[ { "id": "authors:qgqdz-p2n39", "collection": "authors", "collection_id": "qgqdz-p2n39", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220526-173305519", "type": "monograph", "title": "Neutrino follow-up with the Zwicky Transient Facility: Results from the first 24 campaigns", "author": [ { "family_name": "Stein", "given_name": "Robert", "orcid": "0000-0003-2434-0387", "clpid": "Stein-Robert-D" }, { "family_name": "Reusch", "given_name": "Simeon", "orcid": "0000-0002-7788-628X" }, { "family_name": "Franckowiak", "given_name": "Anna", "orcid": "0000-0002-5605-2219" }, { "family_name": "Kowalski", "given_name": "Marek", "orcid": "0000-0001-8594-8666" }, { "family_name": "Necker", "given_name": "Jannis", "orcid": "0000-0003-0280-7484" }, { "family_name": "Weimann", "given_name": "Sven" }, { "family_name": "Kasliwal", "given_name": "Mansi M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Sollerman", "given_name": "Jesper", "orcid": "0000-0003-1546-6615" }, { "family_name": "Ahumada", "given_name": "Tom\u00e1s", "orcid": "0000-0002-2184-6430" }, { "family_name": "Amaro Seoane", "given_name": "Pau", "orcid": "0000-0003-3993-3249" }, { "family_name": "Anand", "given_name": "Shreya", "orcid": "0000-0003-3768-7515", "clpid": "Anand-Shreya-G" }, { "family_name": "Andreoni", "given_name": "Igor", "orcid": "0000-0002-8977-1498" }, { "family_name": "Bellm", "given_name": "Eric C.", "orcid": "0000-0001-8018-5348" }, { "family_name": "Bloom", "given_name": "Joshua S.", "orcid": "0000-0002-7777-216X" }, { "family_name": "Coughlin", "given_name": "Michael", "orcid": "0000-0002-8262-2924" }, { "family_name": "De", "given_name": "Kishalay", "orcid": "0000-0002-8989-0542" }, { "family_name": "Fremling", "given_name": "Christoffer", "orcid": "0000-0002-4223-103X", "clpid": "Fremling-Christoffer" }, { "family_name": "Gezari", "given_name": "Suvi", "orcid": "0000-0003-3703-5154" }, { "family_name": "Graham", "given_name": "Matthew", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Groom", "given_name": "Steven L.", "orcid": "0000-0001-5668-3507", "clpid": "Groom-Steven-L" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Kaplan", "given_name": "David L.", "orcid": "0000-0001-6295-2881" }, { "family_name": "Karambelkar", "given_name": "Viraj", "orcid": "0000-0003-2758-159X", "clpid": "Karambelkar-Viraj-R" }, { "family_name": "Kong", "given_name": "Albert K. H.", "orcid": "0000-0002-5105-344X" }, { "family_name": "Kool", "given_name": "Erik C.", "orcid": "0000-0002-7252-3877" }, { "family_name": "Lincetto", "given_name": "Massimiliano", "orcid": "0000-0002-1460-3369" }, { "family_name": "Mahabal", "given_name": "Ashish A.", "orcid": "0000-0003-2242-0244", "clpid": "Mahabal-Ashish-A" }, { "family_name": "Masci", "given_name": "Frank J.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-Frank-J" }, { "family_name": "Medford", "given_name": "Michael S.", "orcid": "0000-0002-7226-0659" }, { "family_name": "Morgan", "given_name": "Robert", "orcid": "0000-0002-7016-5471" }, { "family_name": "Nordin", "given_name": "Jakob", "orcid": "0000-0001-8342-6274" }, { "family_name": "Rodriguez", "given_name": "Hector", "clpid": "Rodriguez-Hector" }, { "family_name": "Sharma", "given_name": "Yashvi", "orcid": "0000-0003-4531-1745", "clpid": "Sharma-Yashvi" }, { "family_name": "van Santen", "given_name": "Jakob", "orcid": "0000-0002-2412-9728" }, { "family_name": "van Velzen", "given_name": "Sjoert", "orcid": "0000-0002-3859-8074" }, { "family_name": "Yan", "given_name": "Lin", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "The Zwicky Transient Transient Facility (ZTF) performs a systematic neutrino follow-up program, searching for optical counterparts to high-energy neutrinos with dedicated Target-of-Opportunity (ToO) observations. Since first light in March 2018, ZTF has taken prompt observations for 24 high-quality neutrino alerts from the IceCube Neutrino Observatory, with a median latency of 12.2 hours from initial neutrino detection. From two of these campaigns, we have already reported tidal disruption event (TDE) AT2019dsg and likely TDE AT2019fdr as probable counterparts, suggesting that TDEs contribute >7.8% of the astrophysical neutrino flux. We here present the full results of our program through to December 2021. No additional candidate neutrino sources were identified by our program, allowing us to place the first constraints on the underlying optical luminosity function of astrophysical neutrino sources. Transients with optical absolutes magnitudes brighter that -21 can contribute no more than 87% of the total, while transients brighter than -22 can contribute no more than 58% of the total, neglecting the effect of extinction. These are the the first observational constraints on the neutrino emission of bright populations such as superluminous supernovae. None of the neutrinos were coincident with bright optical AGN flares comparable to that observed for TXS 0506+056/IC170922A, suggesting that most astrophysical neutrinos are not produced during such optical flares. We highlight the outlook for electromagnetic neutrino follow-up programs, including the expected potential for the Rubin