2010p10038Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/c8q1b-mwj60/files/Eales2010p10038Publ_Astron_Soc_Pac.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Eales, S.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/skb2d-ytn18", "eprint_id": 18043, "eprint_status": "archive", "datestamp": "2023-08-22 09:10:55", "lastmod": "2023-10-20 15:31:51", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mac\u00edas-P\u00e9rez-J-F", "name": { "family": "Mac\u00edas-P\u00e9rez", "given": "J. F." } }, { "id": "Lagache-G", "name": { "family": "Lagache", "given": "G." } }, { "id": "Maffei-B", "name": { "family": "Maffei", "given": "B." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Bourachot-A", "name": { "family": "Bourrachot", "given": "A." } }, { "id": "Ade-P", "name": { "family": "Ade", "given": "P." } }, { "id": "Amblard-A", "name": { "family": "Amblard", "given": "A." } }, { "id": "Ansari-R", "name": { "family": "Ansari", "given": "R." } }, { "id": "Auborg-E", "name": { "family": "Auborg", "given": "E." } }, { "id": "Aumont-J", "name": { "family": "Aumont", "given": "J." } }, { "id": "Bargot-S", "name": { "family": "Bargot", "given": "S." } }, { "id": "Bartlett-James", "name": { "family": "Bartlett", "given": "J." } }, { "id": "Beno\u00eet-A", "name": { "family": "Beno\u00eet", "given": "A." } }, { "id": "Bernard-J-Ph", "name": { "family": "Bernard", "given": "J.-Ph." } }, { "id": "Bhatia-R", "name": { "family": "Bhatia", "given": "R." } }, { "id": "Blanchard-A", "name": { "family": "Blanchard", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Bouchet-F-R", "name": { "family": "Bouchet", "given": "F. R." } }, { "id": "Camus-P", "name": { "family": "Camus", "given": "P." } }, { "id": "Cardoso-J-F", "name": { "family": "Cardoso", "given": "J.-F." } }, { "id": "Couchot-F", "name": { "family": "Couchot", "given": "F." } }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "Delabrouille-J", "name": { "family": "Delabrouille", "given": "J." } }, { "id": "D\u00e9sert-F-X", "name": { "family": "D\u00e9sert", "given": "F.-X." } }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Douspis-M", "name": { "family": "Douspis", "given": "M." } }, { "id": "Dumoulin-L", "name": { "family": "Dumoulin", "given": "L." } }, { "id": "Dupac-X", "name": { "family": "Dupac", "given": "X." } }, { "id": "Filliatre-P", "name": { "family": "Filliatre", "given": "Ph." } }, { "id": "Fosalba-P", "name": { "family": "Fosalba", "given": "P." } }, { "id": "Gannaway-F", "name": { "family": "Gannaway", "given": "F." } }, { "id": "Gautier-B", "name": { "family": "Gautier", "given": "B." } }, { "id": "Giard-M", "name": { "family": "Giard", "given": "M." } }, { "id": "Giraud-H\u00e9raud-Y", "name": { "family": "Giraud-H\u00e9raud", "given": "Y." } }, { "id": "Gispert-R", "name": { "family": "Gispert", "given": "R." } }, { "id": "Guglielmi-L", "name": { "family": "Guglielmi", "given": "L." } }, { "id": "Hamilton-J-Ch", "name": { "family": "Hamilton", "given": "J.-Ch." } }, { "id": "Hanany-S", "name": { "family": "Hanany", "given": "S." } }, { "id": "Henrot-Versill\u00e9-S", "name": { "family": "Henrot-Versill\u00e9", "given": "S." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V." } }, { "id": "Kaplan-J-D", "name": { "family": "Kaplan", "given": "J." } }, { "id": "Lamarre-J-M", "name": { "family": "Lamarre", "given": "J.-M" } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Madet-K", "name": { "family": "Madet", "given": "K." } }, { "id": "Magneville-C", "name": { "family": "Magneville", "given": "Ch." } }, { "id": "Marrone-D-P", "name": { "family": "Marrone", "given": "D. P." }, "orcid": "0000-0002-2367-1080" }, { "id": "Masi-S", "name": { "family": "Masi", "given": "S." }, "orcid": "0000-0001-5105-1439" }, { "id": "Mayet-F", "name": { "family": "Mayet", "given": "F." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Naraghi-F", "name": { "family": "Naraghi", "given": "F." } }, { "id": "Nati-F", "name": { "family": "Nati", "given": "F." } }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "G." } }, { "id": "Perdereau-O", "name": { "family": "Perdereau", "given": "O." } }, { "id": "Perrin-G", "name": { "family": "Perrin", "given": "G." } }, { "id": "Plaszczynski-S", "name": { "family": "Plaszczynski", "given": "S." } }, { "id": "Piat-M", "name": { "family": "Piat", "given": "M." } }, { "id": "Ponthieu-N", "name": { "family": "Ponthieu", "given": "N." } }, { "id": "Prunet-S", "name": { "family": "Prunet", "given": "S." } }, { "id": "Puget-J-L", "name": { "family": "Puget", "given": "J.-L" } }, { "id": "Renault-C", "name": { "family": "Renault", "given": "C." } }, { "id": "Rosset-C", "name": { "family": "Rosset", "given": "C." } }, { "id": "Santos-D", "name": { "family": "Santos", "given": "D." } }, { "id": "Starobinsky-A", "name": { "family": "Starobinsky", "given": "A." } }, { "id": "Strukov-I", "name": { "family": "Strukov", "given": "I." } }, { "id": "Sudiwala-R-V", "name": { "family": "Sudiwala", "given": "R. V." } }, { "id": "Tessyier-D", "name": { "family": "Teyssier", "given": "D." } }, { "id": "Tristram-M", "name": { "family": "Tristram", "given": "M." } }, { "id": "Tucker-C", "name": { "family": "Tucker", "given": "C." } }, { "id": "Vanel-J-Ch", "name": { "family": "Vanel", "given": "J.-Ch." } }, { "id": "Vibert-D", "name": { "family": "Vibert", "given": "D." } }, { "id": "Wakui-E", "name": { "family": "Wakui", "given": "E." } }, { "id": "Yvon-D", "name": { "family": "Yvon", "given": "D." } } ] }, "title": "Archeops in-flight performance, data processing, and map making", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: data analysis; cosmic microwave background", "note": "\u00a9 2007 ESO. \n\nReceived 23 March 2006; accepted 10 January 2007. \n\nWe would like to pay tribute to the memory of Pierre Faucon who led the CNES team during several difficult and long campaigns. We thank the Russian recovery teams who worked under very harsh conditions\nto retrieve the precious instrument and data. The Swedish Kiruna Esrange base is warmly thanked for all the help during the launch preparations. We thank the CNES balloon program, Programme National de Cosmologie, and the participating laboratories for financial support. We thank Juan R. Pardo for helping us with\natmospheric modeling and Bruno B\u00e9zard for planet calibration. The HEALPix package was used throughout the data analysis (Gorski et al. 1999). We thank the anonymous referee for constructive remarks and improvement to the manuscript.\n\nPublished - MACaanda07b.pdf
", "abstract": "Aims. Archeops is a balloon-borne experiment inspired by the Planck satellite and its high frequency instrument (HFI). It is designed to measure the cosmic microwave background (CMB) temperature anisotropies at high angular resolution (~12 arcmin) over a large fraction of the sky (around 30%) at 143, 217, 353, and 545 GHz. The Archeops 353 GHz channel consists of three pairs of polarized sensitive bolometers designed to detect the polarized diffuse emission of Galactic dust. \nMethods. In this paper we present an update of the instrumental setup, as well as the flight performance for the last Archeops flight campaign (February 2002 from Kiruna, Sweden). We also describe the processing and analysis of the Archeops time-ordered data for that campaign, which led to measurement of the CMB anisotropy power spectrum in the multipole range \u2113 = 10-700 and to the first measurements of both the polarized emission of dust at large angular scales and its power spectra in the multipole range \u2113 = 3-70\nResults. We present maps covering approximately 30% of the sky. These maps contain Galactic emission, including the Galactic plane, in the four Archeops channels at 143, 217, 353, and 545 GHz and CMB anisotropies at 143 and 217 GHz. These are one of the first sub-degree-resolution maps in the millimeter and submillimeter ranges of the large angular-scale diffuse Galactic dust emission and CMB temperature anisotropies, respectively.", "date": "2010-04-22", "date_type": "published", "publication": "Astronomy and Astrophysics", "volume": "467", "number": "3", "publisher": "EDP Sciences", "pagerange": "1313-1344", "id_number": "CaltechAUTHORS:20100421-122423105", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100421-122423105", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Programme National de Cosmologie et Galaxies (PNCG)" } ] }, "doi": "10.1051/0004-6361:20065258", "primary_object": { "basename": "MACaanda07b.pdf", "url": "https://authors.library.caltech.edu/records/skb2d-ytn18/files/MACaanda07b.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Mac\u00edas-P\u00e9rez, J. F.; Lagache, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/6hm81-epd44", "eprint_id": 18358, "eprint_status": "archive", "datestamp": "2023-08-21 23:46:47", "lastmod": "2023-10-20 16:08:59", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Veneziani-M", "name": { "family": "Veneziani", "given": "M." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "De-Gasperis-G", "name": { "family": "De Gasperis", "given": "G." } }, { "id": "de-Oliveira-Costa-A", "name": { "family": "de Oliveira-Costa", "given": "A." } }, { "id": "De-Troia-G", "name": { "family": "De Troia", "given": "G." } }, { "id": "Di-Stefano-G", "name": { "family": "Di Stefano", "given": "G." } }, { "id": "Ganga-K-M", "name": { "family": "Ganga", "given": "K. M." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Kisner-T-S", "name": { "family": "Kisner", "given": "T. S." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "MacTavish-C-J", "name": { "family": "MacTavish", "given": "C. J." } }, { "id": "Masi-S", "name": { "family": "Masi", "given": "S." }, "orcid": "0000-0001-5105-1439" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T. E." } }, { "id": "Natoli-P", "name": { "family": "Natoli", "given": "P." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Piacentini-F", "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "id": "Pietrobon-D", "name": { "family": "Pietrobon", "given": "D." } }, { "id": "Polenta-G", "name": { "family": "Polenta", "given": "G." } }, { "id": "Ricciardi-S", "name": { "family": "Ricciardi", "given": "S." } }, { "id": "Romeo-G", "name": { "family": "Romeo", "given": "G." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } } ] }, "title": "Properties of Galactic Cirrus Clouds Observed by BOOMERANG", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmology: observations; ISM: clouds; radio continuum: ISM; submillimeter: ISM", "note": "\u00a9 2010 American Astronomical Society.\n\nReceived 2009 July 28; accepted 2010 March 1; published 2010 March 29.\n\nThe authors acknowledge Jean-Philippe Bernard, Robert\nCrittenden, Alessandro Melchiorri and Max Tegmark for useful\ndiscussions. M.V. acknowledges support from the Faculty of the European Space Astronomy Center (ESAC-ESA). This activity has been supported by Italian Space Agency contracts COFIS, BOOMERanG and HiGal (I/038/08/0). We are grateful to the referee for helpful comments.\n\nPublished - Veneziani2010p9924Astrophys_J.pdf
", "abstract": "The physical properties of galactic cirrus emission are not well characterized. BOOMERANG is a balloon-borne experiment designed to study the cosmic microwave background at high angular resolution in the millimeter range. The BOOMERANG 245 and 345 GHz channels are sensitive to interstellar signals, in a spectral range intermediate between FIR and microwave frequencies. We look for physical characteristics of cirrus structures in a region at high galactic latitudes (b ~ \u201340\u00b0) where BOOMERANG performed its deepest integration, combining the BOOMERANG data with other available data sets at different wavelengths. We have detected eight emission patches in the 345 GHz map, consistent with cirrus dust in the Infrared Astronomical Satellite maps. The analysis technique we have developed allows us to identify the location and the shape of cirrus clouds, and to extract the flux from observations with different instruments at different wavelengths and angular resolutions. We study the integrated flux emitted from these cirrus clouds using data from Infrared Astronomical Satellite (IRAS), DIRBE, BOOMERANG and Wilkinson Microwave Anisotropy Probe in the frequency range 23-3000 GHz (13 mm-100 \u03bcm wavelength). We fit the measured spectral energy distributions with a combination of a gray body and a power-law spectra considering two models for the thermal emission. The temperature of the thermal dust component varies in the 7-20 K range and its emissivity spectral index is in the 1-5 range. We identified a physical relation between temperature and spectral index as had been proposed in previous works. This technique can be proficiently used for the forthcoming Planck and Herschel missions data.", "date": "2010-04-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "713", "number": "2", "publisher": "American Astronomical Society", "pagerange": "959-969", "id_number": "CaltechAUTHORS:20100519-165135784", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100519-165135784", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Faculty of the European Space Astronomy Center (ESAC-ESA)" }, { "agency": "Italian Space Agency", "grant_number": "I/038/08/0" } ] }, "doi": "10.1088/0004-637X/713/2/959", "primary_object": { "basename": "Veneziani2010p9924Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/6hm81-epd44/files/Veneziani2010p9924Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Veneziani, M.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/rtaex-fj188", "eprint_id": 17751, "eprint_status": "archive", "datestamp": "2023-08-21 23:34:04", "lastmod": "2023-10-20 00:12:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Takahashi-Y-d", "name": { "family": "Takahashi", "given": "Y. D." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Barkats-D", "name": { "family": "Barkats", "given": "D." } }, { "id": "Battle-J-O", "name": { "family": "Battle", "given": "J. O." } }, { "id": "Bierman-E-M", "name": { "family": "Bierman", "given": "E. M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chiang-H-C", "name": { "family": "Chiang", "given": "H. C." } }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Duband-L", "name": { "family": "Duband", "given": "L." } }, { "id": "Hivon-E-F", "name": { "family": "Hivon", "given": "E. F." } }, { "id": "Holzapfel-W-L", "name": { "family": "Holzapfel", "given": "W. L." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Keating-B-G", "name": { "family": "Keating", "given": "B. G." } }, { "id": "Kovac-J-M", "name": { "family": "Kovac", "given": "J. M." } }, { "id": "Kuo-Chia-Lam", "name": { "family": "Kuo", "given": "C. L." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E-M", "name": { "family": "Leitch", "given": "E. M." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Matsumura-Tomotake", "name": { "family": "Matsumura", "given": "T." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Ponthieu-N", "name": { "family": "Ponthieu", "given": "N." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Richter-S", "name": { "family": "Richter", "given": "S." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Yoon-K-W", "name": { "family": "Yoon", "given": "K. W." } } ] }, "title": "Characterization of the BICEP Telescope for High-precision Cosmic Microwave Background Polarimetry", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; instrumentation: polarimeters; telescopes", "note": "\u00a9 2010 American Astronomical Society.\n\nIssue 2 (2010 March 10).\n\nReceived 2009 June 26; accepted for publication 2010 January 29; published 2010 February 22.\n\nBicep is supported by NSF Grant OPP-0230438, Caltech Discovery\nFund, Caltech President's Fund PF-471, JPL Research\nand Technology Fund, and the late J. Robinson. We thank our\ncolleagues in Acbar, Boomerang, QUaD, Bolocam, and SPT\nfor advice and helpful discussions, Kathy Deniston for logistical\nand administrative support, and the South Pole Station staff for\ntheir support. We acknowledge support by the NASA Graduate\nFellowship program (H.C.C., E.M.B.), the John B. and Nelly\nKilroy Foundation (J.M.K.), and NSF PECASE Award AST-\n0548262 (B.G.K.).\n\nPublished - Takahashi2010p7255Astrophys_J.pdf
", "abstract": "The Background Imaging of Cosmic Extragalactic Polarization (BICEP) experiment was designed specifically to search for the signature of inflationary gravitational waves in the polarization of the cosmic microwave background (CMB). Using a novel small-aperture refractor and 49 pairs of polarization-sensitive bolometers, BICEP has completed three years of successful observations at the South Pole beginning in 2006 February. To constrain the amplitude of the inflationary B-mode polarization, which is expected to be at least 7 orders of magnitude fainter than the 3 K CMB intensity, precise control of systematic effects is essential. This paper describes the characterization of potential systematic errors for the BICEP experiment, supplementing a companion paper on the initial cosmological results. Using the analysis pipelines for the experiment, we have simulated the impact of systematic errors on the B-mode polarization measurement. Guided by these simulations, we have established benchmarks for the characterization of critical instrumental properties including bolometer relative gains, beam mismatch, polarization orientation, telescope pointing, sidelobes, thermal stability, and timestream noise model. A comparison of the benchmarks with the measured values shows that we have characterized the instrument adequately to ensure that systematic errors do not limit BICEP's two-year results, and identifies which future refinements are likely necessary to probe inflationary B-mode polarization down to levels below a tensor-to-scalar ratio r = 0.1.", "date": "2010-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "711", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1141-1156", "id_number": "CaltechAUTHORS:20100316-103422736", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100316-103422736", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0230438" }, { "agency": "Caltech Discovery Fund" }, { "agency": "Caltech's President's Fund", "grant_number": "PF-471" }, { "agency": "JPL Research and Technology Fund" }, { "agency": "NASA Graduate Fellowship" }, { "agency": "John B. and Nelly Kilroy Foundation" }, { "agency": "NSF", "grant_number": "AST-0548262" } ] }, "doi": "10.1088/0004-637X/711/2/1141", "primary_object": { "basename": "Takahashi2010p7255Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/rtaex-fj188/files/Takahashi2010p7255Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Takahashi, Y. D.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/048yz-qgp18", "eprint_id": 17763, "eprint_status": "archive", "datestamp": "2023-08-21 23:34:20", "lastmod": "2023-10-20 00:12:56", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chiang-H-C", "name": { "family": "Chiang", "given": "H. C." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Barkats-D", "name": { "family": "Barkats", "given": "D." } }, { "id": "Battle-J-O", "name": { "family": "Battle", "given": "J. O." } }, { "id": "Bierman-E-M", "name": { "family": "Bierman", "given": "E. M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Dowell-C-D", "name": { "family": "Dowell", "given": "C. D." } }, { "id": "Duband-L", "name": { "family": "Duband", "given": "L." } }, { "id": "Hivon-E-F", "name": { "family": "Hivon", "given": "E. F." } }, { "id": "Holzapfel-W-L", "name": { "family": "Holzapfel", "given": "W. L." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Keating-B-G", "name": { "family": "Keating", "given": "B. G." } }, { "id": "Kovac-J-M", "name": { "family": "Kovac", "given": "J. M." } }, { "id": "Kuo-Chia-Lam", "name": { "family": "Kuo", "given": "C. L." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E-M", "name": { "family": "Leitch", "given": "E. M." } }, { "id": "Mason-P-V", "name": { "family": "Mason", "given": "P. V." }, "orcid": "0000-0002-7963-7420" }, { "id": "Matsumura-Tomotake", "name": { "family": "Matsumura", "given": "T." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Ponthieu-N", "name": { "family": "Ponthieu", "given": "N." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Richter-S", "name": { "family": "Richter", "given": "S." } }, { "id": "Rocha-G-M", "name": { "family": "Rocha", "given": "G." }, "orcid": "0000-0002-4150-8076" }, { "id": "Sheehy-C", "name": { "family": "Sheehy", "given": "C." } }, { "id": "Takahashi-Y-D", "name": { "family": "Takahashi", "given": "Y. D." } }, { "id": "Tolan-J-E", "name": { "family": "Tolan", "given": "J. E." } }, { "id": "Yoon-K-W", "name": { "family": "Yoon", "given": "K. W." } } ] }, "title": "Measurement of Cosmic Microwave Background Polarization Power Spectra from Two Years of BICEP Data", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization", "note": "\u00a9 2010 American Astronomical Society.\n\nIssue 2 (2010 March 10); received 2009 June 15; accepted for publication 2010 January 29; published 2010 February 22.\n\nWe dedicate this work to the memory of Andrew Lange,\nwhose tragic and untimely death has deeply pained us all. He was\nand always will be an inspiration to us, and he is immeasurably\nmissed.\nBicep is supported by NSF Grant No. OPP-0230438, Caltech\nPresident's Discovery Fund, Caltech President's Fund PF-471,\nJPL Research and Technology Development Fund, and the\nlate J. Robinson. We thank the South Pole Station staff for\nhelping make our observing seasons a success. We also thank\nJoanna Dunkley, Nathan Miller, and our colleagues in Acbar,\nBoomerang, QUaD, Bolocam, SPT, and WMAP for advice\nand helpful discussions, and Kathy Deniston for logistical and\nadministrative support. We gratefully acknowledge support of\nindividual team members by the NASA Graduate Fellowship\nprogram (H.C.C.), NSF PECASE Award No. AST-0548262\n(B.G.K.), the John B. and Nelly Kilroy Foundation (J.M.K.),\nthe U.S. DOE contract to SLAC No. DE-AC02-76SF00515\n(C.L.K. and J.E.T.), KICP (C.P. and C.S.), and the NASA\nScience Mission Directorate via the US Planck Project (G.R.).\n\nPublished - Chiang2010p7250Astrophys_J.pdf
", "abstract": "Background Imaging of Cosmic Extragalactic Polarization (BICEP) is a bolometric polarimeter designed to measure the inflationary B-mode polarization of the cosmic microwave background (CMB) at degree angular scales. During three seasons of observing at the South Pole (2006 through 2008), BICEP mapped ~2% of the sky chosen to be uniquely clean of polarized foreground emission. Here, we present initial results derived from a subset of the data acquired during the first two years. We present maps of temperature, Stokes Q and U, E and B modes, and associated angular power spectra. We demonstrate that the polarization data are self-consistent by performing a series of jackknife tests. We study potential systematic errors in detail and show that they are sub-dominant to the statistical errors. We measure the E-mode angular power spectrum with high precision at 21 \u2264 \u2113 \u2264 335, detecting for the first time the peak expected at \u2113 ~ 140. The measured E-mode spectrum is consistent with expectations from a \u039bCDM model, and the B-mode spectrum is consistent with zero. The tensor-to-scalar ratio derived from the B-mode spectrum is r = 0.02^(+0.31)_(\u20130.26), or r < 0.72 at 95% confidence, the first meaningful constraint on the inflationary gravitational wave background to come directly from CMB B-mode polarization.", "date": "2010-03-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "711", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1123-1140", "id_number": "CaltechAUTHORS:20100317-113552617", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100317-113552617", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-0230438" }, { "agency": "Caltech President's Discovery Fund" }, { "agency": "Caltech President's Fund", "grant_number": "PF-471" }, { "agency": "JPL Research and Technology Development Fund" }, { "agency": "NASA Graduate Fellowship" }, { "agency": "NSF PECASE Award", "grant_number": "AST-0548262" }, { "agency": "John B. and Nelly Kilroy Foundation" }, { "agency": "U.S. Department of Energy (DOE)", "grant_number": "DE-AC02-76SF00515" }, { "agency": "NASA Science Mission Directorate via the US Planck Project" } ] }, "doi": "10.1088/0004-637X/711/2/1123", "primary_object": { "basename": "Chiang2010p7250Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/048yz-qgp18/files/Chiang2010p7250Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Chiang, H. C.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/s7paf-mse63", "eprint_id": 17831, "eprint_status": "archive", "datestamp": "2023-08-19 01:45:06", "lastmod": "2023-10-20 15:19:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Boselli-A", "name": { "family": "Boselli", "given": "A." } }, { "id": "Eales-S-A", "name": { "family": "Eales", "given": "S." } }, { "id": "Cortese-L", "name": { "family": "Cortese", "given": "L." }, "orcid": "0000-0002-7422-9823" }, { "id": "Bendo-G-J", "name": { "family": "Bendo", "given": "G." } }, { "id": "Chanial-P", "name": { "family": "Chanial", "given": "P." } }, { "id": "Buat-V", "name": { "family": "Buat", "given": "V." } }, { "id": "Davies-J", "name": { "family": "Davies", "given": "J." }, "orcid": "0000-0002-4108-4357" }, { "id": "Auld-R", "name": { "family": "Auld", "given": "R." } }, { "id": "Rigby-E-E", "name": { "family": "Rigby", "given": "E." } }, { "id": "Baes-M", "name": { "family": "Baes", "given": "M." } }, { "id": "Barlow-M-J", "name": { "family": "Barlow", "given": "M." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bradford-M-C", "name": { "family": "Bradford", "given": "M." } }, { "id": "Castro-Rodr\u00edguez-N", "name": { "family": "Castro-Rodr\u00edguez", "given": "N." } }, { "id": "Charlot-S", "name": { "family": "Charlot", "given": "S." } }, { "id": "Clements-D-L", "name": { "family": "Clements", "given": "D." }, "orcid": "0000-0002-9548-5033" }, { "id": "Cormier-D", "name": { "family": "Cormier", "given": "D." } }, { "id": "Dwek-E", "name": { "family": "Dwek", "given": "E." }, "orcid": "0000-0001-8033-1181" }, { "id": "Elbaz-David", "name": { "family": "Elbaz", "given": "D." }, "orcid": "0000-0002-7631-647X" }, { "id": "Galametz-M", "name": { "family": "Galametz", "given": "M." }, "orcid": "0000-0002-0283-8689" }, { "id": "Galliano-F", "name": { "family": "Galliano", "given": "F." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Gomez-H-L", "name": { "family": "Gomez", "given": "H." } }, { "id": "Griffin-M-J", "name": { "family": "Griffin", "given": "M." } }, { "id": "Hony-S", "name": { "family": "Hony", "given": "S." } }, { "id": "Isaak-K-G", "name": { "family": "Isaak", "given": "K." } }, { "id": "Levenson-L-R", "name": { "family": "Levenson", "given": "L." } }, { "id": "Lu-Nanyao", "name": { "family": "Lu", "given": "N." }, "orcid": "0000-0002-8948-1044" }, { "id": "Madden-S-C", "name": { "family": "Madden", "given": "S." } }, { "id": "O'Halloran-B", "name": { "family": "O'Halloran", "given": "B." } }, { "id": "Okamura-Katsutomo", "name": { "family": "Okamura", "given": "K." } }, { "id": "Oliver-Sebastian-J", "name": { "family": "Oliver", "given": "S." }, "orcid": "0000-0001-7862-1032" }, { "id": "Page-M-J", "name": { "family": "Page", "given": "M." }, "orcid": "0000-0002-6689-6271" }, { "id": "Panuzzo-P", "name": { "family": "Panuzzo", "given": "P." } }, { "id": "Papageorgiou-A", "name": { "family": "Papageorgiou", "given": "A." }, "orcid": "0000-0002-3039-9257" }, { "id": "Parkin-T-J", "name": { "family": "Parkin", "given": "T." } }, { "id": "P\u00e9rez-Fournon-I", "name": { "family": "P\u00e9rez-Fournon", "given": "I." } }, { "id": "Pohlen-M", "name": { "family": "Pohlen", "given": "M." } }, { "id": "Rangwala-N", "name": { "family": "Rangwala", "given": "N." } }, { "id": "Roussel-H", "name": { "family": "Roussel", "given": "H." } }, { "id": "Rykala-A", "name": { "family": "Rykala", "given": "A." } }, { "id": "Sacchi-N", "name": { "family": "Sacchi", "given": "N." } }, { "id": "Sauvage-M", "name": { "family": "Sauvage", "given": "M." } }, { "id": "Schulz-B", "name": { "family": "Schulz", "given": "B." } }, { "id": "Schirm-M-R-P", "name": { "family": "Schirm", "given": "M." } }, { "id": "Smith-M-W-L", "name": { "family": "Smith", "given": "M. W. L." }, "orcid": "0000-0002-3532-6970" }, { "id": "Spinoglio-L", "name": { "family": "Spinoglio", "given": "L." } }, { "id": "Stevens-J", "name": { "family": "Stevens", "given": "J." } }, { "id": "Symeonidis-M", "name": { "family": "Symeonidis", "given": "M." } }, { "id": "Vaccari-Mattia", "name": { "family": "Vaccari", "given": "M." }, "orcid": "0000-0002-6748-0577" }, { "id": "Vigroux-L", "name": { "family": "Vigroux", "given": "L." } }, { "id": "Wilson-C-D", "name": { "family": "Wilson", "given": "C." }, "orcid": "0000-0001-5817-0991" }, { "id": "Wozniak-H", "name": { "family": "Wozniak", "given": "H." } }, { "id": "Wright-G-S", "name": { "family": "Wright", "given": "G." } }, { "id": "Zeilinger-W-W", "name": { "family": "Zeilinger", "given": "W." } } ] }, "title": "The Herschel Reference Survey", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2010. The Astronomical Society of the Pacific. Received 2008 August 17; accepted 2010 January 26; published 2010 February 26. We would like to thank the Herschel Project Scientist, G.\nPilbratt; the SPIRE team; and all the people involved in the construction\nand the launch of Herschel. This research has made use\nof the NASA/IPAC Extragalactic Database (NED) which is operated\nby the Jet Propulsion Laboratory, California Institute of\nTechnology, under contract with the National Aeronautics and\nSpace Administration; and of the GOLD Mine database. A. B.\nwishes to thank S. Boissier for his help in the construction of the\nHRS database. We are grateful to the anonymous referee forinvaluable\ncomments and suggestions which helped to improve\nthe quality of the manuscript.\n\nPublished - Boselli2010p7284Publ_Astron_Soc_Pac.pdf
