[ { "id": "authors:ghaab-tfd31", "collection": "authors", "collection_id": "ghaab-tfd31", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190131-104830528", "type": "article", "title": "Constraints on the Thermal Contents of the X-Ray Cavities of Cluster MS 0735.6+7421 with Sunyaev\u2013Zel'dovich Effect Observations", "author": [ { "family_name": "Abdulla", "given_name": "Zubair", "orcid": "0000-0002-0664-7812", "clpid": "Abdulla-Zubair" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Mantz", "given_name": "Adam B.", "orcid": "0000-0002-8031-1217", "clpid": "Mantz-A-B" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Greer", "given_name": "Christopher H.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "O'Donnell", "given_name": "Christine", "clpid": "O'Donnell-Christine" }, { "family_name": "Plagge", "given_name": "Thomas J.", "clpid": "Plagge-T-J" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "Outbursts from active galactic nuclei (AGN) can inflate cavities in the intracluster medium (ICM) of galaxy clusters and are believed to play the primary role in offsetting radiative cooling in the ICM. However, the details of how the energy from AGN feedback thermalizes to heat the ICM is not well understood, partly due to the unknown composition and energetics of the cavities. The Sunyaev\u2013Zel'dovich (SZ) effect, a measure of the integrated pressure along the line of sight, provides a means of measuring the thermal contents of the cavities, to discriminate between thermal, nonthermal, and other sources of pressure support. Here we report measurements of the SZ effect at 30 GHz toward the galaxy cluster MS 0735.6+7421 (MS0735), using the Combined Array for Research in Millimeter-wave Astronomy (CARMA). MS0735 hosts the most energetic AGN outburst known and lobes of radio synchrotron emission coincident with a pair of giant X-ray cavities ~200 kpc across. Our CARMA maps show a clear deficit in the SZ signal coincident with the X-ray identified cavities, when compared to a smooth X-ray derived pressure model. We find that the cavities have very little SZ-contributing material, suggesting that they are either supported by very diffuse thermal plasma with temperature in excess of hundreds of keV, or are not supported thermally. Our results represent the first detection (with 4.4\u03c3 significance) of this phenomenon with the SZ effect.", "doi": "10.3847/1538-4357/aaf888", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2019-02-01", "series_number": "2", "volume": "871", "issue": "2", "pages": "Art. No. 195" }, { "id": "authors:38z9d-5cf64", "collection": "authors", "collection_id": "38z9d-5cf64", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161117-133957434", "type": "article", "title": "COPSS II: The Molecular Gas Content of Ten Million Cubic Megaparsecs at Redshift z ~ 3", "author": [ { "family_name": "Keating", "given_name": "Garrett K.", "clpid": "Keating-G-K" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Bower", "given_name": "Geoffrey C.", "orcid": "0000-0003-4056-9982", "clpid": "Bower-G-C" }, { "family_name": "Leitch", "given_name": "Erik", "clpid": "Leitch-E-M" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "DeBoer", "given_name": "David R.", "clpid": "DeBoer-D-R" } ], "abstract": "We present a measurement of the abundance of carbon monoxide in the early universe, utilizing the final results from the CO Power Spectrum Survey (COPSS). Between 2013 and 2015, we performed observations with the Sunyaev\u2013Zel'dovich Array to measure aggregate CO emission from z ~ 3 galaxies with the intensity mapping technique. Data were collected on 19 fields, covering an area of 0.7 square degrees, over the frequency range 27-35 GHz. With these data, along with data analyzed in COPSS I, we are able to observe the CO(1\u20130) transition within the redshift range z = 2.3-3.3 for spatial frequencies between k=0.5-10 h Mpc}^(-1), spanning a comoving volume of 4.9 x 10^6 h^(-3) Mpc^(-3). We present estimates of contributions from continuum sources and ground illumination within our measurement. We constrain the amplitude of the CO power spectrum to P_(CO) = 3.0_(-1.3)^(+1.3) x 10^3 \u00b5K^2 (h^(-1) Mpc)^3, or \u0394_(CO)^2 (k =1 h Mpc^(-1)) = 1.5_(-0.7}^(+0.7)} x 10^3 \u00b5K^2, at 68% confidence, and P_(CO) > 0 at 98.9% confidence. These results are a factor of 10 improvement in sensitivity compared to those of COPSS I. With this measurement, we constrain on the CO(1\u20130) galaxy luminosity function at z ~ 3. Assuming that CO emission is proportional to halo mass and using theoretical estimates of the scatter in this relationship, we constrain the ratio of CO(1-0) luminosity to halo mass to A_(CO) = 6.3_(-2.1)^(+1.4) x 10^(-7), L_\u2299M_\u2299^(-1). Assuming a Milky Way-like linear relationship between CO luminosity and molecular gas mass, we estimate a mass fraction of molecular gas of f_(H_2) = 5.5_(-2.2)^(+3.4) x 10^(-2) for halos with masses of ~10^(12) M_\u2299. Using theoretical estimates for the scaling of molecular gas mass fraction and halo mass, we estimate the cosmic molecular gas density to be \u03c1_(z ~ 3)(H_2) = 1.1_(-0.4)^(+0.7) x 10^8 M_\u2299 Mpc^(-3).", "doi": "10.3847/0004-637X/830/1/34", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2016-10-10", "series_number": "1", "volume": "830", "issue": "1", "pages": "Art. No. 34" }, { "id": "authors:4sj0z-69b93", "collection": "authors", "collection_id": "4sj0z-69b93", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160208-074401358", "type": "article", "title": "The CARMA Paired Antenna Calibration System: Atmospheric Phase Correction for Millimeter Wave Interferometry and its Application to Mapping the Ultraluminous Galaxy Arp 193", "author": [ { "family_name": "Zauderer", "given_name": "B. Ashley", "orcid": "0000-0003-1152-518X", "clpid": "Zauderer-B-A" }, { "family_name": "Bolatto", "given_name": "Alberto D.", "orcid": "0000-0002-5480-5686", "clpid": "Bolatto-A-D" }, { "family_name": "Vogel", "given_name": "Stuart N.", "clpid": "Vogel-S-N" }, { "family_name": "Carpenter", "given_name": "John M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "P\u00e9rez", "given_name": "Laura M.", "orcid": "0000-0002-1199-9564", "clpid": "P\u00e9rez-L-M" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Woody", "given_name": "David P.", "clpid": "Woody-D-P" }, { "family_name": "Bock", "given_name": "Douglas C.-J.", "clpid": "Bock-D-C-J" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas L.", "clpid": "Culverhouse-T-L" }, { "family_name": "Curley", "given_name": "Roger", "clpid": "Curley-R" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Plambeck", "given_name": "Richard L.", "clpid": "Plambeck-R-L" }, { "family_name": "Pound", "given_name": "Marc W.", "clpid": "Pound-M-W" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Muchovej", "given_name": "Stephen J.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Mundy", "given_name": "Lee G.", "clpid": "Mundy-L-G" }, { "family_name": "Teng", "given_name": "Stacy H.", "clpid": "Teng-Stacy-H" }, { "family_name": "Teuben", "given_name": "Peter J.", "clpid": "Teuben-P-J" }, { "family_name": "Volgenau", "given_name": "Nikolaus H.", "clpid": "Volgenau-N-H" }, { "family_name": "Wright", "given_name": "Melvyn C. H.", "clpid": "Wright-M-C-H" }, { "family_name": "Wu", "given_name": "Dalton", "clpid": "Wu-Dalton" } ], "abstract": "Phase fluctuations introduced by the atmosphere are the main limiting factor in attaining diffraction limited performance in extended interferometric arrays at millimeter and submillimeter wavelengths. We report the results of C-PACS, the Combined Array for Research in Millimeter-Wave Astronomy Paired Antenna Calibration System. We present a systematic study of several hundred test observations taken during the 2009\u20132010 winter observing season where we utilize CARMA's eight 3.5 m antennas to monitor an atmospheric calibrator while simultaneously acquiring science observations with 6.1 and 10.4 m antennas on baselines ranging from a few hundred meters to ~2 km. We find that C-PACS is systematically successful at improving coherence on long baselines under a variety of atmospheric conditions. We find that the angular separation between the atmospheric calibrator and target source is the most important consideration, with consistently successful phase correction at CARMA requiring a suitable calibrator located \u227e6\u00b0 away from the science target. We show that cloud cover does not affect the success of C-PACS. We demonstrate C-PACS in typical use by applying it to the observations of the nearby very luminous infrared galaxy Arp 193 in ^(12)CO(2-1) at a linear resolution of \u224870 pc (0\".12 \u00d7 0\".18), 3 times better than previously published molecular maps of this galaxy. We resolve the molecular disk rotation kinematics and the molecular gas distribution and measure the gas surface densities and masses on 90 pc scales. We find that molecular gas constitutes ~30% of the dynamical mass in the inner 700 pc of this object with a surface density ~10^4 M_\u2299 pc^(\u22122); we compare these properties to those of the starburst region of NGC 253.", "doi": "10.3847/0004-6256/151/1/18", "issn": "1538-3881", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "2016-01", "series_number": "1", "volume": "151", "issue": "1", "pages": "Art. No. 18" }, { "id": "authors:2vbv2-kq332", "collection": "authors", "collection_id": "2vbv2-kq332", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160324-112710383", "type": "article", "title": "First Results from COPSS: The CO Power Spectrum Survey", "author": [ { "family_name": "Keating", "given_name": "Garrett K.", "clpid": "Keating-G-K" }, { "family_name": "Bower", "given_name": "Geoffrey C.", "orcid": "0000-0003-4056-9982", "clpid": "Bower-G-C" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "DeBoer", "given_name": "David R.", "clpid": "DeBoer-D-R" }, { "family_name": "Heiles", "given_name": "Carl", "clpid": "Heiles-C" }, { "family_name": "Chang", "given_name": "Tzu-Ching", "clpid": "Chang-Tzu-Ching" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Greer", "given_name": "Christopher H.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "Erik", "clpid": "Leitch-E-M" }, { "family_name": "Miller", "given_name": "Amber D.", "clpid": "Miller-A-D" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Woody", "given_name": "David P.", "clpid": "Woody-D-P" } ], "abstract": "We present constraints on the abundance of carbon monoxide in the early universe from the CO Power Spectrum Survey. We utilize a data set collected between 2005 and 2008 using the Sunyaev\u2013Zel'dovich Array (SZA), which was previously used to measure arcminute-scale fluctuations of the cosmic microwave background. This data set features observations of 44 fields, covering an effective area of 1.7 square degrees, over a frequency range of 27\u201335 GHz. Using the technique of intensity mapping, we are able to probe the CO(1\u20130) transition, with sensitivity to spatial modes between k = 0.5\u20132 h Mpc^(\u22121) over a range in redshift of z = 2.3\u20133.3, spanning a comoving volume of 3.6 \u00d7 10^6 h^(\u22123) Mpc^3. We demonstrate our ability to mitigate foregrounds, and present estimates of the impact of continuum sources on our measurement. We constrain the CO power spectrum to P_(CO) < 2.6 \u00d7 10^4 \u03bcK^2 (h^(\u22121) Mpc)^3, or \u0394^2_(CO)(k = 1 h Mpc^(\u22121)) < 1.3 \u00d7 10^3 \u03bcK^2, at 95% confidence. This limit resides near optimistic predictions for the CO power spectrum. Under the assumption that CO emission is proportional to halo mass during bursts of active star formation, this corresponds to a limit on the ratio of CO(1\u20130) luminosity to host halo mass of A_(CO) < 1.2 \u00d7 10^(\u22125) L\u2299_ M_\u2299^(\u22121). Further assuming a Milky Way-like conversion factor between CO luminosity and molecular gas mass (\u03b1_(CO) = 4.3 M_\u2299 (K km s^(\u22121) pc^(\u22122))^(\u22121)), we constrain the global density of molecular gas to \u03c1_(z~3) (M_H_2) \u2a7d 2.8 x 10^8 M_\u2609 Mpc^(-3).", "doi": "10.1088/0004-637X/814/2/140", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-12-01", "series_number": "2", "volume": "814", "issue": "2", "pages": "Art. No. 140" }, { "id": "authors:bhsjd-3qk47", "collection": "authors", "collection_id": "bhsjd-3qk47", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160105-143458920", "type": "article", "title": "A Multi-wavelength Mass Analysis of RCS2 J232727.6-020437, A ~3 \u00d7 10^(15) M_\u2299 Galaxy Cluster at z = 0.7", "author": [ { "family_name": "Sharon", "given_name": "K.", "clpid": "Sharon-K" }, { "family_name": "Gladders", "given_name": "M. D.", "clpid": "Gladders-M-D" }, { "family_name": "Marrone", "given_name": "D. P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Hoekstra", "given_name": "H.", "clpid": "Hoekstra-H" }, { "family_name": "Rasia", "given_name": "E.", "orcid": "0000-0003-4175-002X", "clpid": "Rasia-E" }, { "family_name": "Bourdin", "given_name": "H.", "clpid": "Bourdin-H" }, { "family_name": "Gifford", "given_name": "D.", "clpid": "Gifford-D" }, { "family_name": "Hicks", "given_name": "A. K.", "clpid": "Hicks-A-K" }, { "family_name": "Greer", "given_name": "C.