[ { "id": "authors:dv7bh-r7v86", "collection": "authors", "collection_id": "dv7bh-r7v86", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20221005-265369100.7", "type": "article", "title": "SuperSpec: On-Chip Spectrometer Design, Characterization, and Performance", "author": [ { "family_name": "Redford", "given_name": "J.", "orcid": "0000-0001-6173-0558" }, { "family_name": "Barry", "given_name": "P. S.", "clpid": "Barry-P-S" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Chapman", "given_name": "S.", "clpid": "Chapman-S-C" }, { "family_name": "Glenn", "given_name": "J.", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Janssen", "given_name": "R. M. J.", "clpid": "Janssen-R-M-J" }, { "family_name": "Karkare", "given_name": "K. S.", "orcid": "0000-0002-5215-6993", "clpid": "Karkare-K-S" }, { "family_name": "LeDuc", "given_name": "H. G.", "clpid": "LeDuc-H-G" }, { "family_name": "Mauskopf", "given_name": "P.", "orcid": "0000-0001-6397-5516", "clpid": "Mauskopf-P-D" }, { "family_name": "McGeehan", "given_name": "R.", "orcid": "0000-0001-5306-8285", "clpid": "McGeehan-Ryan" }, { "family_name": "Shirokoff", "given_name": "E.", "orcid": "0000-0002-2757-1423", "clpid": "Shirokoff-Erik" }, { "family_name": "Wheeler", "given_name": "J.", "orcid": "0000-0003-1678-5570", "clpid": "Wheeler-Jordan-D" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "SuperSpec is an integrated, on-chip spectrometer for millimeter and sub-millimeter astronomy intended to pave the way for large-scale, multi-beam spectrometer instruments. SuperSpec is demonstrating a three beam, dual-polarization instrument for observing star formation in distant galaxies on the Large Millimeter Telescope , a 50 m telescope on Volcan Sierra Negra in Mexico. SuperSpec provides moderate resolution (R\u223c270\u2212290) in the 1 mm atmospheric window (200\u2013300 GHz) with a lithographically patterned filterbank on a 3.5 cm x 5.5 cm chip. The filterbank intended for deployment is implemented in niobium, fed by a lensed antenna, and using a extremely low-volume (2.6\u03bcm\u00b3) titanium nitride lumped element kinetic inductor detectors (LEKIDs) as the sensors. The small size of the spectrometer and inherent multiplexibility of the kinetic inductance detectors will allow the future use of SuperSpec in larger, multi-pixel/multi-object spectrometers far beyond the three-pixel spectrometer being demonstrated soon. We report the design of the spectrometer, laboratory characterization of devices for the upcoming SuperSpec deployment. This involves laboratory testing of the filterbank spectral response, and observing noise in the TiN KIDs.", "doi": "10.1007/s10909-022-02866-x", "issn": "0022-2291", "publisher": "Springer", "publication": "Journal of Low Temperature Physics", "publication_date": "2022-09-26" }, { "id": "authors:qyvas-p7r52", "collection": "authors", "collection_id": "qyvas-p7r52", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190509-160652787", "type": "article", "title": "Origins Space Telescope: Predictions for far-IR spectroscopic surveys", "author": [ { "family_name": "Bonato", "given_name": "Matteo", "orcid": "0000-0001-9139-2342", "clpid": "Bonato-M" }, { "family_name": "De Zotti", "given_name": "Gianfranco", "orcid": "0000-0003-2868-2595", "clpid": "De-Zotti-G" }, { "family_name": "Leisawitz", "given_name": "David", "clpid": "Leisawitz-D-T" }, { "family_name": "Negrello", "given_name": "Mattia", "clpid": "Negrello-M" }, { "family_name": "Massardi", "given_name": "Marcella", "clpid": "Massardi-M" }, { "family_name": "Baronchelli", "given_name": "Ivano", "orcid": "0000-0003-0556-2929", "clpid": "Baronchelli-I" }, { "family_name": "Cai", "given_name": "Zhen-Yi", "clpid": "Cai-Zhen-Yi" }, { "family_name": "Bradford", "given_name": "Charles M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Pope", "given_name": "Alexandra", "orcid": "0000-0001-8592-2706", "clpid": "Pope-Alexandra" }, { "family_name": "Murphy", "given_name": "Eric J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Armus", "given_name": "Lee", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" } ], "abstract": "We illustrate the extraordinary potential of the (far-IR) Origins Survey Spectrometer (OSS) on board the Origins Space Telescope (OST) to address a variety of open issues on the co-evolution of galaxies and AGNs. We present predictions for blind surveys, each of 1000 h, with different mapped areas (a shallow survey covering an area of 10 deg^2 and a deep survey of 1 deg^2) and two different concepts of the OST/OSS: with a 5.9 m telescope (Concept 2, our reference configuration) and with a 9.1 m telescope (Concept 1, previous configuration). In 1 000 h, surveys with the reference concept will detect from \u223c1.9\u00d710^6 to \u223c8.7\u00d710^6 lines from \u223c4.8\u00d710^5 to 2.7\u00d710^6 star-forming galaxies and from \u223c1.4\u00d710^4 to \u223c3.8\u00d710^4 lines from \u223c1.3\u00d710^4 to 3.5\u00d710^4 AGNs. The shallow survey will detect substantially more sources than the deep one; the advantage of the latter in pushing detections to lower luminosities/higher redshifts turns out to be quite limited. The OST/OSS will reach, in the same observing time, line fluxes more than one order of magnitude fainter than the SPICA/SMI and will cover a much broader redshift range. In particular it will detect tens of thousands of galaxies at z \u2265 5, beyond the reach of that instrument. The polycyclic aromatic hydrocarbons lines are potentially bright enough to allow the detection of hundreds of thousands of star-forming galaxies up to z \u223c 8.5, i.e. all the way through the reionisation epoch. The proposed surveys will allow us to explore the galaxy\u2013AGN co-evolution up to z \u223c 5.5\u22126 with very good statistics. OST Concept 1 does not offer significant advantages for the scientific goals presented here.", "doi": "10.1017/pasa.2019.8", "issn": "1323-3580", "publisher": "CSIRO Publishing", "publication": "Publications of the Astronomical Society of Australia", "publication_date": "2019-04-24", "volume": "36", "pages": "Art. No. e017" }, { "id": "authors:749y4-20d76", "collection": "authors", "collection_id": "749y4-20d76", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190822-133904279", "type": "article", "title": "Review: far-infrared instrumentation and technological development for the next decade", "author": [ { "family_name": "Farrah", "given_name": "Duncan", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-D" }, { "family_name": "Bradford", "given_name": "Charles M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" }, { "family_name": "Carey", "given_name": "Sean", "orcid": "0000-0002-0221-6871", "clpid": "Carey-S-J" }, { "family_name": "Lis", "given_name": "Dariusz C.", "orcid": "0000-0002-0500-4700", "clpid": "Lis-D-C" }, { "family_name": "Stierwalt", "given_name": "Sabrina", "orcid": "0000-0002-2596-8531", "clpid": "Stierwalt-S" } ], "abstract": "Far-infrared astronomy has advanced rapidly since its inception in the late 1950s, driven by a maturing technology base and an expanding community of researchers. This advancement has shown that observations at far-infrared wavelengths are important in nearly all areas of astrophysics, from the search for habitable planets and the origin of life to the earliest stages of galaxy assembly in the first few hundred million years of cosmic history. The combination of a still-developing portfolio of technologies, particularly in the field of detectors, and a widening ensemble of platforms within which these technologies can be deployed, means that far-infrared astronomy holds the potential for paradigm-shifting advances over the next decade. We examine the current and future far-infrared observing platforms, including ground-based, suborbital, and space-based facilities, and discuss the technology development pathways that will enable and enhance these platforms to best address the challenges facing far-infrared astronomy in the 21st century.", "doi": "10.1117/1.JATIS.5.2.020901", "issn": "2329-4124", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "publication": "Journal of Astronomical Telescopes, Instruments, and Systems", "publication_date": "2019-04", "series_number": "2", "volume": "5", "issue": "2", "pages": "Art. No. 020901" }, { "id": "authors:kqakc-fps17", "collection": "authors", "collection_id": "kqakc-fps17", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180416-085137740", "type": "article", "title": "Hafnium Films and Magnetic Shielding for TIME, A mm-Wavelength Spectrometer Array", "author": [ { "family_name": "Hunacek", "given_name": "J.", "orcid": "0000-0001-7066-226X", "clpid": "Hunacek-J-R" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Butler", "given_name": "V.", "clpid": "Butler-V" }, { "family_name": "Chang", "given_name": "T.-C.", "clpid": "Chang-Tzu-Ching" }, { "family_name": "Cheng", "given_name": "Y.-T.", "orcid": "0000-0002-5437-0504", "clpid": "Cheng-Yun-Ting" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Crites", "given_name": "A.", "clpid": "Crites-A-T" }, { "family_name": "Frez", "given_name": "C.", "clpid": "Frez-C" }, { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Hoscheit", "given_name": "B.", "clpid": "Hoscheit-B" }, { "family_name": "Kim", "given_name": "D. W.", "clpid": "Kim-Dae-Wook" }, { "family_name": "Li", "given_name": "C.