", "abstract": "The Herschel Reference Survey is a Herschel guaranteed time key project and will be a benchmark study of dust in the nearby universe. The survey will complement a number of other Herschel key projects including large cosmological surveys that trace dust in the distant universe. We will use Herschel to produce images of a statistically-complete sample of 323 galaxies at 250, 350, and 500 \u03bcm. The sample is volume-limited, containing sources with distances between 15 and 25 Mpc and flux limits in the K band to minimize the selection effects associated with dust and with young high-mass stars and to introduce a selection in stellar mass. The sample spans the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the center of the Virgo Cluster) and as such will be useful for other purposes than our own. We plan to use the survey to investigate (i) the dust content of galaxies as a function of Hubble type, stellar mass, and environment; (ii) the connection between the dust content and composition and the other phases of the interstellar medium; and (iii) the origin and evolution of dust in galaxies. In this article, we describe the goals of the survey, the details of the sample and some of the auxiliary observing programs that we have started to collect complementary data. We also use the available multifrequency data to carry out an analysis of the statistical properties of the sample.", "date": "2010-02-26", "date_type": "published", "publication": "Publications of the Astronomical Society of the Pacific", "volume": "122", "number": "889", "publisher": "Astronomical Society of the Pacific", "pagerange": "261-287", "id_number": "CaltechAUTHORS:20100331-134059745", "issn": "0004-6280", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100331-134059745", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" }, { "agency": "GOLD Mine database" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/651535", "primary_object": { "basename": "Boselli2010p7284Publ_Astron_Soc_Pac.pdf", "url": "https://authors.library.caltech.edu/records/s7paf-mse63/files/Boselli2010p7284Publ_Astron_Soc_Pac.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Boselli, A.; Eales, S.; et el." }, { "id": "https://authors.library.caltech.edu/records/rnep3-rh416", "eprint_id": 17581, "eprint_status": "archive", "datestamp": "2023-08-21 23:24:23", "lastmod": "2023-10-20 00:01:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" }, { "id": "Ade-P", "name": { "family": "Ade", "given": "P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Brown-M-L", "name": { "family": "Brown", "given": "M. L." } }, { "id": "Cahill-G", "name": { "family": "Cahill", "given": "G." } }, { "id": "Castro-P-G", "name": { "family": "Castro", "given": "P. G." } }, { "id": "Church-S", "name": { "family": "Church", "given": "S." } }, { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Friedman-R-B", "name": { "family": "Friedman", "given": "R. B." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Gupta-S", "name": { "family": "Gupta", "given": "S." } }, { "id": "Hinderks-J", "name": { "family": "Hinderks", "given": "J." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Melhuish-S-J", "name": { "family": "Melhuish", "given": "S. J." } }, { "id": "Memari-Y", "name": { "family": "Memari", "given": "Y." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "O'Sullivan-C", "name": { "family": "O'Sullivan", "given": "C." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Rajguru-N", "name": { "family": "Rajguru", "given": "N." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Schwarz-R", "name": { "family": "Schwarz", "given": "R." } }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Turner-A-H", "name": { "family": "Turner", "given": "A. H." } }, { "id": "Wu-E-Y-S", "name": { "family": "Wu", "given": "E. Y. S." } } ] }, "title": "Characterization of the Millimeter-Wave Polarization of Centaurus A with QUaD", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic background radiation; galaxies: individual (Centaurus A); instrumentation: polarimeters; radio continuum: general", "note": "\u00a9 2010 American Astronomical Society.\n\nPrint publication: Issue 2 (2010 February 20); received 2009 August 17; accepted for publication 2009 December 30;\npublished 2010 February 1.\n\nQUaD is funded by the National Science Foundation in the\nUSA, through grants ANT-0338138, ANT-0338335, and ANT-\n0338238, by the Science and Technology Facilities Council\n(STFC) in the UK and by the Science Foundation Ireland. The\nBOOMERanG collaboration kindly allowed the use of their\nCMB maps for our calibration purposes. M.Z. acknowledges\nsupport from aNASA Postdoctoral Fellowship. P.G.C. acknowledges funding from the Portuguese FCT. S.E.C. acknowledges support from a Stanford Terman Fellowship. J.R.H. acknowledges the support of an NSF Graduate Research Fellowship, a Stanford Graduate Fellowship, and a NASA Postdoctoral Fellowship. Y.M. acknowledges support from a SUPA Prize studentship. C.P. acknowledges partial support from the Kavli Institute for Cosmological Physics through the grant NSF PHY-0114422. E.Y.W. acknowledges receipt of an NDSEG fellowship.\n\nPublished - Zemcov2010p7140Astrophys_J.pdf
", "abstract": "Centaurus (Cen) A represents one of the best candidates for an isolated, compact, highly polarized source that is bright at typical cosmic microwave background (CMB) experiment frequencies. We present measurements of the 4\u00b0 \u00d7 2\u00b0 region centered on Cen A with QUaD, a CMB polarimeter whose absolute polarization angle is known to an accuracy of 0\u00b0.5. Simulations are performed to assess the effect of misestimation of the instrumental parameters on the final measurement and systematic errors due to the field's background structure and temporal variability from Cen A's nuclear region are determined. The total (Q, U) of the inner lobe region is (1.00 \u00b1 0.07(stat.) \u00b1 0.04(sys.), -1.72 \u00b1 0.06 \u00b1 0.05) Jy at 100 GHz and (0.80 \u00b1 0.06 \u00b1 0.06, \u2013 1.40 \u00b1 0.07 \u00b1 0.08) Jy at 150 GHz, leading to polarization angles and total errors of \u201330.\u00b00 \u00b1 1.\u00b01 and \u201329.\u00b01 \u00b1 1.\u00b07. These measurements will allow the use of Cen A as a polarized calibration source for future millimeter experiments.", "date": "2010-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "710", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1541-1550", "id_number": "CaltechAUTHORS:20100224-112332982", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100224-112332982", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA Postdoctoral Fellowship" }, { "agency": "Portuguese Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia (FCT)" }, { "agency": "Stanford Terman Fellowship" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Stanford Graduate Fellowship" }, { "agency": "SUPA Prize studentship" }, { "agency": "Kavli Institute for Cosmological Physics" }, { "agency": "NSF", "grant_number": "PHY-0114422" }, { "agency": "National Defense Science and Engineering Graduate (NDSEG) fellowship" } ] }, "corp_creators": { "items": [ "QUaD collaboration" ] }, "doi": "10.1088/0004-637X/710/2/1541", "primary_object": { "basename": "Zemcov2010p7140Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/rnep3-rh416/files/Zemcov2010p7140Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Zemcov, M.; Ade, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/8n7ye-28068", "eprint_id": 17222, "eprint_status": "archive", "datestamp": "2023-08-21 23:13:15", "lastmod": "2023-10-19 23:40:01", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Roy-Arabindo", "name": { "family": "Roy", "given": "Arabindo" } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "Peter A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "Edward L." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "Mark J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "Simon R." } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "Matthew" } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "Joshua O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "Mark" }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "Peter C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "David H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "Jeff" } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "Gaelen" } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "Peter G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "Philip" }, "orcid": "0000-0001-6397-5516" }, { "id": "Miville-Desch\u00eanes-M-A", "name": { "family": "Miville-Desch\u00eanes", "given": "Marc-Antoine" } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "Calvin B." } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "Luca" }, "orcid": "0000-0002-1162-7947" }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "Guillaume" } }, { "id": "Rex-M", "name": { "family": "Rex", "given": "Marie" } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "Christopher" } }, { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "Matthew D. P" } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "Carole" } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "Gregory S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "Donald V." } } ] }, "title": "BLAST05: Power Spectra of Bright Galactic Cirrus at Submillimeter Wavelengths", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; ISM: clouds; ISM: structure; submillimeter", "note": "\u00a9 2010 American Astronomical Society. \n\nPrint publication: Issue 2 (2010 January 10); received 2009 October 5; accepted for publication 2009 November 19; published 2009 December 23. \n\nThe BLAST collaboration acknowledges the support of NASA through grant numbers NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space Agency (CSA), the UK Particle Physics & Astronomy Research Council (PPARC), and Canada's Natural Sciences and Engineering Research Council (NSERC). We thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work.\n\nPublished - Roy2010p6719Astrophys_J.pdf
", "abstract": "We report multi-wavelength power spectra of diffuse Galactic dust emission from Balloon-borne Large Aperture Submillimeter Telescope observations at 250, 350, and 500 \u03bcm in Galactic plane fields in Cygnus X and Aquila. These submillimeter power spectra statistically quantify the self-similar structure observable over a broad range of scales and can be used to assess the cirrus noise which limits the detection of faint point sources. The advent of submillimeter surveys with the Herschel Space Observatory makes the wavelength dependence a matter of interest. We show that the observed relative amplitudes of the power spectra can be related through a spectral energy distribution (SED). Fitting a simple modified black body to this SED, we find the dust temperature in Cygnus X to be 19.8 \u00b1 1.5 K and in the Aquila region 16.8 \u00b1 0.8 K. Our empirical estimates provide important new insight into the substantial cirrus noise that will be encountered in forthcoming observations.", "date": "2010-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "708", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1611-1620", "id_number": "CaltechAUTHORS:20100119-143234314", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100119-143234314", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Particle Physics & Astronomy Research Council (PPARC)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "doi": "10.1088/0004-637X/708/2/1611", "primary_object": { "basename": "Roy2010p6719Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/8n7ye-28068/files/Roy2010p6719Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Roy, Arabindo; Ade, Peter A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/e7bb4-b4307", "eprint_id": 17219, "eprint_status": "archive", "datestamp": "2023-08-21 23:13:10", "lastmod": "2024-02-26 17:38:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "name": { "family": "Sayers", "given": "J." } }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aguirre-J-E", "name": { "family": "Aguirre", "given": "J. E." }, "orcid": "0000-0002-4810-666X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Edgington-S-F", "name": { "family": "Edgington", "given": "S. F." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Goldin-A-L", "name": { "family": "Goldin", "given": "A." } }, { "id": "Haig-D", "name": { "family": "Haig", "given": "D." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Laurent-G-T", "name": { "family": "Laurent", "given": "G. T." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Rossinot-P", "name": { "family": "Rossinot", "given": "P." } }, { "id": "Schlaerth-J", "name": { "family": "Schlaerth", "given": "J." } } ] }, "title": "Studies of Millimeter-wave Atmospheric Noise above Mauna Kea", "ispublished": "pub", "full_text_status": "public", "keywords": "atmospheric effects; site testing; techniques: photometric", "note": "\u00a9 2010 American Astronomical Society. \n\nPrint publication: Issue 2 (2010 January 10); received 2009 April 24; accepted for publication 2009 November 24; published 2009 December 23. \n\nWe acknowledge the assistance of the following: Minhee Yun and Anthony D. Turner of NASA's Jet Propulsion Laboratory, who fabricated the Bolocam science array; Toshiro Hatake of the JPL electronic packaging group, who wirebonded the array; Marty Gould of Zen Machine and Ricardo Paniagua and the Caltech PMA/GPS Instrument Shop, who fabricated much of the Bolocam hardware; Carole Tucker of Cardiff University, who tested metal-mesh reflective filters used in Bolocam; Ben Knowles of the University of Colorado, who contributed to the software pipeline, the day crew and Hilo staff of the Caltech Submillimeter Observatory, who provided invaluable assistance during commissioning and data-taking for this survey data set; high school teacher Tobias Jacoby and high school students Jonathon Graff, Gloria Lee, and Dalton Sargent, who helped as summer research assistants; and Kathy Deniston, who provided effective administrative support at Caltech. We thank W. L. Holzapfel for his many useful comments as referee of our manuscript. Bolocam was constructed and commissioned using funds from NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846, NSF/AST-0229008, and NSF/AST-0206158. J.S. and G.L. were partially supported by NASA Graduate Student Research Fellowships, J.S. was partially supported by a NASA Postdoctoral Program Fellowship, J.A. was partially supported by a Jansky Postdoctoral Fellowship, and S.G. was partially supported by a R. A. Millikan Postdoctoral Fellowship at Caltech. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of\nTechnology, under a contract with the National Aeronautics and Space Administration. \n\nFacility: CSO\n\nPublished - Sayers2010p6717Astrophys_J.pdf
", "abstract": "We report measurements of the fluctuations in atmospheric emission (atmospheric noise) above Mauna Kea recorded with Bolocam at 143 and 268 GHz from the Caltech Submillimeter Observatory. The 143 GHz data were collected during a 40 night observing run in late 2003, and the 268 GHz observations were made in early 2004 and early 2005 over a total of 60 nights. Below \u22430.5 Hz, the data time-streams are dominated by atmospheric noise in all observing conditions. The atmospheric noise data are consistent with a Kolmogorov–Taylor turbulence model for a thin wind-driven screen, and the median amplitude of the fluctuations is 280 mK2 rad−5/3 at 143 GHz and 4000 mK2 rad−5/3 at 268 GHz. Comparing our results with previous ACBAR data, we find that the normalization of the power spectrum of the atmospheric noise fluctuations is a factor of \u224380 larger above Mauna Kea than above the South Pole at millimeter wavelengths. Most of this difference is due to the fact that the atmosphere above the South Pole is much drier than the atmosphere above Mauna Kea. However, the atmosphere above the South Pole is slightly more stable as well: the fractional fluctuations in the column depth of precipitable water vapor are a factor of \u2243√2 smaller at the South Pole compared to Mauna Kea. Based on our atmospheric modeling, we developed several algorithms to remove the atmospheric noise, and the best results were achieved when we described the fluctuations using a low-order polynomial in detector position over the 8' field of view. However, even with these algorithms, we were not able to reach photon-background-limited instrument photometer performance at frequencies below \u22430.5 Hz in any observing conditions. We also observed an excess low-frequency noise that is highly correlated between detectors separated by \u2272(f/#)λ; this noise appears to be caused by atmospheric fluctuations, but we do not have an adequate model to explain its source. We hypothesize that the correlations arise from the classical coherence of the electromagnetic field across a distance of \u2243(f/#)λ on the focal plane.
", "date": "2010-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "708", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1674-1691", "id_number": "CaltechAUTHORS:20100119-142858967", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100119-142858967", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-9618798" }, { "agency": "NSF", "grant_number": "AST-0098737" }, { "agency": "NSF", "grant_number": "AST-9980846" }, { "agency": "NSF", "grant_number": "AST-0229008" }, { "agency": "NSF", "grant_number": "AST-0206158" }, { "agency": "NASA Graduate Student Research Fellowship" }, { "agency": "National Radio Astronomy Observatory" }, { "agency": "Caltech Millikan Fellowship" }, { "agency": "NASA Postdoctoral Program" }, { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1088/0004-637X/708/2/1674", "primary_object": { "basename": "Sayers2010p6717Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/e7bb4-b4307/files/Sayers2010p6717Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2010", "author_list": "Sayers, J.; Golwala, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/0qqt9-kx166", "eprint_id": 17078, "eprint_status": "archive", "datestamp": "2023-08-21 22:56:51", "lastmod": "2023-10-19 22:47:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "Donald V." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "Peter A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "Edward L." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "Mark J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "Simon" } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "Matthew" } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "Joshua O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "Mark" }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "Peter C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "David H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "Jeff" } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "Gaelen" } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "Peter G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "Philip" }, "orcid": "0000-0001-6397-5516" }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "Calvin B." } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "Luca" }, "orcid": "0000-0002-1162-7947" }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "Enzo" }, "orcid": "0000-0002-3242-8154" }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "Guillaume" } }, { "id": "Rex-M", "name": { "family": "Rex", "given": "Marie" } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "Christopher" } }, { "id": "Thomas-Nicholas-E", "name": { "family": "Thomas", "given": "Nicholas E." } }, { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "Matthew D. P." } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "Carole" } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "Gregory S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } } ] }, "title": "BLAST Observations of Resolved Galaxies: Temperature Profiles and the Effect of Active Galactic Nuclei on FIR to Submillimeter Emission", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; galaxies: photometry; submillimeter; telescopes", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 2 (2009 December 20); received 2009 July 21; accepted for publication 2009 November 2; published 2009 December 7. \n\nThe BLAST collaboration acknowledges the support of NASA through grant numbers NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space Agency (CSA), Canada's Natural Sciences and Engineering Research Council (NSERC), and the UK Particle Physics & Astronomy Research Council (PPARC). We thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work. L.O. acknowledges partial support by the Puerto Rico Space Grant Consortium and by the Fondo Istitucional para la Investigacion of the University of Puerto Rico. C.B.N. acknowledges support from the Canadian Institute forAdvanced Research. This research has been enabled by the use of WestGrid computing resources. This work is based in part on observations made with the Spitzer Space Telescope, and has also made use of the NASA/IPAC Extragalactic Database (NED), both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contracts with the National Aeronautics and Space Administration. This research also made use of the SIMBAD database, operated at the Centre de Don\u00e9es astronomiques de Strasbourg (CDS), Strasbourg, France.\n\nPublished - Wiebe2009p6671Astrophys_J.pdf
", "abstract": "Over the course of two flights, the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) made resolved maps of seven nearby (<25 Mpc) galaxies at 250, 350, and 500 \u03bcm. During its 2005 June flight from Sweden, BLAST observed a single nearby galaxy, NGC 4565. During the 2006 December flight from Antarctica, BLAST observed the nearby galaxies NGC 1097, NGC 1291, NGC 1365, NGC 1512, NGC 1566, and NGC 1808. We fit physical dust models to a combination of BLAST observations and other available data for the galaxies observed by Spitzer. We fit a modified blackbody to the remaining galaxies to obtain total dust mass and mean dust temperature. For the four galaxies with Spitzer data, we also produce maps and radial profiles of dust column density and temperature. We measure the fraction of BLAST detected flux originating from the central cores of these galaxies and use this to calculate a \"core fraction,\" an upper limit on the \"active galactic nucleus fraction\" of these galaxies. We also find our resolved observations of these galaxies give a dust mass estimate 5-19 times larger than an unresolved observation would predict. Finally, we are able to use these data to derive a value for the dust mass absorption coefficient of \u03ba = 0.29 \u00b1 0.03 m^2 kg^(\u20131) at 250 \u03bcm. This study is an introduction to future higher-resolution and higher-sensitivity studies to be conducted by Herschel and SCUBA-2.", "date": "2009-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "707", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1809-1823", "id_number": "CaltechAUTHORS:20100106-113854541", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100106-113854541", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "University of Puerto Rico" } ] }, "doi": "10.1088/0004-637X/707/2/1809", "primary_object": { "basename": "Wiebe2009p6671Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/0qqt9-kx166/files/Wiebe2009p6671Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Wiebe, Donald V.; Ade, Peter A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/62a8a-grz27", "eprint_id": 17080, "eprint_status": "archive", "datestamp": "2023-08-21 22:56:56", "lastmod": "2023-10-19 22:47:49", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "Matthew D. P" } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "Peter A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "Edward L." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "Mark J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "Simon R." } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "Matthew" } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "Joshua O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "Mark" }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "Peter C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "David H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "Jeff" } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "Gaelen" } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "Peter G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "Philip" }, "orcid": "0000-0001-6397-5516" }, { "id": "Moncelsi-Lorenzo", "name": { "family": "Moncelsi", "given": "Lorenzo" }, "orcid": "0000-0002-4242-3015" }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. Barth" } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "Luca" }, "orcid": "0000-0002-1162-7947" }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "Enzo" }, "orcid": "0000-0002-3242-8154" }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "Guillaume" } }, { "id": "Rex-M", "name": { "family": "Rex", "given": "Marie" } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "Christopher" } }, { "id": "Thomas-Nicholas-E", "name": { "family": "Thomas", "given": "Nicholas E." } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "Carole" } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "Gregory S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "Donald V." } } ] }, "title": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2006: Calibration and Flight Performance", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; submillimeter; telescopes", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 2 (2009 December 20); received 2009 April 6; accepted for publication 2009 September 30; published 2009 December 7. \n\nWe acknowledge the support of NASA through grant Nos. NAG5-12785, NAG5-13301, and NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology Facilities Council (STFC).We thank D. Dowell, T. Jenness, and J. Aguirre for their data. This research has been enabled by the use of WestGrid computing resources. This research also made use of the SIMBAD database, operated at the CDS, France, and the NASA/IPAC Extragalactic Database (NED), operated by the Jet Propulsion Laboratory, under contract with NASA.\n\nPublished - Truch2009p6667Astrophys_J.pdf
", "abstract": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) operated successfully during a 250 hr flight over Antarctica in 2006 December (BLAST06). As part of the calibration and pointing procedures, the red hypergiant star VY CMa was observed and used as the primary calibrator. Details of the overall BLAST06 calibration procedure are discussed. The 1\u03c3 uncertainty on the absolute calibration is accurate to 9.5%, 8.7%, and 9.2% at the 250, 350, and 500 \u03bcm bands, respectively. The errors are highly correlated between bands resulting in much lower errors for the derived shape of the 250-500 \u03bcm continuum. The overall pointing error is < 5'' rms for the 36'', 42'', and 60'' beams. The performance of optics and pointing systems is discussed.", "date": "2009-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "707", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1723-1728", "id_number": "CaltechAUTHORS:20100106-132419629", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100106-132419629", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "NSF" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "doi": "10.1088/0004-637X/707/2/1723", "primary_object": { "basename": "Truch2009p6667Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/62a8a-grz27/files/Truch2009p6667Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Truch, Matthew D. P; Ade, Peter A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/6evdf-h2j43", "eprint_id": 17095, "eprint_status": "archive", "datestamp": "2023-08-21 22:57:01", "lastmod": "2023-10-19 22:48:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Olmi-L", "name": { "family": "Olmi", "given": "Luca" }, "orcid": "0000-0002-1162-7947" }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "Peter A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Angl\u00e9s-Alc\u00e1zar-D", "name": { "family": "Angl\u00e9s-Alc\u00e1zar", "given": "Daniel" }, "orcid": "0000-0001-5769-4945" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "Edward L." } }, { "id": "De-Luca-M", "name": { "family": "De Luca", "given": "Massimo" } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "Mark J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "Simon" } }, { "id": "Elia-D", "name": { "family": "Elia", "given": "Davide" } }, { "id": "Fazio-G-G", "name": { "family": "Fazio", "given": "Giovanni G." }, "orcid": "0000-0002-0670-0708" }, { "id": "Giannini-T", "name": { "family": "Giannini", "given": "Teresa" } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "Matthew" } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "Joshua O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "Mark" }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "Peter C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "David H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "Jeff" } }, { "id": "Lorenzetti-D", "name": { "family": "Lorenzetti", "given": "Dario" } }, { "id": "Marengo-M", "name": { "family": "Marengo", "given": "Massimo" }, "orcid": "0000-0001-9910-9230" }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "Gaelen" } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "Peter G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Massi-F", "name": { "family": "Massi", "given": "Fabrizio" } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "Philip" }, "orcid": "0000-0001-6397-5516" }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "Calvin B." } }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "Guillaume" } }, { "id": "Rex-M", "name": { "family": "Rex", "given": "Marie" } }, { "id": "Salama-A", "name": { "family": "Salama", "given": "Alberto" } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "Christopher" } }, { "id": "Smith-H-A", "name": { "family": "Smith", "given": "Howard A." } }, { "id": "Strafella-F", "name": { "family": "Strafella", "given": "Francesco" } }, { "id": "Thomas-Nicholas-E", "name": { "family": "Thomas", "given": "Nicholas E." } }, { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "Matthew D. P" } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "Carole" } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "Gregory S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "Donald V." } } ] }, "title": "The Blast Survey of the Vela Molecular Cloud: Physical Properties of the Dense Cores in Vela-D", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; ISM: clouds; stars: formation; submillimeter", "note": "\u00a9 2009 American Astronomical Society. \n\nPrint publication: Issue 2 (2009 December 20); received 2009 September 2; accepted for publication 2009 November 3; published 2009 December 7. \n\nWe acknowledge the support of NASA through grant numbers NAG5-12785,NAG5-13301, and NNGO-6GI11G, the NSF Office of Polar Programs, the Canadian Space Agency, the Natural Sciences and Engineering Research Council (NSERC) of Canada, and the UK Science and Technology Facilities Council (STFC). This work is also based, in part, on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. L.O. acknowledges partial support by the Puerto Rico Space Grant Consortium and by the Decanato de Estudios Graduados e Investigaci\u00f3n of the University of Puerto Rico.\n\nPublished - Olmi2009p6665Astrophys_J.pdf