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Mroczkowski", "given_name": "T.", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Barrientos", "given_name": "L. F.", "clpid": "Barrientos-L-F" }, { "family_name": "Bayliss", "given_name": "M.", "clpid": "Bayliss-M-B" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Gilbank", "given_name": "D. G.", "clpid": "Gilbank-D-G" }, { "family_name": "Gralla", "given_name": "M.", "clpid": "Gralla-M-B" }, { "family_name": "Hlavacek-Larrondo", "given_name": "J.", "orcid": "0000-0001-7271-7340", "clpid": "Hlavacek-Larrondo-J" }, { "family_name": "Leitch", "given_name": "E.", "clpid": "Leitch-E" }, { "family_name": "Mazzotta", "given_name": "P.", "orcid": "0000-0002-5411-1748", "clpid": "Mazzotta-P" }, { "family_name": "Miller", "given_name": "C.", "clpid": "Miller-C" }, { "family_name": "Muchovej", "given_name": "S. J. C.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Schrabback", "given_name": "T.", "clpid": "Schrabback-T" }, { "family_name": "Yee", "given_name": "H. K. C.", "clpid": "Yee-H-K-C" }, { "literal": "RCS Team" } ], "abstract": "We present an initial study of the mass and evolutionary state of a massive and distant cluster, RCS2 J232727.6-020437. This cluster, at z = 0.6986, is the richest cluster discovered in the RCS2 project. The mass measurements presented in this paper are derived from all possible mass proxies: X-ray measurements, weak-lensing shear, strong lensing, Sunyaev\u2013Zel'dovich effect decrement, the velocity distribution of cluster member galaxies, and galaxy richness. While each of these observables probe the mass of the cluster at a different radius, they all indicate that RCS2 J232727.6\u2212020437 is among the most massive clusters at this redshift, with an estimated mass of M_(200) ~ 3 x 10^(15)h_(70)^(-1) M_\u2609. In this paper, we demonstrate that the various observables are all reasonably consistent with each other to within their uncertainties. RCS2 J232727.6\u2212020437 appears to be well relaxed\u2014with circular and concentric X-ray isophotes, with a cool core, and no indication of significant substructure in extensive galaxy velocity data.", "doi": "10.1088/0004-637X/814/1/21", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-11-20", "series_number": "1", "volume": "814", "issue": "1", "pages": "Art. No. 21" }, { "id": "authors:cv9vc-qs738", "collection": "authors", "collection_id": "cv9vc-qs738", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160105-135322956", "type": "article", "title": "The Massive and Distant Clusters of WISE Survey: MOO J1142+1527, a 10^(15) M_\u2299 Galaxy Cluster at z = 1.19", "author": [ { "family_name": "Gonzalez", "given_name": "Anthony H.", "orcid": "0000-0002-0933-8601", "clpid": "Gonzalez-A-H" }, { "family_name": "Decker", "given_name": "Bandon", "clpid": "Decker-Bandon" }, { "family_name": "Brodwin", "given_name": "Mark", "orcid": "0000-0002-4208-798X", "clpid": "Brodwin-M" }, { "family_name": "Eisenhardt", "given_name": "Peter R. M.", "clpid": "Eisenhardt-P-R-M" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Stanford", "given_name": "S. A.", "clpid": "Stanford-S-A" }, { "family_name": "Stern", "given_name": "Daniel", "orcid": "0000-0003-2686-9241", "clpid": "Stern-D" }, { "family_name": "Wylezalek", "given_name": "Dominika", "orcid": "0000-0003-2212-6045", "clpid": "Wylezalek-D" }, { "family_name": "Aldering", "given_name": "Greg", "clpid": "Aldering-Greg-S" }, { "family_name": "Abdulla", "given_name": "Zubair", "orcid": "0000-0002-0664-7812", "clpid": "Abdulla-Zubair" }, { "family_name": "Boone", "given_name": "Kyle", "clpid": "Boone-Kyle" }, { "family_name": "Carlstrom", "given_name": "John", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Fagrelius", "given_name": "Parker", "clpid": "Fagrelius-Parker" }, { "family_name": "Gettings", "given_name": "Daniel P.", "clpid": "Gettings-D-P" }, { "family_name": "Greer", "given_name": "Christopher H.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Hayden", "given_name": "Brian", "clpid": "Hayden-Brian" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Lin", "given_name": "Yen-Ting", "clpid": "Lin-Yen-Ting" }, { "family_name": "Mantz", "given_name": "Adam B.", "orcid": "0000-0002-8031-1217", "clpid": "Mantz-A-B" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Perlmutter", "given_name": "Saul", "clpid": "Perlmutter-Saul" }, { "family_name": "Zeimann", "given_name": "Gregory R.", "clpid": "Zeimann-G-R" } ], "abstract": "We present confirmation of the cluster MOO J1142+1527, a massive galaxy cluster discovered as part of the Massive and Distant Clusters of WISE Survey. The cluster is confirmed to lie at z = 1.19, and using the Combined Array for Research in Millimeter-wave Astronomy we robustly detect the Sunyaev\u2013Zel'dovich (SZ) decrement at 13.2\u03c3. The SZ data imply a mass of M_(200m) = (1.1 \u00b1 0.2) \u00d7 10^(15)M_\u2299, making MOO J1142+1527 the most massive galaxy cluster known at z > 1.15 and the second most massive cluster known at z > 1. For a standard \u039bCDM cosmology it is further expected to be one of the ~5 most massive clusters expected to exist at z \u2265 1.19 over the entire sky. Our ongoing Spitzer program targeting ~1750 additional candidate clusters will identify comparably rich galaxy clusters over the full extragalactic sky.", "doi": "10.1088/2041-8205/812/2/L40", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2015-10-20", "series_number": "2", "volume": "812", "issue": "2", "pages": "L40" }, { "id": "authors:xkx5c-8tk34", "collection": "authors", "collection_id": "xkx5c-8tk34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141113-155029950", "type": "article", "title": "The XXL Survey. V. Detection of the Sunyaev-Zel'dovich Effect of the Redshift 1.9 Galaxy Cluster XLSSU J021744.1\u2013034536 with CARMA", "author": [ { "family_name": "Mantz", "given_name": "A. B.", "orcid": "0000-0002-8031-1217", "clpid": "Mantz-A-B" }, { "family_name": "Abdulla", "given_name": "Z.", "orcid": "0000-0002-0664-7812", "clpid": "Abdulla-Zubair" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Greer", "given_name": "C. H.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "Marrone", "given_name": "D. P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Muchovej", "given_name": "S.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Adami", "given_name": "C.", "clpid": "Adami-Christophe-ASTRO-FR" }, { "family_name": "Birkinshaw", "given_name": "M.", "clpid": "Birkinshaw-M" }, { "family_name": "Bremer", "given_name": "M.", "clpid": "Bremer-M" }, { "family_name": "Clerc", "given_name": "N.", "clpid": "Clerc-N" }, { "family_name": "Giles", "given_name": "P.", "clpid": "Giles-P" } ], "abstract": "We report the detection of the Sunyaev-Zel'dovich (SZ) effect of galaxy cluster XLSSU J021744.1\u2013034536, using 30 GHz Combined Array for Research in Millimeter-wave Astronomy (CARMA) data. This cluster was discovered via its extended X-ray emission in the XMM- Newton Large Scale Structure survey, the precursor to the XXL survey. It has a photometrically determined redshift z = 1.91^(+0.19)_(-0.21), making it among the most distant clusters known, and nominally the most distant for which the SZ effect has been measured. The spherically integrated Comptonization is Y _500 = (3.0 \u00b1 0.4) \u00d7 10^(\u201312), a measurement that is relatively insensitive to assumptions regarding the size and redshift of the cluster, as well as the background cosmology. Using a variety of locally calibrated cluster scaling relations extrapolated to z ~ 2, we estimate a mass M _500 ~ (1-2) \u00d7 10^(14) M \u2609 from the X-ray flux and SZ signal. The measured properties of this cluster are in good agreement with the extrapolation of an X-ray luminosity-SZ effect scaling relation calibrated from clusters discovered by the South Pole Telescope at higher masses and lower redshifts. The full XXL-CARMA sample will provide a more complete, multi-wavelength census of distant clusters in order to robustly extend the calibration of cluster scaling relations to these high redshifts.", "doi": "10.1088/0004-637X/794/2/157", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2014-10-20", "series_number": "2", "volume": "794", "issue": "2", "pages": "Art. No. 157" }, { "id": "authors:v64cj-s2p68", "collection": "authors", "collection_id": "v64cj-s2p68", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130722-103105691", "type": "article", "title": "CARMA Measurements of the Sunyaev-Zel'dovich Effect in RX J1347.5\u20131145", "author": [ { "family_name": "Plagge", "given_name": "Thomas J.", "clpid": "Plagge-T-J" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Abdulla", "given_name": "Zubair", "orcid": "0000-0002-0664-7812", "clpid": "Abdulla-Zubair" }, { "family_name": "Bonamente", "given_name": "Massimiliano", "clpid": "Bonamente-M" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Gralla", "given_name": "Megan", "clpid": "Gralla-M" }, { "family_name": "Greer", "given_name": "Christopher H.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Mantz", "given_name": "Adam", "clpid": "Mantz-A" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We demonstrate the Sunyaev-Zel'dovich (SZ) effect imaging capabilities of the Combined Array for Research in Millimeter-wave Astronomy (CARMA) by presenting an SZ map of the galaxy cluster RX J1347.5\u20131145. By combining data from multiple CARMA bands and configurations, we are able to capture the structure of this cluster over a wide range of angular scales, from its bulk properties to its core morphology. We find that roughly 9% of this cluster's thermal energy is associated with sub-arcminute-scale structure imparted by a merger, illustrating the value of high-resolution SZ measurements for pursuing cluster astrophysics and for understanding the scatter in SZ scaling relations. We also find that the cluster's SZ signal is lower in amplitude than suggested by a spherically symmetric model derived from X-ray data, consistent with compression along the line of sight relative to the plane of the sky. Finally, we discuss the impact of upgrades currently in progress that will further enhance CARMA's power as an SZ imaging instrument.", "doi": "10.1088/0004-637X/770/2/112", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2013-06-20", "series_number": "2", "volume": "770", "issue": "2", "pages": "Art. No. 112" }, { "id": "authors:dkr2d-rda13", "collection": "authors", "collection_id": "dkr2d-rda13", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120831-101945253", "type": "article", "title": "LoCuSS: The Sunyaev\u2013Zel'dovich Effect and Weak-lensing Mass Scaling Relation", "author": [ { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Smith", "given_name": "Graham P.", "orcid": "0000-0003-4494-8277", "clpid": "Smith-Graham-P" }, { "family_name": "Okabe", "given_name": "Nobuhiro", "clpid": "Okabe-Nobuhiro" }, { "family_name": "Bonamente", "given_name": "Massimiliano", "clpid": "Bonamente-M" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas L.", "clpid": "Culverhouse-T-L" }, { "family_name": "Gralla", "given_name": "Megan", "clpid": "Gralla-M-B" }, { "family_name": "Greer", "given_name": "Christopher H.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Hasler", "given_name": "Nicole", "clpid": "Hasler-N" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M-K" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Martino", "given_name": "Rosella", "clpid": "Martino-R" }, { "family_name": "Mazzotta", "given_name": "Pasquale", "orcid": "0000-0002-5411-1748", "clpid": "Mazzotta-P" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A-D" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Plagge", "given_name": "Thomas", "clpid": "Plagge-T-J" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Sanderson", "given_name": "Alastair J. R.", "clpid": "Sanderson-A-J-R" }, { "family_name": "Takada", "given_name": "Masahiro", "clpid": "Takada-Masahiro" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" }, { "family_name": "Zhang", "given_name": "Yuying", "clpid": "Zhang-Yuying" } ], "abstract": "We present the first weak-lensing-based scaling relation between galaxy cluster mass, M_WL, and integrated Compton parameter Y_sph. Observations of 18 galaxy clusters at z \u2243 0.2 were obtained with the Subaru 8.2 m telescope and the Sunyaev-Zel'dovich Array. The M_(WL)-Y_(sph) scaling relations, measured at \u0394 = 500, 1000, and 2500 \u03c1_c , are consistent in slope and normalization with previous results derived under the assumption of hydrostatic equilibrium (HSE). We find an intrinsic scatter in M_WL at fixed Y_sph of 20%, larger than both previous measurements of M_(HSE)-Y_(sph) scatter as well as the scatter in true mass at fixed Y_sph found in simulations. Moreover, the scatter in our lensing-based scaling relations is morphology dependent, with 30%-40% larger M_WL for undisturbed compared to disturbed clusters at the same Y_sph at r_500. Further examination suggests that the segregation may be explained by the inability of our spherical lens models to faithfully describe the three-dimensional structure of the clusters, in particular, the structure along the line of sight. We find that the ellipticity of the brightest cluster galaxy, a proxy for halo orientation, correlates well with the offset in mass from the mean scaling relation, which supports this picture. This provides empirical evidence that line-of-sight projection effects are an important systematic uncertainty in lensing-based scaling relations.", "doi": "10.1088/0004-637X/754/2/119", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-08-01", "series_number": "2", "volume": "754", "issue": "2", "pages": "Art. No. 119" }, { "id": "authors:1deq1-3hb06", "collection": "authors", "collection_id": "1deq1-3hb06", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120508-095414829", "type": "article", "title": "Joint