-T.", "clpid": "Li-Cheuk-Ting" }, { "family_name": "Marrone", "given_name": "D.", "orcid": "0000-0002-2367-1080", "clpid": "Marrone-D-P" }, { "family_name": "Moncelsi", "given_name": "L.", "orcid": "0000-0002-4242-3015", "clpid": "Moncelsi-Lorenzo" }, { "family_name": "Shirokoff", "given_name": "E.", "clpid": "Shirokoff-E" }, { "family_name": "Steinbach", "given_name": "B.", "clpid": "Steinbach-B-A" }, { "family_name": "Sun", "given_name": "G.", "orcid": "0000-0003-4070-497X", "clpid": "Sun-Guochao" }, { "family_name": "Trumper", "given_name": "I.", "clpid": "Trumper-I" }, { "family_name": "Turner", "given_name": "A.", "clpid": "Turner-A" }, { "family_name": "Uzgil", "given_name": "B.", "orcid": "0000-0001-8526-3464", "clpid": "Uzgil-B-D" }, { "family_name": "Weber", "given_name": "A.", "clpid": "Weber-A" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "TIME is a mm-wavelength grating spectrometer array that will map fluctuations of the 157.7-\u03bcm emission line of singly ionized carbon ([CII]) during the epoch of reionization (redshift z \u223c5\u20139). Sixty transition-edge sensor (TES) bolometers populate the output arc of each of the 32 spectrometers, for a total of 1920 detectors. Each bolometer consists of gold absorber on a \u223c 3 \u00d7 3 mm silicon nitride micro-mesh suspended near the corners by 1 \u00d7 1 \u00d7 500 \u03bcm silicon nitride legs targeting a photon-noise-dominated NEP \u223c1\u00d710^(-17)W/\u221aHz. Hafnium films are explored as a lower-T_c alternative to Ti (500 mK) for TIME TESs, allowing thicker support legs for improved yield. Hf T_c is shown to vary between 250 and 450 mK when varying the resident Ar pressure during deposition. Magnetic shielding designs and simulations are presented for the TIME first-stage SQUIDs. Total axial field suppression is predicted to be 5\u00d710^7.", "doi": "10.1007/s10909-018-1906-3", "issn": "0022-2291", "publisher": "Springer", "publication": "Journal of Low Temperature Physics", "publication_date": "2018-12", "series_number": "5-6", "volume": "193", "issue": "5-6", "pages": "893-900" }, { "id": "authors:yrfaq-gpa77", "collection": "authors", "collection_id": "yrfaq-gpa77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180906-073742934", "type": "article", "title": "SPICA\u2014A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe", "author": [ { "family_name": "Roelfsema", "given_name": "P. R.", "clpid": "Roelfsema-P-R" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" } ], "abstract": "Measurements in the infrared wavelength domain allow direct assessment of the physical state and energy balance of cool matter in space, enabling the detailed study of the processes that govern the formation and evolution of stars and planetary systems in galaxies over cosmic time. Previous infrared missions revealed a great deal about the obscured Universe, but were hampered by limited sensitivity.\nSPICA takes the next step in infrared observational capability by combining a large 2.5-meter diameter telescope, cooled to below 8 K, with instruments employing ultra-sensitive detectors. A combination of passive cooling and mechanical coolers will be used to cool both the telescope and the instruments. With mechanical coolers the mission lifetime is not limited by the supply of cryogen. With the combination of low telescope background and instruments with state-of-the-art detectors SPICA provides a huge advance on the capabilities of previous missions.\nSPICA instruments offer spectral resolving power ranging from R ~50 through 11 000 in the 17\u2013230 \u03bcm domain and R~28.000 spectroscopy between 12 and 18 \u03bcm. SPICA will provide efficient 30\u201337 \u03bcm broad band mapping, and small field spectroscopic and polarimetric imaging at 100, 200 and 350 \u03bcm. SPICA will provide infrared spectroscopy with an unprecedented sensitivity of ~5 \u00d7 10^(\u221220) W m^(\u22122) (5\u03c3/1 h)\u2014over two orders of magnitude improvement over what earlier missions. This exceptional performance leap, will open entirely new domains in infrared astronomy; galaxy evolution and metal production over cosmic time, dust formation and evolution from very early epochs onwards, the formation history of planetary systems.", "doi": "10.1017/pasa.2018.15", "issn": "1323-3580", "publisher": "CSIRO Publishing", "publication": "Publications of the Astronomical Society of Australia", "publication_date": "2018-08-28", "volume": "35", "pages": "Art. No. e030" }, { "id": "authors:m1aew-7vs21", "collection": "authors", "collection_id": "m1aew-7vs21", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180801-094607666", "type": "article", "title": "The Origins Space Telescope", "author": [ { "family_name": "Battersby", "given_name": "Cara", "orcid": "0000-0002-6073-9320", "clpid": "Battersby-C" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Bradford", "given_name": "C. Matt", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" }, { "family_name": "Carey", "given_name": "Sean", "orcid": "0000-0002-0221-6871", "clpid": "Carey-S-J" } ], "abstract": "The Origins Space Telescope, one of four large Mission Concept Studies sponsored by NASA for review in the 2020 US Astrophysics Decadal Survey, will open unprecedented discovery space in the infrared, unveiling our cosmic origins.", "doi": "10.1038/s41550-018-0540-y", "issn": "2397-3366", "publisher": "Nature Publishing Group", "publication": "Nature Astronomy", "publication_date": "2018-08", "series_number": "8", "volume": "2", "issue": "8", "pages": "596-599" }, { "id": "authors:d8skg-ap749", "collection": "authors", "collection_id": "d8skg-ap749", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180430-111957676", "type": "article", "title": "A massive core for a cluster of galaxies at a redshift of 4.3", "author": [ { "family_name": "Miller", "given_name": "T. B.", "clpid": "Miller-T-B" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" } ], "abstract": "Massive galaxy clusters have been found that date to times as early as three billion years after the Big Bang, containing stars that formed at even earlier epochs. The high-redshift progenitors of these galaxy clusters\u2014termed 'protoclusters'\u2014can be identified in cosmological simulations that have the highest overdensities (greater-than-average densities) of dark matter. Protoclusters are expected to contain extremely massive galaxies that can be observed as luminous starbursts. However, recent detections of possible protoclusters hosting such starbursts do not support the kind of rapid cluster-core formation expected from simulations: the structures observed contain only a handful of starbursting galaxies spread throughout a broad region, with poor evidence for eventual collapse into a protocluster. Here we report observations of carbon monoxide and ionized carbon emission from the source SPT2349-56. We find that this source consists of at least 14 gas-rich galaxies, all lying at redshifts of 4.31. We demonstrate that each of these galaxies is forming stars between 50 and 1,000 times more quickly than our own Milky Way, and that all are located within a projected region that is only around 130 kiloparsecs in diameter. This galaxy surface density is more than ten times the average blank-field value (integrated over all redshifts), and more than 1,000 times the average field volume density. The velocity dispersion (approximately 410 kilometres per second) of these galaxies and the enormous gas and star-formation densities suggest that this system represents the core of a cluster of galaxies that was already at an advanced stage of formation when the Universe was only 1.4 billion years old. A comparison with other known protoclusters at high redshifts shows that SPT2349-56 could be building one of the most massive structures in the Universe today.", "doi": "10.1038/s41586-018-0025-2", "issn": "0028-0836", "publisher": "Nature Publishing Group", "publication": "Nature", "publication_date": "2018-04-26", "series_number": "7702", "volume": "556", "issue": "7702", "pages": "469-472" }, { "id": "authors:f9ym3-xvk97", "collection": "authors", "collection_id": "f9ym3-xvk97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170531-140121068", "type": "article", "title": "A Foreground Masking Strategy for [C II] Intensity Mapping Experiments Using Galaxies Selected by Stellar Mass and Redshift", "author": [ { "family_name": "Sun", "given_name": "G.", "orcid": "0000-0003-4070-497X", "clpid": "Sun-Guochao" }, { "family_name": "Moncelsi", "given_name": "L.", "orcid": "0000-0002-4242-3015", "clpid": "Moncelsi-Lorenzo" }, { "family_name": "Viero", "given_name": "M. P.", "clpid": "Viero-M-P" }, { "family_name": "Silva", "given_name": "M. B.", "orcid": "0000-0003-0209-4816", "clpid": "Silva-M-B" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Chang", "given_name": "T.-C.", "clpid": "Chang-Tzu-Ching" }, { "family_name": "Cheng", "given_name": "Y.-T.", "orcid": "0000-0002-5437-0504", "clpid": "Cheng-Yun-Ting" }, { "family_name": "Cooray", "given_name": "A. R.