", "abstract": "The Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) carried out a 250, 350, and 500 \u03bcm survey of the galactic plane encompassing the Vela Molecular Ridge, with the primary goal of identifying the coldest dense cores possibly associated with the earliest stages of star formation. Here, we present the results from observations of the Vela-D region, covering about 4 deg^2, in which we find 141 BLAST cores. We exploit existing data taken with the Spitzer MIPS, IRAC, and SEST-SIMBA instruments to constrain their (single-temperature) spectral energy distributions, assuming a dust emissivity index \u03b2 = 2.0. This combination of data allows us to determine the temperature, luminosity, and mass of each BLAST core, and also enables us to separate starless from protostellar sources. We also analyze the effects that the uncertainties on the derived physical parameters of the individual sources have on the overall physical properties of starless and protostellar cores, and we find that there appear to be a smooth transition from the pre- to the protostellar phase. In particular, for protostellar cores we find a correlation between the MIPS24 flux, associated with the central protostar, and the temperature of the dust envelope. We also find that the core mass function of the Vela-D cores has a slope consistent with other similar (sub)millimeter surveys.", "date": "2009-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "707", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1836-1851", "id_number": "CaltechAUTHORS:20100107-142047477", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100107-142047477", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "NSF" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "JPL/Caltech" }, { "agency": "Puerto Rico Space Grant Consortium" }, { "agency": "University of Puerto Rico" } ] }, "doi": "10.1088/0004-637X/707/2/1836", "primary_object": { "basename": "Olmi2009p6665Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/6evdf-h2j43/files/Olmi2009p6665Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Olmi, Luca; Ade, Peter A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/rjnzs-xej41", "eprint_id": 16587, "eprint_status": "archive", "datestamp": "2023-08-21 22:39:14", "lastmod": "2023-10-19 22:24:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Brown-M-L", "name": { "family": "Brown", "given": "M. L." } }, { "id": "Ade-P", "name": { "family": "Ade", "given": "P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Cahill-G", "name": { "family": "Cahill", "given": "G." } }, { "id": "Castro-P-G", "name": { "family": "Castro", "given": "P. G." } }, { "id": "Church-S", "name": { "family": "Church", "given": "S." } }, { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Friedman-R-B", "name": { "family": "Friedman", "given": "R. B." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Gupta-S", "name": { "family": "Gupta", "given": "S." } }, { "id": "Hinderks-J", "name": { "family": "Hinderks", "given": "J." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Melhuish-S-J", "name": { "family": "Melhuish", "given": "S. J." } }, { "id": "Memari-Y", "name": { "family": "Memari", "given": "Y." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "O'Sullivan-C", "name": { "family": "O' Sullivan", "given": "C." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Rajguru-N", "name": { "family": "Rajguru", "given": "N." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Schwarz-R", "name": { "family": "Schwarz", "given": "R." } }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Turner-A-H", "name": { "family": "Turner", "given": "A. H." } }, { "id": "Wu-E-Y-S", "name": { "family": "Wu", "given": "E. Y. S." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Improved Measurements of the Temperature and Polarization of the Cosmic Microwave Background from QUaD", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmological parameters; cosmology: observations; polarization", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2009 June 5; accepted 2009 August 31; published 2009 October 16.\nQUaD is funded by the National Science Foundation in the\nUSA through grants ANT-0338138, ANT-0338335, and ANT-\n0338238, by the Science and Technology Facilities Council\n(STFC) in the UK and by the Science Foundation Ireland. The\nBOOMERanG collaboration kindly allowed the use of their\nCMB maps for our calibration purposes. P.G.C. acknowledges\nfunding from the Portuguese FCT. S.E.C. acknowledges support\nfrom a Stanford Terman Fellowship. J.R.H. acknowledges the\nsupport of an NSF Graduate Research Fellowship, a Stanford\nGraduate Fellowship and a NASA Postdoctoral Fellowship.\nY.M. acknowledges support from a SUPA Prize studentship.\nC.P. acknowledges partial support from the Kavli Institute for\nCosmological Physics through the grant NSF PHY-0114422.\nE.Y.W. acknowledges receipt of an NDSEG fellowship. M.Z.\nacknowledges support from a NASA Postdoctoral Fellowship.\nPart of the analysis described in this paper was carried out on\nthe University of Cambridge's distributed computing facility,\nCAMGRID. We acknowledge the use of the FFTW (Frigo &\nJohnson 2005), CAMB (Lewis et al. 2000), CosmoMC (Lewis\n& Bridle 2002), and HEALPix (G\u00b4orski et al. 2005) packages.\nWe acknowledge the use of the Legacy Archive for Microwave\nBackground Data Analysis (LAMBDA). Support for LAMBDA\nis provided by the NASA Office of Space Science.\n\nPublished - Brown2009p6238Astrophys_J.pdf
", "abstract": "We present an improved analysis of the final data set from the QUaD experiment. Using an improved technique to remove ground contamination, we double the effective sky area and hence increase the precision of our cosmic microwave background (CMB) power spectrum measurements by ~30% versus that previously reported. In addition, we have improved our modeling of the instrument beams and have reduced our absolute calibration uncertainty from 5% to 3.5% in temperature. The robustness of our results is confirmed through extensive jackknife tests, and by way of the agreement that we find between our two fully independent analysis pipelines. For the standard six-parameter \u039bCDM model, the addition of QUaD data marginally improves the constraints on a number of cosmological parameters over those obtained from the WMAP experiment alone. The impact of QUaD data is significantly greater for a model extended to include either a running in the scalar spectral index, or a possible tensor component, or both. Adding both the QUaD data and the results from the Arcminute Cosmology Bolometer Array Receiver experiment, the uncertainty in the spectral index running is reduced by ~25% compared to WMAP alone, while the upper limit on the tensor-to-scalar ratio is reduced from r < 0.48 to r < 0.33 (95% c.l.). This is the strongest limit on tensors to date from the CMB alone. We also use our polarization measurements to place constraints on parity-violating interactions to the surface of last scattering, constraining the energy scale of Lorentz violating interactions to <1.5 \u00d7 10^(\u201343) GeV (68% c.l.). Finally, we place a robust upper limit on the strength of the lensing B-mode signal. Assuming a single flat band power between \u2113 = 200 and \u2113 = 2000, we constrain the amplitude of B-modes to be <0.57 \u03bcK^2 (95% c.l.).", "date": "2009-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "705", "number": "1", "publisher": "American Astronomical Society", "pagerange": "978-999", "id_number": "CaltechAUTHORS:20091105-090201427", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091105-090201427", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Science Foundation Ireland" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Stanford Graduate Fellowship" }, { "agency": "NASA Postdoctoral Fellowship" }, { "agency": "Scottish Universities Physics Alliance (SUPA) Prize studentship" }, { "agency": "Kavli Institute for Cosmological Physics", "grant_number": "NSF PHY-0114422" }, { "agency": "National Defense Science and Engineering Graduate Fellowship (NDSEG)" } ] }, "corp_creators": { "items": [ "The QUaD collaboration" ] }, "doi": "10.1088/0004-637X/705/1/978", "primary_object": { "basename": "Brown2009p6238Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/rjnzs-xej41/files/Brown2009p6238Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Brown, M. L.; Ade, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/t5akv-mvr98", "eprint_id": 16582, "eprint_status": "archive", "datestamp": "2023-08-21 22:38:53", "lastmod": "2023-10-19 22:24:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bradford-C-M", "name": { "family": "Bradford", "given": "C. M." }, "orcid": "0000-0001-5261-7094" }, { "id": "Aguirre-J-E", "name": { "family": "Aguirre", "given": "J. E." }, "orcid": "0000-0002-4810-666X" }, { "id": "Aikin-R", "name": { "family": "Aikin", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Earle-L", "name": { "family": "Earle", "given": "L." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Inami-Hanae", "name": { "family": "Inami", "given": "H." }, "orcid": "0000-0003-4268-0393" }, { "id": "Maloney-P-R", "name": { "family": "Maloney", "given": "P. R." } }, { "id": "Matsuhara-Hideo", "name": { "family": "Matsuhara", "given": "H." } }, { "id": "Naylor-B-J", "name": { "family": "Naylor", "given": "B. J." } }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } }, { "id": "Zmuidzinas-J", "name": { "family": "Zmuidzinas", "given": "J." } } ] }, "title": "The Warm Molecular Gas around the Cloverleaf Quasar", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: ISM; instrumentation: spectrographs; ISM: clouds; stars: luminosity function, mass function; techniques: spectroscopic", "note": "\u00a9 2009 The American Astronomical Society.\nReceived 2009 May 29; accepted 2009 August 18; published 2009 October 8.\nWe are indebted to the staff of the Caltech Submillimeter\nObservatory for their help in Z-Spec's commissioning and\nobserving. We acknowledge Peter Ade and his group for some of\nthe filters and Lionel Duband for the 3He/4He refrigerator in ZSpec,\nand are grateful for their help in the early integration of the\ninstrument. We benefitted from conversations with Tom Phillips,\nPaul Goldsmith, Simon Radford, and Andy Harris, as well as\nhelpful comments from Xinyu Dai and an anonymous referee.\nFinally, we acknowledge the following grants and fellowships:\nNASA SARA grants NAGS-11911 and NAGS-12788, an NSF\nCareer grant (AST-0239270) and a Research Corporation Award\n(RI0928) to J. Glenn, a Caltech Millikan and JPL Director's\nfellowships to C.M.B., a NRAO Jansky fellowship to J. Aguirre,\nand NASA GSRP fellowship to L. Earle.\n\nPublished - Bradford2009p6229Astrophys_J.pdf
", "abstract": "We present the first broadband \u03bb = 1 mm spectrum toward the z = 2.56 Cloverleaf quasar, obtained with Z-Spec, a grating spectrograph on the 10.4 m Caltech Submillimeter Observatory. The 190-305 GHz observation band corresponds to the rest frame 272-444 \u03bcm, and we measure the dust continuum as well as all four transitions of carbon monoxide (CO) lying in this range. The power-law dust emission, F_\u03bd = 14 mJy(\u03bd/240 GHz)^(3.9) is consistent with the published continuum measurements. The CO J = 6 \u2192 5, J = 8 \u2192 7, and J = 9 \u2192 8 measurements are the first, and now provide the highest-J CO information in this source. Our measured CO intensities are very close to the previously published interferometric measurements of J = 7 \u2192 6, and we use all available transitions and our ^(13)CO upper limits to constrain the physical conditions in the Cloverleaf molecular gas disk. We find a large mass (2-50 \u00d7 10^9 M_\u2299) of highly excited gas with thermal pressure nT > 10^6 K cm^(\u20133). The ratio of the total CO cooling to the far-IR dust emission exceeds that in the local dusty galaxies, and we investigate the potential heating sources for this bulk of warm molecular gas. We conclude that both UV photons and X-rays likely contribute, and discuss implications for a top-heavy stellar initial mass function arising in the X-ray-irradiated starburst. Finally, we present tentative identifications of other species in the spectrum, including a possible detection of the H_2O 2_(0,2) \u2192 1_(1,1) transition at \u03bb_(rest) = 303 \u03bcm.", "date": "2009-11-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "705", "number": "1", "publisher": "American Astronomical Society", "pagerange": "112-122", "id_number": "CaltechAUTHORS:20091104-144315878", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091104-144315878", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAGS-11911" }, { "agency": "NASA", "grant_number": "NAGS-12788" }, { "agency": "NSF", "grant_number": "AST-0239270" }, { "agency": "Research Corporation", "grant_number": "RI0928" }, { "agency": "NASA Graduate Student Research Fellowship" } ] }, "doi": "10.1088/0004-637X/705/1/112", "primary_object": { "basename": "Bradford2009p6229Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/t5akv-mvr98/files/Bradford2009p6229Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Bradford, C. M.; Aguirre, J. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/jfmk9-yg253", "eprint_id": 16074, "eprint_status": "archive", "datestamp": "2023-08-21 22:22:06", "lastmod": "2023-10-19 21:55:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rex-M", "name": { "family": "Rex", "given": "Marie" } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "Peter A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "Itziar" }, "orcid": "0000-0002-6590-3994" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "Edward L." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "Mark J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "Simon R." } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "Matthew" } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "Joshua O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "Mark" }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "Peter C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "David H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "Jeff" } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "Gaelen" } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "Peter G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "Philip" }, "orcid": "0000-0001-6397-5516" }, { "id": "Monta\u00f1a-A", "name": { "family": "Monta\u00f1a", "given": "Alfredo" }, "orcid": "0000-0003-4229-381X" }, { "id": "Netterfield-C-B", "name": { "family": "Nettefield", "given": "Calvin B." } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "Luca" }, "orcid": "0000-0002-1162-7947" }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "Enzo" }, "orcid": "0000-0002-3242-8154" }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "Guillaume" } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "Douglas" }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "Christopher" } }, { "id": "Thomas-Nicholas-E", "name": { "family": "Thomas", "given": "Nicholas E." } }, { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "Matthew D. P" } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "Carole" } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "Gregory S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "Marco P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "Donald V." } } ] }, "title": "A Bright Submillimeter Source in the Bullet Cluster (1E0657-56) Field Detected with Blast", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: clusters: individual (1E0657-56); submillimeter", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 1 (2009 September 20); received 2009 April 7; accepted for publication 2009 July 29;\npublished 2009 August 27.\n\nWe acknowledge the support of NASA through grant NAG5-\n12785, NAG5- 13301, and NNGO-6GI11G, the NSF Office of\nPolar Programs, the Canadian Space Agency, the Natural Sciences\nand Engineering Research Council (NSERC) of Canada,\nand the UK Science and Technology Facilities Council (STFC).\nWe thank Tony Mroczkowski for his help with the SZE simulations.\nThis research has been enabled by the use of West-\nGrid computing resources. This research also made use of the\nSIMBAD database, observations made with the Spitzer Space\nTelescope, which is operated by the Jet Propulsion Laboratory,\nCalifornia Institute of Technology under a contract with NASA,\nand SAOImage DS9, developed by Smithsonian Astrophysical\nObservatory.\n\nPublished - Rex2009p5940Astrophys_J.pdf
", "abstract": "We present the 250, 350, and 500 \u03bcm detection of bright submillimeter emission in the direction of the Bullet Cluster measured by the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST). The 500 \u03bcm centroid is coincident with an AzTEC 1.1 mm point-source detection at a position close to the peak lensing magnification produced by the cluster. However, the 250 \u03bcm and 350 \u03bcm centroids are elongated and shifted toward the south with a differential shift between bands that cannot be explained by pointing uncertainties. We therefore conclude that the BLAST detection is likely contaminated by emission from foreground galaxies associated with the Bullet Cluster. The submillimeter redshift estimate based on 250-1100 \u03bcm photometry at the position of the AzTEC source is z_(phot) = 2.9^(+0.6)_(\u20130.3), consistent with the infrared color redshift estimation of the most likely Infrared Array Camera counterpart. These flux densities indicate an apparent far-infrared (FIR) luminosity of L_(FIR) = 2 \u00d7 10^(13) L_\u2609 . When the amplification due to the gravitational lensing of the cluster is removed, the intrinsic FIR luminosity of the source is found to be L_(FIR) \u2264 10^(12) L_\u2609, consistent with typical luminous infrared galaxies.", "date": "2009-09-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "703", "number": "1", "publisher": "American Astronomical Society", "pagerange": "348-353", "id_number": "CaltechAUTHORS:20090928-115957244", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090928-115957244", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "NSF" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Science and Technology Facilities Council (STFC)" } ] }, "doi": "10.1088/0004-637X/703/1/348", "primary_object": { "basename": "Rex2009p5940Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/jfmk9-yg253/files/Rex2009p5940Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Rex, Marie; Ade, Peter A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/x9txv-h8838", "eprint_id": 15741, "eprint_status": "archive", "datestamp": "2023-08-21 22:16:36", "lastmod": "2023-10-19 14:48:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Veneziani-M", "name": { "family": "Veneziani", "given": "M." } }, { "id": "Amblard-A", "name": { "family": "Amblard", "given": "A." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Piacentini-F", "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "id": "Pietrobon-D", "name": { "family": "Pietrobon", "given": "D." } }, { "id": "Serra-P", "name": { "family": "Serra", "given": "P." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bond-J-R", "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Borrill-J", "name": { "family": "Borrill", "given": "J." } }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Cabella-P", "name": { "family": "Cabella", "given": "P." } }, { "id": "Contaldi-C-R", "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "De-Gasperis-G", "name": { "family": "De Gasperis", "given": "G." } }, { "id": "de-Oliveira-Costa-A", "name": { "family": "de Oliveira-Costa", "given": "A." } }, { "id": "De-Troia-G", "name": { "family": "De Troia", "given": "G." } }, { "id": "di-Stefano-G", "name": { "family": "di Stefano", "given": "G." } }, { "id": "Ganga-K-M", "name": { "family": "Ganga", "given": "K. M." } }, { "id": "Hivon-E", "name": { "family": "Hivon", "given": "E." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Kisner-T-S", "name": { "family": "Kisner", "given": "T. S." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "MacTavish-C-J", "name": { "family": "MacTavish", "given": "C. J." } }, { "id": "Masi-S", "name": { "family": "Masi", "given": "S." }, "orcid": "0000-0001-5105-1439" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Melchiorri-A", "name": { "family": "Melchiorri", "given": "A." } }, { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T. E." } }, { "id": "Natoli-P", "name": { "family": "Natoli", "given": "P." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Polenta-G", "name": { "family": "Polenta", "given": "G." } }, { "id": "Ricciardi-S", "name": { "family": "Ricciardi", "given": "S." } }, { "id": "Romeo-G", "name": { "family": "Romeo", "given": "G." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Santini-P", "name": { "family": "Santini", "given": "P." } }, { "id": "Tegmark-M", "name": { "family": "Tegmark", "given": "M." } }, { "id": "Vittorio-N", "name": { "family": "Vittorio", "given": "N." } } ] }, "title": "Subdegree Sunyaev-Zel'dovich Signal from Multifrequency BOOMERANG Observations", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmological parameters; cosmology: observations; large-scale structure of universe", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 1 (2009 September 1); received 2009 April 28; accepted for publication 2009 July 23; published 2009 August 14.\n\nWe gratefully acknowledge support from NSF CAREER\nAST-0645427 at UCI. We also acknowledge support from\nthe Italian Space Agency (contracts I/087/06/0 and I/016/\n07/0), and from Programma Nazionale Ricerche in Antartide.\nThe authors acknowledge the use of the Planck Sky Model,\ndeveloped by theComponent SeparationWorking Group (WG2)\nof the Planck Collaboration.\n\nPublished - Veneziani2009p5807Astrophys_J_Lett.pdf
", "abstract": "The Sunyaev-Zel'dovich (SZ) effect is the inverse Compton-scattering of cosmic microwave background (CMB) photons by hot electrons in the intervening gas throughout the universe. The effect has a distinct spectral signature that allows its separation from other signals in multifrequency CMB data sets. Using CMB anisotropies measured at three frequencies by the BOOMERANG 2003 flight we constrain SZ fluctuations in the 10 arcmin to 1 deg angular range. Propagating errors and potential systematic effects through simulations, we obtain an overall upper limit of 15.3 \u03bcK (2\u03c3) for rms SZ fluctuations in a broad bin between multipoles of 250 and 1200 at the Rayleigh-Jeans (RJ) end of the spectrum. The resulting upper limit on the local universe normalization of the density perturbations with BOOMERANG SZ data alone is \u03c3^(SZ)_8 < 1.14 at the 95% confidence level. When combined with other CMB anisotropy and SZ measurements, we find \u03c3^(SZ)_8 < 0.92 (95% c.l.).", "date": "2009-09-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "702", "publisher": "American Astronomical Society", "pagerange": "L61-L65", "id_number": "CaltechAUTHORS:20090910-142750424", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090910-142750424", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0645427" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/087/06/0" }, { "agency": "Agenzia Spaziale Italiana (ASI)", "grant_number": "I/016/07/0" }, { "agency": "Programma Nazionale Ricerche in Antartide" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1088/0004-637X/702/1/L61", "primary_object": { "basename": "Veneziani2009p5807Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/x9txv-h8838/files/Veneziani2009p5807Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Veneziani, M.; Amblard, A.; et el." }, { "id": "https://authors.library.caltech.edu/records/7t8sj-0bt04", "eprint_id": 15296, "eprint_status": "archive", "datestamp": "2023-08-21 22:06:18", "lastmod": "2023-10-18 21:37:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Castro-P-G", "name": { "family": "Castro", "given": "P. G." } }, { "id": "Ade-P", "name": { "family": "Ade", "given": "P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Brown-M-L", "name": { "family": "Brown", "given": "M. L." } }, { "id": "Cahill-G", "name": { "family": "Cahill", "given": "G." } }, { "id": "Church-S", "name": { "family": "Church", "given": "S." } }, { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Friedman-R-B", "name": { "family": "Friedman", "given": "R. B." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Gupta-S", "name": { "family": "Gupta", "given": "S." } }, { "id": "Hinderks-J", "name": { "family": "Hinderks", "given": "J." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Melhuish-S-J", "name": { "family": "Melhuish", "given": "S. J." } }, { "id": "Memari-Y", "name": { "family": "Memari", "given": "Y." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Schwarz-R", "name": { "family": "Schwarz", "given": "R." } }, { "id": "O'Sullivan-C", "name": { "family": "O'Sullivan", "given": "C." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Rajguru-N", "name": { "family": "Rajguru", "given": "N." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Turner-A-H", "name": { "family": "Turner", "given": "A. H." } }, { "id": "Wu-E-Y-S", "name": { "family": "Wu", "given": "E. Y. S." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Cosmological Parameters from the QUaD CMB Polarization Experiment", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmological parameters; methods: statistical; polarization", "note": "\u00a9 2009. The American Astronomical Society. Received 2008 December 19; accepted 2009 May 11; published 2009 July 28.\nQUaD is funded by the National Science Foundation\nin the USA, through grants AST-0096778, ANT-0338138,\nANT-0338335, and ANT-0338238, by the UK Science and\nTechnology Facilities Council (STFC) and its predecessor the\nParticle Physics and Astronomy Research Council (PPARC),\nand by the Science Foundation Ireland. J.R.H. acknowledges\nthe support of an NSF Graduate Research Fellowship, a\nStanford Graduate Fellowship and a NASA Postdoctoral\nFellowship. C.P. and J.E.C. acknowledge partial support from\nthe Kavli Institute for Cosmological Physics through the grant\nNSF PHY-0114422. E.Y.W. acknowledges receipt of an NDSEG\nfellowship.Y.M. acknowledges support from a SUPAPrize\nstudentship. P.G.C. acknowledges funding from the Funda\u00e7\u00e3o\npara a Ci\u00eancia e a Tecnologia. M.Z. acknowledges support from\na NASA Postdoctoral Fellowship. This work has made use of\nthe resources provided by the Edinburgh Compute and Data\nFacility (ECDF) that is partially supported by the eDIKT initiative.\nWe also thank Licia Verde and Joanna Dunkley for useful\ndiscussion.\n\nPublished - Castro2009p5711Astrophys_J.pdf
", "abstract": "In this paper, we present a parameter estimation analysis of the polarization and temperature power spectra from the second and third season of observations with the QUaD experiment. QUaD has for the first time detected multiple acoustic peaks in the E-mode polarization spectrum with high significance. Although QUaD-only parameter constraints are not competitive with previous results for the standard six-parameter \u039bCDM cosmology, they do allow meaningful polarization-only parameter analyses for the first time. In a standard six-parameter \u039bCDM analysis, we find the QUaD TT power spectrum to be in good agreement with previous results. However, the QUaD polarization data show some tension with \u039bCDM. The origin of this 1\u03c3-2\u03c3 tension remains unclear, and may point to new physics, residual systematics, or simple random chance. We also combine QUaD with the five-year WMAP data set and the SDSS luminous red galaxies 4th data release power spectrum, and extend our analysis to constrain individual isocurvature mode fractions, constraining cold dark matter density, \u03b1_(cdmi) < 0.11 (95% confidence limit (CL)), neutrino density, \u03b1_(ndi) < 0.26 (95% CL), and neutrino velocity, \u03b1_(nvi) < 0.23 (95% CL), modes. Our analysis sets a benchmark for future polarization experiments.", "date": "2009-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "701", "number": "2", "publisher": "American Astronomical Society", "pagerange": "857-864", "id_number": "CaltechAUTHORS:20090825-104125123", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090825-104125123", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0096778" }, { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Science and Technology Facilities Council" }, { "agency": "NSF", "grant_number": "PHY-0114422" }, { "agency": "NASA" }, { "agency": "Department of Defense" }, { "agency": "SUPA Prize studentship" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia" }, { "agency": "e-Science Data, Information and Knowledge Transformation" }, { "agency": "Particle Physics and Astronomy Research Council" }, { "agency": "Science Foundation Ireland" }, { "agency": "Stanford University" } ] }, "corp_creators": { "items": [ "The QUaD collaboration" ] }, "doi": "10.1088/0004-637X/701/2/857", "primary_object": { "basename": "Castro2009p5711Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/7t8sj-0bt04/files/Castro2009p5711Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Castro, P. G.; Ade, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/a7kcf-fx758", "eprint_id": 14909, "eprint_status": "archive", "datestamp": "2023-08-21 22:02:41", "lastmod": "2023-10-18 20:22:35", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ashby-M-L-N", "name": { "family": "Ashby", "given": "M. L. N." }, "orcid": "0000-0002-3993-0745" }, { "id": "Stern-D", "name": { "family": "Stern", "given": "D." }, "orcid": "0000-0003-2686-9241" }, { "id": "Brodwin-M", "name": { "family": "Brodwin", "given": "M." }, "orcid": "0000-0002-4208-798X" }, { "id": "Griffith-R", "name": { "family": "Griffith", "given": "R." } }, { "id": "Eisenhardt-P-R-M", "name": { "family": "Eisenhardt", "given": "P." } }, { "id": "Kozlowski-S", "name": { "family": "Kozlowski", "given": "S." } }, { "id": "Kochanek-C-S", "name": { "family": "Kochanek", "given": "C. S." }, "orcid": "0000-0001-6017-2961" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Borys-C-J-K", "name": { "family": "Borys", "given": "C." } }, { "id": "Brand-K", "name": { "family": "Brand", "given": "K." } }, { "id": "Brown-M-J-I", "name": { "family": "Brown", "given": "M. J. I." }, "orcid": "0000-0002-1207-9137" }, { "id": "Cool-R-J", "name": { "family": "Cool", "given": "R." } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "A." }, "orcid": "0000-0002-3892-0190" }, { "id": "Croft-S-K", "name": { "family": "Croft", "given": "S." } }, { "id": "Dey-A", "name": { "family": "Dey", "given": "A." }, "orcid": "0000-0002-4928-4003" }, { "id": "Eisenstein-D-J", "name": { "family": "Eisenstein", "given": "D." } }, { "id": "Gonzalez-A-H", "name": { "family": "Gonzalez", "given": "A. H." }, "orcid": "0000-0002-0933-8601" }, { "id": "Gorjian-V", "name": { "family": "Gorjian", "given": "V." } }, { "id": "Grogin-N-A", "name": { "family": "Grogin", "given": "N. A." } }, { "id": "Ivison-R-J", "name": { "family": "Ivison", "given": "R. J." }, "orcid": "0000-0001-5118-1313" }, { "id": "Jacob-J-C", "name": { "family": "Jacob", "given": "J." } }, { "id": "Jannuzi-B-T", "name": { "family": "Jannuzi", "given": "B. T." }, "orcid": "0000-0002-1578-6582" }, { "id": "Mainzer-A-K", "name": { "family": "Mainzer", "given": "A." } }, { "id": "Moustakas-L-A", "name": { "family": "Moustakas", "given": "L. A." }, "orcid": "0000-0003-3030-2360" }, { "id": "R\u00f6ttgering-H-J-A", "name": { "family": "R\u00f6ttgering", "given": "H. J. A." } }, { "id": "Seymour-N", "name": { "family": "Seymour", "given": "N." }, "orcid": "0000-0003-3506-5536" }, { "id": "Smith-H-A", "name": { "family": "Smith", "given": "H. A." } }, { "id": "Stanford-S-A", "name": { "family": "Stanford", "given": "S. A." } }, { "id": "Stauffer-J-R", "name": { "family": "Stauffer", "given": "J. R." }, "orcid": "0000-0003-3595-7382" }, { "id": "Sullivan-Ian", "name": { "family": "Sullivan", "given": "I." }, "orcid": "0000-0003-0632-4607" }, { "id": "van-Breugel-W", "name": { "family": "van Breugel", "given": "W." } }, { "id": "Willner-S-P", "name": { "family": "Willner", "given": "S. P." }, "orcid": "0000-0002-9895-5758" }, { "id": "Wright-E-L", "name": { "family": "Wright", "given": "E. L." }, "orcid": "0000-0001-5058-1593" } ] }, "title": "The Spitzer Deep, Wide-field Survey", "ispublished": "pub", "full_text_status": "public", "keywords": "infrared: galaxies; infrared: stars; surveys", "note": "\u00a9 2009. The American Astronomical Society. \n\nReceived 2009 February 3; accepted 2009 June 1; published 2009 July 23. Print publication: Issue 1 (2009 August 10). \n\nThis work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through award number 1314516 issued by JPL/Caltech. This research made use of Montage, funded by the NASA's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Support for M.B. was provided by the W. M. Keck Foundation. The authors thank Andy Gould, whose suggestions improved the manuscript.\nFacilities: Spitzer Space Telescope (IRAC)\n\nPublished - Ashby2009p5563Astrophys_J.pdf