Analysis of X-Ray and Sunyaev-Zel'dovich Observations of Galaxy Clusters Using an Analytic Model of the Intracluster Medium", "author": [ { "family_name": "Hasler", "given_name": "Nicole", "clpid": "Hasler-N" }, { "family_name": "Bulbul", "given_name": "Esra", "clpid": "Bulbul-E" }, { "family_name": "Bonamente", "given_name": "Massimiliano", "clpid": "Bonamente-M" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas L.", "clpid": "Culverhouse-T-L" }, { "family_name": "Gralla", "given_name": "Megan", "clpid": "Gralla-M" }, { "family_name": "Greer", "given_name": "Christopher", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Kolodziejczak", "given_name": "Jeffrey", "clpid": "Kolodziejczak-J" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Landry", "given_name": "David", "clpid": "Landy-D" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Mantz", "given_name": "Adam", "clpid": "Mantz-A" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Plagge", "given_name": "Thomas", "clpid": "Plagge-T" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We perform a joint analysis of X-ray and Sunyaev-Zel'dovich effect data using an analytic model that describes the gas properties of galaxy clusters. The joint analysis allows the measurement of the cluster gas mass fraction profile and Hubble constant independent of cosmological parameters. Weak cosmological priors are used to calculate the overdensity radius within which the gas mass fractions are reported. Such an analysis can provide direct constraints on the evolution of the cluster gas mass fraction with redshift. We validate the model and the joint analysis on high signal-to-noise data from the Chandra X-ray Observatory and the Sunyaev-Zel'dovich Array for two clusters, A2631 and A2204.", "doi": "10.1088/0004-637X/748/2/113", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-04-01", "series_number": "2", "volume": "748", "issue": "2", "pages": "Art. No. 113" }, { "id": "authors:gkk5n-xds90", "collection": "authors", "collection_id": "gkk5n-xds90", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120501-092742062", "type": "article", "title": "Comparison of pressure profiles of massive relaxed\n galaxy clusters using the Sunyaev\u2013Zel'dovich and\n x-ray data", "author": [ { "family_name": "Bonamente", "given_name": "Massimiliano", "clpid": "Bonamente-M" }, { "family_name": "Hasler", "given_name": "Nicole", "clpid": "Hasler-N" }, { "family_name": "Bulbul", "given_name": "Esra", "clpid": "Bulbul-E" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas L.", "clpid": "Culverhouse-T-L" }, { "family_name": "Gralla", "given_name": "Megan", "clpid": "Gralla-M" }, { "family_name": "Greer", "given_name": "Christopher", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Kolodziejczak", "given_name": "Jeffrey", "clpid": "Kolodziejczak-J" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Landry", "given_name": "David", "clpid": "Landy-D" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Plagge", "given_name": "Thomas", "clpid": "Plagge-T" }, { "family_name": "Sharp", "given_name": "Matthew", "clpid": "Sharp-M" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We present the Sunyaev\u2013Zel'dovich (SZ) effect observations of a sample of 25 massive relaxed galaxy clusters observed with the Sunyaev\u2013Zel'dovich array (SZA), an eight-element interferometer that is part of the Combined Array for Research in Millimeter-wave Astronomy (CARMA). We performed an analysis of new SZA data and archival Chandra observations of this sample to investigate the integrated pressure\u2014a proxy for cluster mass\u2014determined from x-ray and SZ observations, two independent probes of the intra-cluster medium (ICM). This analysis makes use of a model for the ICM introduced by Bulbul (2010 Astrophys. J. 720 1038) which can be applied simultaneously to the SZ and x-ray data. With this model, we estimated the pressure profile for each cluster using a joint analysis of the SZ and x-ray data, and using the SZ data alone. We found that the integrated pressures measured from the x-ray and SZ data are consistent. This conclusion is in agreement with recent results obtained using WMAP and Planck data, confirming that SZ and x-ray observations of massive clusters detect the same amount of thermal pressure from the ICM. To test for possible biases introduced by our choice of model, we also fitted the SZ data using the universal pressure profile proposed by Arnaud (2010 Astron. Astrophys. 517 A92) and found consistency between the two models out to r_(500) in the pressure profiles and integrated pressures.", "doi": "10.1088/1367-2630/14/2/025010", "issn": "1367-2630", "publisher": "IOP", "publication": "New Journal of Physics", "publication_date": "2012-02-29", "volume": "14", "pages": "Art. No. 025010" }, { "id": "authors:grsnz-pcm61", "collection": "authors", "collection_id": "grsnz-pcm61", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110429-111613223", "type": "article", "title": "Cosmological Constraints from a 31 GHz Sky Survey with the Sunyaev-Zel'dovich Array", "author": [ { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Leitch", "given_name": "Erik", "clpid": "Leitch-E" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas", "clpid": "Culverhouse-T" }, { "family_name": "Greer", "given_name": "Chris", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Lamb", "given_name": "James", "clpid": "Lamb-J" }, { "family_name": "Loh", "given_name": "Michael", "clpid": "Loh-M" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Sharp", "given_name": "Matthew", "clpid": "Sharp-M" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We present the results of an analysis of 4.4 deg^2 selected from a 6.1 deg^2 survey for clusters of galaxies via their Sunyaev-Zel'dovich effect at 31 GHz. From late 2005 to mid 2007, the Sunyaev-Zel'dovich Array observed four fields of roughly 1.5 deg^2 each. One of the fields shows evidence for significant diffuse Galactic emission, and is therefore excised from this analysis. We estimate the cluster detectability for the survey using mock observations of simulations of clusters of galaxies and determine that, at intermediate redshifts (z ~ 0.8), the survey is 50% complete to a limiting mass (M_(200\u03c1[overbar]) of ~6.0 \u00d7 10^(14) M_\u2299, with the mass limit decreasing at higher redshifts. We detect no clusters at a significance greater than five times the rms noise level in the maps, and place an upper limit on \u03c3_8, the amplitude of mass density fluctuations on a scale of 8 h^(-1) Mpc, of 0.84 + 0.04 + 0.04 at 95% confidence, where the first uncertainty reflects an estimate of additional sample variance due to non-Gaussianity in the distribution of clusters and the second reflects calibration and systematic effects. This result is consistent with estimates from other cluster surveys and cosmic microwave background anisotropy experiments.", "doi": "10.1088/0004-637X/732/1/28", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2011-05-01", "series_number": "1", "volume": "732", "issue": "1", "pages": "Art. No. 28" }, { "id": "authors:2nca9-qhq20", "collection": "authors", "collection_id": "2nca9-qhq20", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101215-141057173", "type": "article", "title": "Atmospheric phase correction using CARMA-PACS: high angular resolution observations of the FU Orionis star PP 13S*", "author": [ { "family_name": "P\u00e9rez", "given_name": "Laura M.", "orcid": "0000-0002-1199-9564", "clpid": "P\u00e9rez-L-M" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Woody", "given_name": "David P.", "clpid": "Woody-D-P" }, { "family_name": "Carpenter", "given_name": "John M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Zauderer", "given_name": "B. Ashley", "orcid": "0000-0003-1152-518X", "clpid": "Zauderer-B-A" }, { "family_name": "Isella", "given_name": "Andrea", "orcid": "0000-0001-8061-2207", "clpid": "Isella-A" }, { "family_name": "Bock", "given_name": "Douglas C.", "clpid": "Bock-D-C-J" }, { "family_name": "Bolatto", "given_name": "Alberto D.", "orcid": "0000-0002-5480-5686", "clpid": "Bolatto-A-D" }, { "family_name": "Carlstrom", "given_name": "John", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas L.", "clpid": "Culverhouse-T-L" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Kwon", "given_name": "Woojin", "clpid": "Kwon-Woojin" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Muchovej", "given_name": "Stephen J.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Plambeck", "given_name": "Richard L.", "clpid": "Plambeck-R-L" }, { "family_name": "Scott", "given_name": "Stephen L.", "clpid": "Scott-S-L" }, { "family_name": "Teuben", "given_name": "Peter J.", "clpid": "Teuben-P-J" }, { "family_name": "Wright", "given_name": "Melvyn C. H.", "clpid": "Wright-M-C-H" } ], "abstract": "We present 0\".15 resolution observations of the 227 GHz continuum emission from the circumstellar disk around\nthe FU Orionis star PP 13S*. The data were obtained with the Combined Array for Research in Millimeter-wave\nAstronomy (CARMA) Paired Antenna Calibration System (C-PACS), which measures and corrects the atmospheric\ndelay fluctuations on the longest baselines of the array in order to improve the sensitivity and angular resolution of\nthe observations. A description of the C-PACS technique and the data reduction procedures are presented. C-PACS\nwas applied to CARMA observations of PP 13S*, which led to a factor of 1.6 increase in the observed peak flux\nof the source, a 36% reduction in the noise of the image, and a 52% decrease in the measured size of the source\nmajor axis. The calibrated complex visibilities were fitted with a theoretical disk model to constrain the disk surface\ndensity. The total disk mass from the best-fit model corresponds to 0.06 M_\u2299, which is larger than the median mass of a disk around a classical T Tauri star. The disk is optically thick at a wavelength of 1.3 mm for orbital radii less than 48 AU. At larger radii, the inferred surface density of the PP 13S* disk is an order of magnitude lower than that needed to develop a gravitational instability.", "doi": "10.1088/0004-637X/724/1/493", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-11-20", "series_number": "1", "volume": "724", "issue": "1", "pages": "493-501" }, { "id": "authors:e9dbz-6mn14", "collection": "authors", "collection_id": "e9dbz-6mn14", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20101206-092457615", "type": "article", "title": "Galaxy Clusters at z \u2265 1: Gas Constraints from the Sunyaev\u2013Zel'dovich Array", "author": [ { "family_name": "Culverhouse", "given_name": "T. L.", "clpid": "Culverhouse-T-L" }, { "family_name": "Bonamente", "given_name": "M.", "clpid": "Bonamente-M" }, { "family_name": "Bulbul", "given_name": "E.", "clpid": "Bulbul-E" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Gralla", "given_name": "M. B.", "clpid": "Gralla-M-B" }, { "family_name": "Greer", "given_name": "C.", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Hasler", "given_name": "N.", "clpid": "Hasler-N" }, { "family_name": "Hawkins", "given_name": "D.", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "R.", "clpid": "Hennessy-R" }, { "family_name": "Jetha", "given_name": "N. N.", "clpid": "Jetha-N-N" }, { "family_name": "Joy", "given_name": "M.", "clpid": "Joy-M" }, { "family_name": "Lamb", "given_name": "J. W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "Marrone", "given_name": "D. P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Miller", "given_name": "A.", "clpid": "Miller-A" }, { "family_name": "Mroczkowski", "given_name": "T.", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Muchovej", "given_name": "S.