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A-R" }, { "family_name": "Crites", "given_name": "A.", "clpid": "Crites-A-T" }, { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Uzgil", "given_name": "B.", "orcid": "0000-0001-8526-3464", "clpid": "Uzgil-B-D" }, { "family_name": "Hunacek", "given_name": "J. R.", "orcid": "0000-0001-7066-226X", "clpid": "Hunacek-J-R" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "Intensity mapping provides a unique means to probe the epoch of reionization (EoR), when the neutral intergalactic medium was ionized by energetic photons emitted from the first galaxies. The [C II] 158 \u03bcm fine-structure line is typically one of the brightest emission lines of star-forming galaxies and thus a promising tracer of the global EoR star formation activity. However, [C II] intensity maps at 6 \u227e z \u227e 8 are contaminated by interloping CO rotational line emission (3 \u2a7d J_(upp) \u2a7d 6) from lower-redshift galaxies. Here we present a strategy to remove the foreground contamination in upcoming [C II] intensity mapping experiments, guided by a model of CO emission from foreground galaxies. The model is based on empirical measurements of the mean and scatter of the total infrared luminosities of galaxies at z < 3 and with stellar masses M* > 10^8 M\u2299 selected in the K-band from the COSMOS/UltraVISTA survey, which can be converted to CO line strengths. For a mock field of the Tomographic Ionized-carbon Mapping Experiment, we find that masking out the \"voxels\" (spectral\u2013spatial elements) containing foreground galaxies identified using an optimized CO flux threshold results in a z-dependent criterion m^(AB)_K \u227e 22 (or M* \u2273 10^9 M\u2299)) at z < 1 and makes a [C II]/CO_(tot) power ratio of \u227310 at k = 0.1 h/Mpc achievable, at the cost of a moderate \u227e 8% loss of total survey volume.", "doi": "10.3847/1538-4357/aab3e3", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2018-04-01", "series_number": "2", "volume": "856", "issue": "2", "pages": "Art. No. 107" }, { "id": "authors:7vfy7-dwj11", "collection": "authors", "collection_id": "7vfy7-dwj11", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180202-075643915", "type": "article", "title": "Probing the Baryon Cycle of Galaxies with SPICA Mid- and Far-Infrared Observations", "author": [ { "family_name": "van der Tak", "given_name": "F. F. S.", "clpid": "van-der-Tak-F-F-S" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" } ], "abstract": "The SPICA mid- and far-infrared telescope will address fundamental issues in our understanding of star formation and ISM physics in galaxies. A particular hallmark of SPICA is the outstanding sensitivity enabled by the cold telescope, optimised detectors, and wide instantaneous bandwidth throughout the mid- and far-infrared. The spectroscopic, imaging, and polarimetric observations that SPICA will be able to collect will help in clarifying the complex physical mechanisms which underlie the baryon cycle of galaxies. In particular, (i) the access to a large suite of atomic and ionic fine-structure lines for large samples of galaxies will shed light on the origin of the observed spread in star-formation rates within and between galaxies, (ii) observations of HD rotational lines (out to ~10 Mpc) and fine structure lines such as [C ii] 158 \u03bcm (out to ~100 Mpc) will clarify the main reservoirs of interstellar matter in galaxies, including phases where CO does not emit, (iii) far-infrared spectroscopy of dust and ice features will address uncertainties in the mass and composition of dust in galaxies, and the contributions of supernovae to the interstellar dust budget will be quantified by photometry and monitoring of supernova remnants in nearby galaxies, (iv) observations of far-infrared cooling lines such as [O i] 63 \u03bcm from star-forming molecular clouds in our Galaxy will evaluate the importance of shocks to dissipate turbulent energy. The paper concludes with requirements for the telescope and instruments, and recommendations for the observing strategy.", "doi": "10.1017/pasa.2017.67", "issn": "1323-3580", "publisher": "Cambridge University Press", "publication": "Publications of the Astronomical Society of Australia", "publication_date": "2018-01-18", "volume": "35", "pages": "Art. No. e002" }, { "id": "authors:dffb8-n1h85", "collection": "authors", "collection_id": "dffb8-n1h85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180131-103854699", "type": "article", "title": "Galaxy Evolution Studies with the SPace IR Telescope for Cosmology and Astrophysics (SPICA): The Power of IR Spectroscopy", "author": [ { "family_name": "Spinoglio", "given_name": "L.", "clpid": "Spinoglio-L" }, { "family_name": "Armus", "given_name": "L.", "orcid": "0000-0003-3498-2973", "clpid": "Armus-L" }, { "family_name": "Bradford", "given_name": "C.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" } ], "abstract": "IR spectroscopy in the range 12\u2013230 \u03bcm with the SPace IR telescope for Cosmology and Astrophysics (SPICA) will reveal the physical processes governing the formation and evolution of galaxies and black holes through cosmic time, bridging the gap between the James Webb Space Telescope and the upcoming Extremely Large Telescopes at shorter wavelengths and the Atacama Large Millimeter Array at longer wavelengths. The SPICA, with its 2.5-m telescope actively cooled to below 8 K, will obtain the first spectroscopic determination, in the mid-IR rest-frame, of both the star-formation rate and black hole accretion rate histories of galaxies, reaching lookback times of 12 Gyr, for large statistically significant samples. Densities, temperatures, radiation fields, and gas-phase metallicities will be measured in dust-obscured galaxies and active galactic nuclei, sampling a large range in mass and luminosity, from faint local dwarf galaxies to luminous quasars in the distant Universe. Active galactic nuclei and starburst feedback and feeding mechanisms in distant galaxies will be uncovered through detailed measurements of molecular and atomic line profiles. The SPICA's large-area deep spectrophotometric surveys will provide mid-IR spectra and continuum fluxes for unbiased samples of tens of thousands of galaxies, out to redshifts of z ~ 6.", "doi": "10.1017/pasa.2017.48", "issn": "1323-3580", "publisher": "Cambridge University Press", "publication": "Publications of the Astronomical Society of Australia", "publication_date": "2017-11-16", "volume": "34", "pages": "Art. No. e057" }, { "id": "authors:t2ggk-qcj55", "collection": "authors", "collection_id": "t2ggk-qcj55", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171009-152948437", "type": "article", "title": "Stacked Average Far-infrared Spectrum of Dusty Star-forming Galaxies from the Herschel/SPIRE Fourier Transform Spectrometer", "author": [ { "family_name": "Wilson", "given_name": "Derek", "orcid": "0000-0001-6002-423X", "clpid": "Wilson-D-M" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Nayyeri", "given_name": "Hooshang", "orcid": "0000-0001-8242-9983", "clpid": "Nayyeri-H" }, { "family_name": "Bonato", "given_name": "Matteo", "orcid": "0000-0001-9139-2342", "clpid": "Bonato-M" }, { "family_name": "Bradford", "given_name": "Charles M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Clements", "given_name": "David L.", "orcid": "0000-0002-9548-5033", "clpid": "Clements-D-L" }, { "family_name": "De Zotti", "given_name": "Gianfranco", "orcid": "0000-0003-2868-2595", "clpid": "De-Zotti-G" }, { "family_name": "D\u00edaz-Santos", "given_name": "Tanio", "orcid": "0000-0003-0699-6083", "clpid": "D\u00edaz-Santos-T" }, { "family_name": "Farrah", "given_name": "Duncan", "orcid": "0000-0003-1748-2010", "clpid": "Farrah-D" }, { "family_name": "Magdis", "given_name": "Georgios", "orcid": "0000-0002-4872-2294", "clpid": "Magdis-G-E" }, { "family_name": "Micha\u0142owski", "given_name": "Micha\u0142 J.", "clpid": "Micha\u0142owski-M-J" }, { "family_name": "Pearson", "given_name": "Chris", "orcid": "0000-0001-6139-649X", "clpid": "Pearson-C-P" }, { "family_name": "Rigopoulou", "given_name": "Dimitra", "orcid": "0000-0001-6854-7545", "clpid": "Rigopoulou-D" }, { "family_name": "Valtchanov", "given_name": "Ivan", "orcid": "0000-0001-9930-7886", "clpid": "Valtchanov-I" }, { "family_name": "Wang", "given_name": "Lingyu", "clpid": "Wang-Lingyu" }, { "family_name": "Wardlow", "given_name": "Julie", "orcid": "0000-0003-2376-8971", "clpid": "Wardlow-J-L" } ], "abstract": "We present stacked average far-infrared spectra of a sample of 197 dusty star-forming galaxies (DSFGs) at 0.005 < z < 4 using about 90% of the Herschel Space Observatory SPIRE Fourier Transform Spectrometer (FTS) extragalactic data archive based on 3.5 years of science operations. These spectra explore an observed-frame 447\u20131568 GHz frequency range, allowing us to observe the main atomic and molecular lines emitted by gas in the interstellar medium. The sample is subdivided into redshift bins, and a subset of the bins are stacked by infrared luminosity as well. These stacked spectra are used to determine the average gas density