", "abstract": "The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 deg^(2) in the Bootes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit-for the first time-the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z ~ 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z ~ 1.5. This paper explains the SDWFS observing strategy and data processing, presents the SDWFS mosaics and source catalogs, and discusses some early scientific findings. The publicly released, full-depth catalogs contain 6.78, 5.23, 1.20, and 0.96 x 10^(5) distinct sources detected to the average 5 sigma, 4\"-diameter, aperture-corrected limits of 19.77, 18.83, 16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0 mu m, respectively. The SDWFS number counts and color-color distribution are consistent with other, earlier Spitzer surveys. At the 6 minute integration time of the SDWFS IRAC imaging, > 50% of isolated Faint Images of the Radio Sky at Twenty cm radio sources and > 80% of on-axis XBootes sources are detected out to 8.0 mu m. Finally, we present the four highest proper motion IRAC-selected sources identified from the multi-epoch imaging, two of which are likely field brown dwarfs of mid-T spectral class.", "date": "2009-08-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "701", "number": "1", "publisher": "American Astronomical Society", "pagerange": "428-453", "id_number": "CaltechAUTHORS:20090808-142505714", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090808-142505714", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "1314516" }, { "agency": "NASA", "grant_number": "NCC5-626" }, { "agency": "NSF" }, { "agency": "W. M. Keck Foundation" } ] }, "local_group": { "items": [ { "id": "TAPIR" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1088/0004-637X/701/1/428", "primary_object": { "basename": "Ashby2009p5563Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/a7kcf-fx758/files/Ashby2009p5563Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Ashby, M. L. N.; Stern, D.; et el." }, { "id": "https://authors.library.caltech.edu/records/89192-3ag63", "eprint_id": 15177, "eprint_status": "archive", "datestamp": "2023-08-21 22:00:01", "lastmod": "2023-10-18 21:03:16", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Friedman-R-B", "name": { "family": "Friedman", "given": "R. B." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Brown-M-L", "name": { "family": "Brown", "given": "M. L." } }, { "id": "Cahill-G", "name": { "family": "Cahill", "given": "G." } }, { "id": "Castro-P-G", "name": { "family": "Castro", "given": "P. G." } }, { "id": "Church-S", "name": { "family": "Church", "given": "S." } }, { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Gupta-S", "name": { "family": "Gupta", "given": "S." } }, { "id": "Hinderks-J", "name": { "family": "Hinderks", "given": "J." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Melhuish-S-J", "name": { "family": "Melhuish", "given": "S. J." } }, { "id": "Memari-Y", "name": { "family": "Memari", "given": "Y." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "O'Sullivan-C", "name": { "family": "O'Sullivan", "given": "C." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Rajguru-N", "name": { "family": "Rajguru", "given": "N." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Schwarz-R", "name": { "family": "Schwarz", "given": "R." } }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Turner-A-H", "name": { "family": "Turner", "given": "A. H." } }, { "id": "Wu-E-Y-S", "name": { "family": "Wu", "given": "E. Y. S." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Small Angular Scale Measurements of the Cosmic Microwave Background Temperature Power Spectrum From QUaD", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmology: observations", "note": "\u00a9 2009 American Astronomical Society.\n\nPrint publication: Issue 2 (2009 August 1); received 2009 January 27, accepted for publication 2009 June 26; published 2009 July 20.\n\nWe thank Gianfranco De Zotti for providing us with his radio\nsource counts at 100 and 150 GHz. QUaD is funded by the\nNational Science Foundation in the USA, through grants AST-\n0096778, ANT-0338138, ANT-0338335, and ANT-0338238, by\nthe UK Science and Technology Facilities Council (STFC) and\nits predecessor the Particle Physics and Astronomy Research\nCouncil (PPARC), and by the Science Foundation Ireland.\nJ.R.H. acknowledges the support of an NSF Graduate Research\nFellowship, a Stanford Graduate Fellowship and a NASA\nPostdoctoral Fellowship. C.P. acknowledges partial support\nfrom the Kavli Institute for Cosmological Physics through\nthe grant NSF PHY-0114422. E.Y.W. acknowledges receipt\nof an NDSEG fellowship. Y.M. acknowledges support from\na SUPA Prize studentship. P.G.C. acknowledges funding from\nthe Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia. M.Z. acknowledges support from a NASA Postdoctoral Fellowship.\n\nPublished - Friedman2009p5235Astrophys_J_Lett.pdf
", "abstract": "We present measurements of the cosmic microwave background (CMB) radiation temperature anisotropy in the multipole range 2000 < \u2113 < 3000 from the QUaD telescope's second and third observing seasons. After masking the brightest point sources our results are consistent with the primary \u039bCDM expectation alone. We estimate the contribution of residual (un-masked) radio point sources using a model calibrated to our own bright source observations, and a full simulation of the source finding and masking procedure. Including this contribution slightly improves the \u03c7^2. We also fit a standard Sunyaev-Zel'dovich (SZ) template to the bandpowers and see no strong evidence of an SZ contribution, which is as expected for \u03c3_8 \u2248 0.8.", "date": "2009-08-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "700", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L187-L191", "id_number": "CaltechAUTHORS:20090819-153500287", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090819-153500287", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0096778" }, { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "UK Science and Technology Facilities Council" }, { "agency": "Particle Physics and Astronomy Research Council" }, { "agency": "Science Foundation Ireland" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "NASA Postdoctoral Fellowship" }, { "agency": "NSF", "grant_number": "PHY-0114422" }, { "agency": "National Defense Science and Engineering (NDSEG) Graduate Fellowship" }, { "agency": "Scottish Universities Physics Alliance (SUPA) Prize" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia" } ] }, "doi": "10.1088/0004-637X/700/2/L187", "primary_object": { "basename": "Friedman2009p5235Astrophys_J_Lett.pdf", "url": "https://authors.library.caltech.edu/records/89192-3ag63/files/Friedman2009p5235Astrophys_J_Lett.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Friedman, R. B.; Ade, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/zyed2-2t624", "eprint_id": 15483, "eprint_status": "archive", "datestamp": "2023-08-21 21:11:13", "lastmod": "2023-10-19 14:30:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Reichardt-C-L", "name": { "family": "Reichardt", "given": "C. L." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bond-J-R", "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Brevik-J-A", "name": { "family": "Brevik", "given": "J. A." } }, { "id": "Contaldi-C-R", "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Daub-M-D", "name": { "family": "Daub", "given": "M. D." } }, { "id": "Dempsey-J-T", "name": { "family": "Dempsey", "given": "J. T." } }, { "id": "Goldstein-J-H", "name": { "family": "Goldstein", "given": "J. H." } }, { "id": "Holzapfel-W-L", "name": { "family": "Holzapfel", "given": "W. L." } }, { "id": "Kuo-Chia-Lam", "name": { "family": "Kuo", "given": "C. L." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Lueker-M", "name": { "family": "Lueker", "given": "M." } }, { "id": "Newcomb-M", "name": { "family": "Newcomb", "given": "M." } }, { "id": "Peterson-J-B", "name": { "family": "Peterson", "given": "J. B." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Runyan-M-C", "name": { "family": "Runyan", "given": "M. C." } }, { "id": "Staniszewski-Z", "name": { "family": "Staniszewski", "given": "Z." } } ] }, "title": "High-Resolution CMB Power Spectrum from the Complete ACBAR Data Set", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmology: observations", "note": "\u00a9 2009 The American Astronomical Society. \n\nReceived 2008 January 12; accepted 2008 November 9; published 2009 March 24. \n\nThe ACBAR program has been primarily supported by NSF office of polar programs grants OPP-8920223 and OPP-0091840. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC03-76SF00098. Some computations were performed on the Canada Foundation for Innovation funded CITA Sunnyvale cluster. Chao-Lin Kuo acknowledges support from a NASA postdoctoral fellowship, and Marcus Runyan acknowledges support from a Fermi fellowship. Christian Reichardt acknowledges support from a National Science Foundation Graduate Research Fellowship. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. We thank members of the BOOMERANG team, in particular Brendan Crill, Bill Jones, and Tom Montroy for\nproviding access to the B03 data, the pipeline used to generate simulation maps, and assistance with its operation. We thank Antony Lewis for discussions about ways to parameterize tests for weak lensing in the data.\n\nPublished - Reichardt2009p1366Astrophys_J.pdf
", "abstract": "In this paper, we present results from the complete set of cosmic microwave background (CMB) radiation temperature anisotropy observations made with the Arcminute Cosmology Bolometer Array Receiver (ACBAR) operating at 150 GHz. We include new data from the final 2005 observing season, expanding the number of detector hours by 210% and the sky coverage by 490% over that used for the previous ACBAR release. As a result, the band-power uncertainties have been reduced by more than a factor of two on angular scales encompassing the third to fifth acoustic peaks as well as the damping tail of the CMB power spectrum. The calibration uncertainty has been reduced from 6% to 2.1% in temperature through a direct comparison of the CMB anisotropy measured by ACBAR with that of the dipole-calibrated WMAP5 experiment. The measured power spectrum is consistent with a spatially flat, \u039bCDM cosmological model. We include the effects of weak lensing in the power spectrum model computations and find that this significantly improves the fits of the models to the combined ACBAR+WMAP5 power spectrum. The preferred strength of the lensing is consistent with theoretical expectations. On fine angular scales, there is weak evidence (1.1\u03c3) for excess power above the level expected from primary anisotropies. We expect any excess power to be dominated by the combination of emission from dusty protogalaxies and the Sunyaev-Zel'dovich effect (SZE). However, the excess observed by ACBAR is significantly smaller than the excess power at \u2113 > 2000 reported by the CBI experiment operating at 30 GHz. Therefore, while it is unlikely that the CBI excess has a primordial origin; the combined ACBAR and CBI results are consistent with the source of the CBI excess being either the SZE or radio source contamination.", "date": "2009-04-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "694", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1200-1219", "id_number": "CaltechAUTHORS:20090831-110123089", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-110123089", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "OPP-8920223" }, { "agency": "NSF", "grant_number": "OPP-0091840" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC03-76SF00098" }, { "agency": "NASA Postdoctoral Fellowship" }, { "agency": "NASA Fermi Fellowship" }, { "agency": "NSF Graduate Research Fellowship" } ] }, "doi": "10.1088/0004-637X/694/2/1200", "primary_object": { "basename": "Reichardt2009p1366Astrophys_J.pdf", "url": "https://authors.library.caltech.edu/records/zyed2-2t624/files/Reichardt2009p1366Astrophys_J.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Reichardt, C. L.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/scehr-qvk60", "eprint_id": 15497, "eprint_status": "archive", "datestamp": "2023-08-21 20:50:49", "lastmod": "2023-10-19 14:30:45", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Hinderks-J-R", "name": { "family": "Hinderks", "given": "J. R." } }, { "id": "Ade-P", "name": { "family": "Ade", "given": "P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Brown-M-L", "name": { "family": "Brown", "given": "M. L." } }, { "id": "Cahill-G", "name": { "family": "Cahill", "given": "G." } }, { "id": "Carlstrom-J-E", "name": { "family": "Carlstrom", "given": "J. E." }, "orcid": "0000-0002-2044-7665" }, { "id": "Castro-P-G", "name": { "family": "Castro", "given": "P. G." } }, { "id": "Church-S", "name": { "family": "Church", "given": "S." } }, { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Friedman-R", "name": { "family": "Friedman", "given": "R." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Gupta-S", "name": { "family": "Gupta", "given": "S." } }, { "id": "Harris-J", "name": { "family": "Harris", "given": "J." } }, { "id": "Haynes-V", "name": { "family": "Haynes", "given": "V." } }, { "id": "Keating-B-G", "name": { "family": "Keating", "given": "B. G." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Kirby-E-N", "name": { "family": "Kirby", "given": "E." }, "orcid": "0000-0001-6196-5162" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Mallie-O-E", "name": { "family": "Mallie", "given": "O. E." } }, { "id": "Melhuish-S", "name": { "family": "Melhuish", "given": "S." } }, { "id": "Memari-Y", "name": { "family": "Memari", "given": "Y." } }, { "id": "Murphy-A", "name": { "family": "Murphy", "given": "A." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Schwarz-R", "name": { "family": "Schwarz", "given": "R." } }, { "id": "O'Sullivan-C", "name": { "family": "O'Sullivan", "given": "C." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Rajguru-N", "name": { "family": "Rajguru", "given": "N." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Tucker-C", "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-A-H", "name": { "family": "Turner", "given": "A. H." } }, { "id": "Wu-E-Y-S", "name": { "family": "Wu", "given": "E. Y. S." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "QUaD: A High-Resolution Cosmic Microwave Background Polarimeter", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; instrumentation: polarimeters", "note": "\u00a9 2009 The American Astronomical Society. Received 2008 May 14; accepted 2008 October 2; published 2009 February 24. We acknowledge the staff of the Amundsen-Scott South Pole\nStation and all involved in the United States Antarctic Program\nfor their superb support during the construction and operation\nof this experiment. Special thanks go to our brave winter-over\nscientist Robert Schwarzwho has spent three consecutivewinter\nseasons with the QUaD. We also acknowledge the tremendous\nefforts of the Stanford University Physics Department machine\nshop in the construction of the focal plane assembly. J.R.H.\nthanks David Chuss for useful comments on this draft and\nSimon Radford for providing the 350 \u03bcm tipper data. QUaD is\nfunded by the National Science Foundation in the USA, through\ngrants AST-0096778,ANT-0338138,ANT-0338335, and ANT-\n0338238, by the UK Science and technology Facilities Council\n(STFC) and its predecessor the Particle Physics and Astronomy Research Council (PPARC), and by the Science Foundation\nIreland.\nJ.R.H. acknowledges the support of an NSF Graduate Research\nFellowship, a Stanford Graduate Fellowship, and a\nNASA Postdoctoral Fellowship. M.L.B. and A.O. acknowledge\nthe award of PPARC fellowships. P.G.C. is funded by\nthe Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia. S.E.C. acknowledges\nsupport from a Stanford Terman Fellowship. J.M.K.\nacknowledges support from a John B. and Nelly L. Kilroy\nFoundation Fellowship. C.P. and J.E.C. acknowledge partial\nsupport from the Kavli Institute for Cosmological Physics\nthrough the grant NSF PHY-0114422. E.Y.W. acknowledges\nreceipt of an NDSEG fellowship. M.Z. acknowledges the support\nof a NASA Postdoctoral Fellowship. This research was\nsupported in part by appointments to the NASA Postdoctoral\nProgram at the Goddard Space Flight Center (J.R.H.) and the\nJet Propulsion Laboratory (M.Z.), administered by Oak Ridge\nAssociated Universities through a contract with NASA.\n\nPublished - Hinderks2009p66310.10880004-637X69221221.pdf
", "abstract": "We describe the QUaD experiment, a millimeter-wavelength polarimeter designed to observe the cosmic microwave background (CMB) from a site at the South Pole. The experiment comprises a 2.64 m Cassegrain telescope equipped with a cryogenically cooled receiver containing an array of 62 polarization-sensitive bolometers. The focal plane contains pixels at two different frequency bands, 100 GHz and 150 GHz, with angular resolutions of 5' and 35, respectively. The high angular resolution allows observation of CMB temperature and polarization anisotropies over a wide range of scales. The instrument commenced operation in early 2005 and collected science data during three successive Austral winter seasons of observation.", "date": "2009-02-24", "date_type": "published", "publication": "Astrophysical Journal", "volume": "692", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1221-1246", "id_number": "CaltechAUTHORS:20090831-141710879", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-141710879", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0096778" }, { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Science Foundation Ireland" }, { "agency": "NSF Graduate Research Fellowship" }, { "agency": "Stanford Graduate Fellowship" }, { "agency": "NASA Postdoctoral Fellowship" }, { "agency": "Funda\u00e7\u00e3o para a Ci\u00eancia e a Tecnologia" }, { "agency": "Stanford Terman Fellowship" }, { "agency": "John B. and Nelly L. Kilroy Foundation" }, { "agency": "NSF", "grant_number": "PHY-0114422" }, { "agency": "Kavli Institute for Cosmological Physics" } ] }, "doi": "10.1088/0004-637X/692/2/1221", "primary_object": { "basename": "Hinderks2009p66310.10880004-637X69221221.pdf", "url": "https://authors.library.caltech.edu/records/scehr-qvk60/files/Hinderks2009p66310.10880004-637X69221221.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Hinderks, J. R.; Ade, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/zynqx-y1196", "eprint_id": 16041, "eprint_status": "archive", "datestamp": "2023-08-21 20:50:28", "lastmod": "2023-10-19 21:54:22", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Ade-P", "name": { "family": "Ade", "given": "P." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Brown-M-L", "name": { "family": "Brown", "given": "M. L." } }, { "id": "Cahill-G", "name": { "family": "Cahill", "given": "G." } }, { "id": "Castro-P-G", "name": { "family": "Castro", "given": "P. G." } }, { "id": "Church-S", "name": { "family": "Church", "given": "S." } }, { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Friedman-R", "name": { "family": "Friedman", "given": "R." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Gupta-S", "name": { "family": "Gupta", "given": "S." } }, { "id": "Hinderks-J", "name": { "family": "Hinderks", "given": "J." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E", "name": { "family": "Leitch", "given": "E." } }, { "id": "Melhuish-S-J", "name": { "family": "Melhuish", "given": "S. J." } }, { "id": "Memari-Y", "name": { "family": "Memari", "given": "Y." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Schwarz-R", "name": { "family": "Schwarz", "given": "R." } }, { "id": "\u00d3-Sullivan-C", "name": { "family": "\u00d3 Sullivan", "given": "C." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Rajguru-N", "name": { "family": "Rajguru", "given": "N." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Turner-A-H", "name": { "family": "Turner", "given": "A. H." } }, { "id": "Wu-E-Y-S", "name": { "family": "Wu", "given": "E. Y. S." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "Second and Third Season QUaD Cosmic Microwave Background Temperature and Polarization Power Spectra", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmology: observations; polarization", "note": "\u00a9 2009 The American Astronomical Society. Received 2008 May 14; accepted 2008 October 2; published 2009 February 24.\nQUaD is funded by the National Science Foundation in\nthe USA, through grants AST-0096778, ANT-0338138, ANT-\n0338335, and ANT-0338238, by the Particle Physics and\nAstronomy Research Council in the UK, and by the Science\nFoundation Ireland. We would like to thank the staff of the\nAmundsen\u2013Scott South Pole Station and all involved in the\nUnited States Antarctic Program for the superb support operation\nwhich makes the science presented here possible. Special\nthanks go to our intrepid winter over scientist Robert\nSchwarz who spent three consecutive winter seasons tending\nthe QUaD experiment. The BOOMERanG Collaboration kindly\nallowed the use of their CMB maps for our calibration purposes.\nM.L.B. acknowledges the award of a PPARC fellowship.\nS.E.C. acknowledges support from a Stanford Terman Fellowship.\nJ.R.H. acknowledges the support of an NSF Graduate Research\nFellowship and a Stanford Graduate Fellowship. C.P. and\nJ.E.C. acknowledge partial support from the Kavli Institute for\nCosmological Physics through the grant NSF PHY-0114422.\nE.Y.W. acknowledges receipt of an NDSEG fellowship. J.M.K\nacknowledges support from a John B. and Nelly L. Kilroy Foundation\nFellowship.\n\nPublished - Pryke2009p66210.10880004-637X69221247.pdf
", "abstract": "We report results from the second and third seasons of observation with the QUaD experiment. Angular power spectra of the cosmic microwave background are derived for both temperature and polarization at both 100 GHz and 150 GHz, and as cross-frequency spectra. All spectra are subjected to an extensive set of jackknife tests to probe for possible systematic contamination. For the implemented data cuts and processing technique such contamination is undetectable. We analyze the difference map formed between the 100 and 150 GHz bands and find no evidence of foreground contamination in polarization. The spectra are then combined to form a single set of results which are shown to be consistent with the prevailing LCDM model. The sensitivity of the polarization results is considerably better than that of any previous experiment\u2014for the first time multiple acoustic peaks are detected in the E-mode power spectrum at high significance.", "date": "2009-02-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "692", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1247-1270", "id_number": "CaltechAUTHORS:20090924-141617154", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090924-141617154", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0096778" }, { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Particle Physics and Astronomy Research Council" }, { "agency": "Science Foundation Ireland" }, { "agency": "Department of Defense" }, { "agency": "Stanford University" }, { "agency": "NSF", "grant_number": "PHY-0114422" }, { "agency": "John B. and Nelly L. Kilroy Foundation" } ] }, "corp_creators": { "items": [ "QUaD Collaboration" ] }, "doi": "10.1088/0004-637X/692/2/1247", "primary_object": { "basename": "Pryke2009p66210.10880004-637X69221247.pdf", "url": "https://authors.library.caltech.edu/records/zynqx-y1196/files/Pryke2009p66210.10880004-637X69221247.pdf" }, "resource_type": "article", "pub_year": "2009", "author_list": "Pryke, C.; Ade, P.; et el." }, { "id": "https://authors.library.caltech.edu/records/9y6zr-qw224", "eprint_id": 12824, "eprint_status": "archive", "datestamp": "2023-08-22 14:12:07", "lastmod": "2024-02-26 17:27:53", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "name": { "family": "Sayers", "given": "J." } }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Rossinot-P", "name": { "family": "Rossinot", "given": "P." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Aguirre-J-E", "name": { "family": "Aguirre", "given": "J. E." }, "orcid": "0000-0002-4810-666X" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Edgington-S-F", "name": { "family": "Edgington", "given": "S. F." } }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Goldin-A-L", "name": { "family": "Goldin", "given": "A." } }, { "id": "Haig-D", "name": { "family": "Haig", "given": "D." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Laurent-G-T", "name": { "family": "Laurent", "given": "G. T." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Nguyen-Hien-Trong", "name": { "family": "Nguyen", "given": "H. T." } } ] }, "title": "A Search for Cosmic Microwave Background Anisotropies on Arcminute Scales with Bolocam", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmological parameters; cosmology: observations; methods: data analysis; large-scale structure of universe", "note": "\u00a9 2009. The American Astronomical Society. \n\nReceived 2008 May 20; accepted 2008 September 14; published 2008 December 22. Print publication: Issue 2 (2009 January 10). \n\nWe acknowledge the assistance of Minhee Yun and Anthony D. Turner of NASA's Jet Propulsion Laboratory, who fabricated the Bolocam science array; Toshiro Hatake of the JPL electronic packaging group, who wire-bonded the array; Marty Gould of Zen Machine and Ricardo Paniagua and the Caltech PMA/GPS Instrument Shop, who fabricated much of the Bolocam hardware; Carole Tucker of Cardiff University, who tested metal-mesh reflective filters used in Bolocam; Ben Knowles of the University of Colorado, who contributed to the software pipeline, the day crew and Hilo staff of the Caltech Submillimeter Observatory, who provided invaluable assistance during commissioning and data-taking for this survey data set; and Kathy Deniston, who provided effective administrative support at Caltech. Bolocam was constructed and commissioned using funds from NSF/AST-9618798, NSF/AST-0098737, NSF/AST-9980846, NSF/AST-0229008, and NSF/AST-0206158. J.S. and G.L. were partially supported by NASA Graduate Student Research Fellowships and S.G. was partially supported by an R.A. Millikan Postdoctoral Fellowship at Caltech. \n\n[J.E.A. was a] Jansky Fellow, National Radio Astronomy Observatory. \n\nFacilities: CSO.\n\nErratum: \"A Search for Cosmic Microwave Background Anisotropies on Arcminute Scales With Bolocam\" (2009, ApJ, 690, 1597)\nJ. Sayers, S. R. Golwala, P. Rossinot, P. A. R. Ade, J. E. Aguirre, J. J. Bock, S. F. Edgington, J. Glenn, A. Goldin, D. Haig, A. E. Lange, G. T. Laurent, P. D. Mauskopf, and H. T. Nguyen 2009 ApJ 692 942 doi: 10.1088/0004-637X/692/1/942\n\nPublished - SAYapj09.pdf
Erratum - Sayers2009p15810.10880004-637X6921942.pdf
", "abstract": "We have surveyed two science fields totaling 1 deg2 with Bolocam at 2.1 mm to search for secondary Cosmic Microwave Background (CMB) anisotropies caused by the Sunyaev-Zel'dovich effect (SZE). The fields are in the Lynx and Subaru/XMM SDS1 fields. Our survey is sensitive to angular scales with an effective angular multipole of \u2113eff = 5700 with FWHM\u2113 = 2800 and has an angular resolution of 60 arcsec FWHM. Our data provide no evidence for anisotropy. We are able to constrain the level of total astronomical anisotropy, modeled as a flat-band power in C_\u2113, with most frequent 68%, 90%, and 95% CL upper limits of 590, 760, and 830 μK2CMB. We statistically subtract the known contribution from primary CMB anisotropy, including cosmic variance, to obtain constraints on the SZE anisotropy contribution. Now including flux calibration uncertainty, our most frequent 68%, 90%, and 95% CL upper limits on a flat-band power in C_\u2113 are 690, 960, and 1000 μK2CMB. When we instead employ the analytical spectrum suggested by Komatsu and Seljack in 2002, and account for the non-Gaussianity of the SZE anisotropy signal, we obtain upper limits on the average amplitude of their spectrum weighted by our transfer function of 790, 1060, and 1080 μK2CMB. We obtain a 90% CL upper limit on σ8, which normalizes the power spectrum of density fluctuations, of 1.57. These are the first constraints on anisotropy and σ8 from survey data at these angular scales at frequencies near 150 GHz.