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Pryke", "given_name": "C.", "clpid": "Pryke-C" }, { "family_name": "Sharp", "given_name": "M.", "clpid": "Sharp-M" }, { "family_name": "Woody", "given_name": "D. P.", "clpid": "Woody-D-P" }, { "family_name": "Andreon", "given_name": "S.", "clpid": "Andreon-S" }, { "family_name": "Maughan", "given_name": "B.", "clpid": "Maughan-B" }, { "family_name": "Stanford", "given_name": "S. A.", "clpid": "Stanford-S-A" } ], "abstract": "We present gas constraints from Sunyaev-Zel'dovich (SZ) effect measurements in a sample of 11 X-ray and infrared (IR) selected galaxy clusters at z \u2265 1, using data from the Sunyaev-Zel'dovich Array (SZA). The cylindrically integrated Compton-y parameter, Y, is calculated by fitting the data to a two-parameter gas pressure profile. Where possible, we also determine the temperature of the hot intracluster plasma from Chandra and XMM-Newton data and constrain the gas mass within the same aperture (r_(2500)) as Y. The SZ effect is detected in the clusters for which the X-ray data indicate gas masses above ~10^(13) M _\u2299, including XMMU J2235 \u2013 2557 at redshift z = 1.39, which to date is one of the most distant clusters detected using the SZ effect. None of the IR-selected targets are detected by the SZA measurements, indicating low gas masses for these objects. For these and the four other undetected clusters, we quote upper limits on Y and M_(gas,SZ), with the latter derived from scaling relations calibrated with lower redshift clusters. We compare the constraints on Y and X-ray-derived gas mass M_(gas,X-ray) to self-similar scaling relations between these observables determined from observations of lower redshift clusters, finding consistency given the measurement error.", "doi": "10.1088/2041-8205/723/1/L78", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "2010-11-01", "series_number": "1", "volume": "723", "issue": "1", "pages": "L78-L83" }, { "id": "authors:2v6h4-vpc33", "collection": "authors", "collection_id": "2v6h4-vpc33", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100616-152038470", "type": "article", "title": "Radio Sources from a 31 GHz Sky Survey with the Sunyaev-Zel'dovich Array", "author": [ { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Leitch", "given_name": "Erik", "clpid": "Leitch-E" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas", "clpid": "Culverhouse-T" }, { "family_name": "Greer", "given_name": "Chris", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Lamb", "given_name": "James", "clpid": "Lamb-J" }, { "family_name": "Loh", "given_name": "Michael", "clpid": "Loh-M" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Sharp", "given_name": "Matthew", "clpid": "Sharp-M" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We present the first sample of 31 GHz selected sources to flux levels of 1 mJy. From late 2005 to mid-2007, the Sunyaev-Zel'dovich Array observed 7.7 deg^2 of the sky at 31 GHz to a median rms of 0.18 mJy beam^(-1). We identify 209 sources at greater than 5\u03c3 significance in the 31 GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NVSS data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. We determine the maximum-likelihood integrated source count to be N(>S) = (27.2 \u00b1 2.5)deg^(\u20132) \u00d7 (S_(mJy))^(\u20131.18\u00b10.12) over the flux range 0.7-15 mJy. This result is significantly higher than predictions based on 1.4 GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4 GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, we derive an overdensity of 6.8 \u00b1 4.4, relative to field sources.", "doi": "10.1088/0004-637X/716/1/521", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-06-10", "series_number": "1", "volume": "716", "issue": "1", "pages": "521-529" }, { "id": "authors:3pp0r-ksb47", "collection": "authors", "collection_id": "3pp0r-ksb47", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100413-105916911", "type": "article", "title": "A Measurement of Arcminute Anisotropy in the Cosmic Microwave Background with the Sunyaev-Zel'dovich Array", "author": [ { "family_name": "Sharp", "given_name": "Matthew K.", "clpid": "Sharp-M-K" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas", "clpid": "Culverhouse-T" }, { "family_name": "Greer", "given_name": "Christopher", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Loh", "given_name": "Michael", "clpid": "Loh-M" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We present 30 GHz measurements of the angular power spectrum of the cosmic microwave background (CMB) obtained with the Sunyaev-Zel'dovich Array. The measurements are sensitive to arcminute angular scales, where secondary anisotropy from the Sunyaev-Zel'dovich effect (SZE) is expected to dominate. For a broad bin centered at multipole 4066, we find 67^(+77)_(\u201350) \u03bcK^2; of which 26 \u00b1 5 \u03bcK^2 is the expected contribution from primary CMB anisotropy and 80 \u00b1 54 \u03bcK^2 is the expected contribution from undetected radio sources. These results imply an upper limit of 155 \u03bcK^2 (95% CL) on the secondary contribution to the anisotropy in our maps. This level of SZE anisotropy power is consistent with expectations based on recent determinations of the normalization of the matter power spectrum, i.e., \u03c3_8 ~ 0.8.", "doi": "10.1088/0004-637X/713/1/82", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2010-04-10", "series_number": "1", "volume": "713", "issue": "1", "pages": "82-89" }, { "id": "authors:3j9yg-23z28", "collection": "authors", "collection_id": "3j9yg-23z28", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-152321083", "type": "article", "title": "LoCuSS: A Comparison of Sunyaev-Zel'dovich Effect and Gravitational-Lensing Measurements of Galaxy Clusters", "author": [ { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Smith", "given_name": "Graham P.", "orcid": "0000-0003-4494-8277", "clpid": "Smith-Graham-P" }, { "family_name": "Richard", "given_name": "Johan", "orcid": "0000-0001-5492-1049", "clpid": "Richard-Johan" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M-K" }, { "family_name": "Bonamente", "given_name": "Massimiliano", "clpid": "Bonamente-M" }, { "family_name": "Hasler", "given_name": "Nicole", "clpid": "Hasler-N" }, { "family_name": "Hamilton-Morris", "given_name": "Victoria", "clpid": "Hamilton-Morris-V" }, { "family_name": "Kneib", "given_name": "Jean-Paul", "orcid": "0000-0002-4616-4989", "clpid": "Kneib-J-P" }, { "family_name": "Culverhouse", "given_name": "Thomas", "clpid": "Culverhouse-T-L" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Greer", "given_name": "Christopher", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Loh", "given_name": "Michael", "clpid": "Loh-M" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Sharp", "given_name": "Matthew K.", "clpid": "Sharp-M-K" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We present the first measurement of the relationship between the Sunyaev-Zel'dovich effect (SZE) signal and the mass of galaxy clusters that uses gravitational lensing to measure cluster mass, based on 14 X-ray luminous clusters at z \u2243 0.2 from the Local Cluster Substructure Survey. We measure the integrated Compton y-parameter, Y, and total projected mass of the clusters (M_(GL)) within a projected clustercentric radius of 350 kpc, corresponding to mean overdensities of 4000-8000 relative to the critical density. We find self-similar scaling between M GL and Y, with a scatter in mass at fixed Y of 32%. This scatter exceeds that predicted from numerical cluster simulations, however, it is smaller than comparable measurements of the scatter in mass at fixed T_(X). We also find no evidence of segregation in Y between disturbed and undisturbed clusters, as had been seen with T_(X) on the same physical scales. We compare our scaling relation to the Bonamente et al. relation based on mass measurements that assume hydrostatic equilibrium, finding no evidence for a hydrostatic mass bias in cluster cores (M_(GL) = 0.98 \u00b1 0.13 M_(HSE)), consistent with both predictions from numerical simulations and lensing/X-ray-based measurements of mass-observable scaling relations at larger radii. Overall our results suggest that the SZE may be less sensitive than X-ray observations to the details of cluster physics in cluster cores.", "doi": "10.1088/0004-637X/701/2/L114", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-08-20", "series_number": "2", "volume": "701", "issue": "2", "pages": "L114-L118" }, { "id": "authors:pdbt9-k4330", "collection": "authors", "collection_id": "pdbt9-k4330", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090506-113043599", "type": "article", "title": "Application of a self-similar pressure profile to Sunyaev\u2013Zel'dovich effect data from galaxy clusters", "author": [ { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Bonamente", "given_name": "Max", "clpid": "Bonamente-M" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Culverhouse", "given_name": "Thomas L.", "clpid": "Culverhouse-T-L" }, { "family_name": "Greer", "given_name": "Christopher", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C-H" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M-K" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Loh", "given_name": "Michael", "clpid": "Loh-M" }, { "family_name": "Maughan", "given_name": "Ben", "clpid": "Maughan-B" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Miller", "given_name": "Amber", "clpid": "Miller-A-D" }, { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Nagai", "given_name": "Daisuke", "orcid": "0000-0002-6766-5942", "clpid": "Nagai-Daisuke" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Sharp", "given_name": "Matthew", "clpid": "Sharp-M-K" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" } ], "abstract": "We investigate the utility of a new, self-similar pressure profile for fitting Sunyaev\u2013Zel'dovich (SZ) effect observations of galaxy clusters. Current SZ imaging instruments\u2013such as the Sunyaev\u2013Zel'dovich Array (SZA)\u2013 are capable of probing clusters over a large range in a physical scale. A model is therefore required that can accurately describe a cluster's pressure profile over a broad range of radii from the core of the cluster out to a significant fraction of the virial radius. In the analysis presented here, we fit a radial pressure profile derived from simulations and detailed X-ray analysis of relaxed clusters to SZA observations of three clusters with exceptionally high-quality X-ray data: A1835, A1914, and CL J1226.9+3332. From the joint analysis of the SZ and X-ray data, we derive physical properties such as gas mass, total mass, gas fraction and the intrinsic, integrated Compton y-parameter. We find that parameters derived from the joint fit to the SZ and X-ray data agree well with a detailed, independent X-ray-only analysis of the same clusters. In particular, we find that, when combined with X-ray imaging data, this new pressure profile yields an independent electron radial temperature profile that is in good agreement with spectroscopic X-ray measurements.", "doi": "10.1088/0004-637X/694/2/1034", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-04-01", "series_number": "2", "volume": "694", "issue": "2", "pages": "1034-1044" }, { "id": "authors:scehr-qvk60", "collection": "authors", "collection_id": "scehr-qvk60", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-141710879", "type": "article", "title": "QUaD: A High-Resolution Cosmic Microwave Background Polarimeter", "author": [ { "family_name": "Hinderks", "given_name": "J. R.", "clpid": "Hinderks-J-R" }, { "family_name": "Ade", "given_name": "P.", "clpid": "Ade-P" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bowden", "given_name": "M.", "clpid": "Bowden-M" }, { "family_name": "Brown", "given_name": "M. L.", "clpid": "Brown-M-L" }, { "family_name": "Cahill", "given_name": "G.", "clpid": "Cahill-G" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Castro", "given_name": "P. G.", "clpid": "Castro-P-G" }, { "family_name": "Church", "given_name": "S.", "clpid": "Church-S" }, { "family_name": "Culverhouse", "given_name": "T.", "clpid": "Culverhouse-T" }, { "family_name": "Friedman", "given_name": "R.", "clpid": "Friedman-R" }, { "family_name": "Ganga", "given_name": "K.", "clpid": "Ganga-K" }, { "family_name": "Gear", "given_name": "W. K.", "clpid": "Gear-W-K" }, { "family_name": "Gupta", "given_name": "S.", "clpid": "Gupta-S" }, { "family_name": "Harris", "given_name": "J.", "clpid": "Harris-J" }, { "family_name": "Haynes", "given_name": "V.", "clpid": "Haynes-V" }, { "family_name": "Keating", "given_name": "B. G.", "clpid": "Keating-B-G" }, { "family_name": "Kovac", "given_name": "J.", "clpid": "Kovac-J" }, { "family_name": "Kirby", "given_name": "E.", "orcid": "0000-0001-6196-5162", "clpid": "Kirby-E-N" }, { "family_name": "Lange", "given_name": "A. E.", "clpid": "Lange-A-E" }, { "family_name": "Leitch", "given_name": "E.", "clpid": "Leitch-E" }, { "family_name": "Mallie", "given_name": "O. E.", "clpid": "Mallie-O-E" }, { "family_name": "Melhuish", "given_name": "S.", "clpid": "Melhuish-S" }, { "family_name": "Memari", "given_name": "Y.", "clpid": "Memari-Y" }, { "family_name": "Murphy", "given_name": "A.", "clpid": "Murphy-A" }, { "family_name": "Orlando", "given_name": "A.", "clpid": "Orlando-A" }, { "family_name": "Schwarz", "given_name": "R.", "clpid": "Schwarz-R" }, { "family_name": "O'Sullivan", "given_name": "C.", "clpid": "O'Sullivan-C" }, { "family_name": "Piccirillo", "given_name": "L.", "clpid": "Piccirillo-L" }, { "family_name": "Pryke", "given_name": "C.", "clpid": "Pryke-C" }, { "family_name": "Rajguru", "given_name": "N.", "clpid": "Rajguru-N" }, { "family_name": "Rusholme", "given_name": "B.", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-B" }, { "family_name": "Taylor", "given_name": "A. N.", "clpid": "Taylor-A-N" }, { "family_name": "Thompson", "given_name": "K. L.", "clpid": "Thompson-K-L" }, { "family_name": "Tucker", "given_name": "C.", "clpid": "Tucker-C" }, { "family_name": "Turner", "given_name": "A. H.", "clpid": "Turner-A-H" }, { "family_name": "Wu", "given_name": "E. Y. S.", "clpid": "Wu-E-Y-S" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "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.", "doi": "10.1088/0004-637X/692/2/1221", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-02-24", "series_number": "2", "volume": "692", "issue": "2", "pages": "1221-1246" }, { "id": "authors:c9jsf-bav61", "collection": "authors", "collection_id": "c9jsf-bav61", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180717-152432620", "type": "book_section", "title": "BICEP2/SPUD: searching for inflation with degree scale polarimetry from the South Pole", "book_title": "Millimeter and Submillimeter Detectors and Instrumentation for Astronomy IV", "author": [ { "family_name": "Nguyen", "given_name": "Hien