and radiation field strength in the photodissociation regions (PDRs) of DSFGs. For the low-redshift sample, we present the average spectral line energy distributions of CO and H_2O rotational transitions and consider PDR conditions based on observed [C I] 370 and 609 \u03bcm, and CO (7-6) lines. For the high-z (0.8 < z < 4) sample, PDR models suggest a molecular gas distribution in the presence of a radiation field that is at least a factor of 10^3 larger than the Milky Way and with a neutral gas density of roughly 10^(4.5)-10^(5.5) cm^(\u22123). The corresponding PDR models for the low-z sample suggest a UV radiation field and gas density comparable to those at high-z. Given the challenges in obtaining adequate far-infrared observations, the stacked average spectra we present here will remain the measurements with the highest signal-to-noise ratio for at least a decade and a half until the launch of the next far-infrared facility.", "doi": "10.3847/1538-4357/aa8cc7", "issn": "1538-4357", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2017-10-10", "series_number": "1", "volume": "848", "issue": "1", "pages": "Art. No. 30" }, { "id": "authors:zqa23-cyx36", "collection": "authors", "collection_id": "zqa23-cyx36", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161205-153231425", "type": "article", "title": "Constraining the ISM Properties of the Cloverleaf Quasar Host Galaxy with Herschel Spectroscopy", "author": [ { "family_name": "Uzgil", "given_name": "Bade D.", "orcid": "0000-0001-8526-3464", "clpid": "Uzgil-B-D" }, { "family_name": "Bradford", "given_name": "C. Matt", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Hailey-Dunsheath", "given_name": "Steve", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Maloney", "given_name": "Philip R.", "clpid": "Maloney-P-R" }, { "family_name": "Aguirre", "given_name": "James E.", "orcid": "0000-0002-4810-666X", "clpid": "Aguirre-J-E" } ], "abstract": "We present Herschel observations of the far-infrared (FIR) fine-structure (FS) lines [C II]158 \u03bcm, [O I]63 \u03bcm, [O III]52 \u03bcm, and [Si II]35 \u03bcm in the z = 2.56 Cloverleaf quasar, and combine them with published data in an analysis of the dense interstellar medium (ISM) in this system. Observed [C II]158 \u03bcm, [O I]63 \u03bcm, and FIR continuum flux ratios are reproduced with photodissociation region (PDR) models characterized by moderate far-ultraviolet (FUV) radiation fields with G_0 = 0.3\u20131 \u00d7 10^3 and atomic gas densities n_H = 3\u20135 \u00d7 10^3 cm^(\u22123), depending on contributions to [C II]158 \u03bcm from ionized gas. We assess the contribution to the [C II]158 \u03bcm flux from an active galactic nucleus (AGN) narrow line region (NLR) using ground-based measurements of the [N II]122 \u03bcm transition, finding that the NLR can contribute at most 20%\u201330% of the observed [C II]158 \u03bcm flux. The PDR density and far-UV radiation fields inferred from the atomic lines are not consistent with the CO emission, indicating that the molecular gas excitation is not solely provided via UV heating from local star formation (SF), but requires an additional heating source. X-ray heating from the AGN is explored, and we find that X-ray-dominated region (XDR) models, in combination with PDR models, can match the CO cooling without overproducing the observed FS line emission. While this XDR/PDR solution is favored given the evidence for both X-rays and SF in the Cloverleaf, we also investigate alternatives for the warm molecular gas, finding that either mechanical heating via low-velocity shocks or an enhanced cosmic-ray ionization rate may also contribute. Finally, we include upper limits on two other measurements attempted in the Herschel program: [C II]158 \u03bcm in FSC 10214 and [O I]63 \u03bcm in APM 08279+5255.", "doi": "10.3847/0004-637X/832/2/209", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2016-12-01", "series_number": "2", "volume": "832", "issue": "2", "pages": "Art. No. 209" }, { "id": "authors:v31k7-47287", "collection": "authors", "collection_id": "v31k7-47287", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161017-144435669", "type": "article", "title": "Spectral Line De-confusion in an Intensity Mapping Survey", "author": [ { "family_name": "Cheng", "given_name": "Yun-Ting", "orcid": "0000-0002-5437-0504", "clpid": "Cheng-Yun-Ting" }, { "family_name": "Chang", "given_name": "Tzu-Ching", "clpid": "Chang-Tzu-Ching" }, { "family_name": "Bock", "given_name": "James J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. Matt", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" } ], "abstract": "Spectral line intensity mapping (LIM) has been proposed as a promising tool to efficiently probe the cosmic reionization and the large-scale structure. Without detecting individual sources, LIM makes use of all available photons and measures the integrated light in the source confusion limit to efficiently map the three-dimensional matter distribution on large scales as traced by a given emission line. One particular challenge is the separation of desired signals from astrophysical continuum foregrounds and line interlopers. Here we present a technique to extract large-scale structure information traced by emission lines from different redshifts, embedded in a three-dimensional intensity mapping data cube. The line redshifts are distinguished by the anisotropic shape of the power spectra when projected onto a common coordinate frame. We consider the case where high-redshift [C ii] lines are confused with multiple low-redshift CO rotational lines. We present a semi-analytic model for [C ii] and CO line estimates based on the cosmic infrared background measurements, and show that with a modest instrumental noise level and survey geometry, the large-scale [C ii] and CO power spectrum amplitudes can be successfully extracted from a confusion-limited data set, without external information. We discuss the implications and limits of this technique for possible LIM experiments.", "doi": "10.3847/0004-637X/832/2/165", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2016-12-01", "series_number": "2", "volume": "832", "issue": "2", "pages": "Art. No. 165" }, { "id": "authors:7dfcc-20n50", "collection": "authors", "collection_id": "7dfcc-20n50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151124-115155769", "type": "article", "title": "Design and Fabrication of TES Detector Modules for the TIME-Pilot [CII] Intensity Mapping Experiment", "author": [ { "family_name": "Hunacek", "given_name": "J. R.", "orcid": "0000-0001-7066-226X", "clpid": "Hunacek-J-R" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Bumble", "given_name": "B.", "clpid": "Bumble-B" }, { "family_name": "Chang", "given_name": "T.-C.", "clpid": "Chang-Tzu-Ching" }, { "family_name": "Cheng", "given_name": "Y.-T.", "orcid": "0000-0002-5437-0504", "clpid": "Cheng-Yun-Ting" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Crites", "given_name": "A.", "clpid": "Crites-A-T" }, { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Gong", "given_name": "Y.", "clpid": "Gong-Y" }, { "family_name": "Kenyon", "given_name": "M.", "clpid": "Kenyon-M" }, { "family_name": "Koch", "given_name": "P.", "orcid": "0000-0003-2777-5861", "clpid": "Koch-P-M" }, { "family_name": "Li", "given_name": "C.-T.", "clpid": "Li-Cheuk-Ting" }, { "family_name": "O'Brient", "given_name": "R.", "clpid": "O'Brient-R-C" }, { "family_name": "Shirokoff", "given_name": "E.", "clpid": "Shirokoff-E" }, { "family_name": "Shiu", "given_name": "C.", "clpid": "Shiu-Corwin" }, { "family_name": "Staniszewski", "given_name": "Z.", "clpid": "Staniszewski-Z-K" }, { "family_name": "Uzgil", "given_name": "B.", "orcid": "0000-0001-8526-3464", "clpid": "Uzgil-B-D" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "We are developing a series of close-packed modular detector arrays for TIME-Pilot, a new mm-wavelength grating spectrometer array that will map the intensity fluctuations of the redshifted 157.7 \u03bcm emission line of singly ionized carbon ([CII]) from redshift z\u223c5 to 9. TIME-Pilot's two banks of 16 parallel-plate waveguide spectrometers (one bank per polarization) will have a spectral range of 183\u2013326 GHz and a resolving power of R\u223c100. The spectrometers use a curved diffraction grating to disperse and focus the light on a series of output arcs, each sampled by 60 transition edge sensor (TES) bolometers with gold micro-mesh absorbers. These low-noise detectors will be operated from a 250 mK base temperature and are designed to have a background-limited NEP of \u223c10^(\u221217) W/Hz^(1/2). This proceeding presents an overview of the detector design in the context of the TIME-Pilot instrument. Additionally, a prototype detector module produced at the Microdevices Laboratory at JPL is shown.", "doi": "10.1007/s10909-015-1359-x", "issn": "0022-2291", "publisher": "Springer", "publication": "Journal of Low Temperature Physics", "publication_date": "2016-08", "series_number": "3", "volume": "184", "issue": "3", "pages": "733-738" }, { "id": "authors:299j6-fz226", "collection": "authors", "collection_id": "299j6-fz226", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151222-084916037", "type": "article", "title": "Low