Observatory.", "doi": "10.48550/arXiv.2203.17135", "publisher": "arXiv", "publication_date": "2022-03-31" }, { "id": "authors:t21jf-jyk53", "collection": "authors", "collection_id": "t21jf-jyk53", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20220411-225157319", "type": "monograph", "title": "Illuminating Galaxy Evolution at Cosmic Noon with ISCEA: the Infrared Satellite for Cosmic Evolution Astrophysics", "author": [ { "family_name": "Wang", "given_name": "Yun", "orcid": "0000-0002-4749-2984", "clpid": "Wang-Yun" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-Lee" }, { "family_name": "Benson", "given_name": "Andrew", "orcid": "0000-0001-5501-6008", "clpid": "Benson-Andrew-J" }, { "family_name": "Daddi", "given_name": "Emanuele", "orcid": "0000-0002-3331-9590", "clpid": "Daddi-Emanuele" }, { "family_name": "Faisst", "given_name": "Andreas", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-Andreas-L" }, { "family_name": "Gonzalez", "given_name": "Anthony", "orcid": "0000-0002-0933-8601", "clpid": "Gonzalez-Anthony-H" }, { "family_name": "Papovich", "given_name": "Casey", "orcid": "0000-0001-7503-8482", "clpid": "Papovich-Casey-J" }, { "family_name": "Ninkov", "given_name": "Zoran", "clpid": "Ninkov-Zoran" }, { "family_name": "Robberto", "given_name": "Massimo", "orcid": "0000-0002-9573-3199", "clpid": "Robberto-Massimo" }, { "family_name": "Rose", "given_name": "Randall J.", "clpid": "Rose-Randall-J" }, { "family_name": "Rose", "given_name": "Thomas", "clpid": "Rose-Thomas" }, { "family_name": "Scarlata", "given_name": "Claudia", "orcid": "0000-0002-9136-8876", "clpid": "Scarlata-Claudia-M" }, { "family_name": "Stanford", "given_name": "S. A.", "orcid": "0000-0003-0122-0841", "clpid": "Stanford-Specncer-A" }, { "family_name": "Veach", "given_name": "Todd", "clpid": "Veach-Todd" }, { "family_name": "Zhai", "given_name": "Zhongxu", "orcid": "0000-0001-7984-5476", "clpid": "Zhai-Zhongxu" }, { "family_name": "Benson", "given_name": "Bradford", "orcid": "0000-0002-5108-6823", "clpid": "Benson-Bradford-A" }, { "family_name": "Bleem", "given_name": "L. E.", "orcid": "0000-0001-7665-5079", "clpid": "Bleem-Lindsey-E" }, { "family_name": "Davis", "given_name": "Michael W.", "clpid": "Davis-Michael-W" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Hillenbrand", "given_name": "Lynne", "clpid": "Hillenbrand-L-A" } ], "abstract": "ISCEA (Infrared Satellite for Cosmic Evolution Astrophysics) is a small astrophysics mission whose Science Goal is to discover how galaxies evolved in the cosmic web of dark matter at cosmic noon. Its Science Objective is to determine the history of star formation and its quenching in galaxies as a function of local density and stellar mass when the Universe was 3-5 Gyrs old (1.2 < z < 2.1). ISCEA is designed to test the Science Hypothesis that during the period of cosmic noon, at 1.7 < z < 2.1, environmental quenching is the dominant quenching mechanism for typical galaxies not only in clusters and groups, but also in the extended cosmic web surrounding these structures. ISCEA meets its Science Objective by making a 10% shot noise measurement of star formation rate down to 6 M_\u2299\u2002 yr\u207b\u00b9 using H-\u03b1 out to a radius > 10 Mpc in each of 50 protocluster (cluster and cosmic web) fields at 1.2 < z < 2.1. ISCEA measures the star formation quenching factor in those fields, and galaxy kinematics with a precision < 50 km s\u207b\u00b9 to deduce the 3D spatial distribution in each field. ISCEA will transform our understanding of galaxy evolution at cosmic noon. \n\nISCEA is a small satellite observatory with a 30 cm equivalent diameter aperture telescope with a FoV of 0.32 deg\u00b2, and a multi-object spectrograph with a digital micro-mirror device (DMD) as its programmable slit mask. ISCEA will obtain spectra of 1000 galaxies simultaneously at an effective resolving power of R = 1000, with 2.8\" x 2.8\" slits, over the NIR wavelength range of 1.1 to 2.0 \u00b5m, a regime not accessible from the ground without large gaps in coverage. ISCEA will achieve a pointing accuracy of \u2264 2\" FWHM over 200s. ISCEA will be launched into a Low Earth Orbit, with a prime mission of 2.5 years. ISCEA's space-qualification of DMDs opens a new window for spectroscopy from space, enabling revolutionary advances in astrophysics.", "doi": "10.48550/arXiv.2112.02387", "publisher": "arXiv", "publication_date": "2021-12-04" }, { "id": "authors:qaf81-a9v18", "collection": "authors", "collection_id": "qaf81-a9v18", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200916-112945883", "type": "monograph", "title": "A kilometer-scale asteroid inside Venus's orbit", "author": [ { "family_name": "Ip", "given_name": "W.-H.", "orcid": "0000-0002-3140-5014", "clpid": "Ip-Wing-Huen" }, { "family_name": "Bolin", "given_name": "B.", "orcid": "0000-0002-4950-6323", "clpid": "Bolin-Bryce-T" }, { "family_name": "Masci", "given_name": "F. J.", "orcid": "0000-0002-8532-9395", "clpid": "Masci-Frank-J" }, { "family_name": "Ye", "given_name": "Q.