Trong", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Kovac", "given_name": "John", "clpid": "Kovac-J-M" }, { "family_name": "Ade", "given_name": "Pete", "orcid": "0000-0002-5127-0401", "clpid": "Ade-P-A-R" }, { "family_name": "Aikin", "given_name": "Randol", "clpid": "Aikin-R-W" }, { "family_name": "Benton", "given_name": "Steve", "clpid": "Benton-S-J" }, { "family_name": "Bock", "given_name": "Jamie", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Brevik", "given_name": "Justus", "clpid": "Brevik-J-A" }, { "family_name": "Carlstrom", "given_name": "John", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Dowell", "given_name": "Darren", "clpid": "Dowell-D" }, { "family_name": "Duband", "given_name": "Lionel", "clpid": "Duband-L" }, { "family_name": "Golwala", "given_name": "Sunil", "orcid": "0000-0002-1098-7174", "clpid": "Golwala-S-R" }, { "family_name": "Halpern", "given_name": "Mark", "orcid": "0000-0002-1760-0868", "clpid": "Halpern-M" }, { "family_name": "Hasselfield", "given_name": "Matthew", "clpid": "Hasselfield-M" }, { "family_name": "Irwin", "given_name": "Kent", "clpid": "Irwin-K-D" }, { "family_name": "Jones", "given_name": "William", "clpid": "Jones-W" }, { "family_name": "Kaufman", "given_name": "Jonathan", "clpid": "Kaufman-J" }, { "family_name": "Keating", "given_name": "Brian", "clpid": "Keating-B-G" }, { "family_name": "Kuo", "given_name": "Chao-Lin", "clpid": "Kuo-Chao-Lin" }, { "family_name": "Lange", "given_name": "Andrew", "clpid": "Lange-A-E" }, { "family_name": "Matsumura", "given_name": "Tomotake", "clpid": "Matsumura-Tomotake" }, { "family_name": "Netterfield", "given_name": "Barth", "clpid": "Netterfield-C-B" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Ruhl", "given_name": "John", "clpid": "Ruhl-J-E" }, { "family_name": "Sheehy", "given_name": "Chris", "clpid": "Sheehy-C-D" }, { "family_name": "Sudiwala", "given_name": "Rashmi", "clpid": "Sudiwala-R-V" } ], "contributor": [ { "family_name": "Duncan", "given_name": "William D.", "clpid": "Duncan-W-D" }, { "family_name": "Holland", "given_name": "Wayne S.", "clpid": "Holland-W-S" }, { "family_name": "Withington", "given_name": "Stafford", "clpid": "Withington-S" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "clpid": "Zmuidzinas-J" } ], "abstract": "BICEP2/SPUD is the new powerful upgrade of the existing BICEP1 experiment, a bolometric receiver to study the polarization of the cosmic microwave background radiation, which has been in operation at the South Pole since January 2006. BICEP2 will provide an improvement up to 10 times mapping speed at 150 GHz compared to BICEP1, using the same BICEP telescope mount. SPUD, a series of compact, mechanically-cooled receivers deployed on the DASI mount at the Pole, will provide similar mapping speed in to BICEP2 in three bands, 100, 150, and 220 GHz. The new system will use large TES focal plane arrays to provide unprecedented sensitivity and excellent control of foreground contamination.", "doi": "10.1117/12.787997", "isbn": "9780819472304", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2008-07-21", "pages": "Art. No. 70201F" }, { "id": "authors:35s3f-afb37", "collection": "authors", "collection_id": "35s3f-afb37", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090407-101728774", "type": "article", "title": "Scaling relations from Sunyaev-Zel'dovich effect and Chandra X-ray measurements of high-redshift galaxy clusters", "author": [ { "family_name": "Bonamente", "given_name": "Massimiliano", "clpid": "Bonamente-M" }, { "family_name": "Marshall", "given_name": "Joy", "clpid": "Marshall-J" }, { "family_name": "LaRoque", "given_name": "Samuel J.", "clpid": "LaRoque-S-J" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Nagai", "given_name": "Daisuke", "orcid": "0000-0002-6766-5942", "clpid": "Nagai-Daisuke" }, { "family_name": "Marrone", "given_name": "Daniel P.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" } ], "abstract": "We present Sunyaev-Zel'dovich Effect (SZE) scaling relations for 38 massive galaxy clusters at redshifts 0.14 \u2264 z\u2264 0.89, observed with both the Chandra X-ray Observatory and the centimeter-wave SZE imaging system at the BIMA and OVRO interferometric arrays. An isothermal \u03b2-model with the central 100 kpc excluded from the X-ray data is used to model the intracluster medium and to measure global cluster properties. For each cluster, we measure the X-ray spectroscopic temperature, SZE gas mass, total mass, and integrated Compton y-parameters within r2500. Our measurements are in agreement with the expectations based on a simple self-similar model of cluster formation and evolution. We compare the cluster properties derived from our SZE observations with and without Chandra spatial and spectral information and find them to be in good agreement. We compare our results with cosmological numerical simulations and find that simulations that include radiative cooling, star formation, and feedback match well both the slope and normalization of our SZE scaling relations.", "doi": "10.1086/525517", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2008-03-01", "series_number": "1", "volume": "675", "issue": "1", "pages": "106-114" }, { "id": "authors:qxnd5-ztk79", "collection": "authors", "collection_id": "qxnd5-ztk79", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:ADEapj08", "type": "article", "title": "First season QUaD CMB temperature and polarization power spectra", "author": [ { "family_name": "Ade", "given_name": "P.", "orcid": "0000-0002-5127-0401", "clpid": "Ade-P-A-R" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bowden", "given_name": "M.", "clpid": "Bowden-M" }, { "family_name": "Brown", "given_name": "M. L.", "clpid": "Brown-M-L" }, { "family_name": "Cahill", "given_name": "V.", "clpid": "Cahill-V" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Castro", "given_name": "P. G.", "clpid": "Castro-P-G" }, { "family_name": "Church", "given_name": "S.", "clpid": "Church-S" }, { "family_name": "Culverhouse", "given_name": "T.", "clpid": "Culverhouse-T" }, { "family_name": "Friedman", "given_name": "R.", "clpid": "Friedman-R" }, { "family_name": "Ganga", "given_name": "K.", "clpid": "Ganga-K" }, { "family_name": "Gear", "given_name": "W. K.", "clpid": "Gear-W-K" }, { "family_name": "Hinderks", "given_name": "J.", "clpid": "Hinderks-J" }, { "family_name": "Kovac", "given_name": "J.", "clpid": "Kovac-J" }, { "family_name": "Lange", "given_name": "A. E.", "clpid": "Lange-A-E" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "Melhuish", "given_name": "S. J.", "clpid": "Melhuish-S-J" }, { "family_name": "Murphy", "given_name": "J. A.", "clpid": "Murphy-J-A" }, { "family_name": "Orlando", "given_name": "A.", "clpid": "Orlando-A" }, { "family_name": "Schwarz", "given_name": "R.", "clpid": "Schwarz-R-B" }, { "family_name": "O'Sullivan", "given_name": "C.", "clpid": "O'Sullivan-C" }, { "family_name": "Piccirillo", "given_name": "L.", "clpid": "Piccirillo-L" }, { "family_name": "Pryke", "given_name": "C.", "clpid": "Pryke-C" }, { "family_name": "Rajguru", "given_name": "N.", "clpid": "Rajguru-N" }, { "family_name": "Rusholme", "given_name": "B.", "orcid": "0000-0001-7648-4142", "clpid": "Rusholme-B" }, { "family_name": "Taylor", "given_name": "A. N.", "clpid": "Taylor-A-N" }, { "family_name": "Thompson", "given_name": "K. L.", "clpid": "Thompson-K-L" }, { "family_name": "Wu", "given_name": "E. Y. S.", "clpid": "Wu-E-Y-S" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "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.", "doi": "10.1086/524922", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2008-02-10", "series_number": "1", "volume": "674", "issue": "1", "pages": "22-28" }, { "id": "authors:ymx2b-dcd35", "collection": "authors", "collection_id": "ymx2b-dcd35", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100219-111648129", "type": "article", "title": "COSMOS: Hubble Space Telescope Observations", "author": [ { "family_name": "Scoville", "given_name": "N.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Abraham", "given_name": "R. G.", "orcid": "0000-0002-4542-921X", "clpid": "Abraham-R-G" }, { "family_name": "Aussel", "given_name": "H.", "orcid": "0000-0002-1371-5705", "clpid": "Aussel-Herve" }, { "family_name": "Barnes", "given_name": "J. E.", "clpid": "Barnes-J-E" }, { "family_name": "Benson", "given_name": "A.", "orcid": "0000-0001-5501-6008", "clpid": "Benson-A-J" }, { "family_name": "Blain", "given_name": "A. W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Calzetti", "given_name": "D.", "orcid": "0000-0002-5189-8004", "clpid": "Calzetti-D" }, { "family_name": "Comastri", "given_name": "A.", "orcid": "0000-0003-3451-9970", "clpid": "Comastri-A" }, { "family_name": "Capak", "given_name": "P.", "orcid": "0000-0003-3578-6843", "clpid": "Capak-P" }, { "family_name": "Carilli", "given_name": "C.", "orcid": "0000-0001-6647-3861", "clpid": "Carilli-C-L" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Carollo", "given_name": "C. M.", "orcid": "0000-0003-1624-7609", "clpid": "Carollo-C-Marcella" }, { "family_name": "Colbert", "given_name": "J.", "clpid": "Colbert-J-W" }, { "family_name": "Daddi", "given_name": "E.", "orcid": "0000-0002-3331-9590", "clpid": "Daddi-Emanuele" }, { "family_name": "Ellis", "given_name": "R. S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Elvis", "given_name": "M.", "clpid": "Elvis-M" }, { "family_name": "Ewald", "given_name": "S. P.", "orcid": "0000-0002-1567-9154", "clpid": "Ewald-S-P" }, { "family_name": "Fall", "given_name": "M.", "clpid": "Fall-M" }, { "family_name": "Franceschini", "given_name": "A.", "clpid": "Franceschini-A" }, { "family_name": "Giavalisco", "given_name": "M.", "orcid": "0000-0002-7831-8751", "clpid": "Giavalisco-M" }, { "family_name": "Green", "given_name": "W.", "clpid": "Green-W" }, { "family_name": "Griffiths", "given_name": "R. E.", "clpid": "Griffiths-R-E" }, { "family_name": "Guzzo", "given_name": "L.", "clpid": "Guzzo-L" }, { "family_name": "Hasinger", "given_name": "G.", "orcid": "0000-0002-0797-0646", "clpid": "Hasinger-G" }, { "family_name": "Impey", "given_name": "C.", "clpid": "Impey-C-D" }, { "family_name": "Kneib", "given_name": "J.-P.", "orcid": "0000-0002-4616-4989", "clpid": "Kneib-J-P" }, { "family_name": "Koda", "given_name": "J.", "orcid": "0000-0002-8762-7863", "clpid": "Koda-Jin" }, { "family_name": "Koekemoer", "given_name": "A.", "orcid": "0000-0002-6610-2048", "clpid": "Koekemoer-A-M" }, { "family_name": "Le F\u00e8vre", "given_name": "O.", "orcid": "0000-0001-5891-2596", "clpid": "Le-F\u00e8vre-O" }, { "family_name": "Lilly", "given_name": "S.", "orcid": "0000-0002-6423-3597", "clpid": "Lilly-S-J" }, { "family_name": "Liu", "given_name": "C. T.", "orcid": "0000-0002-4314-8713", "clpid": "Liu-Charles-T" }, { "family_name": "McCracken", "given_name": "H. J.", "orcid": "0000-0002-9489-7765", "clpid": "McCracken-H-J" }, { "family_name": "Massey", "given_name": "R.", "orcid": "0000-0002-6085-3780", "clpid": "Massey-R-J" }, { "family_name": "Mellier", "given_name": "Y.", "clpid": "Mellier-Y" }, { "family_name": "Miyazaki", "given_name": "S.", "clpid": "Miyazaki-Satoshi" }, { "family_name": "Mobasher", "given_name": "B.", "clpid": "Mobasher-B" }, { "family_name": "Mould", "given_name": "J.", "orcid": "0000-0003-3820-1740", "clpid": "Mould-J-R" }, { "family_name": "Norman", "given_name": "C.", "clpid": "Norman-C" }, { "family_name": "Refregier", "given_name": "A.", "clpid": "Refregier-A" }, { "family_name": "Renzini", "given_name": "A.", "orcid": "0000-0002-7093-7355", "clpid": "Renzini-A" }, { "family_name": "Rhodes", "given_name": "J.", "orcid": "0000-0002-4485-8549", "clpid": "Rhodes-J-D" }, { "family_name": "Rich", "given_name": "M.", "clpid": "Rich-M" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Schiminovich", "given_name": "D.", "clpid": "Schiminovich-D" }, { "family_name": "Schinnerer", "given_name": "E.", "orcid": "0000-0002-3933-7677", "clpid": "Schinnerer-E" }, { "family_name": "Scodeggio", "given_name": "M.", "clpid": "Scodeggio-M" }, { "family_name": "Sheth", "given_name": "K.", "orcid": "0000-0002-5496-4118", "clpid": "Sheth-K" }, { "family_name": "Shopbell", "given_name": "P. L.", "clpid": "Shopbell-P-L" }, { "family_name": "Taniguchi", "given_name": "Y.", "orcid": "0000-0003-2247-3741", "clpid": "Taniguchi-Yoshiaki" }, { "family_name": "Tyson", "given_name": "N. D.", "clpid": "Tyson-N-D" }, { "family_name": "Urry", "given_name": "C. M.", "orcid": "0000-0002-0745-9792", "clpid": "Urry-C-M" }, { "family_name": "van Waerbeke", "given_name": "L.", "clpid": "van-Waerbeke-L" }, { "family_name": "Vettolani", "given_name": "P.", "clpid": "Vettolani-P" }, { "family_name": "White", "given_name": "S. D. M.", "clpid": "White-S-D-M" }, { "family_name": "Yan", "given_name": "L.", "orcid": "0000-0003-1710-9339", "clpid": "Yan-Lin" } ], "abstract": "The Cosmic Evolution Survey (COSMOS) was initiated with an extensive allocation (590 orbits in Cycles 12-13) using the Hubble Space Telescope (HST) for high-resolution imaging. Here we review the characteristics of the HST imaging with the Advanced Camera for Surveys (ACS) and parallel observations with NICMOS and WFPC2. A square field (1.8 deg^2) has been imaged with single-orbit ACS I-band F814W exposures with 50% completeness for sources 0.5\" in diameter at I_(AB) = 26.0 mag. The ACS is a key part of the COSMOS survey, providing very high sensitivity and high-resolution (0.09\" FWHM and 0.05\" pixels) imaging and detecting a million objects. These images yield resolved morphologies for several hundred thousand galaxies. The small HST PSF also provides greatly enhanced sensitivity for weak-lensing investigations of the dark matter distribution.", "doi": "10.1086/516580", "issn": "0067-0049", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Supplement