", "date": "2009-01-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "690", "number": "2", "publisher": "American Astronomical Society", "pagerange": "1597-1620", "id_number": "CaltechAUTHORS:SAYapj09", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:SAYapj09", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-9618798" }, { "agency": "NSF", "grant_number": "AST-0098737" }, { "agency": "NSF", "grant_number": "AST-9980846" }, { "agency": "NSF", "grant_number": "AST-0229008" }, { "agency": "NSF", "grant_number": "AST-0206158" }, { "agency": "NASA" }, { "agency": "Caltech Millikan Fellowship" }, { "agency": "National Radio Astronomy Observatory" } ] }, "doi": "10.1088/0004-637X/690/2/1597", "primary_object": { "basename": "SAYapj09.pdf", "url": "https://authors.library.caltech.edu/records/9y6zr-qw224/files/SAYapj09.pdf" }, "related_objects": [ { "basename": "Sayers2009p15810.10880004-637X6921942.pdf", "url": "https://authors.library.caltech.edu/records/9y6zr-qw224/files/Sayers2009p15810.10880004-637X6921942.pdf" } ], "resource_type": "article", "pub_year": "2009", "author_list": "Sayers, J.; Golwala, S. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/xx8ca-ywd87", "eprint_id": 14292, "eprint_status": "archive", "datestamp": "2023-08-22 13:54:25", "lastmod": "2023-10-18 16:27:42", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "MacTavish-C-J", "name": { "family": "MacTavish", "given": "C. J." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Battistelli-E-S", "name": { "family": "Battistelli", "given": "E. S." }, "orcid": "0000-0001-5210-7625" }, { "id": "Benton-S", "name": { "family": "Benton", "given": "S." } }, { "id": "Bihary-R", "name": { "family": "Bihary", "given": "R." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bond-J-R", "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Brevik-J", "name": { "family": "Brevik", "given": "J." } }, { "id": "Bryan-S", "name": { "family": "Bryan", "given": "S." } }, { "id": "Contaldi-C-R", "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Dor\u00e9-O", "name": { "family": "Dor\u00e9", "given": "O." }, "orcid": "0000-0001-7432-2932" }, { "id": "Fissel-Laura-M", "name": { "family": "Fissel", "given": "L." }, "orcid": "0000-0002-3242-8154" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Hilton-G", "name": { "family": "Hilton", "given": "G." } }, { "id": "Holmes-W", "name": { "family": "Holmes", "given": "W." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Irwin-K", "name": { "family": "Irwin", "given": "K." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Kuo-Chia-Lam", "name": { "family": "Kuo", "given": "C. L." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Lawrie-C", "name": { "family": "Lawrie", "given": "C." } }, { "id": "Martin-T-G", "name": { "family": "Martin", "given": "T. G." } }, { "id": "Mason-P", "name": { "family": "Mason", "given": "P." } }, { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T. E." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Riley-D", "name": { "family": "Riley", "given": "D." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Runyan-M", "name": { "family": "Runyan", "given": "M." } }, { "id": "Trangsrud-Amy-R", "name": { "family": "Trangsrud", "given": "A." } }, { "id": "Tucker-C", "name": { "family": "Tucker", "given": "C." } }, { "id": "Turner-A", "name": { "family": "Turner", "given": "A." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M." } }, { "id": "Wiebe-D", "name": { "family": "Wiebe", "given": "D." } } ] }, "title": "Spider optimization: probing the systematics of a large-scale B-mode experiment", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; gravitational waves; methods: data analysis; polarization", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 October 1, accepted for publication 2008 July 28. \n\nThis research used the McKenzie cluster at CITA, funded by the Canada Foundation for Innovation. Some of the results in this paper have been derived using the HEALPix package (Gorski et al. 2005), as well as the FFTW package (Frigo & Johnson 2005). We thank the anonymous referee for helpful comments and corrections.\n\nPublished - MACapj08b.pdf
", "abstract": "Spider is a long-duration, balloon-borne polarimeter designed to measure large-scale cosmic microwave background (CMB) polarization with very high sensitivity and control of systematics. The instrument will map over half the sky with degree angular resolution in the I, Q, and U Stokes parameters in four frequency bands from 96 to 275 GHz. Spider's ultimate goal is to detect the primordial gravity-wave signal imprinted on the CMB B-mode polarization. One of the challenges in achieving this goal is the minimization of the contamination of B-modes by systematic effects. This paper explores a number of instrument systematics and observing strategies in order to optimize B-mode sensitivity. This is done by injecting realistic-amplitude, time-varying systematics into a set of simulated time streams. Tests of the impact of detector noise characteristics, pointing jitter, payload pendulations, polarization angle offsets, beam systematics, and receiver gain drifts are shown. Spider's default observing strategy is to spin continuously in azimuth, with polarization modulation achieved by either a rapidly spinning half-wave plate or a rapidly spinning gondola and a slowly stepped half-wave plate. Although the latter is more susceptible to systematics, the results shown here indicate that either mode of operation can be used by Spider.", "date": "2008-12-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "689", "number": "2", "publisher": "American Astronomical Society", "pagerange": "655-665", "id_number": "CaltechAUTHORS:20090524-204222732", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090524-204222732", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canada Foundation for Innovation" } ] }, "doi": "10.1086/592732", "primary_object": { "basename": "MACapj08b.pdf", "url": "https://authors.library.caltech.edu/records/xx8ca-ywd87/files/MACapj08b.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "MacTavish, C. J.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/6z9x1-c3692", "eprint_id": 100996, "eprint_status": "archive", "datestamp": "2023-08-20 00:08:03", "lastmod": "2023-10-19 22:19:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Perera-T-A", "name": { "family": "Perera", "given": "T. A." } }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "E. L." } }, { "id": "Austermann-J-E", "name": { "family": "Austermann", "given": "J. E." } }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Pope-Alexandra", "name": { "family": "Pope", "given": "A." }, "orcid": "0000-0001-8592-2706" }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" }, { "id": "Lowenthal-J-D", "name": { "family": "Lowenthal", "given": "J. D." } }, { "id": "Morrison-G-E", "name": { "family": "Morrison", "given": "G." } }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "I." }, "orcid": "0000-0002-6590-3994" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Coppin-K-E-K", "name": { "family": "Coppin", "given": "K." } }, { "id": "Crowe-M", "name": { "family": "Crowe", "given": "M." } }, { "id": "Frey-L", "name": { "family": "Frey", "given": "L." } }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Kang-Y", "name": { "family": "Kang", "given": "Y." } }, { "id": "Kim-S", "name": { "family": "Kim", "given": "S." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" } ] }, "title": "An AzTEC 1.1 mm survey of the GOODS-N field \u2013 I. Maps, catalogue and source statistics", "ispublished": "pub", "full_text_status": "public", "keywords": "instrumentation: detectors, galaxies: high redshift, galaxies: starburst, submillimetre", "note": "\u00a9 2008 The Authors. Journal compilation \u00a9 2008 RAS. \n\nAccepted 2008 September 1. Received 2008 September 1; in original form 2008 April 17. Published: 27 November 2008. \n\nThe authors are grateful to J. Aguirre, J. Karakla, K. Souccar, I. Coulson, R. Tilanus, R. Kackley, D. Haig, S. Doyle, and the observatory staff at the JCMT who made these observations possible. Support for this work was provided, in part, by the NSF grant AST 05-40852 and the grant from the Korea Science & Engineering Foundation (KOSEF) under a cooperative Astrophysical Research Center of the Structure and Evolution of the Cosmos (ARCSEC). DHH and IA acknowledge partial support by CONACT from research grants 60878 and 50786. AP acknowledges support provided by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. KC acknowledges support from the Science and Technology Facilities Council. DS and MH acknowledge support from the Natural Sciences and Engineering Research Council of Canada.\n\nPublished - mnras391-1227.pdf
Submitted - 0806.3791.pdf
", "abstract": "We have conducted a deep and uniform 1.1 mm survey of the Great Observatories Origins Deep Survey-North (GOODS-N) field with AzTEC on the James Clerk Maxwell Telescope. Here, we present the first results from this survey including maps, the source catalogue and 1.1 mm number counts. The results presented here were obtained from a 245 arcmin\u00b2 region with a near uniform coverage to a depth of 0.96\u20131.16 mJy beam\u207b\u00b9. Our robust catalogue contains 28 source candidates detected with S/N \u2265 3.75, only \u223c1\u2013 2 of which are expected to be spurious detections. Of these source candidates, eight are also detected by Submillimetre Common-User Bolometer Array (SCUBA) at 850 \u03bcm in regions where there is a good overlap between the two surveys. The major advantage of our survey over that with SCUBA is the uniformity of coverage. We calculate number counts using two different techniques: the first using a frequentist parameter estimation and the second using a Bayesian method. The two sets of results are in good agreement. We find that the 1.1 mm differential number counts are well described in the 2\u20136 mJy range by the functional form dN/dS=N\u2032(S\u2032/S) exp(\u2212S/S\u2032) with fitted parameters S\u2032= 1.25 \u00b1 0.38 mJy and dN/dS= 300 \u00b1 90 mJy\u207b\u00b9deg\u207b\u00b2 at 3 mJy.", "date": "2008-12", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "391", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "1227-1238", "id_number": "CaltechAUTHORS:20200130-074148107", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200130-074148107", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 05-40852" }, { "agency": "Korea Science and Engineering Foundation (KOSEF)" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "60878" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "50786" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2008.13902.x", "primary_object": { "basename": "0806.3791.pdf", "url": "https://authors.library.caltech.edu/records/6z9x1-c3692/files/0806.3791.pdf" }, "related_objects": [ { "basename": "mnras391-1227.pdf", "url": "https://authors.library.caltech.edu/records/6z9x1-c3692/files/mnras391-1227.pdf" } ], "resource_type": "article", "pub_year": "2008", "author_list": "Perera, T. A.; Chapin, E. L.; et el." }, { "id": "https://authors.library.caltech.edu/records/r6fmg-dwf28", "eprint_id": 12874, "eprint_status": "archive", "datestamp": "2023-08-19 23:55:02", "lastmod": "2023-10-17 21:12:44", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Holmes-W-A", "name": { "family": "Holmes", "given": "Warren A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "Brendan P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Koch-T-C", "name": { "family": "Koch", "given": "Timothy C." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "William C." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." } }, { "id": "Paine-C-G", "name": { "family": "Paine", "given": "Christopher G." } } ] }, "title": "Initial test results on bolometers for the Planck high frequency instrument", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2008 Optical Society of America. \n\nReceived 6 June 2008; accepted 11 August 2008; posted 10 October 2008 (Doc. ID 97085); published 4 November 2008. \n\nThis work was performed for the Jet Propulsion Laboratory, California Institute of Technology, sponsored by the National Aeronautics and Space Administration (NASA). We acknowledge all staff at JPL who have contributed to this effort, particularly Jerry Mulder, Debi Romero, Minhee Yun, and Anarosa Villanueva for their key contributions. We also thank our collaborators at UCW, LERMA, College de France and IAS, Orsay, Paris.\n\nPublished - HOLao08.pdf
", "abstract": "We summarize the fabrication, flight qualification, and dark performance of bolometers completed at the Jet Propulsion Laboratory for the High Frequency Instrument (HFI) of the joint ESA/NASA Herschel/Planck mission to be launched in 2009. The HFI is a multicolor focal plane which consists of 52 bolometers operated at 100 mK. Each bolometer is mounted to a feedhorn-filter assembly which defines one of six frequency bands centered between 100-857 GHz. Four detectors in each of five bands from 143-857 GHz are coupled to both linear polarizations and thus measure the total intensity. In addition, eight detectors in each of four bands (100, 143, 217, and 353 GHz) couple only to a single linear polarization and thus provide measurements of the Stokes parameters, Q and U, as well as the total intensity. The measured noise equivalent power (NEP) of all detectors is at or below the background limit for the telescope and time constants are a few ms, short enough to resolve point sources as the 5 to 9 arc min beams move across the sky at 1 rpm.", "date": "2008-11-10", "date_type": "published", "publication": "Applied Optics", "volume": "47", "number": "32", "publisher": "Optical Society of America", "pagerange": "5996-6008", "id_number": "CaltechAUTHORS:HOLao08", "issn": "0003-6935", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:HOLao08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA" } ] }, "doi": "10.1364/AO.47.005996", "primary_object": { "basename": "HOLao08.pdf", "url": "https://authors.library.caltech.edu/records/r6fmg-dwf28/files/HOLao08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Holmes, Warren A.; Bock, James J.; et el." }, { "id": "https://authors.library.caltech.edu/records/jrj46-11v83", "eprint_id": 14245, "eprint_status": "archive", "datestamp": "2023-08-22 12:28:23", "lastmod": "2023-10-18 16:26:06", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "G." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "E. L." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "M. J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "S." } }, { "id": "Griffin-M-J", "name": { "family": "Griffin", "given": "M." } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "J. O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "P. C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "J." } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "G." } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "P. G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P." }, "orcid": "0000-0001-6397-5516" }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "L." }, "orcid": "0000-0002-1162-7947" }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Rex-M", "name": { "family": "Rex", "given": "M." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "C." } }, { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "M. D. P." } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "C." } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "G. S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "D. V." } } ] }, "title": "SANEPIC: a mapmaking method for time stream data from large arrays", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; methods: data analysis; submillimeter; techniques: image processing", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 May 29; accepted 2007 November 27. \n\nThe BLAST collaboration acknowledges the support of NASA through grants NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space Agency (CSA), Canada's Natural Sciences and Engineering Research Council (NSERC), and the UK Particle Physics and Astronomy Research Council (PPARC). We would also like to thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work. We are grateful to Matthew Hasselfield and DuncanHanson for valuable discussions that contributed to the development of SANEPIC. L. O. acknowledges partial support by the Puerto Rico Space Grant Consortium and by the Fondo Istitucional para la Investigacion of the University of Puerto Rico. C. B. N. acknowledges support from the Canadian Institute for Advanced Research. This research made use of WestGrid computing resources, which are funded in part by the Canada Foundation for Innovation, Alberta Innovation and Science, BC Advanced Education, and the participating research institutions.\n\nPublished - PATapj08b.pdf
", "abstract": "We describe a mapmaking method that we have developed for the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) experiment, but which should have general application to data from other submillimeter arrays. Our method uses a maximum likelihood-based approach, with several approximations, which allows images to be constructed using large amounts of data with fairly modest computer memory and processing requirements. This new approach, Signal and Noise Estimation Procedure Including Correlations (SANEPIC), builds on several previous methods but focuses specifically on the regime where there are a large number of detectors sampling the same map of the sky, and explicitly allowing for the possibility of strong correlations between the detector time streams. We provide real and simulated examples of how well this method performs compared with more simplistic mapmakers based on filtering. We discuss two separate implementations of SANEPIC: a brute-force approach, in which the inverse pixel-pixel covariance matrix is computed, and an iterative approach, which is much more efficient for large maps. SANEPIC has been successfully used to produce maps using data from the 2005 BLAST flight.", "date": "2008-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "681", "number": "1", "publisher": "American Astronomical Society", "pagerange": "708-725", "id_number": "CaltechAUTHORS:20090517-205138563", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090517-205138563", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6G111G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Puerto Rico Space Grant Consortium" }, { "agency": "University of Puerto Rico" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Innovation Alberta" }, { "agency": "British Columbia Ministry of Advanced Education" } ] }, "doi": "10.1086/588543", "primary_object": { "basename": "PATapj08b.pdf", "url": "https://authors.library.caltech.edu/records/jrj46-11v83/files/PATapj08b.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Patanchon, G.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/4yx1j-rfr69", "eprint_id": 14413, "eprint_status": "archive", "datestamp": "2023-08-22 12:28:43", "lastmod": "2023-10-18 16:50:34", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "E. L." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Brunt-C", "name": { "family": "Brunt", "given": "C." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "M. J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "S." } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "M." } }, { "id": "Gunderson-J-O", "name": { "family": "Gunderson", "given": "J. O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "P. C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "J." } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "G." } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "P. G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "L." }, "orcid": "0000-0002-1162-7947" }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "G." } }, { "id": "Rex-M", "name": { "family": "Rex", "given": "M." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "C." } }, { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "M. D. P." } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "C." } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "G. S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "D. V." } } ] }, "title": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 4 deg2 Galactic Plane Survey in Vulpecula (ell = 59\u00b0)", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; ISM: clouds; stars: formation; submillimeter", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 May 29, accepted for publication 2007 October 26. \n\nThe BLAST collaboration acknowledges the support of NASA through grants NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space Agency (CSA), the UK Particle Physics and Astronomy Research Council (PPARC), the Canada Foundation for Innovation (CFI), the Ontario Innovation Trust (OIT), and Canada's Natural Sciences and Engineering Research Council (NSERC).We would also like to thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work. We thank Andy Gibb for helpful discussions. We also thank the anonymous referee for useful comments. L. O. acknowledges partial support by the Puerto Rico Space Grant Consortium and by the Fondo Institucional para la Investigacion of the University of Puerto Rico, and also thanks students Carlos M. Poventud and Jorge L.Morales for assistance with the analysis. C. B. N. acknowledges support from the Canadian Institute for Advanced Research. D. H. H. acknowledges the support of Consejo Nacional de Cienciay Technolog\u0131a (CONACYt) grant 39953-F. This research has been enabled by the use of WestGrid computing resources.\n\nPublished - CHAapj08c.pdf
", "abstract": "We present the first results from a new 250, 350, and 500 \u03bcm Galactic plane survey taken with the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) in 2005. This survey's primary goal is to identify and characterize high-mass protostellar objects (HMPOs). The region studied here covers 4 deg^2 near the open cluster NGC 6823 in the constellation Vulpecula (\u2113 = 59\u00b0). We find 60 compact sources (<60'' diameter) detected simultaneously in all three bands. Their SEDs are constrained through BLAST, IRAS, Spitzer MIPS, and MSX photometry, with inferred dust temperatures spanning ~12-40 K assuming a dust emissivity index \u03b2 = 1.5. The luminosity-to-mass ratio, a distance-independent quantity, spans ~0.2-130 L_\u2609 M^(\u22121)_\u2609. Distances are estimated from coincident ^(13)CO(1\u2192 0) velocities combined with a variety of other velocity and morphological data in the literature. In total, 49 sources are associated with a molecular cloud complex encompassing NGC 6823 (distance ~2.3 kpc), 10 objects with the Perseus arm (~8.5 kpc), and one object is probably in the outer Galaxy (~14 kpc). Near NGC 6823, the inferred luminosities and masses of BLAST sources span ~40-10^4 L_\u2609 and ~15-700 M_\u2609, respectively. The mass spectrum is compatible with molecular gas masses in other high-mass star-forming regions. Several luminous sources appear to be ultracompact H II regions powered by early B stars. However, many of the objects are cool, massive gravitationally bound clumps with no obvious internal radiation from a protostar, and hence excellent HMPO candidates.", "date": "2008-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "681", "number": "1", "publisher": "American Astronomical Society", "pagerange": "428-452", "id_number": "CaltechAUTHORS:20090618-202204043", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090618-202204043", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6GI11G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Ontario Innovation Trust" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Puerto Rico Space Grant Consortium" }, { "agency": "University of Puerto Rico" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACYT)", "grant_number": "39953-F" } ] }, "doi": "10.1086/588544", "primary_object": { "basename": "CHAapj08c.pdf", "url": "https://authors.library.caltech.edu/records/4yx1j-rfr69/files/CHAapj08c.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Chapin, E. L.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/ezapb-gvz38", "eprint_id": 14225, "eprint_status": "archive", "datestamp": "2023-08-22 12:28:18", "lastmod": "2023-10-18 16:24:04", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "M. D. P." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "E. L." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "M. J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "S." } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "M." } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "J. O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "P. C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "J." } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "G." } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "P. G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P." }, "orcid": "0000-0001-6397-5516" }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "L." }, "orcid": "0000-0002-1162-7947" }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "G." } }, { "id": "Rex-M", "name": { "family": "Rex", "given": "M." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "C." } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "C. E." } }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "D. V." } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "G. S." }, "orcid": "0000-0002-6954-6947" } ] }, "title": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: calibration and targeted sources", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; submillimeter; telescopes", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 May 29, accepted for publication 2008 February 28. \n\nThe BLAST collaboration acknowledges the support of NASA through grants NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space Agency (CSA), Canada's Natural Sciences and Engineering Research Council (NSERC), and the UK Particle Physics and Astronomy Research Council (PPARC). We would also like to thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work, as well as T. G. Muller for valuable discussions on Pallas. L. O. acknowledges partial support by the Puerto Rico Space Grant Consortium and by the Fondo Istitucional para la Investigacion of the University of Puerto Rico. C.B.N. acknowledges support from the Canadian Institute for Advanced Research. This research has been enabled by the use of WestGrid computing resources. This research also made use of the SIMBAD database, operated at the Centre de Don\u00e9es astronomiques de Strasbourg (CDS), Strasbourg, France, and the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - TRUapj08.pdf
", "abstract": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) operated successfully during a 100 hr flight from northern Sweden in 2005 June (BLAST05). As part of the calibration and pointing procedures, several compact sources were mapped, including solar system, Galactic, and extragalactic targets, specifically Pallas, CRL 2688, LDN 1014, IRAS 20126+4104, IRAS 21078+5211, IRAS 21307+5049, IRAS 22134+5834, IRAS 23011+6126, K3-50, W75N, and Mrk 231. One additional source, Arp 220, was observed and used as our primary calibrator. Details of the overall BLAST05 calibration procedure are discussed here. The BLAST observations of each compact source are described, flux densities and spectral energy distributions are reported, and these are compared with previous measurements at other wavelengths. The 250, 350, and 500 \u03bcm BLAST data can provide useful constraints to the amplitude and slope of the submillimeter continuum, which in turn may be useful for the improved calibration of other submillimeter instruments.", "date": "2008-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "681", "number": "1", "publisher": "American Astronomical Society", "pagerange": "415-427", "id_number": "CaltechAUTHORS:20090514-172906404", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090514-172906404", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6G111G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Particle Physics and Astronomy Research Council" }, { "agency": "Puerto Rico Space Grant Consortium" }, { "agency": "University of Puerto Rico" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" } ] }, "doi": "10.1086/588542", "primary_object": { "basename": "TRUapj08.pdf", "url": "https://authors.library.caltech.edu/records/ezapb-gvz38/files/TRUapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Truch, M. D. P.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/19gys-4eh43", "eprint_id": 14246, "eprint_status": "archive", "datestamp": "2023-08-22 12:28:28", "lastmod": "2023-10-18 16:26:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Chapin-E-L", "name": { "family": "Chapin", "given": "E. L." } }, { "id": "Chung-J", "name": { "family": "Chung", "given": "J." } }, { "id": "Devlin-M-J", "name": { "family": "Devlin", "given": "M. J." } }, { "id": "Dicker-S-R", "name": { "family": "Dicker", "given": "S." } }, { "id": "Griffin-M", "name": { "family": "Griffin", "given": "M." } }, { "id": "Gundersen-J-O", "name": { "family": "Gundersen", "given": "J. O." } }, { "id": "Halpern-M", "name": { "family": "Halpern", "given": "M." }, "orcid": "0000-0002-1760-0868" }, { "id": "Hargrave-P-C", "name": { "family": "Hargrave", "given": "P. C." }, "orcid": "0000-0002-3109-6629" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Klein-J", "name": { "family": "Klein", "given": "J." } }, { "id": "MacTavish-C-J", "name": { "family": "MacTavish", "given": "C. J." } }, { "id": "Marsden-Gaelen", "name": { "family": "Marsden", "given": "G." } }, { "id": "Martin-P-G", "name": { "family": "Martin", "given": "P. G." }, "orcid": "0000-0002-5236-3896" }, { "id": "Martin-T-G", "name": { "family": "Martin", "given": "T. G." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P." }, "orcid": "0000-0001-6397-5516" }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Olmi-L", "name": { "family": "Olmi", "given": "L." }, "orcid": "0000-0002-1162-7947" }, { "id": "Patanchon-G", "name": { "family": "Patanchon", "given": "G." } }, { "id": "Rex-M", "name": { "family": "Rex", "given": "M." } }, { "id": "Scott-Douglas", "name": { "family": "Scott", "given": "D." }, "orcid": "0000-0002-6878-9840" }, { "id": "Semisch-C", "name": { "family": "Semisch", "given": "C." } }, { "id": "Thomas-Nicholas-E", "name": { "family": "Thomas", "given": "N." } }, { "id": "Truch-M-D-P", "name": { "family": "Truch", "given": "M. D. P." } }, { "id": "Tucker-C-E", "name": { "family": "Tucker", "given": "C." } }, { "id": "Tucker-G-S", "name": { "family": "Tucker", "given": "G. S." }, "orcid": "0000-0002-6954-6947" }, { "id": "Viero-M-P", "name": { "family": "Viero", "given": "M. P." } }, { "id": "Wiebe-D-V", "name": { "family": "Wiebe", "given": "D. V." } } ] }, "title": "The Balloon-borne Large Aperture Submillimeter Telescope: BLAST", "ispublished": "pub", "full_text_status": "public", "keywords": "balloons; galaxies: evolution; instrumentation: miscellaneous; stars: formation; submillimeter", "note": "\u00a9 2008 The American Astronomical Society. \n\nReceived 2007 May 29; accepted 2008 March 20. \n\nThe BLAST collaboration acknowledges the support of NASA through grants NAG5-12785, NAG5-13301, and NNGO-6GI11G, the Canadian Space Agency (CSA), the Science and Technology Facilities Council (STFC), Canada's Natural Sciences and Engineering Research Council (NSERC), the Canada Foundation for Innovation, the Ontario Innovation Trust, the Puerto Rico Space Grant Consortium, the Fondo Istitucional para la Investigacion of the University of Puerto Rico, and the National Science Foundation Office of Polar Programs; C. B. N. also acknowledges support from the Canadian Institute for Advanced Research. L. O. would like to acknowledge Pietro Bolli for his help with physical optics simulations during the testing phase of the BLAST06 telescope. We would also like to thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work, the Precision Machining Group at Lawrence Livermore Laboratory, the support received from Empire Dynamic Structures in the design and construction of the gondola, Daniele Mortari for helpful discussions in the development of the Pyramid code, Dan Swetz for building the Fourier transform spectrometer, and Luke Bruneaux, Kyle Lepage, Danica Marsden, Vjera Miovic, and James Watt for their contribution to the project.\n\nPublished - PASapj08.pdf