-Z.", "orcid": "0000-0002-4838-7676" }, { "family_name": "Kramer", "given_name": "E. A.", "orcid": "0000-0003-0457-2519", "clpid": "Kramer-Emily-A" }, { "family_name": "Helou", "given_name": "G.", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Ahumada", "given_name": "T.", "orcid": "0000-0002-2184-6430", "clpid": "Ahumada-Tom\u00e1s" }, { "family_name": "Coughlin", "given_name": "M. W.", "orcid": "0000-0002-8262-2924", "clpid": "Coughlin-Michael-W" }, { "family_name": "Graham", "given_name": "M. J.", "orcid": "0000-0002-3168-0139", "clpid": "Graham-M-J" }, { "family_name": "Walters", "given_name": "R.", "orcid": "0000-0002-1835-6078", "clpid": "Walters-Richard-S" }, { "family_name": "Deshmukh", "given_name": "K. P." }, { "family_name": "Fremling", "given_name": "C.", "orcid": "0000-0002-4223-103X", "clpid": "Fremling-Christoffer" }, { "family_name": "Lin", "given_name": "Z.-Y." }, { "family_name": "Milburn", "given_name": "J. W.", "clpid": "Milburn-Jennifer-W" }, { "family_name": "Purdum", "given_name": "J. N." }, { "family_name": "Quimby", "given_name": "R.", "orcid": "0000-0001-9171-5236" }, { "family_name": "Bodewits", "given_name": "D.", "orcid": "0000-0002-2668-7248" }, { "family_name": "Chang", "given_name": "C.-K." }, { "family_name": "Ngeow", "given_name": "C.-C.", "orcid": "0000-0001-8771-7554", "clpid": "Ngeow-Chow-Choong" }, { "family_name": "Tan", "given_name": "H." }, { "family_name": "Zhai", "given_name": "C.", "orcid": "0000-0002-0291-4522" }, { "family_name": "van Dokkum", "given_name": "P.", "orcid": "0000-0002-8282-9888" }, { "family_name": "Granvik", "given_name": "M.", "orcid": "0000-0002-5624-1888" }, { "family_name": "Harikane", "given_name": "Y.", "orcid": "0000-0002-6047-430X" }, { "family_name": "Mowla", "given_name": "L. A." }, { "family_name": "Burdge", "given_name": "K. B.", "orcid": "0000-0002-7226-836X", "clpid": "Burdge-Kevin-B" }, { "family_name": "Bellm", "given_name": "E. C.", "orcid": "0000-0001-8018-5348" }, { "family_name": "De", "given_name": "K.", "orcid": "0000-0002-8989-0542", "clpid": "De-Kishalay" }, { "family_name": "Cenko", "given_name": "S. B.", "orcid": "0000-0003-1673-970X" }, { "family_name": "Copperwheat", "given_name": "C. M.", "orcid": "0000-0001-7983-8698" }, { "family_name": "Dekany", "given_name": "R.", "orcid": "0000-0002-5884-7867", "clpid": "Dekany-Richard-G" }, { "family_name": "Duev", "given_name": "D. A.", "orcid": "0000-0001-5060-8733", "clpid": "Duev-Dmitry-A" }, { "family_name": "Hale", "given_name": "D.", "clpid": "Hale-David-D-S" }, { "family_name": "Kasliwal", "given_name": "M. M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Kupfer", "given_name": "T.", "orcid": "0000-0002-6540-1484" }, { "family_name": "Mahabal", "given_name": "A.", "orcid": "0000-0003-2242-0244", "clpid": "Mahabal-Ashish-A" }, { "family_name": "Mr\u00f3z", "given_name": "P. J.", "orcid": "0000-0001-7016-1692", "clpid": "Mr\u00f3z-Przemek" }, { "family_name": "Neill", "given_name": "J. D.", "orcid": "0000-0002-0466-1119", "clpid": "Neill-James-D" }, { "family_name": "Riddle", "given_name": "R.", "orcid": "0000-0002-0387-370X", "clpid": "Riddle-Reed-L" }, { "family_name": "Rodriguez", "given_name": "H.", "clpid": "Rodriguez-Hector" }, { "family_name": "Serabyn", "given_name": "E.", "clpid": "Serabyn-Eugene" }, { "family_name": "Smith", "given_name": "R. M.", "orcid": "0000-0001-7062-9726", "clpid": "Smith-R-M" }, { "family_name": "Sollerman", "given_name": "J.", "orcid": "0000-0003-1546-6615" }, { "family_name": "Soumagnac", "given_name": "M. T.", "orcid": "0000-0001-6753-1488" }, { "family_name": "Southworth", "given_name": "J.", "orcid": "0000-0002-3807-3198" }, { "family_name": "Yan", "given_name": "L.", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "Near-Earth asteroid population models predict the existence of asteroids located inside the orbit of Venus. However, despite searches up to the end of 2019, none have been found. Here we report the discovery by the Zwicky Transient Facility of the first known asteroid located inside of Venus' orbit, 2020 AV\u2082, possessing an aphelion distance of 0.65 au and \u223c2 km in size. While it is possible that 2020 AV\u2082 is the largest of its kind, we find that its discovery is surprising in the context of population models where the expected count is close to zero. If this discovery is not a statistical fluke, then 2020 AV\u2082 may come from a yet undiscovered source population of asteroids interior to Venus, and currently favored asteroid population models may need to be adjusted.", "publisher": "arXiv", "publication_date": "2020-09-09" }, { "id": "authors:xqcv3-79f72", "collection": "authors", "collection_id": "xqcv3-79f72", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200908-091428952", "type": "monograph", "title": "Joint Survey Processing of Euclid, Rubin and Roman: Final Report", "author": [ { "family_name": "Chary", "given_name": "Ranga Ram", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Brammer", "given_name": "Gabriel", "orcid": "0000-0003-2680-005X", "clpid": "Brammer-G" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Faisst", "given_name": "Andreas", "orcid": "0000-0002-9382-9832", "clpid": "Faisst-A-L" }, { "family_name": "Flynn", "given_name": "Dave", "clpid": "Flynn-D" }, { "family_name": "Groom", "given_name": "Steven", "orcid": "0000-0001-5668-3507", "clpid": "Groom-S-L" }, { "family_name": "Ferguson", "given_name": "Henry