Series", "publication_date": "2007-09", "series_number": "1", "volume": "172", "issue": "1", "pages": "38-45" }, { "id": "authors:qyws2-c8b12", "collection": "authors", "collection_id": "qyws2-c8b12", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100419-141045535", "type": "article", "title": "Observations of High-Redshift X-Ray Selected Clusters with the Sunyaev-Zel'dovich Array", "author": [ { "family_name": "Muchovej", "given_name": "Stephen", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Mroczkowski", "given_name": "Tony", "orcid": "0000-0003-3816-5372", "clpid": "Mroczkowski-T-K" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Cartwright", "given_name": "John", "clpid": "Cartwright-J" }, { "family_name": "Greer", "given_name": "Christopher", "orcid": "0000-0002-9590-0508", "clpid": "Greer-C" }, { "family_name": "Hennessy", "given_name": "Ryan", "clpid": "Hennessy-R" }, { "family_name": "Loh", "given_name": "Michael", "clpid": "Loh-M" }, { "family_name": "Pryke", "given_name": "Clem", "clpid": "Pryke-C" }, { "family_name": "Reddall", "given_name": "Ben", "clpid": "Reddall-B" }, { "family_name": "Runyan", "given_name": "Marcus", "clpid": "Runyan-M" }, { "family_name": "Sharp", "given_name": "Matthew", "clpid": "Sharp-M" }, { "family_name": "Hawkins", "given_name": "David", "clpid": "Hawkins-D" }, { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" }, { "family_name": "Joy", "given_name": "Marshall", "clpid": "Joy-M" }, { "family_name": "Leitch", "given_name": "Erik M.", "clpid": "Leitch-E-M" }, { "family_name": "Miller", "given_name": "Amber D.", "clpid": "Miller-A-D" } ], "abstract": "We report measurements of the Sunyaev-Zel'dovich (SZ) effect in three high-redshift (0.89 \u2264 z \u2264 1.03), X-ray selected galaxy clusters. The observations were obtained at 30 GHz during the commissioning period of a new, eight-element interferometer\u2014the Sunyaev-Zel'dovich Array (SZA)\u2014built for dedicated SZ effect observations. The SZA observations are sensitive to angular scales larger than those subtended by the virial radii of the clusters. Assuming isothermality and hydrostatic equilibrium for the intracluster medium and gas-mass fractions consistent with those for clusters at moderate redshift, we calculate electron temperatures, gas masses, and total cluster masses from the SZ data. The SZ-derived masses, integrated approximately to the virial radii, are 1.9^(+0.5)_(-0.4) \u00d7 10^(14) M_\u2609 for Cl J1415.1+3612, 3.4^(+0.6)_(-0.5) \u00d7 10^(14) M_\u2609 for Cl J1429.0+4241, and 7.2^(+1.3)_(-0.9) \u00d7 10^(14) M_\u2609 for Cl J1226.9+3332. The SZ-derived quantities are in good agreement with the cluster properties derived from X-ray measurements.", "doi": "10.1086/511971", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2007-07-10", "series_number": "2", "volume": "663", "issue": "2", "pages": "708-716" }, { "id": "authors:d8fwy-kda77", "collection": "authors", "collection_id": "d8fwy-kda77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110602-110322292", "type": "article", "title": "X-Ray and Sunyaev-Zel'dovich Effect Measurements of the Gas Mass Fraction in Galaxy Clusters", "author": [ { "family_name": "LaRoque", "given_name": "Samuel J.", "clpid": "LaRoque-S-J" }, { "family_name": "Bonamente", "given_name": "Massimiliano", "clpid": "Bonamente-M" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Joy", "given_name": "Marshall K.", "clpid": "Joy-M-K" }, { "family_name": "Nagai", "given_name": "Daisuke", "orcid": "0000-0002-6766-5942", "clpid": "Nagai-Daisuke" }, { "family_name": "Reese", "given_name": "Erik D.", "orcid": "0000-0002-8700-7082", "clpid": "Reese-E-D" }, { "family_name": "Dawson", "given_name": "Kyle S.", "orcid": "0000-0002-0553-3805", "clpid": "Dawson-Kyle-S" } ], "abstract": "We present gas mass fractions of 38 massive galaxy clusters at redshifts 0.14 \u2264 z \u2264 0.89, derived from Chandra X-ray and OVRO/BIMA interferometric Sunyaev-Zel'dovich effect (SZE) measurements. We use three models for the gas distribution: (1) an isothermal \u03b2-model fit jointly to the X-ray data at radii beyond 100 kpc and to all of the SZE data, (2) a nonisothermal double \u03b2-model in hydrostatic equilibrium with a Navarro-Frenk-White (NFW) dark matter distribution, fit jointly to all of the X-ray and SZE data, and (3) an isothermal \u03b2-model fit only to the SZE spatial data. We show that the isothermal model well characterizes the intracluster medium outside the cluster core and provides good fits to clusters with a range of morphological properties. X-ray and SZE mean gas mass fractions for model 1 are f_(gas)(X-ray) = 0.110 \u00b1 0.003^(+0.006)_(-0.018) and f_(gas)(SZE) = 0.116 \u00b1 0.005^(+0.009)_(-0.027) assuming (\u03a9_M, \u03a9_\u039b, h) = (0.3, 0.7, 0.7); uncertainties are statistical followed by systematic at 68% confidence. For model 2, f_(gas)(X-ray) = 0.119 \u00b1 0.003^(+0.007)_(-0.014) and f_(gas)(SZE) = 0.121 \u00b1 0.005^(+0.009)_(-0.016). For model 3, f_(gas)(SZE) = 0.120 \u00b1 0.009^(+0.009)_(-0.027). The agreement in the results shows that the core can be accounted for satisfactorily by either excluding it from fits to the X-ray data or modeling the intracluster gas with a nonisothermal double \u03b2-model. We find that the SZE is largely insensitive to core structure. Our results indicate that the ratio of gas mass fraction within r_(2500) to the cosmic baryon fraction, f_(gas)/(\u03a9_(B)/\u03a9_(M)) is 0.68^(+0.10)_(-0.16), where statistical and systematic uncertainties are included at 68% confidence. By assuming that cluster gas mass fractions are independent of redshift, we find that the results agree with standard \u039bCDM cosmology and are inconsistent with a flat matter-dominated (\u03a9_M = 1) universe.", "doi": "10.1086/508139", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2006-12-01", "series_number": "2", "volume": "652", "issue": "2", "pages": "917-936" }, { "id": "authors:zn8tc-yrh09", "collection": "authors", "collection_id": "zn8tc-yrh09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141202-152432483", "type": "article", "title": "Polarization Observations with the Cosmic Background Imager", "author": [ { "family_name": "Readhead", "given_name": "A. C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Myers", "given_name": "S. T.", "clpid": "Myers-Steven-Theodore" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Sievers", "given_name": "J. L.", "clpid": "Sievers-J-L" }, { "family_name": "Mason", "given_name": "B. S.", "clpid": "Mason-B-S" }, { "family_name": "Contaldi", "given_name": "C. R.", "clpid": "Contaldi-C-R" }, { "family_name": "Bond", "given_name": "J. R.", "orcid": "0000-0003-2358-9949", "clpid": "Bond-J-R" }, { "family_name": "Bustos", "given_name": "R.", "clpid": "Bustos-R" }, { "family_name": "Altamirano", "given_name": "P.", "clpid": "Altamirano-P" }, { "family_name": "Achermann", "given_name": "C.", "clpid": "Achermann-C" }, { "family_name": "Bronfman", "given_name": "L.", "clpid": "Bronfman-L" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Cartwright", "given_name": "J. K.", "clpid": "Cartwright-J-K" }, { "family_name": "Casassus", "given_name": "S.", "clpid": "Casassus-S" }, { "family_name": "Dickinson", "given_name": "C.", "orcid": "0000-0002-0045-442X", "clpid": "Dickinson-C" }, { "family_name": "Holzapfel", "given_name": "W. L.", "clpid": "Holzapfel-W-L" }, { "family_name": "Kovac", "given_name": "J. M.", "clpid": "Kovac-J-M" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "May", "given_name": "J.", "clpid": "May-J" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Pogosyan", "given_name": "D.", "clpid": "Pogosyan-D" }, { "family_name": "Pospieszalski", "given_name": "M.", "clpid": "Pospieszalski-M" }, { "family_name": "Pryke", "given_name": "C.", "clpid": "Pryke-C" }, { "family_name": "Reeves", "given_name": "R.", "orcid": "0000-0001-5704-271X", "clpid": "Reeves-R-A" }, { "family_name": "Shepherd", "given_name": "M. C.", "clpid": "Shepherd-Martin-C" }, { "family_name": "Torres", "given_name": "S.", "clpid": "Torres-S" } ], "abstract": "Polarization observations of the cosmic microwave background with the Cosmic Background Imager from September 2002 to May 2004 provide a significant detection of the E-mode polarization and reveal an angular power spectrum of polarized emission showing peaks and valleys that are shifted in phase by half a cycle relative to those of the total intensity spectrum. This key agreement between the phase of the observed polarization spectrum and that predicted on the basis of the total intensity spectrum provides support for the standard model of cosmology, in which dark matter and dark energy are the dominant constituents, the geometry is close to flat, and primordial density fluctuations are predominantly adiabatic with a matter power spectrum commensurate with inflationary cosmological models.", "doi": "10.1126/science.1105598", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "2004-10-29", "series_number": "5697", "volume": "306", "issue": "5697", "pages": "836-844" }, { "id": "authors:64p04-p2663", "collection": "authors", "collection_id": "64p04-p2663", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180725-084429622", "type": "book_section", "title": "CARMA: a new heterogeneous millimeter-wave interferometer", "book_title": "Millimeter and Submillimeter Detectors for Astronomy II", "author": [ { "family_name": "Woody", "given_name": "D. P.", "clpid": "Woody-D-P" }, { "family_name": "Beasley", "given_name": "A. J.", "clpid": "Beasley-A-J" }, { "family_name": "Bolatto", "given_name": "A.", "orcid": "0000-0002-5480-5686", "clpid": "Bolatto-A-D" }, { "family_name": "Carlstrom", "given_name": "J.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Harris", "given_name": "A.", "clpid": "Harris-A" }, { "family_name": "Hawkins", "given_name": "D.", "clpid": "Hawkins-D-W" }, { "family_name": "Lamb", "given_name": "J.", "clpid": "Lamb-J-W" }, { "family_name": "Looney", "given_name": "L.", "clpid": "Looney-L" }, { "family_name": "Mundy", "given_name": "L. G.", "clpid": "Mundy-L-G" }, { "family_name": "Plambeck", "given_name": "R.", "clpid": "Plambeck-R-L" }, { "family_name": "Scott", "given_name": "S.", "clpid": "Scott-S" }, { "family_name": "Wright", "given_name": "M.", "clpid": "Wright-M-C-H" } ], "contributor": [ { "family_name": "Zmuidzinas", "given_name": "Jonas", "clpid": "Zmuidzinas-J" }, { "family_name": "Holland", "given_name": "Wayne S.", "clpid": "Holland-W-S" }, { "family_name": "Withington", "given_name": "Stafford", "clpid": "Withington-S" } ], "abstract": "A new Combined Array for Research in Millimeter-wave Astronomy (CARMA) interferometer is being assembled from the existing Owens Valley Radio Observatory (OVRO), the Berkeley-Illinois-Maryland Association (BIMA) millimeter interferometers and the new Sunyaev?Zeldovich Array (SZA) at Cedar Flat, a site at 2,200 m altitude in the Inyo Mountains east of OVRO. The array will consist of 23 antennas of three different diameters, 3.5, 6.1 and 10.4 m, and will support observations in the 1 cm, 3 mm and 1.3 mm bands. The fist-light correlator is a flexible FPGA based system that will process up to 8 GHz of bandwidth on the sky for two subarrays consisting of 8 and 15 elements. The array configurations will offer antenna spacings from 5 m to 1.9 km allowing unprecedented high resolution and wide field imaging at millimeter wavelengths. Radiometers observing the 22 GHz water vapor emission line will be used to measure and correct for the water vapor induced path delay along the line of sight for each telescope and thereby minimize the time lost to \"bad seeing\". This university based facility will emphasize technology development and student training along with leading edge astronomical research in areas ranging from Sunyaev-Zeldovich effect galaxy cluster surveys to studying protoplanetary disks.", "doi": "10.1117/12.552446", "isbn": "0819454303", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2004-10-08", "pages": "30-41" }, { "id": "authors:v4wa5-25m84", "collection": "authors", "collection_id": "v4wa5-25m84", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200130-075505900", "type": "article", "title": "Scientific optimization of a ground-based CMB polarization experiment", "author": [ { "family_name": "Bowden", "given_name": "M.", "clpid": "Bowden-M" }, { "family_name": "Taylor", "given_name": "A. N.", "clpid": "Taylor-A-N" }, { "family_name": "Ganga", "given_name": "K. M.", "clpid": "Ganga-K-M" }, { "family_name": "Ade", "given_name": "P. A. R.", "orcid": "0000-0002-5127-0401", "clpid": "Ade-P-A-R" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Cahill", "given_name": "G.", "clpid": "Cahill-G" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Church", "given_name": "S. E.", "clpid": "Church-S-E" }, { "family_name": "Gear", "given_name": "W. K.", "clpid": "Gear-W-K" }, { "family_name": "Hinderks", "given_name": "J. R.", "clpid": "Hinderks-J-R" }, { "family_name": "Hu", "given_name": "W.", "clpid": "Hu-W" }, { "family_name": "Keating", "given_name": "B. G.", "clpid": "Keating-B-G" }, { "family_name": "Kovac", "given_name": "J.", "clpid": "Kovac-J" }, { "family_name": "Lange", "given_name": "A. E.", "clpid": "Lange-A-E" }, { "family_name": "Leitch", "given_name": "E. M.", "clpid": "Leitch-E-M" }, { "family_name": "Maffei", "given_name": "B.", "clpid": "Maffei-B" }, { "family_name": "Mallie", "given_name": "O. E.", "clpid": "Mallie-O-E" }, { "family_name": "Melhuish", "given_name": "S. J.", "clpid": "Melhuish-S-J" }, { "family_name": "Murphy", "given_name": "J. A.", "clpid": "Murphy-J-A" }, { "family_name": "Pisano", "given_name": "G.", "clpid": "Pisano-G" }, { "family_name": "Piccirillo", "given_name": "L.", "clpid": "Piccirillo-L" }, { "family_name": "Pryke", "given_name": "C.", "clpid": "Pryke-C" }, { "family_name": "Rusholme", "given_name": "B. A.", "clpid": "Rusholme-B-A" }, { "family_name": "O'Sullivan", "given_name": "C.", "clpid": "O'Sullivan-C" }, { "family_name": "Thompson", "given_name": "K.", "clpid": "Thompson-K" } ], "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.", "doi": "10.1111/j.1365-2966.2004.07506.x", "issn": "1365-2966", "publisher": "Oxford University Press", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2004-03", "series_number": "1", "volume": "349", "issue": "1", "pages": "321-335" }, { "id": "authors:78175-ptm66", "collection": "authors", "collection_id": "78175-ptm66", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190722-161251070", "type": "article", "title": "Polarizing Grids, Their Assemblies, and Beams of Radiation", "author": [ { "family_name": "Houde", "given_name": "Martin", "clpid": "Houde-M" }, { "family_name": "Akeson", "given_name": "Rachel\u00a0L.