", "abstract": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) is a suborbital surveying experiment designed to study the evolutionary history and processes of star formation in local galaxies (including the Milky Way) and galaxies at cosmological distances. The BLAST continuum camera, which consists of 270 detectors distributed between three arrays, observes simultaneously in broadband (30%) spectral windows at 250, 350, and 500 \u03bcm. The optical design is based on a 2 m diameter telescope, providing a diffraction-limited resolution of 30'' at 250 \u03bcm. The gondola pointing system enables raster mapping of arbitrary geometry, with a repeatable positional accuracy of ~30''; postflight pointing reconstruction to \u227e5'' rms is achieved. The onboard telescope control software permits autonomous execution of a preselected set of maps, with the option of manual override. In this paper we describe the primary characteristics and measured in-flight performance of BLAST. BLAST performed a test flight in 2003 and has since made two scientifically productive long-duration balloon flights: a 100 hr flight from ESRANGE (Kiruna), Sweden to Victoria Island, northern Canada in 2005 June; and a 250 hr, circumpolar flight from McMurdo Station, Antarctica, in 2006 December.", "date": "2008-07-01", "date_type": "published", "publication": "Astrophysical Journal", "volume": "681", "number": "1", "publisher": "University of Chicago Press", "pagerange": "400-414", "id_number": "CaltechAUTHORS:20090517-211252065", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090517-211252065", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-12785" }, { "agency": "NASA", "grant_number": "NAG5-13301" }, { "agency": "NASA", "grant_number": "NNGO-6G111G" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Science and Technology Facilities Council (STFC)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Canada Foundation for Innovation" }, { "agency": "Ontario Innovation Trust" }, { "agency": "Puerto Rico Space Grant Consortium" }, { "agency": "University of Puerto Rico" }, { "agency": "NSF" }, { "agency": "Canadian Institute for Advanced Research (CIFAR)" } ] }, "doi": "10.1086/588541", "primary_object": { "basename": "PASapj08.pdf", "url": "https://authors.library.caltech.edu/records/19gys-4eh43/files/PASapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Pascale, E.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/p79xp-2e929", "eprint_id": 14060, "eprint_status": "archive", "datestamp": "2023-08-22 11:45:32", "lastmod": "2023-10-18 16:05:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } }, { "id": "Austermann-J-E", "name": { "family": "Austermann", "given": "J. E." } }, { "id": "Perera-T-A", "name": { "family": "Perera", "given": "T. A." } }, { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Glenn-J", "name": { "family": "Glenn", "given": "J." }, "orcid": "0000-0001-7527-2017" }, { "id": "Golwala-S-R", "name": { "family": "Golwala", "given": "S. R." }, "orcid": "0000-0002-1098-7174" }, { "id": "Kim-S", "name": { "family": "Kim", "given": "S." } }, { "id": "Kang-Y", "name": { "family": "Kang", "given": "Y." } }, { "id": "Lydon-D", "name": { "family": "Lydon", "given": "D." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Predmore-C-R", "name": { "family": "Predmore", "given": "C. R." } }, { "id": "Roberts-C-M", "name": { "family": "Roberts", "given": "C. M." } }, { "id": "Souccar-K", "name": { "family": "Souccar", "given": "K." } }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" } ] }, "title": "The AzTEC mm-wavelength camera", "ispublished": "pub", "full_text_status": "public", "keywords": "instrumentation: detectors; galaxies: high redshift; galaxies :starburst; submillimetre", "note": "\u00a92008 The Authors. Journal compilation \u00a92008 RAS. \n\nAccepted 2008 January 16. Received 2007 December 21; in original form 2007 October 29. \n\nWe acknowledge the following people for their various and valuable contributions to the success of the AzTEC instrument and/or AzTEC observations: Itziar Aretxaga, Cara Battersby,Yuxi Chen, Iain Coulson, Gary Davis, Simon Doyle, Daniel Ferrusca, Douglas Haig, Salman Hameed, David Hughes, John Karakla, James Lowenthal, GaryWallace and Miguel Valazquez. SK and YK were supported in part by Korea Science & Engineering Foundation (KOSEF) under a cooperative agreement with the Astrophysical Research Centre of the Structure and Evolution of the Cosmos (ARCSEC). This work was supported in part by NSF Grant 0540852.\n\nPublished - WILmnras08.pdf
", "abstract": "AzTEC is a mm-wavelength bolometric camera utilizing 144 silicon nitride micromesh detectors. Here, we describe the AzTEC instrument architecture and its use as an astronomical\ninstrument. We report on several performance metrics measured during a three-month observing campaign at the James Clerk Maxwell Telescope and conclude with our plans for AzTEC as a facility instrument on the Large Millimetre Telescope.", "date": "2008-05-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "386", "number": "2", "publisher": "Royal Astronomical Society", "pagerange": "807-818", "id_number": "CaltechAUTHORS:20090423-201108516", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090423-201108516", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Korea Science and Engineering Foundation" }, { "agency": "Astrophysical Research Centre of the Structure and Evolution of the Cosmos (ARCSEC)" }, { "agency": "NSF", "grant_number": "AST-0540852" } ] }, "doi": "10.1111/j.1365-2966.2008.12980.x", "primary_object": { "basename": "WILmnras08.pdf", "url": "https://authors.library.caltech.edu/records/p79xp-2e929/files/WILmnras08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Wilson, G. W.; Austermann, J. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/khfry-9a133", "eprint_id": 14063, "eprint_status": "archive", "datestamp": "2023-08-22 11:35:27", "lastmod": "2023-10-18 16:05:09", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Scott-K-S", "name": { "family": "Scott", "given": "K. S." } }, { "id": "Austermann-J-E", "name": { "family": "Austermann", "given": "J. E." } }, { "id": "Perera-T-A", "name": { "family": "Perera", "given": "T. A." } }, { "id": "Wilson-G-W", "name": { "family": "Wilson", "given": "G. W." } }, { "id": "Aretxaga-I", "name": { "family": "Aretxaga", "given": "I." }, "orcid": "0000-0002-6590-3994" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Hughes-D-H", "name": { "family": "Hughes", "given": "D. H." } }, { "id": "Kang-Y", "name": { "family": "Kang", "given": "Y." } }, { "id": "Kim-S", "name": { "family": "Kim", "given": "S." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Sanders-D-B", "name": { "family": "Sanders", "given": "D. B." }, "orcid": "0000-0002-1233-9998" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N." }, "orcid": "0000-0002-0438-3323" }, { "id": "Yun-Min-S", "name": { "family": "Yun", "given": "M. S." }, "orcid": "0000-0001-7095-7543" } ] }, "title": "AzTEC millimetre survey of the COSMOS field \u2013 I. data reduction and source catalogue", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxes: high-redshift; galaxies: starburst; submillimetre", "note": "\u00a92008 The Authors. Journal compilation \u00a92008 RAS.\nAccepted 2008 January 17. Received 2008 January 16; in original form 2007 November 16.\nThe authors are grateful to J. Aguirre, J. Karakla, K. Souccar, I. Coulson, R. Tilanus, R. Kackley, D. Haig, S. Doyle, J. Lowenthal and the observatory staff at the JCMT who made these observations possible. Support for this work was provided in part by the NSF grant AST 05-40852 and the grant from the Korea Science & Engineering Foundation (KOSEF) under a cooperative Astrophysical Research Centre of the Structure and Evolution of the Cosmos (ARCSEC). IA and DH acknowledge partial support by CONACyT from research grants 39953-F and 39548-F. This research has made use of the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.\n\nPublished - SCOmnras08.pdf
", "abstract": "We present a 1.1mm wavelength imaging survey covering 0.3 deg^2 in the COSMOS field. These data, obtained with the AzTEC continuum camera on the James Clerk Maxwell Telescope, were centred on a prominent large-scale structure overdensity which includes a rich X-ray cluster at z \u2248 0.73. A total of 50 mm-galaxy candidates, with a significance ranging from 3.5 to 8.5\u03c3, are extracted from the central 0.15 deg^2 area which has a uniform sensitivity of \u223c1.3 mJy beam^\u22121. 16 sources are detected with S/N \u2265 4.5, where the expected false detection rate is zero, of which a surprisingly large number (9) have intrinsic (deboosted) fluxes \u22655 mJy at 1.1 mm. Assuming the emission is dominated by radiation from dust, heated by a massive population of young, optically obscured stars, then these bright AzTEC sources have far-infrared luminosities >6 \u00d7 10^(12)L_\u2609 and star formation rates \u22651100M_\u2609 yr^(\u22121). Two of these nine bright AzTEC sources are found towards the extreme peripheral region of the X-ray cluster, whilst the remainder are distributed across the larger scale overdensity. We describe the AzTEC data reduction pipeline, the source-extraction algorithm, and the characterization of the source catalogue, including the completeness, flux deboosting correction, false-detection rate and the source positional uncertainty, through an extensive set of Monte Carlo simulations. We conclude with a preliminary comparison, via a stacked analysis, of the overlapping MIPS 24-\u03bcm data and radio data with this AzTEC map of the COSMOS field.", "date": "2008-04-21", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "385", "number": "4", "publisher": "Royal Astronomical Society", "pagerange": "2225-2238", "id_number": "CaltechAUTHORS:20090423-212245434", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090423-212245434", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST 05-40852" }, { "agency": "Korea Science & Engineering Foundation (KOSEF)" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "39953-F" }, { "agency": "Consejo Nacional de Ciencia y Tecnolog\u00eda (CONACyT)", "grant_number": "39548-F" } ] }, "local_group": { "items": [ { "id": "COSMOS" }, { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2008.12989.x", "primary_object": { "basename": "SCOmnras08.pdf", "url": "https://authors.library.caltech.edu/records/khfry-9a133/files/SCOmnras08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Scott, K. S.; Austermann, J. E.; et el." }, { "id": "https://authors.library.caltech.edu/records/qxnd5-ztk79", "eprint_id": 12645, "eprint_status": "archive", "datestamp": "2023-08-19 22:09:44", "lastmod": "2023-10-17 20:24:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Brown-M-L", "name": { "family": "Brown", "given": "M. L." } }, { "id": "Cahill-V", "name": { "family": "Cahill", "given": "V." } }, { "id": "Carlstrom-J-E", "name": { "family": "Carlstrom", "given": "J. E." }, "orcid": "0000-0002-2044-7665" }, { "id": "Castro-P-G", "name": { "family": "Castro", "given": "P. G." } }, { "id": "Church-S", "name": { "family": "Church", "given": "S." } }, { "id": "Culverhouse-T", "name": { "family": "Culverhouse", "given": "T." } }, { "id": "Friedman-R", "name": { "family": "Friedman", "given": "R." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Hinderks-J", "name": { "family": "Hinderks", "given": "J." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E-M", "name": { "family": "Leitch", "given": "E. M." } }, { "id": "Melhuish-S-J", "name": { "family": "Melhuish", "given": "S. J." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Orlando-A", "name": { "family": "Orlando", "given": "A." } }, { "id": "Schwarz-R-B", "name": { "family": "Schwarz", "given": "R." } }, { "id": "O'Sullivan-C", "name": { "family": "O'Sullivan", "given": "C." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Rajguru-N", "name": { "family": "Rajguru", "given": "N." } }, { "id": "Rusholme-B", "name": { "family": "Rusholme", "given": "B." }, "orcid": "0000-0001-7648-4142" }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Thompson-K-L", "name": { "family": "Thompson", "given": "K. L." } }, { "id": "Wu-E-Y-S", "name": { "family": "Wu", "given": "E. Y. S." } }, { "id": "Zemcov-M", "name": { "family": "Zemcov", "given": "M." }, "orcid": "0000-0001-8253-1451" } ] }, "title": "First season QUaD CMB temperature and polarization power spectra", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization", "note": "\u00a9 2008 American Astronomical Society. \n\nReceived 2007 May 16; accepted 2007 October 24. \n\nQUaD is funded by the National Science Foundation in the USA, through grants AST-0096778, ANT-0338138, ANT-0338335, and ANT-0338238, by the Particle Physics and Astronomy Research Council in the UK, and by the Science Foundation Ireland. We would like to thank the staff of the Amundsen-Scott South Pole Station and all involved in the United States Antarctic Program for the superb support operation that makes the science presented here possible. Special thanks go to our intrepid winter-over scientist Robert Schwarz, who has spent three consecutive winter seasons tending the QUaD experiment. The BOOMERANG collaboration kindly allowed the use of their CMB maps for our calibration purposes. M.L.B. acknowledges the award of a PPARC fellowship. S.E.C. acknowledges support from a Stanford Terman Fellowship. J.R.H. acknowledges the support of an NSF Graduate Research Fellowship and a Stanford Graduate Fellowship. C.P. and J.E.C. acknowledge partial support from the Kavli Institute for Cosmological Physics through the grant NSF PHY-0114422. E.Y.W. acknowledges receipt of an NDSEG fellowship.\n\nPublished - ADEapj08.pdf
", "abstract": "QUaD is a bolometric CMB polarimeter sited at the South Pole, operating at frequencies of 100 and 150 GHz. In this paper we report preliminary results from the first season of operation (austral winter 2005). All six CMB power spectra are presented derived as cross spectra between the 100 and 150 GHz maps using 67 days of observation in a low foreground region of approximately 60 deg^2. These data are a small fraction of the data acquired to date. The measured spectra are consistent with the \u039bCDM cosmological model. We perform jackknife tests that indicate that the observed signal has negligible contamination from instrumental systematics. In addition, by using a frequency jackknife we find no evidence for foreground contamination.", "date": "2008-02-10", "date_type": "published", "publication": "Astrophysical Journal", "volume": "674", "number": "1", "publisher": "American Astronomical Society", "pagerange": "22-28", "id_number": "CaltechAUTHORS:ADEapj08", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:ADEapj08", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-0096778" }, { "agency": "NSF", "grant_number": "ANT-0338138" }, { "agency": "NSF", "grant_number": "ANT-0338335" }, { "agency": "NSF", "grant_number": "ANT-0338238" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Science Foundation, Ireland" }, { "agency": "Stanford University" }, { "agency": "Kavli Institute for Cosmological Physics" }, { "agency": "NSF", "grant_number": "PHY-0114422" }, { "agency": "National Defense Science and Engineering Graduate (NDSEG) Fellowship" } ] }, "doi": "10.1086/524922", "primary_object": { "basename": "ADEapj08.pdf", "url": "https://authors.library.caltech.edu/records/qxnd5-ztk79/files/ADEapj08.pdf" }, "resource_type": "article", "pub_year": "2008", "author_list": "Ade, P.; Bock, J.; et el." }, { "id": "https://authors.library.caltech.edu/records/etqdy-8y960", "eprint_id": 16858, "eprint_status": "archive", "datestamp": "2023-08-19 21:37:18", "lastmod": "2023-10-19 22:36:50", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "De-Troia-G", "name": { "family": "De Troia", "given": "G." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bond-J-R", "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Borrill-J", "name": { "family": "Borrill", "given": "J." } }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Cabella-P", "name": { "family": "Cabella", "given": "P." } }, { "id": "Contaldi-C-R", "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "De-Gasperis-G", "name": { "family": "De Gasperis", "given": "G." } }, { "id": "de-Oliveira-Costa-A", "name": { "family": "de Oliveira-Costa", "given": "A." } }, { "id": "Di-Stefano-G", "name": { "family": "Di Stefano", "given": "G." } }, { "id": "Ferreira-P-G", "name": { "family": "Ferreira", "given": "P. G." } }, { "id": "Hivon-E", "name": { "family": "Hivon", "given": "E." } }, { "id": "Jaffe-A-H", "name": { "family": "Jaffe", "given": "A. H." } }, { "id": "Kisner-T-S", "name": { "family": "Kisner", "given": "T. S." } }, { "id": "Kinz-M", "name": { "family": "Kunz", "given": "M." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Liguori-M", "name": { "family": "Liguori", "given": "M." } }, { "id": "Masi-S", "name": { "family": "Masi", "given": "S." }, "orcid": "0000-0001-5105-1439" }, { "id": "Matarrese-S", "name": { "family": "Matarrese", "given": "S." } }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "MacTavish-C-J", "name": { "family": "MacTavish", "given": "C. J." } }, { "id": "Melchiorri-A", "name": { "family": "Melchiorri", "given": "A." } }, { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T. E." } }, { "id": "Natoli-P", "name": { "family": "Natoli", "given": "P." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Piacentini-F", "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "id": "Pogosyan-D", "name": { "family": "Pogosyan", "given": "D." } }, { "id": "Polenta-G", "name": { "family": "Polenta", "given": "G." } }, { "id": "Prunet-S", "name": { "family": "Prunet", "given": "S." } }, { "id": "Ricciardi-S", "name": { "family": "Ricciardi", "given": "S." } }, { "id": "Romeo-G", "name": { "family": "Romeo", "given": "G." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Santini-P", "name": { "family": "Santini", "given": "P." } }, { "id": "Tegmark-M", "name": { "family": "Tegmark", "given": "M." } }, { "id": "Veneziani-M", "name": { "family": "Veneziani", "given": "M." } }, { "id": "Vittorio-N", "name": { "family": "Vittorio", "given": "N." } } ] }, "title": "Searching for Non-Gaussian Signals in the BOOMERANG 2003 CMB Maps", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background", "note": "\u00a9 2007 American Astronomical Society.\n\nPrint publication: Issue 2 (2007 December 1); received 2007 May 11; accepted for publication 2007 October 15; published 2007 October 29.\n\nBOOMERANG was supported by CIAR, CSA, and NERSC\nin Canada, ASI, University La Sapienza and PNRA in Italy,\nand NASA and NSF in the US. We thank CASPUR and\nNERSC/LBL. We acknowledge the use of HEALPix.\n\nPublished - TROapjl07.pdf
", "abstract": "We analyze the BOOMERANG 2003 (B03) 145 GHz temperature map to constrain the amplitude of a non-Gaussian, primordial contribution to CMB fluctuations. We perform a pixel-space analysis restricted to a portion of the map chosen in view of high-sensitivity, very low foreground contamination and tight control of systematic effects. We set up an estimator based on the three Minkowski functionals which relies on high-quality simulated data, including non-Gaussian CMB maps. We find good agreement with the Gaussian hypothesis and derive the first limits based on BOOMERANG data for the nonlinear coupling parameter f_(NL) as -300 < f_(NL) < 650 at 68% CL and -800 < f_(NL) < 1050 at 95% CL.", "date": "2007-12-01", "date_type": "published", "publication": "Astrophysical Journal Letters", "volume": "670", "number": "2", "publisher": "American Astronomical Society", "pagerange": "L73-L76", "id_number": "CaltechAUTHORS:20091202-122207165", "issn": "2041-8205", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091202-122207165", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NERSC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "University La Sapienza" }, { "agency": "Programma Nazionale Ricerche in Antartide (PNRA)" }, { "agency": "NASA" }, { "agency": "NSF" } ] }, "doi": "10.1086/524402", "primary_object": { "basename": "TROapjl07.pdf", "url": "https://authors.library.caltech.edu/records/etqdy-8y960/files/TROapjl07.pdf" }, "resource_type": "article", "pub_year": "2007", "author_list": "De Troia, G.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/natpy-dv072", "eprint_id": 12808, "eprint_status": "archive", "datestamp": "2023-08-22 06:21:50", "lastmod": "2023-10-17 20:56:10", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bond-J-R", "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Borrill-J", "name": { "family": "Borrill", "given": "J." } }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Cabella-P", "name": { "family": "Cabella", "given": "P." } }, { "id": "Contaldi-C-R", "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "De-Gasperis-G", "name": { "family": "De Gasperis", "given": "G." } }, { "id": "de-Oliveira-Costa-A", "name": { "family": "de Oliveira-Costa", "given": "A." } }, { "id": "De-Troia-G", "name": { "family": "De Troia", "given": "G." } }, { "id": "di-Stefano-G", "name": { "family": "di Stefano", "given": "G." } }, { "id": "Hivon-E", "name": { "family": "Hivon", "given": "E." } }, { "id": "Jaffe-A-H", "name": { "family": "Jaffe", "given": "A. H." } }, { "id": "Kisner-T-S", "name": { "family": "Kisner", "given": "T. S." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "MacTavish-C-J", "name": { "family": "MacTavish", "given": "C. J." } }, { "id": "Masi-S", "name": { "family": "Masi", "given": "S." }, "orcid": "0000-0001-5105-1439" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Melchiorri-A", "name": { "family": "Melchiorri", "given": "A." } }, { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T. E." } }, { "id": "Natoli-P", "name": { "family": "Natoli", "given": "P." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Piacentini-F", "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "id": "Pogosyan-D", "name": { "family": "Pogosyan", "given": "D." } }, { "id": "Polenta-G", "name": { "family": "Polenta", "given": "G." } }, { "id": "Prunet-S", "name": { "family": "Prunet", "given": "S." } }, { "id": "Ricciardi-S", "name": { "family": "Ricciardi", "given": "S." } }, { "id": "Romeo-G", "name": { "family": "Romeo", "given": "G." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Santini-P", "name": { "family": "Santini", "given": "P." } }, { "id": "Tegmark-M", "name": { "family": "Tegmark", "given": "M." } }, { "id": "Veneziani-M", "name": { "family": "Veneziani", "given": "M." } }, { "id": "Vittorio-N", "name": { "family": "Vittorio", "given": "N." } } ] }, "title": "A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background; cosmology: observations; instrumentation: detectors", "note": "Copyright is not claimed for this article. Printed in U.S.A. \n\nReceived 2005 July 21; accepted 2006 April 28. Print publication: Issue 2 (2006 August 20). \n\nWe gratefully acknowledge support from the CIAR, CSA, and NSERC in Canada, ASI, University La Sapienza, and PNRA in Italy, PPARC and the Leverhulme Trust in the UK, and NASA (awards NAG5-9251 and NAG5-12723) and NSF (awards OPP 99-80654 and OPP 04-07592) in the US. Additional support for detector development was provided by CIT and the Jet Propulsion Laboratory (JPL). C.B.N. acknowledges support from a Sloan Foundation Fellowship; W.C.J. and T.E.M. were partially supported by NASA GSRP Fellowships. Field, logistical, and flight support were supplied by USAP and NSBF; data recovery was particularly appreciated. This research used resources at NERSC, supported by the DOE under contract DE-AC03-76SF00098, and the MacKenzie cluster at CITA, funded by the Canada Foundation for Innovation. We also thank the CASPUR, Rome, computational facilities and the Applied Cluster Computing Technologies Group at JPL for computing time and technical support. Some of the results in this paper have been derived using the HEALPix package (G\u00f3rski et al. 2005), and nearly all have benefitted from the FFTW implementation of discrete Fourier transforms (Frigo & Johnson 2005). Finally, we would like to thank the referee for making significant contributions to the quality of this paper.\n\nPublished - JONapj06.pdf
", "abstract": "We report on observations of the cosmic microwave background (CMB) obtained during the 2003 January flight of BOOMERANG. These results are derived from 195 hr of observation with four 145 GHz polarization-sensitive bolometer (PSB) pairs, identical in design to the four 143 GHz Planck High Frequency Instrument (HFI) polarized pixels. The data include 75 hr of observations distributed over 1.84% of the sky with an additional 120 hr concentrated on the central portion of the field, which represents 0.22% of the full sky. From these data we derive an estimate of the angular power spectrum of temperature fluctuations of the CMB in 24 bands over the multipole range 50 \u2264 l \u2264 1500. A series of features, consistent with those expected from acoustic oscillations in the primordial photon-baryon fluid, are clearly evident in the power spectrum, as is the exponential damping of power on scales smaller than the photon mean free path at the epoch of last scattering (l \u2273 900). As a consistency check, the collaboration has performed two fully independent analyses of the time-ordered data, which are found to be in excellent agreement.", "date": "2006-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "647", "number": "2", "publisher": "American Astronomical Society", "pagerange": "823-832", "id_number": "CaltechAUTHORS:JONapj06", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:JONapj06", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERCC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "University La Sapienza" }, { "agency": "Programma Nazionale di Ricerche in Antartide (PNRA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Leverhulme Trust" }, { "agency": "NASA", "grant_number": "NAG5-9251" }, { "agency": "NASA", "grant_number": "NAG5-12723" }, { "agency": "NSF", "grant_number": "OPP 99-80654" }, { "agency": "NSF", "grant_number": "OPP 04-07592" }, { "agency": "NASA/JPL/Caltech" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "Department of Energy (DOE)", "grant_number": "DE-AC03-76SF00098" }, { "agency": "Canada Foundation for Innovation" } ] }, "doi": "10.1086/505559", "primary_object": { "basename": "JONapj06.pdf", "url": "https://authors.library.caltech.edu/records/natpy-dv072/files/JONapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Jones, W. C.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/4m1yp-yj755", "eprint_id": 24258, "eprint_status": "archive", "datestamp": "2023-08-22 06:22:22", "lastmod": "2023-10-23 20:25:39", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T. E." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "Hivon-E", "name": { "family": "Hivon", "given": "E." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } } ] }, "title": "A Measurement of the CMBPublished - MONapj06b.pdf
", "abstract": "We report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R.A. = 82\u00b0.5, decl. = -45\u00b0. The observations were made using four pairs of polarization-sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a nonzero signal in the range 201 < l < 1000 with a significance of 4.8 \u03c3, a 2 \u03c3 upper limit of 8.6 \u03bcK^2 for any contribution, and a 2 \u03c3 upper limit of 7.0 \u03bcK^2 for the spectrum. Estimates of foreground intensity fluctuations and the nondetection of and signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a \u039bCDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors.", "date": "2006-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "647", "number": "2", "publisher": "American Astronomical Society", "pagerange": "813-822", "id_number": "CaltechAUTHORS:20110629-150937119", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110629-150937119", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Institute for Advanced Research (CIAR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council of Canada (NSERC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "University La Sapienza" }, { "agency": "PNRA (Italy)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Leverhulme Trust (United Kingdom)" }, { "agency": "NASA", "grant_number": "NAG5-9251" }, { "agency": "NASA", "grant_number": "NAG5-12723" }, { "agency": "NSF", "grant_number": "OPP 99-80654" }, { "agency": "NSF", "grant_number": "OPP 04-07592" }, { "agency": "Caltech" }, { "agency": "JPL" }, { "agency": "Sloan Foundation Fellowship" }, { "agency": "NASA GSRP Fellowships" }, { "agency": "USAP" }, { "agency": "NSBF" } ] }, "doi": "10.1086/505560", "primary_object": { "basename": "MONapj06b.pdf", "url": "https://authors.library.caltech.edu/records/4m1yp-yj755/files/MONapj06b.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Montroy, T. E.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/xmx8s-16493", "eprint_id": 18851, "eprint_status": "archive", "datestamp": "2023-08-19 18:27:25", "lastmod": "2023-10-20 19:07:19", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Piacentini-F", "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bond-J-R", "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Borrill-J", "name": { "family": "Borrill", "given": "J." } }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Cabella-P", "name": { "family": "Cabella", "given": "P." } }, { "id": "Contaldi-C-R", "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "De-Gasperis-G", "name": { "family": "De Gasperis", "given": "G." } }, { "id": "de-Oliveira-Costa-A", "name": { "family": "de Oliveira-Costa", "given": "A." } }, { "id": "De-Troia-G", "name": { "family": "De Troia", "given": "G." } }, { "id": "di-Stefano-G", "name": { "family": "di Stefano", "given": "G." } }, { "id": "Hivon-E", "name": { "family": "Hivon", "given": "E." } }, { "id": "Jaffe-A-H", "name": { "family": "Jaffe", "given": "A. H." } }, { "id": "Kisner-T-S", "name": { "family": "Kisner", "given": "T. S." } }, { "id": "Jones-W-C", "name": { "family": "Jones", "given": "W. C." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Masi-S", "name": { "family": "Masi", "given": "S." }, "orcid": "0000-0001-5105-1439" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "MacTavish-C-J", "name": { "family": "MacTavish", "given": "C. J." } }, { "id": "Melchiorri-A", "name": { "family": "Melchiorri", "given": "A." } }, { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T. E." } }, { "id": "Natoli-P", "name": { "family": "Natoli", "given": "P." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Pogosyan-D", "name": { "family": "Pogosyan", "given": "D." } }, { "id": "Polenta-G", "name": { "family": "Polenta", "given": "G." } }, { "id": "Prunet-S", "name": { "family": "Prunet", "given": "S." } }, { "id": "Ricciardi-S", "name": { "family": "Ricciardi", "given": "S." } }, { "id": "Romeo-G", "name": { "family": "Romeo", "given": "G." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } }, { "id": "Santini-P", "name": { "family": "Santini", "given": "P." } }, { "id": "Tegmark-M", "name": { "family": "Tegmark", "given": "M." } }, { "id": "Veneziani-M", "name": { "family": "Veneziani", "given": "M." } }, { "id": "Vittorio-N", "name": { "family": "Vittorio", "given": "N." } } ] }, "title": "A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background", "note": "\u00a9 2006 American Astronomical Society.\n\nReceived 2005 July 21; accepted 2006 February 10.\n\nWe gratefully acknowledge support from CIAR, CSA, and\nNSERC in Canada, ASI, University La Sapienza and PNRA in\nItaly, PPARC and the Leverhulme Trust in the UK, and NASA\n(awards NAG5-9251 and NAG5-12723) and NSF (awards OPP\n99-80654 and OPP 04-07592) in the US. Additional support for\ndetector development was provided by CITand the Jet Propulsion\nLaboratory (JPL). C. B. N. acknowledges support from a Sloan\nFoundation Fellowship; W. C. J. and T. E. M. were partially\nsupported by NASA GSRP Fellowships. Field, logistical, and\nflight support was outstandingly supplied by USAP and NSBF;\ndata recovery was especially appreciated. This research used resources\nat NERSC, supported by the DOE under contract DEAC03-\n76SF00098, and the MacKenzie cluster at CITA, funded\nby the Canada Foundation for Innovation. We also thank the\nCASPUR (Rome, Italy) computational facilities and the Applied\nCluster Computing Technologies Group at the JPL for computing\ntime and technical support. Some of the results in this paper\nhave been derived using the HEALPix (Go\u00b4rski et al. 2005) package,\nand nearly all have benefited from the FFTW3 implementation\nof fast Fourier transform (Frigo & Johnson 2005). We\nacknowledge the referee for useful comments. The BOOMERANG\nfield team is also grateful to the Coffee House at McMurdo\nStation, Antarctica, for existing.\n\nPublished - PIAapj06.pdf