C.", "orcid": "0000-0001-7113-2738", "clpid": "Ferguson-H-C" }, { "family_name": "Grillmair", "given_name": "Carl", "orcid": "0000-0003-4072-169X", "clpid": "Grillmair-C-J" }, { "family_name": "Hemmati", "given_name": "Shoubaneh", "orcid": "0000-0003-2226-5395", "clpid": "Hemmati-S" }, { "family_name": "Koekemoer", "given_name": "Anton", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Lee", "given_name": "BoMee", "clpid": "Lee-BoMee" }, { "family_name": "Malhotra", "given_name": "Sangeeta", "orcid": "0000-0002-9226-5350", "clpid": "Malhotra-Sangeeta" }, { "family_name": "Miyatake", "given_name": "Hironao", "clpid": "Miyatake-H" }, { "family_name": "Melchior", "given_name": "Peter", "orcid": "0000-0002-8873-5065", "clpid": "Melchior-P" }, { "family_name": "Momcheva", "given_name": "Ivelina", "clpid": "Momcheva-I-G" }, { "family_name": "Newman", "given_name": "Jeffrey", "orcid": "0000-0001-8684-2222", "clpid": "Newman-J-A" }, { "family_name": "Masiero", "given_name": "Joseph", "orcid": "0000-0003-2638-720X", "clpid": "Masiero-J-R" }, { "family_name": "Paladini", "given_name": "Roberta", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Prakash", "given_name": "Abhishek", "orcid": "0000-0003-4451-4444", "clpid": "Prakash-Abhishek" }, { "family_name": "Rusholme", "given_name": "Benjamin", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-B" }, { "family_name": "Stickley", "given_name": "Nathaniel", "clpid": "Stickley-N-R" }, { "family_name": "Smith", "given_name": "Arfon", "clpid": "Smith-A-M" }, { "family_name": "Wood-Vasey", "given_name": "Michael", "clpid": "Wood-Vasey-W-M" }, { "family_name": "Teplitz", "given_name": "Harry I.", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" } ], "abstract": "The Euclid, Rubin/LSST and Roman (WFIRST) projects will undertake flagship optical/near-infrared surveys in the next decade. By mapping thousands of square degrees of sky and covering the electromagnetic spectrum between 0.3 and\n2 microns with sub-arcsec resolution, these projects will detect several tens\nof billions of sources, enable a wide range of astrophysical investigations by\nthe astronomical community and provide unprecedented constraints on the nature\nof dark energy and dark matter. The ultimate cosmological, astrophysical and\ntime-domain science yield from these missions will require joint survey\nprocessing (JSP) functionality at the pixel level that is outside the scope of\nthe individual survey projects. The JSP effort scoped here serves two\nhigh-level objectives: 1) provide precise concordance multi-wavelength images\nand catalogs over the entire sky area where these surveys overlap, which\naccounts for source confusion and mismatched isophotes, and 2) provide a\nscience platform to analyze concordance images and catalogs to enable a wide\nrange of astrophysical science goals to be formulated and addressed by the\nresearch community. For the cost of about 200WY, JSP will allow the U.S. (and\ninternational) astronomical community to manipulate the flagship data sets and\nundertake innovative science investigations ranging from solar system object\ncharacterization, exoplanet detections, nearby galaxy rotation rates and dark\nmatter properties, to epoch of reionization studies. It will also allow for the\nultimate constraints on cosmological parameters and the nature of dark energy,\nwith far smaller uncertainties and a better handle on systematics than by any one survey alone.", "doi": "10.48550/arXiv.2008.10663", "publisher": "arXiv", "publication_date": "2020-08-24" }, { "id": "authors:t5mct-16v77", "collection": "authors", "collection_id": "t5mct-16v77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20191002-085537714", "type": "monograph", "title": "The Potential of Exozodiacal Disks Observations with the WFIRST Coronagraph Instrument", "author": [ { "family_name": "Mennesson", "given_name": "Bertrand", "orcid": "0000-0003-4205-4800", "clpid": "Mennesson-B" }, { "family_name": "Akeson", "given_name": "R.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Berriman", "given_name": "B.", "orcid": "0000-0001-8388-534X", "clpid": "Berriman-G-B" }, { "family_name": "Calchi Novati", "given_name": "S.", "orcid": "0000-0002-7669-1069", "clpid": "Calchi-Novati-S" }, { "family_name": "Gelino", "given_name": "C.", "clpid": "Gelino-C-R" }, { "family_name": "Gelino", "given_name": "D.", "orcid": "0000-0003-1274-2784", "clpid": "Gelino-D-M" }, { "family_name": "Helou", "given_name": "G.", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Laine", "given_name": "S.", "orcid": "0000-0003-1250-8314", "clpid": "Laine-S-J" }, { "family_name": "Lowrance", "given_name": "P.", "orcid": "0000-0001-8014-0270", "clpid": "Lowrance-P-J" }, { "family_name": "Meshkat", "given_name": "T.", "orcid": "0000-0001-6126-2467", "clpid": "Meshkat-T" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Ramirez", "given_name": "S.", "clpid": "Ramirez-S-V" }, { "family_name": "Ygouf", "given_name": "M.", "orcid": "0000-0001-7591-2731", "clpid": "Ygouf-M" } ], "abstract": "The Wide Field Infrared