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Carlstrom", "given_name": "John\u00a0E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Lamb", "given_name": "James\u00a0W.", "clpid": "Lamb-J-W" }, { "family_name": "Schleuning", "given_name": "David\u00a0A.", "clpid": "Schleuning-D-A" }, { "family_name": "Woody", "given_name": "David\u00a0P.", "clpid": "Woody-D-P" } ], "abstract": "This paper gives an analysis of the behavior of polarizing grids and reflecting polarizers by solving Maxwell's equations, for arbitrary angles of incidence and grid rotation, for cases where the excitation is provided by an incident plane wave or a beam of radiation. The scattering and impedance matrix representations are derived and used to solve more complicated configurations of grid assemblies. The results are also compared with data obtained in the calibration of reflecting polarizers at the Owens Valley Radio Observatory. From this analysis, we propose a method for choosing the optimum grid parameters (wire radius and spacing). We also provide a study of the effects of two types of errors (in wire separation and radius size) that can be introduced in the fabrication of a grid.", "doi": "10.1086/320287", "issn": "0004-6280", "publisher": "Astronomical Society of the Pacific", "publication": "Publications of the Astronomical Society of the Pacific", "publication_date": "2001-05", "series_number": "783", "volume": "113", "issue": "783", "pages": "622-638" }, { "id": "authors:wd2h2-0ks75", "collection": "authors", "collection_id": "wd2h2-0ks75", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:CHAieeemgwl98", "type": "article", "title": "A 96-GHz ortho-mode transducer for the Polatron", "author": [ { "family_name": "Chattopadhyay", "given_name": "Goutam", "orcid": "0000-0001-7942-5025", "clpid": "Chattopadhyay-G" }, { "family_name": "Philhour", "given_name": "Byron", "clpid": "Philhour-B" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Church", "given_name": "Sarah", "clpid": "Church-S" }, { "family_name": "Lange", "given_name": "Andrew", "clpid": "Lange-A-E" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We describe the design, simulation, fabrication, and performance of a 96-GHz ortho-mode transducer (OMT) to be used for the Polatron-a bolometric receiver with polarization capability. The OMT has low loss, good isolation, and moderately broad bandwidth, and its performance closely resembles simulation results.", "doi": "10.1109/75.746762", "issn": "1051-8207", "publisher": "IEEE", "publication": "IEEE Microwave and Guided Wave Letters", "publication_date": "1998-12", "series_number": "12", "volume": "8", "issue": "12", "pages": "421-423" }, { "id": "authors:s17xf-20927", "collection": "authors", "collection_id": "s17xf-20927", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140701-145831775", "type": "article", "title": "50 \u00b5as resolution VLBI images of AGN's at \u03bb3mm", "author": [ { "family_name": "Rantakyro", "given_name": "F. T.", "clpid": "Rantakyro-F-T" }, { "family_name": "B\u00e5\u00e5th", "given_name": "L. B.", "clpid": "B\u00e5\u00e5th-L-B" }, { "family_name": "Backer", "given_name": "D. C.", "clpid": "Backer-D-C" }, { "family_name": "Booth", "given_name": "R. S.", "clpid": "Booth-R-S" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Emerson", "given_name": "D. T.", "clpid": "Emerson-D-T" }, { "family_name": "Grewing", "given_name": "M.", "clpid": "Grewing-M" }, { "family_name": "Hirabayashi", "given_name": "H.", "clpid": "Hirabayashi-H" }, { "family_name": "Hodges", "given_name": "M. W.", "clpid": "Hodges-M-W" }, { "family_name": "Inoue", "given_name": "M.", "clpid": "Inoue-M" }, { "family_name": "Kobayashi", "given_name": "H.", "clpid": "Kobayashi-H" }, { "family_name": "Krichbaum", "given_name": "T. P.", "clpid": "Krichbaum-T-P" }, { "family_name": "Kus", "given_name": "A. J.", "clpid": "Kus-A-J" }, { "family_name": "Moran", "given_name": "J. M.", "clpid": "Moran-J-M" }, { "family_name": "Morimoto", "given_name": "M.", "clpid": "Morimoto-M" } ], "abstract": "We present 15 images from the global mm-VLBI sessions in 1990 April at 100GHz and 1993 April at 86GHz. These observations probe the central engines of the 16 observed AGN's with up to 50 \u00b5as resolution. Among other sources previously observed with \u03bb3mm VLBI we present the first \u03bb3mm maps of 0735+178, 0748+126, 1055+018, 2145+067, and CTA102, in total we have been able to image 13 out of the 16 observed sources. 6 out of the 13 imaged sources observed exhibit curvature and rapid structural changes, although the low dynamic range in two thirds of the maps limits the detection of weak features. Most of the sources have unresolved cores even at this high resolution. There is substantial evidence that the observed sources can be grouped into two general groups: A misaligned population with parsec scale jets in the form of low pitch helices and an aligned population with straight jets with small changes in PA due to intrinsic bends.", "doi": "10.1051/aas:1998282", "issn": "0365-0138", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics Supplement Series", "publication_date": "1998-09", "series_number": "3", "volume": "131", "issue": "3", "pages": "451-457" }, { "id": "authors:c6zfz-py187", "collection": "authors", "collection_id": "c6zfz-py187", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180507-141344201", "type": "article", "title": "50 \u03bcas resolution VLBI images of AGN's at \u03bb3 mm", "author": [ { "family_name": "Rantakyro", "given_name": "F. T.", "clpid": "Rantakyro-F-T" }, { "family_name": "B\u00e5\u00e5th", "given_name": "L. B.", "clpid": "B\u00e5\u00e5th-L-B" }, { "family_name": "Backer", "given_name": "D. C.", "clpid": "Backer-D-C" }, { "family_name": "Booth", "given_name": "R. S.", "clpid": "Booth-R-S" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Emerson", "given_name": "D. T.", "clpid": "Emerson-D-T" }, { "family_name": "Grewing", "given_name": "M.", "clpid": "Grewing-M" }, { "family_name": "Hirabayashi", "given_name": "H.", "clpid": "Hirabayashi-H" }, { "family_name": "Hodges", "given_name": "M. W.", "clpid": "Hodges-M-W" }, { "family_name": "Inoue", "given_name": "M.", "clpid": "Inoue-M" }, { "family_name": "Kobayashi", "given_name": "H.", "clpid": "Kobayashi-H" }, { "family_name": "Krichbaum", "given_name": "T. P.", "clpid": "Krichbaum-T-P" }, { "family_name": "Kus", "given_name": "A. J.", "clpid": "Kus-A-J" }, { "family_name": "Moran", "given_name": "J. M.", "clpid": "Moran-J-M" }, { "family_name": "Morimoto", "given_name": "M.", "clpid": "Morimoto-M" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Plambeck", "given_name": "R. L.", "clpid": "Plambeck-R-L" }, { "family_name": "Predmore", "given_name": "R.", "clpid": "Predmore-R" }, { "family_name": "Rogers", "given_name": "A. E. E.", "clpid": "Rogers-A-E-E" }, { "family_name": "Schalinski", "given_name": "C.", "clpid": "Schalinski-C" }, { "family_name": "Witzel", "given_name": "A.", "clpid": "Witzel-A" }, { "family_name": "Woody", "given_name": "D.", "clpid": "Woody-D-P" }, { "family_name": "Wright", "given_name": "M. C. H.", "clpid": "Wright-M-C-H" }, { "family_name": "Zensus", "given_name": "A.", "clpid": "Zensus-A" } ], "abstract": "We present 15 images from the global mm-VLBI sessions in 1990 April at 100GHz and 1993 April at 86GHz. These observations probe the central engines of the 16 observed AGN's with up to 50 \u00b5as resolution. Among other sources previously observed with \u03bb3mm VLBI we present the first \u03bb3mm maps of 0735+178, 0748+126, 1055+018, 2145+067, and CTA102, in total we have been able to image 13 out of the 16 observed sources. 6 out of the 13 imaged sources observed exhibit curvature and rapid structural changes, although the low dynamic range in two thirds of the maps limits the detection of weak features. Most of the sources have unresolved cores even at this high resolution. There is substantial evidence that the observed sources can be grouped into two general groups: A misaligned population with parsec scale jets in the form of low pitch helices and an aligned population with straight jets with small changes in PA due to intrinsic bends.", "doi": "10.1051/aas:1998282", "issn": "0365-0138", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics Supplement Series", "publication_date": "1998-09", "series_number": "3", "volume": "131", "issue": "3", "pages": "451-467" }, { "id": "authors:gpw8v-kj071", "collection": "authors", "collection_id": "gpw8v-kj071", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180809-161901893", "type": "book_section", "title": "Plans for a 10-m submillimeter-wave telescope at the South Pole", "book_title": "Advanced Technology MMW, Radio, and Terahertz Telescopes", "author": [ { "family_name": "Stark", "given_name": "Antony A.", "clpid": "Stark-A-A" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Israel", "given_name": "Frank P.", "clpid": "Israel-F-P" }, { "family_name": "Menten", "given_name": "Karl M.", "orcid": "0000-0001-6459-0669", "clpid": "Menten-K-M" }, { "family_name": "Peterson", "given_name": "Jeffrey B.", "clpid": "Peterson-J-B" }, { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" }, { "family_name": "Sironi", "given_name": "Giorgio", "clpid": "Sironi-G" }, { "family_name": "Walker", "given_name": "Christopher K.", "clpid": "Walker-C-K" } ], "contributor": [ { "family_name": "Phillips", "given_name": "Thomas G.", "clpid": "Phillips-T-G" } ], "abstract": "A 10 meter diameter submillimeter-wave telescope has been proposed for installation and scientific use at the NSF Amundsen-Scott South Pole Station. Current evidence indicates that the South Pole is the best submillimeter-wave telescope site among all existing or proposed ground-based observatories. Proposed scientific programs place stringent requirements on the optical quality of the telescope design. In particular, reduction of the thermal background and offsets requires an off-axis, unblocked aperture, and the large field of view needed for survey observations requires shaped optics. This mix of design elements is well-suited for large-scale (square degree) mapping of line and continuum radiation from submillimeter-wave sources at moderate spatial resolutions (4 to 60 arcsecond beam size) and high sensitivity (milliJansky flux density levels). The telescope will make arcminute angular scale, high frequency Cosmic Microwave Background measurements from the best possible ground-based site, using an aperture which is larger than is currently possible on orbital or airborne platforms. The telescope design is homologous. Gravitational changes in pointing and focal length will be accommodated by active repositioning of the secondary mirror. The secondary support, consisting of a large, enclosed beam, permits mounting of either a standard set of Gregorian optics, or prime focus instrumentation packages for CMBR studies. A tertiary chopper is located at the exit pupil of the instrument. An optical design with a hyperboloidal primary mirror and a concave secondary mirror provides a flat focal surface. The relatively large classical aberrations present in such an optical arrangement can be small compared to diffraction at submillimeter wavelengths. Effective use of this telescope will require development of large (1000 element) arrays of submillimeter detectors which are background-limited when illuminated by antenna temperatures near 50 K.", "doi": "10.1117/12.317383", "isbn": "9780819428042", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1998-07-31", "pages": "495-506" }, { "id": "authors:936yd-a9c07", "collection": "authors", "collection_id": "936yd-a9c07", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120912-155108732", "type": "article", "title": "A \u03bb = 1.3 Millimeter Aperture Synthesis Molecular Line Survey of Orion Kleinmann-Low", "author": [ { "family_name": "Blake", "given_name": "Geoffrey A.", "orcid": "0000-0003-0787-1610", "clpid": "Blake-G-A" }, { "family_name": "Mundy", "given_name": "L. G.", "clpid": "Mundy-L-G" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Scott", "given_name": "S. L.", "clpid": "Scott-S-L" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Woody", "given_name": "D. P.", "clpid": "Woody-D-P" } ], "abstract": "We present a 1\".3 spatial resolution interferometric spectral line survey of the core of the Orion molecular cloud, obtained with the OVRO millimeter array. Covering 4 GHz bandwidth in