", "abstract": "We present a measurement of the polarization-temperature angular cross power spectra, and , of the cosmic microwave background. The result is based on ~200 hr of data from eight polarization-sensitive bolometers operating at 145 GHz during the 2003 flight of BOOMERANG. We detect a significant TE correlation in the l-range between 50 and 950 with a statistical significance of >3.5 \u03c3. Contamination by polarized foreground emission and systematic effects are negligible in comparison with statistical uncertainties. The spectrum is consistent with previous detections and with the \"concordance model\" that assumes adiabatic initial conditions. This is the first measurement of polarization-temperature angular cross-power spectra using bolometric detectors.", "date": "2006-08-20", "date_type": "published", "publication": "Astrophysical Journal", "volume": "647", "number": "2", "publisher": "American Astronomical Society", "pagerange": "833-839", "id_number": "CaltechAUTHORS:20100629-095444366", "issn": "0004-637X", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100629-095444366", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Canadian Institute for Advanced Research (CIFAR)" }, { "agency": "Canadian Space Agency (CSA)" }, { "agency": "Natural Sciences and Engineering Research Council (NSERC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "University La Sapienza" }, { "agency": "Programma Nazionale Ricerche in Antartide (PNRA)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "Leverhulme Trust" }, { "agency": "NASA", "grant_number": "NAG5-9251" }, { "agency": "NASA", "grant_number": "NAG5-12723" }, { "agency": "NSF", "grant_number": "OPP 99-80654" }, { "agency": "NSF", "grant_number": "OPP 04-07592" }, { "agency": "Alfred P. Sloan Foundation" }, { "agency": "NASA Graduate Student Research Fellowship" } ] }, "doi": "10.1086/505557", "primary_object": { "basename": "PIAapj06.pdf", "url": "https://authors.library.caltech.edu/records/xmx8s-16493/files/PIAapj06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Piacentini, F.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/tyxew-qea43", "eprint_id": 24568, "eprint_status": "archive", "datestamp": "2023-08-19 18:08:20", "lastmod": "2023-10-23 23:28:24", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Rabii-B", "name": { "family": "Rabii", "given": "B." } }, { "id": "Winant-C-D", "name": { "family": "Winant", "given": "C. D." } }, { "id": "Collins-J-S", "name": { "family": "Collins", "given": "J. S." } }, { "id": "Lee-Adrian-T", "name": { "family": "Lee", "given": "A. T." } }, { "id": "Richards-P-L", "name": { "family": "Richards", "given": "P. L." } }, { "id": "Abroe-M-E", "name": { "family": "Abroe", "given": "M. E." } }, { "id": "Hanany-S", "name": { "family": "Hanany", "given": "S." } }, { "id": "Johnson-B-R", "name": { "family": "Johnson", "given": "B. R." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P." }, "orcid": "0000-0002-5127-0401" }, { "id": "Balbi-A", "name": { "family": "Balbi", "given": "A." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Borrill-J", "name": { "family": "Borrill", "given": "J." } }, { "id": "Stompor-R", "name": { "family": "Stompor", "given": "R." } }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "Ferreira-P-G", "name": { "family": "Ferreira", "given": "P. G." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Jaffe-A-H", "name": { "family": "Jaffe", "given": "A. H." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Smoot-George-F", "name": { "family": "Smoot", "given": "G. F." } }, { "id": "Wu-J-H-P", "name": { "family": "Wu", "given": "J. H. P." } } ] }, "title": "MAXIMA: A balloon-borne cosmic microwave background anisotropy experiment", "ispublished": "pub", "full_text_status": "public", "keywords": "radiofrequency cosmic radiation, astronomical instruments, imaging, bolometers", "note": "\u00a9 2006 American Institute of Physics. Received 3 March 2004; accepted 3 June 2006; published online 21 July 2006. Two of the authors J.H.P.W. and A.H.J. acknowledge\nsupport from NASA LTSA Grant No. NAG5-6552 and NSF\nKDI Grant No. 9872979. Another author P.G.F. acknowledges\nsupport from the RS. Two of the authors B.R. and\nC.D.W. acknowledge support from NASA GSRP Grant Nos.\nS00-GSRP-032 and S00-GSRP-031. Two of the authors\nM.E.A. and R.S. acknowledge support from NASA Grant\nNo. NRA-00-01-AISR-004. MAXIMA is supported by\nNASA Grant Nos. NAG5-3941 and NAG5-4454 and by the\nNSF through the Center for Particle Astrophysics at UC Berkeley,\nNSF Cooperative Agreement No. AST-9120005. Computing\nresources were provided by the National Energy Research\nScientific Computing Center, which is supported by\nthe Office of Science of the U.S. Department of Energy under\nContract No. DE-AC03-76SF00098, and by the University\nof Minnesota Supercomputing Institute in Minneapolis,\nMinnesota. MAXIMA field and flight support was provided\nby the National Scientific Balloon Facility. The MAXIMA\nteam would like to thank P. Timbie for the use a Gunn oscillator\nand P. Mauskopf for providing electronic readout units.\nThe authors also thank S. Young for his help in preparing\nfigures for this manuscript.\n\nPublished - RABrsi06.pdf
", "abstract": "We describe the Millimeter wave Anisotropy eXperiment IMaging Array (MAXIMA), a balloon-borne experiment which measured the temperature anisotropy of the cosmic microwave background (CMB) on angular scales of 10\u2032 to 5\u00b0. MAXIMA mapped the CMB using 16 bolometric detectors in spectral bands centered at 150, 240, and 410\u2004GHz, with 10\u2032 resolution at all frequencies. The combined receiver sensitivity to CMB anisotropy was ~40\u2004\u03bcK \u221as. The bolometric detectors, which were cooled to 100\u2004mK, were a prototype of the detectors which will be used on the Planck Surveyor Satellite of the European Space Agency. Systematic parasitic contributions were controlled by using four uncorrelated spatial modulations, thorough cross-linking, multiple independent CMB observations, heavily baffled optics, and strong spectral discrimination. Pointing reconstruction was accurate to 1\u2032, and absolute calibration was better than 4%. Two MAXIMA flights with more than 8.5\u2004h of CMB observations have mapped a total of 300\u2004deg^2 of the sky in regions of negligible known foreground emission. MAXIMA results have been released in previous publications and shown to be consistent with the Wilkinson Microwave Anisotropy Probe. MAXIMA I maps, power spectra, and correlation matrices are publicly available at http://cosmology.berkeley.edu/maxima.", "date": "2006-07", "date_type": "published", "publication": "Review of Scientific Instruments", "volume": "77", "number": "7", "publisher": "American Institute of Physics", "pagerange": "Art. No. 071101", "id_number": "CaltechAUTHORS:20110727-112202154", "issn": "0034-6748", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110727-112202154", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NAG5-6552" }, { "agency": "NSF", "grant_number": "KDI-9872979" }, { "agency": "RS" }, { "agency": "NASA", "grant_number": "S00-GSRP-032" }, { "agency": "NASA", "grant_number": "S00-GSRP-031" }, { "agency": "NASA", "grant_number": "NRA-00-01-AISR-004" }, { "agency": "NASA", "grant_number": "NAG5-3941" }, { "agency": "NASA", "grant_number": "NAG5-4454" }, { "agency": "NSF", "grant_number": "AST-9120005" }, { "agency": "Department of Energy (DOE)", "grant_number": "DEAC03-76SF00098" }, { "agency": "University of Minnesota Supercomputing Institute" }, { "agency": "National Scientific Balloon Facility" } ] }, "doi": "10.1063/1.2219723", "primary_object": { "basename": "RABrsi06.pdf", "url": "https://authors.library.caltech.edu/records/tyxew-qea43/files/RABrsi06.pdf" }, "resource_type": "article", "pub_year": "2006", "author_list": "Rabii, B.; Winant, C. D.; et el." }, { "id": "https://authors.library.caltech.edu/records/tjs1w-t4x15", "eprint_id": 21838, "eprint_status": "archive", "datestamp": "2023-08-22 05:14:03", "lastmod": "2023-10-23 15:25:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James" }, "orcid": "0000-0002-5710-5212" }, { "id": "Battle-J", "name": { "family": "Battle", "given": "John" } }, { "id": "Cooray-A", "name": { "family": "Cooray", "given": "Asantha" }, "orcid": "0000-0002-3892-0190" }, { "id": "Kawada-Misunobu", "name": { "family": "Kawada", "given": "Misunobu" } }, { "id": "Keating-B", "name": { "family": "Keating", "given": "Brian" } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew" } }, { "id": "Lee-Dae-Hea", "name": { "family": "Lee", "given": "Dae-Hea" } }, { "id": "Matsumoto-Toshio", "name": { "family": "Matsumoto", "given": "Toshio" }, "orcid": "0000-0001-6066-5221" }, { "id": "Matsuura-Shuji", "name": { "family": "Matsuura", "given": "Shuji" }, "orcid": "0000-0002-5698-9634" }, { "id": "Pak-Soojong", "name": { "family": "Pak", "given": "Soojong" } }, { "id": "Renbarger-T", "name": { "family": "Renbarger", "given": "Tom" } }, { "id": "Sullivan-I", "name": { "family": "Sullivan", "given": "Ian" } }, { "id": "Tsumura-Kohji", "name": { "family": "Tsumura", "given": "Kohji" } }, { "id": "Wada-Takehiko", "name": { "family": "Wada", "given": "Takehiko" } }, { "id": "Watabe-Toyoki", "name": { "family": "Watabe", "given": "Toyoki" } } ] }, "title": "The cosmic infrared background experiment", "ispublished": "pub", "full_text_status": "restricted", "keywords": "Extragalactic background; Primordial galaxies; Infrared", "note": "\u00a9 2005 Published by Elsevier B.V. Available online 3 February 2006. The authors wish to acknowledge the support of NASA\nGrant NNG05WC18G.", "abstract": "The extragalactic background, based on absolute measurements reported by DIRBE and IRTS at 1.2 and 2.2 \u00b5m, exceeds the brightness\nderived from galaxy counts by up to a factor 5. Furthermore, both DIRBE and the IRTS report fluctuations in the near-infrared sky\nbrightness that appear to have an extra-galactic origin, but are larger than expected from local (z = 1\u20133) galaxies. These observations\nhave led to speculation that a new class of high-mass stars or mini-quasars may dominate primordial star formation at high-redshift\n(z ~ 10\u201320), which, in order to explain the excess in the near-infrared background, must be highly luminous but produce a limited\namount of metals and X-ray photons. Regardless of the nature of the sources, if a significant component of the near-infrared background\ncomes from first-light galaxies, theoretical models generically predict a prominent near-infrared spectral feature from the redshifted\nLyman cutoff, and a distinctive fluctuation power spectrum.\nWe are developing a rocket-borne instrument (the Cosmic Infrared Background ExpeRiment, or CIBER) to search for signatures of\nprimordial galaxy formation in the cosmic near-infrared extra-galactic background. CIBER consists of a wide-field two-color camera, a\nlow-resolution absolute spectrometer, and a high-resolution narrow-band imaging spectrometer.\nThe cameras will search for spatial fluctuations in the background on angular scales from 7\" to 2\u00b0, where a first-light galaxy signature\nis expected to peak, over a range of angular scales poorly covered by previous experiments. CIBER will determine if the fluctuations\nreported by the IRTS arise from first-light galaxies or have a local origin. In a short rocket flight CIBER has sensitivity to probe fluctuations\n100x fainter than IRTS/DIRBE, with sufficient resolution to remove local-galaxy correlations. By jointly observing regions of\nthe sky studied by Spitzer and ASTRO-F, CIBER will build a multi-color view of the near-infrared background, accurately assessing the\ncontribution of local (z = 1\u20133) galaxies to the observed background fluctuations, allowing a deep and comprehensive survey for first-light\ngalaxy background fluctuations.\nThe low-resolution spectrometer will search for a redshifted Lyman cutoff feature between 0.8 and 2.0 \u00b5m. The high-resolution\nspectrometer will trace zodiacal light using the intensity of scattered Fraunhofer lines, providing an independent measurement of the\nzodiacal emission and a new check of DIRBE zodiacal dust models. The combination will systematically search for the infrared\nexcess background light reported in near-infrared DIRBE/IRTS data, compared with the small excess reported at optical\nwavelengths.", "date": "2006-03", "date_type": "published", "publication": "New Astronomy Reviews", "volume": "50", "number": "1-3", "publisher": "Elsevier", "pagerange": "215-220", "id_number": "CaltechAUTHORS:20110120-144321793", "issn": "1387-6473", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110120-144321793", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA", "grant_number": "NNG05WC18G" } ] }, "local_group": { "items": [ { "id": "TAPIR" } ] }, "doi": "10.1016/j.newar.2005.11.034", "resource_type": "article", "pub_year": "2006", "author_list": "Bock, James; Battle, John; et el." }, { "id": "https://authors.library.caltech.edu/records/v4wa5-25m84", "eprint_id": 100998, "eprint_status": "archive", "datestamp": "2023-08-19 13:12:27", "lastmod": "2023-10-19 22:19:29", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bowden-M", "name": { "family": "Bowden", "given": "M." } }, { "id": "Taylor-A-N", "name": { "family": "Taylor", "given": "A. N." } }, { "id": "Ganga-K-M", "name": { "family": "Ganga", "given": "K. M." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Cahill-G", "name": { "family": "Cahill", "given": "G." } }, { "id": "Carlstrom-J-E", "name": { "family": "Carlstrom", "given": "J. E." }, "orcid": "0000-0002-2044-7665" }, { "id": "Church-S-E", "name": { "family": "Church", "given": "S. E." } }, { "id": "Gear-W-K", "name": { "family": "Gear", "given": "W. K." } }, { "id": "Hinderks-J-R", "name": { "family": "Hinderks", "given": "J. R." } }, { "id": "Hu-W", "name": { "family": "Hu", "given": "W." } }, { "id": "Keating-B-G", "name": { "family": "Keating", "given": "B. G." } }, { "id": "Kovac-J", "name": { "family": "Kovac", "given": "J." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Leitch-E-M", "name": { "family": "Leitch", "given": "E. M." } }, { "id": "Maffei-B", "name": { "family": "Maffei", "given": "B." } }, { "id": "Mallie-O-E", "name": { "family": "Mallie", "given": "O. E." } }, { "id": "Melhuish-S-J", "name": { "family": "Melhuish", "given": "S. J." } }, { "id": "Murphy-J-A", "name": { "family": "Murphy", "given": "J. A." } }, { "id": "Pisano-G", "name": { "family": "Pisano", "given": "G." } }, { "id": "Piccirillo-L", "name": { "family": "Piccirillo", "given": "L." } }, { "id": "Pryke-C", "name": { "family": "Pryke", "given": "C." } }, { "id": "Rusholme-B-A", "name": { "family": "Rusholme", "given": "B. A." } }, { "id": "O'Sullivan-C", "name": { "family": "O'Sullivan", "given": "C." } }, { "id": "Thompson-K", "name": { "family": "Thompson", "given": "K." } } ] }, "title": "Scientific optimization of a ground-based CMB polarization experiment", "ispublished": "pub", "full_text_status": "public", "keywords": "polarization \u2013 methods: observational \u2013 techniques: polarimetric \u2013 cosmic microwave background \u2013 cosmological parameters", "note": "\u00a9 2004 RAS. \n\nAccepted 2003 December 3. Received 2003 December 1; in original form 2003 August 26. Published: 21 March 2004. \n\nMB would like to acknowledge a departmental grant from the University of Wales, Cardiff. ANT thanks the PPARC for an Advanced Research Fellowship. The US contribution to this work is supported by the National Science Foundation under grants 9987360 and 0096778.\n\nPublished - 349-1-321.pdf
Accepted Version - 0309610.pdf
", "abstract": "We investigate the science goals achievable with the upcoming generation of ground-based cosmic microwave background polarization experiments, focusing on one particular experiment, QUaD [QUEST (Q and U Extragalactic Submillimetre Telescope) and DASI (Degree Angular Scale Interferometer)], a proposed bolometric polarimeter operating from the South Pole. We calculate the optimal sky coverage for this experiment, including the effects of foregrounds and gravitational lensing. We find that an E-mode measurement will be sample-limited, whereas a B-mode measurement will be detector-noise-limited. We conclude that a 300 deg\u00b2 survey is an optimal compromise for a 2-yr experiment to measure both E and B modes, and that a ground-based polarization experiment can make an important contribution to B-mode surveys. QUaD can make a high significance measurement of the acoustic peaks in the E-mode spectrum, over a multipole range of 25 < \u2113 < 2500, and will be able to detect the gravitational lensing signal in the B-mode spectrum. Such an experiment could also directly detect the gravitational wave component of the B-mode spectrum if the amplitude of the signal is close to current upper limits. We also investigate how QUaD can improve constraints on the cosmological parameters. We estimate that combining two years of QUaD data with the 4-yr Wilkinson Microwave Anisotropy Probe (WMAP) data can improve constraints on \u03a9_bh\u00b2, \u03a9_mh\u00b2, h, r and n_s by a factor of 2. If the foreground contamination can be reduced, the measurement of r can be improved by up to a factor of 6 over that obtainable from WMAP alone. These improved accuracies will place strong constraints on the potential of the inflaton field.", "date": "2004-03", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "349", "number": "1", "publisher": "Oxford University Press", "pagerange": "321-335", "id_number": "CaltechAUTHORS:20200130-075505900", "issn": "1365-2966", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200130-075505900", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "University of Wales" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "NSF", "grant_number": "AST-9987360" }, { "agency": "NSF", "grant_number": "AST-0096778" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1111/j.1365-2966.2004.07506.x", "primary_object": { "basename": "0309610.pdf", "url": "https://authors.library.caltech.edu/records/v4wa5-25m84/files/0309610.pdf" }, "related_objects": [ { "basename": "349-1-321.pdf", "url": "https://authors.library.caltech.edu/records/v4wa5-25m84/files/349-1-321.pdf" } ], "resource_type": "article", "pub_year": "2004", "author_list": "Bowden, M.; Taylor, A. N.; et el." }, { "id": "https://authors.library.caltech.edu/records/0m8p5-wqy33", "eprint_id": 1846, "eprint_status": "archive", "datestamp": "2023-08-22 01:23:04", "lastmod": "2023-10-13 23:02:36", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Yun-Minhee-H", "name": { "family": "Yun", "given": "Minhee" } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "Jamie" }, "orcid": "0000-0002-5710-5212" }, { "id": "Holmes-W", "name": { "family": "Holmes", "given": "Warren" } }, { "id": "Koch-T", "name": { "family": "Koch", "given": "Tim" } }, { "id": "Mulder-J", "name": { "family": "Mulder", "given": "Jerry" } }, { "id": "Vasquez-R-P", "name": { "family": "Vasquez", "given": "Richard P." } }, { "id": "Wild-L", "name": { "family": "Wild", "given": "Larry" } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew" } } ] }, "title": "Microfabrication of silicon\u2013nitride micromesh bolometric detectors for Planck high frequency instrument", "ispublished": "pub", "full_text_status": "public", "keywords": "bolometers; silicon compounds; radiofrequency cosmic radiation; electromagnetic wave polarisation; heat sinks; specific heat; light absorption; microsensors", "note": "\u00a9 2004 American Vacuum Society. \n\n(Received 11 November 2002; accepted 24 November 2003; published 23 January 2004) \n\nThis research was performed at the Jet Propulsion Laboratory, an operating division of the California Institute of Technology, under a contract with the National Aeronautics and Space Administration. \n\nPresented at the AVS 49th International Symposium, 4\u20138 November 2002, Denver, CO.\n\nPublished - YUNjvstb04.pdf
", "abstract": "The high frequency instrument (HFI) on the National Aeronautics and Space Administration/European Space Agency Planck Surveyor, scheduled for launch in 2007, will map the entire sky in six frequency bands ranging from 100 to 857 GHz to probe cosmic microwave background anisotropy and polarization with angular resolution ranging from 9[prime] to 5[prime]. The HFI focal plane will contain 48 silicon\u2013nitride micromesh bolometers operating from a 100 mK heat sink. Four detectors in each of the six bands will detect unpolarized radiation. An additional four pairs of detectors will provide sensitivity to linear polarization of emissions at 143, 217, and 353 GHz. We have fabricated and developed sensitive Si3N4 micromesh spider-web bolometers for submillimeter observation using microelectromechanical system techniques. The spiderweb architecture in this research provides high infrared absorption with minimal heat capacity and volume.", "date": "2004-01", "date_type": "published", "publication": "Journal of Vacuum Science and Technology B", "volume": "22", "number": "1", "publisher": "American Vacuum Society", "pagerange": "220-225", "id_number": "CaltechAUTHORS:YUNjvstb04", "issn": "1071-1023", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:YUNjvstb04", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NASA/JPL/Caltech" } ] }, "doi": "10.1116/1.1642644", "primary_object": { "basename": "YUNjvstb04.pdf", "url": "https://authors.library.caltech.edu/records/0m8p5-wqy33/files/YUNjvstb04.pdf" }, "resource_type": "article", "pub_year": "2004", "author_list": "Yun, Minhee; Bock, Jamie; et el." }, { "id": "https://authors.library.caltech.edu/records/pw47r-bk102", "eprint_id": 3707, "eprint_status": "archive", "datestamp": "2023-08-22 00:54:36", "lastmod": "2023-10-16 16:07:02", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Woodcraft-A-L", "name": { "family": "Woodcraft", "given": "Adam L." } }, { "id": "Sudiwala-R-V", "name": { "family": "Sudiwala", "given": "Rashmi V." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "Peter A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Griffin-M-J", "name": { "family": "Griffin", "given": "Matthew J." } }, { "id": "Wakui-Elley", "name": { "family": "Wakui", "given": "Elley" } }, { "id": "Bhatia-R-S", "name": { "family": "Bhatia", "given": "Ravinder S." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Turner-A-D", "name": { "family": "Turner", "given": "Anthony D." } }, { "id": "Yun-Minhee-H", "name": { "family": "Yun", "given": "Minhee H." } }, { "id": "Beeman-J-W", "name": { "family": "Beeman", "given": "Jeffrey W." } } ] }, "title": "Predicting the response of a submillimeter bolometer to cosmic rays", "ispublished": "pub", "full_text_status": "public", "keywords": "Noise in imaging systems; Photon statistics; Quantum optics : Fluctuations, relaxations, and noise; Astronomy and astrophysics", "note": "\u00a9 2003 Optical Society of America. \n\nReceived 16 January 2003; revised manuscript received 9 May 2003.\n\nPublished - WOOao03.pdf
", "abstract": "Bolometers designed to detect. submillimeter radiation also respond to cosmic, gamma, and x rays. Because detectors cannot be fully shielded from such energy sources, it is necessary to understand the effect of a photon or cosmic-ray particle being absorbed. The resulting signal (known as a glitch) can then be removed from raw data. We present measurements using an Americium-241 gamma radiation source to irradiate a prototype bolometer for the High Frequency Instrument in the Planck Surveyor satellite. Our measurements showed no variation in response depending on where the radiation was absorbed, demonstrating that the bolometer absorber and thermistor thermalize quickly. The bolometer has previously been fully characterized both electrically and optically. We find that using optically measured time constants underestimates the time taken for the detector to recover from a radiation absorption event. However, a full thermal model for the bolometer, with parameters taken from electrical and optical measurements, provides accurate time constants. Slight deviations from the model were seen at high energies; these can be accounted for by use of an extended model.", "date": "2003-09-01", "date_type": "published", "publication": "Applied Optics", "volume": "42", "number": "25", "publisher": "Optical Society of America", "pagerange": "5009-5016", "id_number": "CaltechAUTHORS:WOOao03", "issn": "0003-6935", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:WOOao03", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "primary_object": { "basename": "WOOao03.pdf", "url": "https://authors.library.caltech.edu/records/pw47r-bk102/files/WOOao03.pdf" }, "resource_type": "article", "pub_year": "2003", "author_list": "Woodcraft, Adam L.; Sudiwala, Rashmi V.; et el." }, { "id": "https://authors.library.caltech.edu/records/0c6c7-x3c03", "eprint_id": 74331, "eprint_status": "archive", "datestamp": "2023-08-22 00:40:55", "lastmod": "2023-10-24 22:31:00", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Marsh-K-A", "name": { "family": "Marsh", "given": "K." }, "orcid": "0000-0003-0107-7803" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "G." } }, { "id": "Matthews-Keith-Astronomy", "name": { "family": "Matthews", "given": "K." } }, { "id": "Egami-Eichi", "name": { "family": "Egami", "given": "E." } }, { "id": "Armus-L", "name": { "family": "Armus", "given": "L." }, "orcid": "0000-0003-3498-2973" } ] }, "title": "High Spatial Resolution Mid-Infrared Observations of Three Seyfert Galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies: individual (NGC 1275 NGC 4151 NGC 7469); galaxies: Seyfert; infrared radiation", "note": "\u00a9 2003. The American Astronomical Society. \n\nReceived 2003 January 27. Accepted 2003 April 1. \n\nWe thank the staff of the Keck Observatory for their assistance in making these observations possible. The W. M. Keck Observatory is operated as a scientific partnership between the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. It was made possible by the generous financial support of the W. M. Keck Foundation. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, none of the observations presented herein would have been possible. We thank Carol Lonsdale for supplying the VLBI image of NGC 7469. B. T. S. and E. E. were supported by grants from the NSF and NASA. B. T. S. and L. A. are supported by the SIRTF Science Center at Caltech. SIRTF is carried out at JPL, operated by Caltech under an agreement with NASA.\n\nPublished - Soifer_2003_AJ_126_143.pdf
Accepted Version - 0304105.pdf
", "abstract": "Images at 12.5 \u03bcm of nuclei of three nearby Seyfert galaxies\u2014NGC 1275, NGC 4151, and NGC 7469\u2014have been obtained with the 10 m Keck Telescope. NGC 7469 is resolved and deconvolution delineates a structure (<0farcs04) \u00d7 0farcs08, or less than 13 \u00d7 26 pc at a position angle of 135\u00b0. From a comparison with structure seen at millimeter wavelengths, this structure is interpreted as a disk aligned with the molecular gas in the central few hundred parsecs of the galaxy. NGC 1275 and NGC 4151 are not resolved; limits on the sizes of these nuclei are 0farcs08 and 0farcs16, corresponding to physical spatial scales of 28 and 10 pc. The lower limits to the brightness temperatures implied by these size limits and the measured flux densities are within ~50 K of the 12\u201325 \u03bcm color temperatures of these systems, as inferred from IRAS observations. The angular size limits are within a factor of 2 of the sizes required to spatially resolve thermal emission from dust heated by a central luminosity source. These sizes preclude significant contributions to the nuclear infrared emission from star-forming regions.", "date": "2003-07", "date_type": "published", "publication": "Astronomical Journal", "volume": "126", "number": "1", "publisher": "American Astronomical Society", "pagerange": "143-152", "id_number": "CaltechAUTHORS:20170215-134941436", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170215-134941436", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF" }, { "agency": "Caltech SIRTF Science Center" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1086/375647", "primary_object": { "basename": "0304105.pdf", "url": "https://authors.library.caltech.edu/records/0c6c7-x3c03/files/0304105.pdf" }, "related_objects": [ { "basename": "Soifer_2003_AJ_126_143.pdf", "url": "https://authors.library.caltech.edu/records/0c6c7-x3c03/files/Soifer_2003_AJ_126_143.pdf" } ], "resource_type": "article", "pub_year": "2003", "author_list": "Soifer, B. T.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/2jqq5-43m96", "eprint_id": 100999, "eprint_status": "archive", "datestamp": "2023-08-19 11:43:18", "lastmod": "2023-10-19 22:19:32", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "De-Troia-G", "name": { "family": "De Troia", "given": "G." } }, { "id": "Ade-P-A-R", "name": { "family": "Ade", "given": "P. A. R." }, "orcid": "0000-0002-5127-0401" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Bond-J-R", "name": { "family": "Bond", "given": "J. R." }, "orcid": "0000-0003-2358-9949" }, { "id": "Boscaleri-A", "name": { "family": "Boscaleri", "given": "A." } }, { "id": "Contaldi-C-R", "name": { "family": "Contaldi", "given": "C. R." } }, { "id": "Crill-B-P", "name": { "family": "Crill", "given": "B. P." }, "orcid": "0000-0002-4650-8518" }, { "id": "de-Bernardis-P", "name": { "family": "de Bernardis", "given": "P." }, "orcid": "0000-0001-6547-6446" }, { "id": "Ferreira-P-G", "name": { "family": "Ferreira", "given": "P. G." } }, { "id": "Giacometti-M", "name": { "family": "Giacometti", "given": "M." } }, { "id": "Hivon-E", "name": { "family": "Hivon", "given": "E." } }, { "id": "Hristov-V-V", "name": { "family": "Hristov", "given": "V. V." } }, { "id": "Kunz-M", "name": { "family": "Kunz", "given": "M." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Masi-S", "name": { "family": "Masi", "given": "S." }, "orcid": "0000-0001-5105-1439" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Montroy-T-E", "name": { "family": "Montroy", "given": "T." } }, { "id": "Natoli-P", "name": { "family": "Natoli", "given": "P." } }, { "id": "Netterfield-C-B", "name": { "family": "Netterfield", "given": "C. B." } }, { "id": "Pascale-E", "name": { "family": "Pascale", "given": "E." }, "orcid": "0000-0002-3242-8154" }, { "id": "Piacentini-F", "name": { "family": "Piacentini", "given": "F." }, "orcid": "0000-0002-5444-9327" }, { "id": "Polenta-G", "name": { "family": "Polenta", "given": "G." } }, { "id": "Romeo-G", "name": { "family": "Romeo", "given": "G." } }, { "id": "Ruhl-J-E", "name": { "family": "Ruhl", "given": "J. E." } } ] }, "title": "The trispectrum of the cosmic microwave background on subdegree angular scales: an analysis of the BOOMERanG data", "ispublished": "pub", "full_text_status": "public", "keywords": "methods: statistical \u2013 cosmic microwave background", "note": "\u00a9 2003 RAS. \n\nAccepted 2003 March 27. Received 2003 March 26; in original form 2003 January 20. Published: 21 July 2003. \n\nGDT acknowledges financial support from the Dottorato in Astronomia dell'Universit\u00e0 La Sapienza and from a Marie Curie pre-doctoral fellowship. MK acknowledges financial support from the Swiss National Science foundation. PGF acknowledges the support of the Royal Society. The BOOMERanG project has been supported by Programma Nazionale di Ricerche in Antartide, Universit\u00e1 di Roma 'La Sapienza', and Agenzia Spaziale Italiana in Italy, by NASA and by NSF OPP in the US. We acknowledge the use of the HEALPix package and of the Oxford Beowulf cluster for our computations. We thank Andrew Jaffe and Alessandro Melchiorri for their helpful comments and Jonathan Patterson for his help.\n\nPublished - 343-1-284.pdf