Survey Telescope (WFIRST) Coronagraph Instrument (CGI) will be the first high-performance stellar coronagraph using active wavefront control for deep starlight suppression in space, providing unprecedented levels of contrast, spatial resolution, and sensitivity for astronomical observations in the optical. One science case enabled by the CGI will be taking images and(R~50)spectra of faint interplanetary dust structures present in the habitable zone of nearby sunlike stars (~10 pc) and within the snow-line of more distant ones(~20pc), down to dust density levels commensurate with that of the solar system zodiacal cloud. Reaching contrast levels below~10-7 for the first time, CGI will cross an important threshold in debris disks physics, accessing disks with low enough optical depths that their structure is dominated by transport phenomena than collisions. Hence, CGI results will be crucial for determining how exozodiacal dust grains are produced and transported in low-density disks around mature stars. Additionally, CGI will be able to measure the brightness level and constrain the degree of asymmetry of exozodiacal clouds around individual nearby sunlike stars in the optical, at the ~10x solar zodiacal emission level. This information will be extremely valuable for optimizing the observational strategy of possible future exo-Earth direct imaging missions, especially those planning to operate at optical wavelengths, such as Habitable Exoplanet Observatory (HabEx) and the Large Ultraviolet/Optical/Infrared Surveyor (LUVOIR).", "doi": "10.48550/arXiv.1909.02161", "publication_date": "2019-09-05" }, { "id": "authors:edp4c-jkp25", "collection": "authors", "collection_id": "edp4c-jkp25", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-152042633", "type": "monograph", "title": "The Science Advantage of a Redder Filter for WFIRST", "author": [ { "family_name": "Stauffer", "given_name": "John", "orcid": "0000-0003-3595-7382", "clpid": "Stauffer-John-R" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Benjamin", "given_name": "Robert A.", "clpid": "Benjamin-Robert-A" }, { "family_name": "Marengo", "given_name": "Massimo", "orcid": "0000-0001-9910-9230", "clpid": "Marengo-Massimo" }, { "family_name": "Kirkpatrick", "given_name": "J. Davy", "orcid": "0000-0003-4269-260X", "clpid": "Kirkpatrick-J-Davy" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-Peter" }, { "family_name": "Kasliwal", "given_name": "Mansi", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Bauer", "given_name": "James M.", "clpid": "Bauer-James-M" }, { "family_name": "Minniti", "given_name": "Dante", "orcid": "0000-0002-7064-099X", "clpid": "Minniti-Dante" }, { "family_name": "Bally", "given_name": "John", "orcid": "0000-0001-8135-6612", "clpid": "Bally-John" }, { "family_name": "Lodieu", "given_name": "Nicolas", "clpid": "Lodieu-Nicolas" }, { "family_name": "Bowler", "given_name": "Brendan", "orcid": "0000-0003-2649-2288", "clpid": "Bowler-Brendan-P" }, { "family_name": "Zhang", "given_name": "ZengHua", "clpid": "Zhang-ZengHua" }, { "family_name": "Carey", "given_name": "Sean J.", "orcid": "0000-0002-0221-6871", "clpid": "Carey-Sean-J" }, { "family_name": "Milam", "given_name": "Stefanie", "orcid": "0000-0001-7694-4129", "clpid": "Milam-Stefanie-N" }, { "family_name": "Holler", "given_name": "Bryan", "clpid": "Holler-Bryan-J" } ], "abstract": "WFIRST will be capable of providing Hubble-quality imaging performance over several thousand square degrees of the sky. The wide-area, high spatial resolution survey data from WFIRST will be unsurpassed for many decades into the future. With the current baseline design, the WFIRST filter complement will extend from the bluest wavelength allowed by the optical design to a reddest filter (F184W) that has a red cutoff at 2.0 microns. In this white paper, we outline some of the science advantages for adding a K_s filter with a 2.15 micron central wavelength in order to extend the wavelength coverage for WFIRST as far to the red as the possible given the thermal performance of the observatory and the sensitivity of the detectors.", "doi": "10.48550/arXiv.1806.00554", "publisher": "arXiv", "publication_date": "2018-06-01" }, { "id": "authors:2d6nt-2j991", "collection": "authors", "collection_id": "2d6nt-2j991", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180904-161455265", "type": "monograph", "title": "WFIRST Science Investigation Team \"Cosmology with the High Latitude Survey\" Annual Report 2017", "author": [ { "family_name": "Dor\u00e9", "given_name": "Olivier", "orcid": "0000-0001-7432-2932", "clpid": "Dor\u00e9-O" }, { "family_name": "Hirata", "given_name": "Christopher", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Wang", "given_name": "Yun", "clpid": "Wang-Yun" }, { "family_name": "Weinberg", "given_name": "David", "clpid": "Weinberg-D" }, { "family_name": "Baronchelli", "given_name": "Ivano", "orcid": "0000-0003-0556-2929", "clpid": "Baronchelli-I" }, { "family_name": "Benson", "given_name": "Andrew", "orcid": "0000-0001-5501-6008", "clpid": "Benson-A-J" }, { "family_name": "Capak", "given_name": "Peter", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Choi", "given_name": "Ami", "clpid": "Choi-Ami" }, { "family_name": "Eifler", "given_name": "Tim", "orcid": "0000-0002-1894-3301", "clpid": "Eifler-T-F" }, { "family_name": "Hemmati", "given_name": "Shoubaneh", "orcid": "0000-0003-2226-5395", "clpid": "Hemmati-S" }, { "family_name": "Ho", "given_name": "Shirley", "clpid": "Ho-Shirley" }, { "family_name": "Izard", "given_name": "Albert", "clpid": "Izard-A" }, { "family_name": "Jain", "given_name": "Bhuvnesh", "clpid": "Jain-B" }, { "family_name": "Jarvis", "given_name": "Mike", "clpid": "Jarvis-M" }, { "family_name": "Kiessling", "given_name": "Alina", "clpid": "Kiessling-A" }, { "family_name": "Krause", "given_name": "Elisabeth", "clpid": "Krause-E" }, { "family_name": "Massara", "given_name": "Elena", "clpid": "Massara-E" }, { "family_name": "Masters", "given_name": "Dan", "orcid": "0000-0001-5382-6138", "clpid": "Masters-D-C" }, { "family_name": "Merson", "given_name": "Alex", "clpid": "Merson-A-I" }, { "family_name": "Miyatake", "given_name": "Hironao", "clpid": "Miyatake-Hironao" }, { "family_name": "Malagon", "given_name": "Andres Plazas", "clpid": "Malagon-A-P" }, { "family_name": "Mandelbaum", "given_name": "Rachel", "orcid": "0000-0003-2271-1527", "clpid": "Mandelbaum-R" }, { "family_name": "Samushia", "given_name": "Lado", "clpid": "Samushia-L" }, { "family_name": "Shapiro", "given_name": "Chaz", "clpid": "Shapiro-C" }, { "family_name": "Simet", "given_name": "Melanie", "clpid": "Simet-M" }, { "family_name": "Spergel", "given_name": "David", "orcid": "0000-0002-5151-0006", "clpid": "Spergel-D-N" }, { "family_name": "Teplitz", "given_name": "Harry", "orcid": "0000-0002-7064-5424", "clpid": "Teplitz-H-I" }, { "family_name": "Troxel", "given_name": "Michael", "clpid": "Troxel-M" }, { "family_name": "Bean", "given_name": "Rachel", "clpid": "Bean-R" }, { "family_name": "Colbert", "given_name": "James", "clpid": "Colbert-J-W" }, { "family_name": "Heinrich", "given_name": "Chen He", "clpid": "Heinrich-Chen-He" }, { "family_name": "Heitmann", "given_name": "Katrin", "clpid": "Heitmann-K" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Hudson", "given_name": "Michael", "clpid": "Hudson-M-J" }, { "family_name": "Huff", "given_name": "Eric", "orcid": "0000-0002-9378-3424", "clpid": "Huff-E-M" }, { "family_name": "Leauthaud", "given_name": "Alexie", "orcid": "0000-0002-3677-3617", "clpid": "Leauthaud-A" }, { "family_name": "MacCrann", "given_name": "Niall", "clpid": "MacCrann-N" }, { "family_name": "Padmanabhan", "given_name": "Nikhil", "clpid": "Padmanabhan-N" }, { "family_name": "Pisani", "given_name": "Alice", "clpid": "Pisani-A" }, { "family_name": "Rhodes", "given_name": "Jason", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Rozo", "given_name": "Eduardo", "clpid": "Rozo-E" }, { "family_name": "Seiffert", "given_name": "Mike", "clpid": "Seiffert-M" }, { "family_name": "Smith", "given_name": "Kendrick", "clpid": "Smith-Kendrick" }, { "family_name": "Takada", "given_name": "Masahiro", "clpid": "Takada-Masahiro" }, { "family_name": "von der Linden", "given_name": "Anja", "clpid": "von-der-Linden-A" }, { "family_name": "Lupton", "given_name": "Robert", "orcid": "0000-0003-1666-0962", "clpid": "Lupton-R-H" }, { "family_name": "Yoshida", "given_name": "Naoki", "clpid": "Yoshida-Naoki" }, { "family_name": "Wu", "given_name": "Hao-Yi", "clpid": "Wu-Hao-Yi" }, { "family_name": "Zu", "given_name": "Ying", "clpid": "Zu-Ying" } ], "abstract": "Cosmic acceleration is the most surprising cosmological discovery in many decades. Testing and distinguishing among possible explanations requires cosmological measurements of extremely high precision probing the full history of cosmic expansion and structure growth and, ideally, compare and contrast matter and relativistic tracers of the gravity potential. This program is one of the defining objectives of the Wide-Field Infrared Survey Telescope (WFIRST), as set forth in the New Worlds, New Horizons report (NWNH) in 2010. The WFIRST mission has the ability to improve these measurements by 1-2 orders of magnitude compared to the current state of the art, while simultaneously extending their redshift grasp, greatly improving control of systematic effects, and taking a unified approach to multiple probes that provide complementary physical information and cross-checks of cosmological results. We describe in this annual report the activities of the Science Investigation Team (SIT) \"Cosmology with the High Latitude Survey (HLS)\" during the year 2017. This team was selected by NASA in December 2015 in order to address the stringent challenges of the WFIRST dark energy (DE) program through the Project's formulation phase. This SIT has elected to jointly address Galaxy Redshift Survey, Weak Lensing and Cluster Growth and thus fully embrace the fact that the imaging and spectroscopic elements of the HLS will be realized as an integrated observing program, and they jointly impose requirements on performance and operations. WFIRST is designed to be able to deliver a definitive result on the origin of cosmic acceleration. It is not optimized for Figure of Merit sensitivity but for control of systematic uncertainties