Noise Titanium Nitride KIDs for SuperSpec: A Millimeter-Wave On-Chip Spectrometer", "author": [ { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Shirokoff", "given_name": "E.", "clpid": "Shirokoff-E" }, { "family_name": "Barry", "given_name": "P. S.", "clpid": "Barry-P-S" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Chapman", "given_name": "S.", "clpid": "Chapman-S" }, { "family_name": "Che", "given_name": "G.", "clpid": "Che-G" }, { "family_name": "Glenn", "given_name": "J.", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Hollister", "given_name": "M.", "clpid": "Hollister-M" }, { "family_name": "Kov\u00e1cs", "given_name": "A.", "clpid": "Kov\u00e1cs-A" }, { "family_name": "LeDuc", "given_name": "H. G.", "clpid": "LeDuc-H-G" }, { "family_name": "Mauskopf", "given_name": "P.", "orcid": "0000-0001-6397-5516", "clpid": "Mauskopf-P-D" }, { "family_name": "McKenney", "given_name": "C.", "clpid": "McKenney-C" }, { "family_name": "O'Brient", "given_name": "R.", "clpid": "O'Brient-R" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Reck", "given_name": "T.", "clpid": "Reck-T" }, { "family_name": "Shiu", "given_name": "C.", "clpid": "Shiu-C" }, { "family_name": "Tucker", "given_name": "C. E.", "clpid": "Tucker-C-E" }, { "family_name": "Wheeler", "given_name": "J.", "clpid": "Wheeler-J-C" }, { "family_name": "Williamson", "given_name": "R.", "clpid": "Williamson-R" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "SuperSpec is a novel on-chip spectrometer we are developing for multi-object, moderate resolution (R= 100\u2013500), large bandwidth (\u223c1.65:1), submillimeter and millimeter survey spectroscopy of high-redshift galaxies. The spectrometer employs a filter bank architecture, and consists of a series of half-wave resonators formed by lithographically-patterned superconducting transmission lines. The signal power admitted by each resonator is detected by a lumped element titanium nitride (TiN) kinetic inductance detector operating at 100\u2013200 MHz. We have tested a new prototype device that achieves the targeted R=100R=100 resolving power, and has better detector sensitivity and optical efficiency than previous devices. We employ a new method for measuring photon noise using both coherent and thermal sources of radiation to cleanly separate the contributions of shot and wave noise. We report an upper limit to the detector NEP of 1.4\u00d710^(\u221217) W Hz^(\u22121/2), within 10 % of the photon noise-limited NEP for a ground-based R=100R=100 spectrometer.", "doi": "10.1007/s10909-015-1375-x", "issn": "0022-2291", "publisher": "Springer", "publication": "Journal of Low Temperature Physics", "publication_date": "2016-07", "series_number": "1", "volume": "184", "issue": "1", "pages": "180-187" }, { "id": "authors:0c0h2-ptn58", "collection": "authors", "collection_id": "0c0h2-ptn58", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140520-145421640", "type": "article", "title": "The Tomographic Ionized-Carbon Mapping Experiment (TIME) CII Imaging Spectrometer", "author": [ { "family_name": "Staniszewski", "given_name": "Z.", "clpid": "Staniszewski-Z" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Brevik", "given_name": "J.", "clpid": "Brevik-J" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Gong", "given_name": "Y.", "clpid": "Gong-Y" }, { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "O'Brient", "given_name": "R.", "clpid": "O'Brient-R" }, { "family_name": "Santos", "given_name": "M.", "clpid": "Santos-M" }, { "family_name": "Shirokoff", "given_name": "E.", "clpid": "Shirokoff-E" }, { "family_name": "Silva", "given_name": "M.", "clpid": "Silva-M" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "The Tomographic Ionized-Carbon Mapping Experiment (TIME) and TIME-Pilot are proposed imaging spectrometers to measure reionization and large scale structure at redshifts 5\u20139. We seek to exploit the 158 \u03bcm restframe emission of [CII], which becomes measurable at 200\u2013300 GHz at reionization redshifts. Here we describe the scientific motivation, give an overview of the proposed instrument, and highlight key technological developments underway to enable these measurements.", "doi": "10.1007/s10909-014-1126-4", "issn": "0022-2291", "publisher": "Springer", "publication": "Journal of Low Temperature Physics", "publication_date": "2014-09", "series_number": "5-6", "volume": "176", "issue": "5-6", "pages": "767-772" }, { "id": "authors:9bmzn-nt797", "collection": "authors", "collection_id": "9bmzn-nt797", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140225-134352590", "type": "article", "title": "Design and Performance of SuperSpec: An On-Chip, KID-Based, mm-Wavelength Spectrometer", "author": [ { "family_name": "Shirokoff", "given_name": "E.", "clpid": "Shirokoff-E" }, { "family_name": "Barry", "given_name": "P. S.", "clpid": "Barry-P-S" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Chattopadhyay", "given_name": "G.", "orcid": "0000-0001-7942-5025", "clpid": "Chattopadhyay-G" }, { "family_name": "Day", "given_name": "P.", "clpid": "Day-P" }, { "family_name": "Doyle", "given_name": "S.", "clpid": "Doyle-S" }, { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Hollister", "given_name": "M. I.", "clpid": "Hollister-M-I" }, { "family_name": "Kov\u00e1cs", "given_name": "A.", "clpid": "Kov\u00e1cs-A" }, { "family_name": "LeDuc", "given_name": "H. G.", "clpid": "LeDuc-H-G" }, { "family_name": "McKenney", "given_name": "C. M.", "orcid": "0000-0003-4917-4872", "clpid": "McKenney-C-M" }, { "family_name": "Mauskopf", "given_name": "P.", "orcid": "0000-0001-6397-5516", "clpid": "Mauskopf-P-D" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "O'Brient", "given_name": "R.", "clpid": "O'Brient-R" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Reck", "given_name": "T. J.", "orcid": "0000-0003-1425-0177", "clpid": "Reck-T-J" }, { "family_name": "Swenson", "given_name": "L. J.", "clpid": "Swenson-L-J" }, { "family_name": "Tucker", "given_name": "C. E.", "clpid": "Tucker-C-E" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "SuperSpec is an ultra-compact spectrometer-on-a-chip for mm and submm wavelength astronomy. Its very small size, wide spectral bandwidth, and highly multiplexed detector readout will enable construction of powerful multi-object spectrometers for observations of galaxies at high redshift. SuperSpec is a filter bank with planar, lithographed, superconducting transmission line resonator filters and lumped-element kinetic inductance detectors made from Titanium Nitride. We have built an 81 detector prototype that operates in the 195\u2013310 GHz band. The prototype has a wide-band metal feed horn with a transition to microstrip that feeds the filter bank. The prototype has demonstrated optical filter bank channels with a range of resolving powers from 300 to 700, measured fractional frequency noise of 10^(\u221217)Hz^(\u22121) at 1 Hz.", "doi": "10.1007/s10909-014-1122-8", "issn": "0022-2291", "publisher": "Springer", "publication": "Journal of Low Temperature Physics", "publication_date": "2014-09", "series_number": "5", "volume": "176", "issue": "5", "pages": "657-662" }, { "id": "authors:hh8n2-bw977", "collection": "authors", "collection_id": "hh8n2-bw977", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140129-105001183", "type": "article", "title": "Optical Measurements of SuperSpec: A Millimeter-Wave On-Chip Spectrometer", "author": [ { "family_name": "Hailey-Dunsheath", "given_name": "S.", "orcid": "0000-0002-8504-7988", "clpid": "Hailey-Dunsheath-S" }, { "family_name": "Barry", "given_name": "P. S.", "clpid": "Barry-P-S" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Chattopadhyay", "given_name": "G.", "orcid": "0000-0001-7942-5025", "clpid": "Chattopadhyay-G" }, { "family_name": "Day", "given_name": "P.", "clpid": "Day-P" }, { "family_name": "Doyle", "given_name": "S.", "clpid": "Doyle-S" }, { "family_name": "Hollister", "given_name": "M.", "clpid": "Hollister-M" }, { "family_name": "Kovacs", "given_name": "A.", "clpid": "Kovacs-A" }, { "family_name": "LeDuc", "given_name": "H. G.", "clpid": "LeDuc-H-G" }, { "family_name": "Llombart", "given_name": "N.", "clpid": "Llombart-N" }, { "family_name": "Mauskopf", "given_name": "P.", "orcid": "0000-0001-6397-5516", "clpid": "Mauskopf-P-D" }, { "family_name": "McKenney", "given_name": "C.", "clpid": "McKenney-C" }, { "family_name": "Monroe", "given_name": "R.", "clpid": "Monroe-R" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "O'Brient", "given_name": "R.", "clpid": "O'Brient-R" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Reck", "given_name": "T.", "clpid": "Reck-T" }, { "family_name": "Shirokoff", "given_name": "E.", "clpid": "Shirokoff-E" }, { "family_name": "Swenson", "given_name": "L.", "clpid": "Swenson-L" }, { "family_name": "Tucker", "given_name": "C. E.", "clpid": "Tucker-C-E" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "SuperSpec is a novel on-chip spectrometer we are developing for (sub)millimeter wavelength astronomy. Our approach utilizes a filterbank of moderate resolution (R\u223c500) channels, coupled to