Submitted - 0301294.pdf
", "abstract": "The trispectrum of the cosmic microwave background can be used to assess the level of non-Gaussianity on cosmological scales. It probes the fourth-order moment, as a function of angular scale, of the probability distribution function of fluctuations and has been shown to be sensitive to primordial non-Gaussianity, secondary anisotropies (such as the Ostriker\u2013Vishniac effect) and systematic effects (such as astrophysical foregrounds). In this paper we develop a formalism for estimating the trispectrum from high-resolution sky maps that incorporates the impact of finite sky coverage. This leads to a series of operations applied to the data set to minimize the effects of contamination due to the Gaussian component and correlations between estimates at different scales. To illustrate the effect of the estimation process, we apply our procedure to the BOOMERanG data set and show that it is consistent with Gaussianity. This work presents the first estimation of the cosmic microwave background trispectrum on subdegree scales.", "date": "2003-07", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "343", "number": "1", "publisher": "Royal Astronomical Society", "pagerange": "284-292", "id_number": "CaltechAUTHORS:20200130-080407664", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200130-080407664", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Dottorato in Astronomia dell'Universit\u00e0 La Sapienza" }, { "agency": "Marie Curie Fellowship" }, { "agency": "Swiss National Science Foundation (SNSF)" }, { "agency": "Royal Society" }, { "agency": "Programma Nazionale di Ricerche in Antartide (PNRA)" }, { "agency": "Universit\u00e1 di Roma La Sapienza" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "NASA" }, { "agency": "NSF" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" } ] }, "doi": "10.1046/j.1365-8711.2003.06665.x", "primary_object": { "basename": "0301294.pdf", "url": "https://authors.library.caltech.edu/records/2jqq5-43m96/files/0301294.pdf" }, "related_objects": [ { "basename": "343-1-284.pdf", "url": "https://authors.library.caltech.edu/records/2jqq5-43m96/files/343-1-284.pdf" } ], "resource_type": "article", "pub_year": "2003", "author_list": "De Troia, G.; Ade, P. A. R.; et el." }, { "id": "https://authors.library.caltech.edu/records/frkd8-hn452", "eprint_id": 84717, "eprint_status": "archive", "datestamp": "2023-08-19 11:00:02", "lastmod": "2023-10-18 16:38:28", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Beno\u00eet-A", "name": { "family": "Beno\u00eet", "given": "A." } }, { "id": "Bhatia-R-S", "name": { "family": "Bhatia", "given": "R. S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } } ] }, "title": "Cosmological constraints from Archeops", "ispublished": "pub", "full_text_status": "public", "keywords": "cosmic microwave background - cosmological parameters - early Universe - large-scale structure of the Universe", "note": "\u00a9 2003 ESO. \n\nReceived: 16 October 2002. Accepted: 22 November 2002. \n\nThe authors would like to thank the following institutes for funding and balloon launching capabilities: CNES (French space agency), PNC (French Cosmology Program), ASI (Italian Space Agency), PPARC, NASA, the University of Minnesota, the American Astronomical Society and a CMBNet Research Fellowship from the European Commission.\n\nPublished - aaej162.pdf
Submitted - 0210306.pdf
", "abstract": "We analyze the cosmological constraints that Archeops (Beno\u00eet et al. 2003) places on adiabatic cold dark matter models with passive power-law initial fluctuations. Because its angular power spectrum has small bins in \u2113 and large \u2113 coverage down to COBE scales, Archeops provides a precise determination of the first acoustic peak in terms of position at multipole l_(peak) = 220 \u00b1 6, height and width. An analysis of Archeops data in combination with other CMB datasets constrains the baryon content of the Universe, \u03a9_bh^2 = 0.022^(+0.003)_(-0.004), compatible with Big-Bang nucleosynthesis and with a similar accuracy. Using cosmological priors obtained from recent non-CMB data leads to yet tighter constraints on the total density, e.g. \u03a9_(tot) = 1.00^(+0.03)_(-0.02) using the HST determination of the Hubble constant. An excellent absolute calibration consistency is found between Archeops and other CMB experiments, as well as with the previously quoted best fit model. The spectral index n is measured to be 1.04^(+0.10)_(-0.12) when the optical depth to reionization, \u03c4, is allowed to vary as a free parameter, and 0.96^(+0.03)_(-0.04) when \u03c4 is fixed to zero, both in good agreement with inflation.", "date": "2003-02-14", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "399", "publisher": "EDP Sciences", "pagerange": "L25-L30", "id_number": "CaltechAUTHORS:20180207-112040907", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180207-112040907", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Programme National de Cosmologie (PNC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "NASA" }, { "agency": "University of Minnesota" }, { "agency": "American Astronomical Society" }, { "agency": "European Commission" } ] }, "doi": "10.1051/0004-6361:20021722", "primary_object": { "basename": "0210306.pdf", "url": "https://authors.library.caltech.edu/records/frkd8-hn452/files/0210306.pdf" }, "related_objects": [ { "basename": "aaej162.pdf", "url": "https://authors.library.caltech.edu/records/frkd8-hn452/files/aaej162.pdf" } ], "resource_type": "article", "pub_year": "2003", "author_list": "Beno\u00eet, A.; Bhatia, R. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/vw0jk-0vt32", "eprint_id": 84723, "eprint_status": "archive", "datestamp": "2023-08-19 11:00:08", "lastmod": "2023-10-18 16:38:40", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Beno\u00eet-A", "name": { "family": "Beno\u00eet", "given": "A." } }, { "id": "Bhatia-R-S", "name": { "family": "Bhatia", "given": "R. S." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } }, { "id": "Ganga-K", "name": { "family": "Ganga", "given": "K." } } ] }, "title": "The cosmic microwave background anisotropy power spectrum\n measured by Archeops", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2003 ESO. \n\nReceived: 16 October 2002. Accepted: 15 December 2002. \n\nThe authors would like to thank the following institutes for funding and balloon launching capabilities: CNES (French space agency), PNC (French Cosmology Program), ASI (Italian Space Agency), PPARC, NASA, the University of Minnesota, the American Astronomical Society and a CMBNet Research Fellowship from the European Commission. Healpix package was used throughout the data analysis (1998).\n\nPublished - aaej161.pdf
Submitted - 0210305.pdf
", "abstract": "We present a determination by the Archeops experiment of the angular power spectrum of the cosmic microwave background anisotropy in 16 bins over the multipole range \u2113 = 15-350. Archeops was conceived as a precursor of the Planck HFI instrument by using the same optical design and the same technology for the detectors and their cooling. Archeops is a balloon\u2013borne instrument consisting of a 1.5 m aperture diameter telescope and an array of 21 photometers maintained at mK that are operating in 4 frequency bands centered at 143, 217, 353 and 545 GHz. The data were taken during the Arctic night of February 7, 2002 after the instrument was launched by CNES from Esrange base (Sweden). The entire data cover ~30% of the sky. This first analysis was obtained with a small subset of the dataset using the most sensitive photometer in each CMB band (143 and 217 GHz) and 12.6% of the sky at galactic latitudes above 30 degrees where the foreground contamination is measured to be negligible. The large sky coverage and medium resolution (better than 15 arcmin) provide for the first time a high signal-to-noise ratio determination of the power spectrum over angular scales that include both the first acoustic peak and scales probed by COBE/DMR. With a binning of \u2113\u0394 = 7 to 25 the error bars are dominated by sample variance for \u2113 below 200. A companion paper details the cosmological implications.", "date": "2003-02-14", "date_type": "published", "publication": "Astronomy & Astrophysics", "volume": "399", "number": "3", "publisher": "EDP Sciences", "pagerange": "L19-L23", "id_number": "CaltechAUTHORS:20180207-131552158", "issn": "0004-6361", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180207-131552158", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Centre National d'\u00c9tudes Spatiales (CNES)" }, { "agency": "Programme National de Cosmologie (PNC)" }, { "agency": "Agenzia Spaziale Italiana (ASI)" }, { "agency": "Particle Physics and Astronomy Research Council (PPARC)" }, { "agency": "NASA" }, { "agency": "University of Minnesota" }, { "agency": "American Astronomical Society" }, { "agency": "European Commission" } ] }, "doi": "10.1051/0004-6361:20021850", "primary_object": { "basename": "0210305.pdf", "url": "https://authors.library.caltech.edu/records/vw0jk-0vt32/files/0210305.pdf" }, "related_objects": [ { "basename": "aaej161.pdf", "url": "https://authors.library.caltech.edu/records/vw0jk-0vt32/files/aaej161.pdf" } ], "resource_type": "article", "pub_year": "2003", "author_list": "Beno\u00eet, A.; Bhatia, R. S.; et el." }, { "id": "https://authors.library.caltech.edu/records/sjd1x-r2p16", "eprint_id": 27593, "eprint_status": "archive", "datestamp": "2023-08-19 08:56:14", "lastmod": "2023-10-24 17:16:15", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Glenn-J", "name": { "family": "Glenn", "given": "Jason" }, "orcid": "0000-0001-7527-2017" }, { "id": "Chattopadhyay-G", "name": { "family": "Chattopadhyay", "given": "Goutam" }, "orcid": "0000-0001-7942-5025" }, { "id": "Edgington-S-F", "name": { "family": "Edgington", "given": "Samantha F." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "Andrew E." } }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "James J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "Philip D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Lee-Adrian-T", "name": { "family": "Lee", "given": "Adrian T." } } ] }, "title": "Numerical optimization of integrating cavities for diffraction-limited millimeter-wave bolometer arrays", "ispublished": "pub", "full_text_status": "public", "note": "\u00a9 2002 Optical Society of America. Received 9 February 2001; revised manuscript received 7 August 2001. We thank Jonas Zmuidzinas for helpful discussions and Sunil Golwala for critical comments on the manuscript. J. Glenn and A. E. Lange acknowledge support from National Science Foundation (NSF) grant AST-9618798. A. Lee was supported by NSF\ngrant AST-9120005.\n\nPublished - GLEao02.pdf
", "abstract": "Far-infrared to millimeter-wave bolometers designed to make astronomical observations are typically encased in integrating cavities at the termination of feedhorns or Winston cones. This photometer combination maximizes absorption of radiation, enables the absorber area to be minimized, and controls the directivity of absorption, thereby reducing susceptibility to stray light. In the next decade, arrays of hundreds of silicon nitride micromesh bolometers with planar architectures will be used in ground-based, suborbital, and orbital platforms for astronomy. The optimization of integrating cavity designs is required for achieving the highest possible sensitivity for these arrays. We report numerical simulations of the electromagnetic fields in integrating cavities with an infinite plane-parallel geometry formed by a solid reflecting backshort and the back surface of a feedhorn array block. Performance of this architecture for the bolometer array camera (Bolocam) for cosmology at a frequency of 214 GHz is investigated. We explore the sensitivity of absorption efficiency to absorber impedance and backshort location and the magnitude of leakage from cavities. The simulations are compared with experimental data from a room-temperature scale model and with the performance of Bolocam at a temperature of 300 mK. The main results of the simulations for Bolocam-type cavities are that (1) monochromatic absorptions as high as 95% are achievable with <1% cross talk between neighboring cavities, (2) the optimum absorber impedances are 400 \u03a9/sq, but with a broad maximum from ~150 to ~700 \u03a9/sq, and (3) maximum absorption is achieved with absorber diameters \u22651.5\u03bb. Good general agreement between the simulations and the experiments was found.", "date": "2002-01-01", "date_type": "published", "publication": "Applied Optics", "volume": "41", "number": "1", "publisher": "Optical Society of America", "pagerange": "136-142", "id_number": "CaltechAUTHORS:20111102-141515126", "issn": "0003-6935", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111102-141515126", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "NSF", "grant_number": "AST-9618798" }, { "agency": "NSF", "grant_number": "AST-9120005" } ] }, "doi": "10.1364/AO.41.000136", "primary_object": { "basename": "GLEao02.pdf", "url": "https://authors.library.caltech.edu/records/sjd1x-r2p16/files/GLEao02.pdf" }, "resource_type": "article", "pub_year": "2002", "author_list": "Glenn, Jason; Chattopadhyay, Goutam; et el." }, { "id": "https://authors.library.caltech.edu/records/nn2m8-cee25", "eprint_id": 74154, "eprint_status": "archive", "datestamp": "2023-08-19 06:51:14", "lastmod": "2023-10-24 22:09:12", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Neugebauer-G", "name": { "family": "Neugebauer", "given": "G." } }, { "id": "Matthews-K", "name": { "family": "Matthews", "given": "K." } }, { "id": "Soifer-B-T", "name": { "family": "Soifer", "given": "B. T." } }, { "id": "Becklin-E-E", "name": { "family": "Becklin", "given": "E. E." } }, { "id": "Ressler-M-E", "name": { "family": "Ressler", "given": "M." } }, { "id": "Marsh-K-A", "name": { "family": "Marsh", "given": "K." }, "orcid": "0000-0003-0107-7803" }, { "id": "Werner-M-W", "name": { "family": "Werner", "given": "M. W." } }, { "id": "Egami-Eichi", "name": { "family": "Egami", "given": "E." } }, { "id": "Blandford-R-D", "name": { "family": "Blandford", "given": "R." }, "orcid": "0000-0002-1854-5506" } ] }, "title": "High Spatial Resolution Imaging of NGC 1068 in the Mid-Infrared", "ispublished": "pub", "full_text_status": "public", "keywords": "galaxies : individual (NGC 1068) \u00c8 infrared radiation", "note": "\u00a9 2000 American Astronomical Society. \n\nReceived 2000 July 21; accepted 2000 September 6. \n\nWe thank the staff of the Keck Observatory, especially Bob Goodrich, for their assistance in making these observations possible. We also thank Pat Shopbell for discussions about the X-ray observations of NGC 1068 and Lee Armus, Bob Goodrich, Nick Scoville, Kris Sellgren, and Dave Thompson for discussions about various aspects of the interpretation. We thank Ski Antonnucci and Makoto Kisimoto for their helpful comments as referees. The W. M. Keck Observatory is operated as a scientific partnership between the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. It was made possible by the generous financial support of the W. M. Keck Foundation. B. T. S., G. N., K. M., and E. E. are supported by grants from the NSF and NASA. B. T. S. is supported by the SIRTF Science Center at Caltech. SIRTF is carried out at J.P.L., operated by Caltech under an agreement with NASA. This work was carried out in part (J. J. B., M. W. W., and M. E. R.) at J.P.L. The development of MIRLIN was supported by NASA's Office of Space Science.\n\nPublished - Bock_2000_AJ_120_2904.pdf
Accepted Version - 0009078
", "abstract": "Mid-infrared observations of the central source of NGC 1068 have been obtained with a spatial resolution in the deconvolved image of 0.\"1 (~7 pc). The central source is extended by ~1'' in the north-south direction but appears unresolved in the east-west direction over most of its length. About 2/3 of its flux can be ascribed to a core structure that is itself elongated north-south and does not show a distinct unresolved compact source. The source is strongly asymmetric, extending significantly farther to the north than to the south. The morphology of the mid-infrared emission appears similar to that of the radio jet and has features which correlate with the images in [O III]. Its 12.5\u201324.5 \u03bcm color temperature ranges from 215 to 260 K and does not decrease smoothly with distance from the core. Silicate absorption is strongest in the core and to the south and is small in the north. The core, apparently containing 2/3 of the bolometric luminosity of the inner 4'' diameter area, may be explained by a thick, dusty torus near the central active galactic nucleus (AGN) viewed at an angle of ~65\u00b0 to its plane. There are, however, detailed difficulties with existing models, especially the narrow east-west width of the thin extended mid-infrared \"tongue\" to the north of the core. We interpret the tongue as reprocessed visual and ultraviolet radiation that is strongly beamed and that originates in the AGN.", "date": "2000-12", "date_type": "published", "publication": "Astronomical Journal", "volume": "120", "number": "6", "publisher": "American Astronomical Society", "pagerange": "2904-2919", "id_number": "CaltechAUTHORS:20170208-103123393", "issn": "0004-6256", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170208-103123393", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "W. M. Keck Foundation" }, { "agency": "NSF" }, { "agency": "NASA/JPL/Caltech" } ] }, "local_group": { "items": [ { "id": "Infrared-Processing-and-Analysis-Center-(IPAC)" }, { "id": "TAPIR" } ] }, "doi": "10.1086/316871", "primary_object": { "basename": "0009078", "url": "https://authors.library.caltech.edu/records/nn2m8-cee25/files/0009078" }, "related_objects": [ { "basename": "Bock_2000_AJ_120_2904.pdf", "url": "https://authors.library.caltech.edu/records/nn2m8-cee25/files/Bock_2000_AJ_120_2904.pdf" } ], "resource_type": "article", "pub_year": "2000", "author_list": "Bock, J. J.; Neugebauer, G.; et el." }, { "id": "https://authors.library.caltech.edu/records/f60py-b9y39", "eprint_id": 11308, "eprint_status": "archive", "datestamp": "2023-08-21 21:05:25", "lastmod": "2023-10-16 23:42:38", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Blain-A-W", "name": { "family": "Blain", "given": "A. W." }, "orcid": "0000-0001-7489-5167" }, { "id": "Frayer-D-T", "name": { "family": "Frayer", "given": "D. T." }, "orcid": "0000-0003-1924-1122" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Scoville-N-Z", "name": { "family": "Scoville", "given": "N. Z." }, "orcid": "0000-0002-0438-3323" } ] }, "title": "Millimetre/submillimetre-wave emission-line searches for high-redshift galaxies", "ispublished": "pub", "full_text_status": "public", "keywords": "molecules; galactic evolution; galaxy formation; cosmology; infrared galaxies; radio lines", "note": "\u00a9 2000 RAS. \n\nAccepted 1999 November 11. Received 1999 November 10; in original form 1999 March 24. \n\nThe results in this paper are based on the properties of the SCUBA lens survey galaxies detected at the Owens Valley Millimeter Array in collaboration with Aaron Evans and Min Yun. The core of the SCUBA lens survey was carried out by Ian Smail, Rob Ivison, AWB and Jean-Paul Kneib. We thank the referee, Paul van der Werf, for his careful reading of the manuscript and valuable comments, and also Jackie Davidson, Kate Isaak, Rob Ivison, Richard Hills, Brett Kornfeld, Malcolm Longair, Phil Lubin, Kate Quirk, John Richer and Gordon Stacey for helpful conversations and comments. AWB - the Raymond & Beverly Sackler Foundation Research Fellow at the IoA, Cambridge - gratefully acknowledges generous support from the Raymond & Beverly Sackler Foundation as part of the Deep Sky Initiative programme at the IoA. AWB also thanks the Caltech AY visitors program for support while this work was conducted.\n\nPublished - BLAmnras00.pdf
", "abstract": "The redshifted spectral line radiation emitted from both atomic fine-structure and molecular rotational transitions in the interstellar medium (ISM) of high-redshift galaxies can be detected in the centimetre, millimetre and submillimetre wavebands. Here we predict the counts of galaxies detectable in an array of molecular and atomic lines. This calculation requires a reasonable knowledge of both the surface density of these galaxies on the sky, and the physical conditions in their ISM. The surface density is constrained using the results of submillimetre-wave continuum surveys. Follow-up OVRO Millimeter Array observations of two of the galaxies detected in the dust continuum have provided direct measurements of CO rotational line emission at redshifts of 2.56 and 2.81. Based on these direct high-redshift observations and on models of the ISM that are constrained by observations of low-redshift ultraluminous infrared galaxies, we predict the surface density of line-emitting galaxies as a function of line flux density and observing frequency. We incorporate the sensitivities and mapping speeds of existing and future millimetre/submillimetre-wave telescopes and spectrographs, and so assess the prospects for blank-field surveys to detect this line emission from gas-rich high-redshift galaxies.", "date": "2000-04-11", "date_type": "published", "publication": "Monthly Notices of the Royal Astronomical Society", "volume": "313", "number": "3", "publisher": "Royal Astronomical Society", "pagerange": "559-570", "id_number": "CaltechAUTHORS:BLAmnras00", "issn": "0035-8711", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BLAmnras00", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Raymond and Beverly Sackler Foundation" }, { "agency": "Caltech Astronomy visitors' program" } ] }, "doi": "10.1046/j.1365-8711.2000.03287.x", "primary_object": { "basename": "BLAmnras00.pdf", "url": "https://authors.library.caltech.edu/records/f60py-b9y39/files/BLAmnras00.pdf" }, "resource_type": "article", "pub_year": "2000", "author_list": "Blain, A. W.; Frayer, D. T.; et el." }, { "id": "https://authors.library.caltech.edu/records/0y9df-nab56", "eprint_id": 29012, "eprint_status": "archive", "datestamp": "2023-08-19 01:02:41", "lastmod": "2023-10-24 18:18:30", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Mauskopf-P-D", "name": { "family": "Mauskopf", "given": "P. D." }, "orcid": "0000-0001-6397-5516" }, { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Del-Castillo-H", "name": { "family": "Del Castillo", "given": "H." } }, { "id": "Holzapfel-W-L", "name": { "family": "Holzapfel", "given": "W. L." } }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } } ] }, "title": "Composite infrared bolometers with Si_3N_4 micromesh absorbers", "ispublished": "pub", "full_text_status": "public", "keywords": "Infrared bolometers, silicon nitride, micromesh.", "note": "\u00a9 1997 Optical Society of America. Received 5 April 1996; revised manuscript received 23 July 1996. This research has been made possible by a grant\nfrom the Center of Space Microelectronics Technology\nto the Microdevices Laboratory at Jet Propulsion\nLaboratory to support the fabrication and development\nof the micromesh absorbers. The authors also\nthank P. L. Richards for many useful discussions, W.\nHolmes for the measurements of the thermal conductivity\nof silicon nitride, and D. Hebert and the staff at\nthe microlab at University of California, Berkeley, for\nassistance in manufacturing the original micromesh\nbolometers. This research has been supported by a\nNASA Graduate Student Research Program grant to\nP. D. Mauskopf.\n\nPublished - MAUao97.pdf
", "abstract": "We report the design and performance of 300-mK composite bolometers that use micromesh absorbers and support structures patterned from thin films of low-stress silicon nitride. The small geometrical filling factor of the micromesh absorber provides 20\u00d7 reduction in heat capacity and cosmic ray cross section relative to a solid absorber with no loss in IR-absorption efficiency. The support structure is mechanically robust and has a thermal conductance, G < 2 \u00d7 10^(\u221211) W/K, which is four times smaller than previously achieved at 300 mK. The temperature rise of the bolometer is measured with a neutron transmutation doped germanium thermistor attached to the absorbing mesh. The dispersion in electrical and thermal parameters of a sample of 12 bolometers optimized for the Sunyaev\u2013Zel'dovich Infrared Experiment is \u00b17% in R (T), \u00b15% in optical efficiency, and \u00b14% in G.", "date": "1997-02-01", "date_type": "published", "publication": "Applied Optics", "volume": "36", "number": "4", "publisher": "Optical Society of America", "pagerange": "765-771", "id_number": "CaltechAUTHORS:20120130-075759922", "issn": "0003-6935", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120130-075759922", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "funders": { "items": [ { "agency": "Center for Space Microelectronics Technology to the Microdevices Laboratory at JPL" }, { "agency": "NASA Graduate Student Research Program" } ] }, "collection": "CaltechAUTHORS", "doi": "10.1364/AO.36.000765", "primary_object": { "basename": "MAUao97.pdf", "url": "https://authors.library.caltech.edu/records/0y9df-nab56/files/MAUao97.pdf" }, "resource_type": "article", "pub_year": "1997", "author_list": "Mauskopf, P. D.; Bock, J. J.; et el." }, { "id": "https://authors.library.caltech.edu/records/6e2ka-zrs61", "eprint_id": 2910, "eprint_status": "archive", "datestamp": "2023-08-22 10:40:33", "lastmod": "2023-10-13 23:48:23", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } } ] }, "title": "Performance of a low-pass filter for far-infrared wavelengths", "ispublished": "pub", "full_text_status": "public", "keywords": "Far-infrared, low-pass filter, spectroscopy", "note": "\u00a9 1995 Optical Society of America \n\nReceived 18 April 1995; revised manuscript received 20 July 1995. \n\nThe authors thank P. L. Richards for the use of his spectrometer. The details of the LP100 filter were kindly provided by M. T. Stier. The authors acknowledge support by NASAunder grants NAGW-1352 and NGT-50771.", "abstract": "We describe a low-pass filter that provides high in-band transmittance and excellent rejection at nu > 100 cm^-1. The transmittance of the filter components was measured at liquid-helium temperatures from 10 to 10,000 cm^-1. The total transmittance is > 50% for nu < 50 cm^-1 and is calculated to be < 10^-9 for nu > 300 cm^-1. The filter was successfully used in a liquid-helium-cooled, rocketborne, far-infrared absolute photometer.", "date": "1995-11-01", "date_type": "published", "publication": "Applied Optics", "volume": "34", "number": "31", "publisher": "Optical Society of America", "pagerange": "7254-7257", "id_number": "CaltechAUTHORS:BOCao95a", "issn": "0003-6935", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BOCao95a", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "primary_object": { "basename": "BOCao95a.pdf", "url": "https://authors.library.caltech.edu/records/6e2ka-zrs61/files/BOCao95a.pdf" }, "resource_type": "article", "pub_year": "1995", "author_list": "Bock, J. J. and Lange, A. E." }, { "id": "https://authors.library.caltech.edu/records/ajjdf-h7q06", "eprint_id": 2909, "eprint_status": "archive", "datestamp": "2023-08-22 10:34:43", "lastmod": "2023-10-13 23:48:21", "type": "article", "metadata_visibility": "show", "creators": { "items": [ { "id": "Bock-J-J", "name": { "family": "Bock", "given": "J. J." }, "orcid": "0000-0002-5710-5212" }, { "id": "Parikh-M-K", "name": { "family": "Parikh", "given": "M. K." } }, { "id": "Fischer-M-L", "name": { "family": "Fischer", "given": "M. L." }, "orcid": "0000-0001-7956-2361" }, { "id": "Lange-A-E", "name": { "family": "Lange", "given": "A. E." } } ] }, "title": "Emissivity measurements of reflective surfaces at near-millimeter wavelengths", "ispublished": "pub", "full_text_status": "public", "keywords": "Emissivity; reflectance; millimeter; infrared; mirrors", "note": "\u00a9 1995 Optical Society of America \n\nReceived 31 October 1994; revised manuscript received 24 January 1995. \n\nThe authors thank Sylvia Li for work with the instrument and acknowledge helpful conversations with Dave Cottingham and Paul Richards. This research was supported in part by the NASA graduate student research program fellowship NGT-50771.", "abstract": "We have developed an instrument for directly measuring the emissivity of reflective surfaces at near-millimeter wavelengths. The thermal emission of a test sample is compared with that of a reference surface, allowing the emissivity of the sample to be determined without heating. The emissivity of the reference surface is determined by one's heating the reference surface and measuring the increase in emission. The instrument has an absolute accuracy of \u0394e = 5 x 10^-4 and can reproducibly measure a difference in emissivity as small as \u0394e = 10^-4 between flat reflective samples. We have used the instrument to measure the emissivity of metal films evaporated on glass and carbon fiber-reinforced plastic composite surfaces. We measure an emissivity of (2.15 \u00b1 0.4) x 10^-3 for gold evaporated on glass and (2.65 \u00b1 0.5) x 10^-3 for aluminum evaporated on carbon fiber-reinforced plastic composite.", "date": "1995-08-01", "date_type": "published", "publication": "Applied Optics", "volume": "34", "number": "22", "publisher": "Optical Society of America", "pagerange": "4812-4816", "id_number": "CaltechAUTHORS:BOCao95b", "issn": "0003-6935", "official_url": "https://resolver.caltech.edu/CaltechAUTHORS:BOCao95b", "rights": "No commercial reproduction, distribution, display or performance rights in this work are provided.", "primary_object": { "basename": "BOCao95b.pdf", "url": "https://authors.library.caltech.edu/records/ajjdf-h7q06/files/BOCao95b.pdf" }, "resource_type": "article", "pub_year": "1995", "author_list": "Bock, J. J.; Parikh, M. K.; et el." } ]