and for having multiple techniques each with multiple cross-checks. Our SIT work focuses on understanding the potential systematics in the WFIRST DE measurements.", "doi": "10.48550/arXiv.1804.03628", "publisher": "arXiv", "publication_date": "2018-04-10" }, { "id": "authors:gccxy-55773", "collection": "authors", "collection_id": "gccxy-55773", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150917-081449249", "type": "monograph", "title": "The Whole is Greater than the Sum of the Parts: Optimizing the Joint Science Return from LSST, Euclid and WFIRST", "author": [ { "family_name": "Jain", "given_name": "B.", "clpid": "Jain-B" }, { "family_name": "Spergel", "given_name": "D.", "orcid": "0000-0002-5151-0006", "clpid": "Spergel-D-N" }, { "family_name": "Bean", "given_name": "R.", "clpid": "Bean-R" }, { "family_name": "Connolly", "given_name": "A.", "clpid": "Connolly-A-J" }, { "family_name": "Dell'Antonio", "given_name": "I.", "clpid": "Dell'Antonio-I-P" }, { "family_name": "Frieman", "given_name": "J.", "clpid": "Frieman-J-A" }, { "family_name": "Gawiser", "given_name": "E.", "clpid": "Gawiser-E" }, { "family_name": "Gehrels", "given_name": "N.", "clpid": "Gehrels-N" }, { "family_name": "Gladney", "given_name": "L.", "clpid": "Gladney-L" }, { "family_name": "Heitmann", "given_name": "K.", "clpid": "Heitmann-K" }, { "family_name": "Helou", "given_name": "G.", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Ho", "given_name": "S.", "clpid": "Ho-S" }, { "family_name": "Ivezi\u0107", "given_name": "\u017d.", "orcid": "0000-0001-5250-2633", "clpid": "Ivezi\u0107-\u017d" }, { "family_name": "Jarvis", "given_name": "M.", "orcid": "0000-0001-7039-9078", "clpid": "Jarvis-M-J" }, { "family_name": "Kahn", "given_name": "S.", "clpid": "Kahn-S" }, { "family_name": "Kalirai", "given_name": "J.", "orcid": "0000-0001-9690-4159", "clpid": "Kalirai-J-S" }, { "family_name": "Kim", "given_name": "A.", "clpid": "Kim-A" }, { "family_name": "Lupton", "given_name": "R.", "clpid": "Lupton-R" }, { "family_name": "Mandelbaum", "given_name": "R.", "orcid": "0000-0003-2271-1527", "clpid": "Mandelbaum-R" }, { "family_name": "Marshall", "given_name": "P.", "clpid": "Marshall-P-J" }, { "family_name": "Newman", "given_name": "J. A.", "orcid": "0000-0001-8684-2222", "clpid": "Newman-J-A" }, { "family_name": "Perlmutter", "given_name": "S.", "clpid": "Perlmutter-S" }, { "family_name": "Postman", "given_name": "M.", "orcid": "0000-0002-9365-7989", "clpid": "Postman-Marc" }, { "family_name": "Rhodes", "given_name": "J.", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Strauss", "given_name": "M. A.", "clpid": "Straus-M-A" }, { "family_name": "Tyson", "given_name": "J. A.", "clpid": "Tyson-J-A" }, { "family_name": "Walkowicz", "given_name": "L.", "clpid": "Walkowics-L" }, { "family_name": "Wood-Vasey", "given_name": "W. M.", "clpid": "Wood-Vasey-W-M" } ], "abstract": "The focus of this report is on the opportunities enabled by the combination of LSST, Euclid and WFIRST, the optical surveys that will be an essential part of the next decade's astronomy. The sum of these surveys has the potential to be significantly greater than the contributions of the individual parts. As is detailed in this report, the combination of these surveys should give us multi-wavelength high-resolution images of galaxies and broadband data covering much of the stellar energy spectrum. These stellar and galactic data have the potential of yielding new insights into topics ranging from the formation history of the Milky Way to the mass of the neutrino. However, enabling the astronomy community to fully exploit this multi-instrument data set is a challenging technical task: for much of the science, we will need to combine the photometry across multiple wavelengths with varying spectral and spatial resolution. We identify some of the key science enabled by the combined surveys and the key technical challenges in achieving the synergies.", "doi": "10.48550/arXiv.1501.07897", "publication_date": "2015-02-19" }, { "id": "authors:haa3c-fxs78", "collection": "authors", "collection_id": "haa3c-fxs78", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-110407615", "type": "monograph", "title": "Wide-Field InfraRed Survey Telescope WFIRST Final Report", "author": [ { "family_name": "Green", "given_name": "J.", "clpid": "Green-J" }, { "family_name": "Hirata", "given_name": "C.", "orcid": "0000-0002-2951-4932", "clpid": "Hirata-C-M" }, { "family_name": "Hillenbrand", "given_name": "L.", "clpid": "Hillenbrand-L-A" }, { "family_name": "Helou", "given_name": "G.", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Cutri", "given_name": "R.", "orcid": "0000-0002-0077-2305", "clpid": "Cutri-R-M" } ], "abstract": "In December 2010, NASA created a Science Definition Team (SDT) for WFIRST, the Wide Field Infra-Red Survey Telescope, recommended by the Astro 2010 Decadal Survey as the highest priority for a large space mission. The SDT was chartered to work with the WFIRST Project Office at GSFC and the Program Office at JPL to produce a Design Reference Mission (DRM) for WFIRST. Part of the original charge was to produce an interim design reference mission by