total, the survey contains ~100 emission lines from 18 chemical species. The spatial distributions of a number of molecules point to source I near the IRc2 complex as the dominant energy source in the region but do not rule out the presence of additional lower luminosity objects. At arcsecond resolution, the offsets between dust emission and various molecular tracers suggest that the spectacular \"hot core\" emission in the Orion core arises via the heating and ablation of material from the surfaces of very high density clumps located \u2273500 AU from source I and traced by the dust emission. We find no evidence for a strong internal heating source within the hot core condensation(s).", "doi": "10.1086/310347", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "1996-11-20", "series_number": "1", "volume": "472", "issue": "1", "pages": "L49-L52" }, { "id": "authors:a408d-kx645", "collection": "authors", "collection_id": "a408d-kx645", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-163101342", "type": "article", "title": "Accretion Disks around Class 0 Protostars: The Case of VLA 1623", "author": [ { "family_name": "Pudritz", "given_name": "Ralph E.", "clpid": "Pudritz-R-E" }, { "family_name": "Wilson", "given_name": "Christine D.", "orcid": "0000-0001-5817-0991", "clpid": "Wilson-C-D" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Lay", "given_name": "Oliver P.", "clpid": "Lay-O-P" }, { "family_name": "Hills", "given_name": "Richard E.", "clpid": "Hills-R-E" }, { "family_name": "Ward-Thompson", "given_name": "Derek", "orcid": "0000-0003-1140-2761", "clpid": "Ward-Thompson-D" } ], "abstract": "Continuum emission at 220 and 355 GHz from the prototype class 0 source VLA 1623 has been detected using the James Clerk Maxwell Telescope-Caltech Submillimeter Observatory interferometer. Gaussian fits to the data place an upper limit of 70 AU on the half-width at half-maximum radius of the emission, which implies an upper limit of ~175 AU for the cutoff radius of the circumstellar disk in the system. In the context of existing collapse models, this disk could be magnetically supported on the largest scales and have an age of ~6 \u00d7 10^4 yr, consistent with previous suggestions that class 0 sources are quite young. The innermost region of the disk within ~6 AU is likely to be in centrifugal support, which is likely large enough to provide a drive for the outflow according to current theoretical models. Alternatively, if 175 AU corresponds to the centrifugal radius of the disk, the age of the system is ~2 \u00d7 10^5 yr, closer to age estimates for class I sources.", "doi": "10.1086/310309", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1996-10-20", "series_number": "2", "volume": "470", "issue": "2", "pages": "L123-L126" }, { "id": "authors:jr8y9-1s792", "collection": "authors", "collection_id": "jr8y9-1s792", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181211-073511185", "type": "book_section", "title": "Introduction to the JCMT-CSO Interferometer", "book_title": "New Light on Galaxy Evolution", "author": [ { "family_name": "Wiedner", "given_name": "M. C.", "orcid": "0000-0003-3912-7095", "clpid": "Wiedner-M-C" }, { "family_name": "Hills", "given_name": "R. E.", "clpid": "Hills-R-E" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Lay", "given_name": "O. P.", "clpid": "Lay-O-P" } ], "contributor": [ { "family_name": "Bender", "given_name": "Ralf", "clpid": "Bender-R" }, { "family_name": "Davies", "given_name": "Roger L.", "clpid": "Davies-R-L" } ], "abstract": "The James Clerk Maxwell Telescope (JCMT) and the Caltech Submillimeter Observatory (CSO) are located 160m apart on Mauna Kea, Hawaii. Recently they have been linked together to allow the first submillimetre interferometric observations (between 300GHz and 490GHz, soon to 690GHz). Submillimetre observations can be used to probe the physical conditions of molecular clouds and dust in starforming regions. Lines from rotational transitions of molecules such as CO, HCN and HCO+ trace densities, temperatures and masses of molecular gas. The thermal emission of cold dust, typically found in dense clouds, also peaks in the submm regime.", "doi": "10.1017/S0074180900233858", "isbn": "9780792339755", "publisher": "Kluwer", "place_of_publication": "Dordrecht", "publication_date": "1996", "pages": "467" }, { "id": "authors:3f2g5-p2j37", "collection": "authors", "collection_id": "3f2g5-p2j37", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160608-180241053", "type": "article", "title": "Infrared CO Emission from Young Stars: Accretion Disks and Neutral Winds", "author": [ { "family_name": "Chandler", "given_name": "C. J.", "clpid": "Chandler-C-J" }, { "family_name": "Carlstrom", "given_name": "J. E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" } ], "abstract": "We have modeled the emission in the first-overtone rotation-vibration bands of CO from accretion disks and neutral winds. We compare our models with high-resolution spectra of five objects: DG Tau, SVS 13, WL 16, NGC 2024 IRS 2, and S106 IRS 4. The emission from accretion disks with accretion rates of \u02dc10^(-8) to 10^(-7) M_(sun) yr^(-1) successfully reproduce the fluxes, the profiles, and the optical depths of the observed spectra. We also find for several objects that the data are best reproduced by the disk model, with higher K-band extinctions to the central star than those measured by other methods. A simple wind model can also account for the flux and line profile in a number of cases, but fails to reproduce the high optical depth obtained by fitting low-resolution data. Furthermore, unreasonably high mass-loss rates are needed to reproduce the flux. However, if there are sources of heating in the wind preventing it from cooling adiabatically, the CO emission region is larger and lower mass-loss rates may be accommodated.", "doi": "10.1086/175836", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1995-06-20", "volume": "446", "pages": "793-800" }, { "id": "authors:tm96q-gvh70", "collection": "authors", "collection_id": "tm96q-gvh70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120928-133940935", "type": "book_section", "title": "Submillimeter spectroscopy of interstellar hydrides", "book_title": "Airborne Astronomy Symposium on the Galactic Ecosystem, From Gas to Stars to Dust", "author": [ { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" }, { "family_name": "Blake", "given_name": "G. A.", "orcid": "0000-0003-0787-1610", "clpid": "Blake-G-A" }, { "family_name": "Carlstrom", "given_name": "J.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Keene", "given_name": "J.", "clpid": "Keene-Jocelyn" }, { "family_name": "Miller", "given_name": "D.", "clpid": "Miller-D" }, { "family_name": "Schilke", "given_name": "P.", "orcid": "0000-0003-2141-5689", "clpid": "Schilke-P" }, { "family_name": "Ugras", "given_name": "N. G.", "clpid": "Ugras-N-G" } ], "contributor": [ { "family_name": "Haas", "given_name": "Michael R.", "clpid": "Haas-M-R" }, { "family_name": "Davidson", "given_name": "Jacqueline A.", "clpid": "Davidson-J-A" }, { "family_name": "Erickson", "given_name": "Edwin F.", "clpid": "Erickson-E-F" } ], "abstract": "We discuss airborne observations of rotational transitions\nof various hydride molecules in the interstellar medium, including H_2^(18)O\nand HCI. The detection of these transitions is now feasible with a new,\nsensitive submillimeter receiver which has been developed for the NASA\nKuiper Airborne Observatory (KAO) over the past several years.", "isbn": "0-937707-92-9", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1995", "pages": "33-40" }, { "id": "authors:2y1r2-82q72", "collection": "authors", "collection_id": "2y1r2-82q72", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181121-083143567", "type": "book_section", "title": "The Owens Valley Millimeter Array", "book_title": "Astronomy with Millimeter and Submillimeter Wave Interferometry", "author": [ { "family_name": "Scoville", "given_name": "N.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Carlstrom", "given_name": "J.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Sargent", "given_name": "A.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scott", "given_name": "S.", "clpid": "Scott-S" }, { "family_name": "Woody", "given_name": "D.", "clpid": "Woody-D-P" } ], "contributor": [ { "family_name": "Ishiguro", "given_name": "M.", "clpid": "Ishiguro-M" }, { "family_name": "Welch", "given_name": "Wm. J.", "clpid": "Welch-Wm-J" } ], "abstract": "The present status and projected two year developments for the Owens Valley Millimeter Array are described and a brief summary of the astronomical research is presented.", "doi": "10.1017/S0252921100019023", "isbn": "9780937707784", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1994", "pages": "10-17" }, { "id": "authors:aer91-vak89", "collection": "authors", "collection_id": "aer91-vak89", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-154938446", "type": "article", "title": "Atomic Carbon in M82", "author": [ { "family_name": "Schilke", "given_name": "Peter", "orcid": "0000-0003-2141-5689", "clpid": "Schilke-P" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Keene", "given_name": "Jocelyn", "clpid": "Keene-Jocelyn" }, { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" } ], "abstract": "We report observations of C I(^3P_1 - ^3P_0) emission at 492 GHz toward the starburst galaxy M82. Both the C I/C II intensity ratio and the C/CO column density ratio are a factor of 2-5 higher than observed toward Galactic photodissociation regions (PDRs) or predicted by PDR models. We argue that current PDR models are insufficient to explain the observations, and propose that some of the emission is due to atomic carbon existing within molecular clouds. Employing new chemical models, which use a fast H_3^+ dissociative recombination rate, we find that enhanced cosmic-ray flux supplied by supernova remnants in the M82 starburst lead to an enhanced atomic carbon abundance and elevated temperatures deep within the molecular clouds, resulting in a higher C I emissivity than found in previous PDR models.", "doi": "10.1086/187096", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1993-11-10", "series_number": "2", "volume": "417", "issue": "2", "pages": "L67-L70" }, { "id": "authors:1973p-sqc39", "collection": "authors", "collection_id": "1973p-sqc39", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190219-120219409", "type": "book_section", "title": "Progress on a Fixed Tuned Waveguide Receiver Using a Series-Parallel Array of SIS Junctions", "author": [ { "family_name": "Halverson", "given_name": "Nils W.", "clpid": "Halverson-N-W" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Woody", "given_name": "David P.", "clpid": "Woody-D-P" }, { "family_name": "LeDuc", "given_name": "H. G.", "clpid": "LeDuc-H-G" }, { "family_name": "Stern", "given_name": "Jeffrey A.", "clpid": "Stern-J-A" } ], "contributor": [ { "family_name": "Hadley", "given_name": "Brenda", "clpid": "Hadley-B" } ], "abstract": "We are developing a 200 - 300 GHz receiver that incorporates multiple SIS junctions\nin a \"series-parallel\" configuration to achieve broadband impedance matching. At RF\nfrequencies the junctions appear in series through capacitors, and at DC and IF frequencies\nthey appear in parallel through inductors, so that the junctions are impedance matched to\nboth the waveguide and the IF amplifier. Using a single fixed backshort and a full height\nwaveguide, the receiver is designed to have a bandwidth of 100 GHz in the 230 GHz band.\nA similar design has been tested at frequencies around 100 GHz with excellent results by\nShitov et al. (1991) and Vystavkin et al. (1993). Although our initial receiver is designed\noperate in the 200 - 300 GHz band, the design may be readily scaled to higher frequencies.\nIn this paper we discuss computer and scale modeling of the device, fabrication, and\npreliminary test results.", "publisher": "NASA Center for Space Terahertz Technology", "publication_date": "1993-04" }, { "id": "authors:87cq6-ard53", "collection": "authors", "collection_id": "87cq6-ard53", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190219-115249920", "type": "book_section", "title": "Development of a Sideband Separation Receiver at 100 GHz", "author": [ { "family_name": "Akeson", "given_name": "R. L.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Carlstrom", "given_name": "John E.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Woody", "given_name": "David", "clpid": "Woody-D-P" }, { "family_name": "Kawamura", "given_name": "J.", "clpid": "Kawamura-J" }, { "family_name": "Kerr", "given_name": "A. R.", "clpid": "Kerr-A-R" }, { "family_name": "Pan", "given_name": "S. K.", "clpid": "Pan-S-K" }, { "family_name": "Wan", "given_name": "K.", "clpid": "Wan-K" } ], "contributor": [ { "family_name": "Hadley", "given_name": "Brenda", "clpid": "Hadley-B" } ], "abstract": "We have built and tested a prototype SIS receiver operating at 100 GHz to\ntest the feasibility of sideband separation through quadrature mixing at millimeter\nand submillimeter wavelengths. We achieved over 40 dB of separation with no\ndegradation of the mixer noise temperature due to the sideband separation. Both\nthe sky signal and atmospheric noise are separated, greatly reducing the system\ntemperature for millimeter and submillimeter observations in which spectral lines\nare present in only one sideband.", "publisher": "NASA Center for Space Terahertz Technology", "publication_date": "1993" } ]