lumped element kinetic inductance detectors (KIDs), all integrated onto a single silicon chip. The channels are half-wave resonators formed by lithographically depositing segments of superconducting transmission line, and the KIDs are titanium nitride resonators. Here we present optical measurements of a first generation prototype, operating in the 180\u2013280 GHz frequency range. We have used a coherent source to measure the spectral profiles of 17 channels, which achieve linewidths corresponding to quality factors as high as Q__(filt)=700, consistent with the designed values plus additional dissipation characterized by Q_i\u22481440. We have also used a Fourier Transform Spectrometer to characterize the spectral purity of all 72 channels on the chip, and measure typical out of band responses \u223c30 dB below the peak response.", "doi": "10.1007/s10909-013-1068-2", "issn": "0022-2291", "publisher": "Springer", "publication": "Journal of Low Temperature Physics", "publication_date": "2014-09", "series_number": "5-6", "volume": "176", "issue": "5-6", "pages": "841-847" }, { "id": "authors:qj7sp-ywb34", "collection": "authors", "collection_id": "qj7sp-ywb34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130502-132215358", "type": "article", "title": "A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34", "author": [ { "family_name": "Riechers", "given_name": "Dominik A.", "orcid": "0000-0001-9585-1462", "clpid": "Riechers-D-A" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Kov\u00e1cs", "given_name": "A.", "clpid": "Kov\u00e1cs-A" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Viero", "given_name": "M.", "clpid": "Viero-M-P" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts\u2014that is, increased rates of star formation\u2014in the most massive dark-matter haloes at early epochs. However, it remains unknown how soon after the Big Bang massive starburst progenitors exist. The measured redshift (z) distribution of dusty, massive starbursts has long been suspected to be biased low in z owing to selection effects, as confirmed by recent findings of systems with redshifts as high as ~5 (refs 2\u20134). Here we report the identification of a massive starburst galaxy at z = 6.34 through a submillimetre colour-selection technique. We unambiguously determined the redshift from a suite of molecular and atomic fine-structure cooling lines. These measurements reveal a hundred billion solar masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at least 40 per cent of the baryonic mass. A 'maximum starburst' converts the gas into stars at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoch. Despite the overall downturn in cosmic star formation towards the highest redshifts, it seems that environments mature enough to form the most massive, intense starbursts existed at least as early as 880 million years after the Big Bang.", "doi": "10.1038/nature12050", "issn": "0028-0836", "publisher": "Nature Publishing Group", "publication": "Nature", "publication_date": "2013-04-18", "series_number": "7445", "volume": "496", "issue": "7445", "pages": "329-333" }, { "id": "authors:z2dt4-3x583", "collection": "authors", "collection_id": "z2dt4-3x583", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130507-093655427", "type": "article", "title": "H_2O emission in high-z ultra-luminous infrared galaxies", "author": [ { "family_name": "Omont", "given_name": "A.", "orcid": "0000-0002-4721-3922", "clpid": "Omont-A" }, { "family_name": "Riechers", "given_name": "D.", "orcid": "0000-0001-9585-1462", "clpid": "Riechers-D-A" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" } ], "abstract": "Using the IRAM Plateau de Bure interferometer (PdBI), we report the detection of water vapor in six new lensed ultra-luminous starburst galaxies at high redshift, discovered in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). The sources are detected either in the 2_(02)\u22121_(11) or 2_(11)\u22122_(02) H_2O emission lines with integrated line fluxes ranging from 1.8 to 14 Jy km s^(-1). The corresponding apparent luminosities are \u03bcL_(H2O) ~ 3\u221212 \u00d7 10^8\u2009L_\u2299, where \u03bc is the lensing magnification factor (3 < \u03bc < 12). These results confirm that H_2O lines are among the strongest molecular lines in high-z ultra-luminous starburst galaxies, with intensities almost comparable to those of the high-J CO lines, and similar profiles and line widths (~200\u2212900 km s^(-1)). With the current sensitivity of the PdBI, the water lines can therefore easily be detected in high-z lensed galaxies (with F(500 \u03bcm)\u2009>\u2009100\u2009mJy) discovered in the Herschel surveys. Correcting the luminosities for amplification, using existing lensing models, L_(H2O) is found to have a strong dependence on the infrared luminosity, varying as ~L_(IR)^(1.2). This relation, which needs to be confirmed with better statistics, may indicate a role of radiative (infrared) excitation of the H_2O lines, and implies that high-z galaxies with L_(IR) \u2273 10^(13)\u2009L_\u2299 tend to be very strong emitters in water vapor, that have no equivalent in the local universe.", "doi": "10.1051/0004-6361/201220811", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2013-03", "volume": "551", "pages": "Art. No. A115" }, { "id": "authors:pz576-cjq62", "collection": "authors", "collection_id": "pz576-cjq62", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121101-142033089", "type": "article", "title": "Measurements of CO Redshifts with Z-Spec for Lensed Submillimeter Galaxies Discovered in the H-ATLAS Survey", "author": [ { "family_name": "Lupu", "given_name": "R. E.", "clpid": "Lupu-R-E" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Cooke", "given_name": "J.", "orcid": "0000-0001-5703-2108", "clpid": "Cooke-J" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We present new observations from Z-Spec, a broadband 185-305 GHz spectrometer, of five submillimeter bright lensed sources selected from the Herschel-Astrophysical Terahertz Large Area Survey science demonstration phase catalog. We construct a redshift-finding algorithm using combinations of the signal to noise of all the lines falling in the Z-Spec bandpass to determine redshifts with high confidence, even in cases where the signal to noise in individual lines is low. We measure the dust continuum in all sources and secure CO redshifts for four out of five (z ~ 1.5-3). In one source, SDP.17, we tentatively identify two independent redshifts and a water line, confirmed at z = 2.308. Our sources have properties characteristic of dusty starburst galaxies, with magnification-corrected star formation rates of 10^(2\u20133) M_\u2609 yr^(\u20131). Lower limits for the dust masses (~a few 10^8 M_\u2609) and spatial extents (~1 kpc equivalent radius) are derived from the continuum spectral energy distributions, corresponding to dust temperatures between 54 and 69 K. In the local thermodynamic equilibrium (LTE) approximation, we derive relatively low CO excitation temperatures (\u2272100 K) and optical depths (\u03c4 \u2272 1). Performing a non-LTE excitation analysis using RADEX, we find that the CO lines measured by Z-Spec (from J = 4 \u2192 3 to 10 \u2192 9, depending on the galaxy) localize the best solutions to either a high-temperature/low-density region or a low/temperature/high-density region near the LTE solution, with the optical depth varying accordingly. Observations of additional CO lines, CO(1-0) in particular, are needed to constrain the non-LTE models.", "doi": "10.1088/0004-637X/757/2/135", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-10-01", "series_number": "2", "volume": "757", "issue": "2", "pages": "Art. No. 135" }, { "id": "authors:d9wkw-zvg05", "collection": "authors", "collection_id": "d9wkw-zvg05", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120516-092304643", "type": "article", "title": "High Spectral Resolution Measurement of the Sunyaev\u2013Zel'dovich Effect Null with Z-Spec", "author": [ { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" }, { "family_name": "Aguirre", "given_name": "J.", "clpid": "Aguirre-J" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Czakon", "given_name": "N. G.", "clpid": "Czakon-N-G" }, { "family_name": "Glenn", "given_name": "J.", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Golwala", "given_name": "S. R.", "orcid": "0000-0002-1098-7174", "clpid": "Golwala-S-R" }, { "family_name": "Lupu", "given_name": "R.", "clpid": "Lupu-R" }, { "family_name": "Maloney", "given_name": "P.", "clpid": "Maloney-P" }, { "family_name": "Mauskopf", "given_name": "P.", "clpid": "Mauskopf-P" }, { "family_name": "Million", "given_name": "E.", "clpid": "Million-E-T" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Naylor", "given_name": "B.", "clpid": "Naylor-B" }, { "family_name": "Nguyen", "given_name": "H.