mid-2011. That document was delivered to NASA and widely circulated within the astronomical community. In late 2011 the Astrophysics Division augmented its original charge, asking for two design reference missions. The first of these, DRM1, was to be a finalized version of the interim DRM, reducing overall mission costs where possible. The second of these, DRM2, was to identify and eliminate capabilities that overlapped with those of NASA's James Webb Space Telescope (henceforth JWST), ESA's Euclid mission, and the NSF's ground-based Large Synoptic Survey Telescope (henceforth LSST), and again to reduce overall mission cost, while staying faithful to NWNH. This report presents both DRM1 and DRM2.", "doi": "10.48550/arXiv.1208.4012", "publisher": "NASA", "publication_date": "2012-08-20" }, { "id": "authors:2q184-ja103", "collection": "authors", "collection_id": "2q184-ja103", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150916-130227932", "type": "monograph", "title": "A complete view of galaxy evolution: panchromatic luminosity functions and the generation of metals", "author": [ { "family_name": "Blain", "given_name": "Andrew W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Bertoldi", "given_name": "Frank", "orcid": "0000-0002-1707-1775", "clpid": "Bertoldi-F" }, { "family_name": "Bock", "given_name": "James", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "Matt", "clpid": "Bradford-M-C" }, { "family_name": "Dowell", "given_name": "C. Darren", "clpid": "Dowell-C-D" }, { "family_name": "Glenn", "given_name": "Jason", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Goldsmith", "given_name": "Paul", "orcid": "0000-0002-6622-8396", "clpid": "Goldsmith-P-F" }, { "family_name": "Harwit", "given_name": "Martin", "clpid": "Harwit-M" }, { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Smith", "given_name": "J. D.", "orcid": "0000-0003-1545-5078", "clpid": "Smith-J-D-T" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Stacey", "given_name": "Gordon", "clpid": "Stacey-G-J" }, { "family_name": "Vieira", "given_name": "Joaquin", "clpid": "Vieira-J-D" }, { "family_name": "Yun", "given_name": "Min", "orcid": "0000-0001-7095-7543", "clpid": "Yun-Min-S" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "When and how did galaxies form and their metals accumulate? Over the last decade, this has moved from an archeological question to a live investigation: there is now a broad picture of the evolution of galaxies in dark matter halos: their masses, stars, metals and supermassive blackholes. Galaxies have been found and studied in which these formation processes are taking place most vigorously, all the way back in cosmic time to when the intergalactic medium (IGM) was still largely neutral. However, the details of how and why the interstellar medium (ISM) in\ndistant galaxies cools, is processed, recycled and enriched in metals by stars, and fuels active\ngalactic nuclei (AGNs) remain uncertain. In particular, the cooling of gas to fuel star formation,\nand the chemistry and physics of the most intensely active regions is hidden from view at optical\nwavelengths, but can be seen and diagnosed at mid- & far-infrared (IR) wavelengths. Rest-frame\nIR observations are important first to identify the most luminous, interesting and important\ngalaxies, secondly to quantify accurately their total luminosity, and finally to use spectroscopy to\ntrace the conditions in the molecular and atomic gas out of which stars form. In order to map out\nthese processes over the full range of environments and large-scale structures found in the\nuniverse - from the densest clusters of galaxies to the emptiest voids \u2013 we require tools for deep,\nlarge area surveys, of millions of galaxies out to z~5, and for detailed follow-up spectroscopy.\nThe necessary tools can be realized technically. Here, we outline the requirements for gathering\nthe crucial information to build, validate and challenge models of galaxy evolution.", "doi": "10.48550/arXiv.0903.1272", "publication_date": "2009-03-06" }, { "id": "authors:r8h40-05z40", "collection": "authors", "collection_id": "r8h40-05z40", "cite_using_url": "https://authors.library.caltech.edu/records/r8h40-05z40", "type": "monograph", "title": "IRAS Small Scale Structure Catalog", "author": [ { "family_name": "Helou", "given_name": "George", "orcid": "0000-0003-3367-3415", "clpid": "Helou-G" }, { "family_name": "Walker", "given_name": "D. W.", "clpid": "Walker-D-W" } ], "abstract": "

The primary mission of the Infrared Astronomical Satellite (IRAS) was to conduct a sensitive and unbiased survey of the sky in four wavelength bands at 12, 25, 60, and 100 μm. Launched in January 1983, IRAS ceased operations in November 1983 after having successfully surveyed 96% of the sky. The IRAS mission, the data processing, and the products are described in detail in the Explanatory Supplement to the IRAS Catalogs and Atlases (Vol. I of this series), with which the reader is assumed to be familiar.
References to chapters and sections in the Supplement are given here prefixed with Suppl., e.g., Suppl. I.A.

", "publisher": "Jet Propulsion Lab", "publication_date": "1983" } ]