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Rosenman", "given_name": "M.", "clpid": "Rosenman-M" }, { "family_name": "Sayers", "given_name": "J.", "orcid": "0000-0002-8213-3784", "clpid": "Sayers-Jack" }, { "family_name": "Scott", "given_name": "K. S.", "clpid": "Scott-K-S" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "The Sunyaev-Zel'dovich (SZ) effect spectrum crosses through a null where \u0394T_CMB = 0 near \u03bd_0 = 217 GHz. In a cluster of galaxies, \u03bd0 can be shifted from the canonical thermal SZ effect value by corrections to the SZ effect scattering due to the properties of the inter-cluster medium. We have measured the SZ effect in the hot galaxy cluster RX J 1347.5 \u2013 1145 with Z-Spec, an R ~ 300 grating spectrometer sensitive between 185 and 305 GHz. These data comprise a high spectral resolution measurement around the null of the SZ effect and clearly exhibit the transition from negative to positive \u0394T_CMB over the Z-Spec band. The SZ null position is measured to be \u03bd_0 = 225.8 \u00b1 2.5(stat.) \u00b1 1.2(sys.) GHz, which differs from the canonical null frequency by 3.0\u03c3 and is evidence for modifications to the canonical thermal SZ effect shape. Assuming the measured shift in \u03bd0 is due only to relativistic corrections to the SZ spectrum, we place the limit kT_e = 17.1 \u00b1 5.3 keV from the zero-point measurement alone. By simulating the response of the instrument to the sky, we are able to generate likelihood functions in {y_0, T_e, v_pec} space. For v_pec = 0 km s^(\u20131), we measure the best-fitting SZ model to be y_0 = 4.6^(+0.6)_(\u20130.9) \u00d7 10^(\u20134), T_e, 0 = 15.2^(+12)_(\u20137.4) keV. When v pec is allowed to vary, a most probable value of v_pec = + 450 \u00b1 810 km s^(\u20131) is found.", "doi": "10.1088/0004-637X/749/2/114", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-04-20", "series_number": "2", "volume": "749", "issue": "2", "pages": "114" }, { "id": "authors:jqwep-kbb08", "collection": "authors", "collection_id": "jqwep-kbb08", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120403-080450129", "type": "article", "title": "Intensity Mapping of the [C II] Fine Structure Line During the Epoch of Reionization", "author": [ { "family_name": "Gong", "given_name": "Yan", "clpid": "Gong-Yan" }, { "family_name": "Cooray", "given_name": "Asantha", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Silva", "given_name": "Marta", "clpid": "Silva-M" }, { "family_name": "Santos", "given_name": "Mario G.", "orcid": "0000-0003-3892-3073", "clpid": "Santos-M-G" }, { "family_name": "Bock", "given_name": "James", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. Matt", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Zemcov", "given_name": "Michael", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" } ], "abstract": "The atomic C II fine-structure line is one of the brightest lines in a typical star-forming galaxy spectrum with a luminosity ~0.1%-1% of the bolometric luminosity. It is potentially a reliable tracer of the dense gas distribution at high redshifts and could provide an additional probe to the era of reionization. By taking into account the spontaneous, stimulated, and collisional emission of the C II line, we calculate the spin temperature and the mean intensity as a function of the redshift. When averaged over a cosmologically large volume, we find that the C II emission from ionized carbon in individual galaxies is larger than the signal generated by carbon in the intergalactic medium. Assuming that the C II luminosity is proportional to the carbon mass in dark matter halos, we also compute the power spectrum of the C II line intensity at various redshifts. In order to avoid the contamination from CO rotational lines at low redshift when targeting a C II survey at high redshifts, we propose the cross-correlation of C II and 21 cm line emission from high redshifts. To explore the detectability of the C II signal from reionization, we also evaluate the expected errors on the C II power spectrum and C II-21 cm cross power spectrum based on the design of the future millimeter surveys. We note that the C II-21 cm cross power spectrum contains interesting features that capture physics during reionization, including the ionized bubble sizes and the mean ionization fraction, which are challenging to measure from 21 cm data alone. We propose an instrumental concept for the reionization C II experiment targeting the frequency range of ~200-300 GHz with 1, 3, and 10 m apertures and a bolometric spectrometer array with 64 independent spectral pixels with about 20,000 bolometers.", "doi": "10.1088/0004-637X/745/1/49", "issn": "0004-637X", "publisher": "American Astro745nomical Society", "publication": "Astrophysical Journal", "publication_date": "2012-01-20", "series_number": "1", "volume": "745", "issue": "1", "pages": "Art. No. 49" }, { "id": "authors:kgr1r-nsy06", "collection": "authors", "collection_id": "kgr1r-nsy06", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111209-094523752", "type": "article", "title": "The Water Vapor Spectrum of APM 08279+5255: X-Ray Heating and Infrared Pumping over Hundreds of Parsecs", "author": [ { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Bolatto", "given_name": "A. D.", "orcid": "0000-0002-5480-5686", "clpid": "Bolatto-A-D" }, { "family_name": "Maloney", "given_name": "P. R.", "clpid": "Maloney-P-R" }, { "family_name": "Aguirre", "given_name": "J. E.", "orcid": "0000-0002-4810-666X", "clpid": "Aguirre-J-E" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Glenn", "given_name": "J.", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Kamenetzky", "given_name": "J.", "clpid": "Kamenetzky-J" }, { "family_name": "Lupu", "given_name": "R.", "clpid": "Lupu-R-E" }, { "family_name": "Matsuhara", "given_name": "H.", "clpid": "Matsuhara-Hideo" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Naylor", "given_name": "B. J.", "clpid": "Naylor-B-J" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Scott", "given_name": "K.", "clpid": "Scott-K-S" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We present the rest-frame 200-320 \u03bcm spectrum of the z = 3.91 quasar APM 08279+5255, obtained with Z-Spec at the Caltech Submillimeter Observatory. In addition to the J = 8 \u2192 7 to J = 13 \u2192 12 CO rotational transitions which dominate the CO cooling, we find six transitions of water originating at energy levels ranging up to 643 K. Most are first detections at high redshift, and we have confirmed one transition with CARMA. The CO cooling is well described by our X-ray dominated region (XDR) model, assuming L_(1-100 keV) ~ 1 \u00d7 10^(46) erg s^(\u20131), and that the gas is distributed over a 550-pc size scale, as per the now-favored \u03bc = 4 lensing model. The total observed cooling in water corresponds to 6.5 \u00d7 109 L_\u2609, comparable to that of CO. We compare the water spectrum with that of Mrk 231, finding that the intensity ratios among the high-lying lines are similar, but with a total luminosity scaled up by a factor of ~50. Using this scaling, we estimate an average water abundance relative to H_2 of 1.4 \u00d7 10^(\u20137), a good match to the prediction of the chemical network in the XDR model. As with Mrk 231, the high-lying water transitions are excited radiatively via absorption in the rest-frame far-infrared, and we show that the powerful dust continuum in APM 08279+5255 is more than sufficient to pump this massive reservoir of warm water vapor.", "doi": "10.1088/2041-8205/741/2/L37", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "2011-11-10", "series_number": "2", "volume": "741", "issue": "2", "pages": "L37" }, { "id": "authors:b4b0d-akx18", "collection": "authors", "collection_id": "b4b0d-akx18", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111004-113055775", "type": "article", "title": "Modeling of the HerMES Submillimeter Source Lensed by a Dark Matter Dominated Foreground Group of Galaxies", "author": [ { "family_name": "Gavazzi", "given_name": "R.", "clpid": "Gavazzo-R" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Blain", "given_name": "A.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" }, { "family_name": "Fu", "given_name": "H.", "orcid": "0000-0001-9608-6395", "clpid": "Fu-Hai" }, { "family_name": "Levenson", "given_name": "L.", "clpid": "Levenson-L" }, { "family_name": "Mahabal", "given_name": "A.", "orcid": "0000-0003-2242-0244", "clpid": "Mahabal-A-A" }, { "family_name": "Murphy", "given_name": "E.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Riechers", "given_name": "D.", "orcid": "0000-0001-9585-1462", "clpid": "Riechers-D-A" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Shupe", "given_name": "D. L.", "orcid": "0000-0003-4401-0430", "clpid": "Shupe-David-L" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Xu", "given_name": "C. K.", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We present the results of a gravitational lensing analysis of the bright z_s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be \u03bc = 10.9 \u00b1 0.7. We measure the half-light radius R_(eff) of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R_(eff),* = [2.0 \u00b1 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (R_(eff,gas) = [1.1 \u00b1 0.5] kpc) by mapping back in the source plane the CO (J = 5 \u2192 4) transition line emission. The lens modeling yields a relatively large Einstein radius R_(Ein) = 4\".10 \u00b1 0\".02, corresponding to a deflector velocity dispersion of [483 \u00b1 16] km s^(\u20131). This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z_l ~ 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f_(dm)(< R_(Ein)) ~ 80%. This fraction reduces to f_(dm)(< R_(eff,G1) \u2243 4.5 kpc) ~ 47% within the effective radius of the main deflecting galaxy of stellar mass M_(*,G1) = [8.5 \u00b1 1.6] \u00d7 10^(11) M_\u2609. At this smaller scale the dark matter fraction is consistent with results already found for massive lensing ellipticals at z ~ 0.2 from the Sloan Lens ACS Survey.", "doi": "10.1088/0004-637X/738/2/125", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2011-09-10", "series_number": "2", "volume": "738", "issue": "2", "pages": "Art. No. 125" }, { "id": "authors:stkd9-dth76", "collection": "authors", "collection_id": "stkd9-dth76", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110927-132054052", "type": "article", "title": "Detection of an ultrabright submillimetre galaxy in the\n Subaru/XMM\u2013Newton Deep Field using AzTEC/ASTE", "author": [ { "family_name": "Ikarashi", "given_name": "S.", "clpid": "Ikarashi-Soh" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We report on the detection of an extremely bright (\u223c37 mJy at 1100\u2002\u03bcm and \u223c91 mJy at 880\u2002\u03bcm) submillimetre galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi), discovered in the 1100\u2002\u03bcm observations of the Subaru/XMM\u2013Newton\u2002Deep Field\u2002using AzTEC on ASTE. Subsequent CARMA 1300-\u03bcm and SMA 880-\u03bcm observations successfully pinpoint the location of Orochi and suggest that it has two components, one extended [full width at half-maximum (FWHM) of \u223c4 arcsec] and one compact (unresolved). Z-Spec on CSO has also been used to obtain a wide-band spectrum from 190 to 308 GHz, although no significant emission/absorption lines were found. The derived upper limit to the line-to-continuum flux ratio is 0.1\u20130.3 (2\u03c3) across the Z-Spec band.\nBased on the analysis of the derived spectral energy distribution from optical to radio wavelengths of possible counterparts near the SMA/CARMA peak position, we suggest that Orochi is a lensed, optically dark SMG lying at\u2002z\u2002\u223c 3.4 behind a foreground, optically visible (but red) galaxy at\u2002z\u2002\u223c 1.4. The deduced apparent (i.e., no correction for magnification) infrared luminosity (L_(IR)) and star formation rate (SFR) are 6 \u00d7 10^(13) L_\u2299 and 11 000 M_\u2299 yr^(\u22121), respectively, assuming that the\u2002L_(IR) is dominated by star formation. These values suggest that Orochi will consume its gas reservoir within a short time-scale (3 \u00d7 10^7 yr), which is indeed comparable to those in extreme starbursts like the centres of local ultraluminous infrared galaxies (ULIRGs).", "doi": "10.1111/j.1365-2966.2011.18918.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2011-08", "series_number": "4", "volume": "415", "issue": "4", "pages": "3081-3096" }, { "id": "authors:x5c59-xw044", "collection": "authors", "collection_id": "x5c59-xw044", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110613-083728464", "type": "article", "title": "Observation of H_2O in a strongly lensed Herschel-ATLAS source at z = 2.3", "author": [ { "family_name": "Omont", "given_name": "A.", "orcid": "0000-0002-4721-3922", "clpid": "Omont-A" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Riechers", "given_name": "D.", "orcid": "0000-0001-9585-1462", "clpid": "Riechers-D-A" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "The Herschel survey, H-ATLAS, with its large areal coverage, has recently discovered a number of bright, strongly lensed high-z submillimeter galaxies. The strong magnification makes it possible to study molecular species other than CO, which are otherwise difficult to observe in high-z galaxies. Among the lensed galaxies already identified by H-ATLAS, the source J090302.9-014127B (SDP.17b) at z = 2.305 is remarkable because of its excitation conditions and a tentative detection of the H_2O 2_(02)-1_(11) emission line (Lupu et al. 2010, ApJ, submitted). We report observations of this line in SDP.17b using the IRAM interferometer equipped with its new 277\u2013371\u2009GHz receivers. The H_2O line is detected at a redshift of z = 2.3049 \u00b1 0.0006, with a flux of 7.8 \u00b1 0.5 Jy km s^(-1) and a FWHM of 250 \u00b1 60 \u2009 km \u2009 s^(-1). The new flux is 2.4 times weaker than the previous tentative detection, although both remain marginally consistent within 1.6\u03c3. The intrinsic line luminosity and ratio of H_2O(2_(02) \u2212 1_(11))/CO(8 \u2212 7) are comparable with those of the nearby starburst/enshrouded-AGN Mrk 231, and the ratio I(H_2O)/L_(FIR) is even higher, suggesting that SDP.17b could also host a luminous AGN. The detection of a strong H_2O 2_(02) \u2212 1_(11) line in SDP.17b implies an efficient excitation mechanism of the water levels that must occur in very dense and warm interstellar gas probably similar to Mrk 231.", "doi": "10.1051/0004-6361/201116921", "issn": "0004-6361", "publisher": "EDP Sciences", "publication": "Astronomy and Astrophysics", "publication_date": "2011-06", "volume": "530", "pages": "Art. No. L3" }, { "id": "authors:qz1tt-9kp38", "collection": "authors", "collection_id": "qz1tt-9kp38", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110531-132533695", "type": "article", "title": "Redshift Determination and CO Line Excitation Modeling for the Multiply Lensed Galaxy HLSW-01", "author": [ { "family_name": "Scott", "given_name": "K. S.", "clpid": "Scott-K-S" }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Carpenter", "given_name": "J. M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Riechers", "given_name": "D.", "orcid": "0000-0001-9585-1462", "clpid": "Riechers-D-A" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We report on the redshift measurement and CO line excitation of HERMES J105751.1+573027 (HLSW-01), a strongly lensed submillimeter galaxy discovered in Herschel/SPIRE observations as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). HLSW-01 is an ultra-luminous galaxy with an intrinsic far-infrared luminosity of L _(FIR) = 1.4 \u00d7 10^(13) L _\u2299, and is lensed by a massive group of galaxies into at least four images with a total magnification of \u03bc = 10.9 \u00b1 0.7. With the 100 GHz instantaneous bandwidth of the Z-Spec instrument on the Caltech Submillimeter Observatory, we robustly identify a redshift of z = 2.958 \u00b1 0.007 for this source, using the simultaneous detection of four CO emission lines (J = 7 \u2192 6, J = 8 \u2192 7, J = 9 \u2192 8, and J = 10 \u2192 9). Combining the measured line fluxes for these high-J transitions with the J = 1 \u2192 0, J = 3 \u2192 2, and J = 5 \u2192 4 line fluxes measured with the Green Bank Telescope, the Combined Array for Research in Millimeter Astronomy, and the Plateau de Bure Interferometer, respectively, we model the physical properties of the molecular gas in this galaxy. We find that the full CO spectral line energy distribution is described well by warm, moderate-density gas with T _(kin) = 86-235 K and n_H_2 = (1.1-3.5)x10^3 cm^(\u20133). However, it is possible that the highest-J transitions are tracing a small fraction of very dense gas in molecular cloud cores, and two-component models that include a warm/dense molecular gas phase with T _(kin) ~ 200 K, n_H_2 ~ 10^5 cm^(\u20133) are also consistent with these data. Higher signal-to-noise measurements of the J _(up) \u2265 7 transitions with high spectral resolution, combined with high spatial resolution CO maps, are needed to improve our understanding of the gas excitation, morphology, and dynamics of this interesting high-redshift galaxy.", "doi": "10.1088/0004-637X/733/1/29", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2011-05-20", "series_number": "1", "volume": "733", "issue": "1", "pages": "Art. No. 29" }, { "id": "authors:2qa3f-jy958", "collection": "authors", "collection_id": "2qa3f-jy958", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110824-083050070", "type": "article", "title": "Discovery of a Multiply Lensed Submillimeter Galaxy in Early HerMES Herschel/SPIRE Data", "author": [ { "family_name": "Conley", "given_name": "A.", "clpid": "Conley-A" }, { "family_name": "Cooray", "given_name": "A.", "orcid": "0000-0002-3892-0190", "clpid": "Cooray-A" }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "Blain", "given_name": "A.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Bridge", "given_name": "C.", "clpid": "Bridge-C" }, { "family_name": "Carpenter", "given_name": "J. M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Dowell", "given_name": "C. D.", "clpid": "Dowell-C-D" }, { "family_name": "Fu", "given_name": "H.", "orcid": "0000-0001-9608-6395", "clpid": "Fu-Hai" }, { "family_name": "Levenson", "given_name": "L.", "clpid": "Levenson-L" }, { "family_name": "Mahabal", "given_name": "A.", "orcid": "0000-0003-2242-0244", "clpid": "Mahabal-A-A" }, { "family_name": "Murphy", "given_name": "E.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Riechers", "given_name": "D.", "orcid": "0000-0001-9585-1462", "clpid": "Riechers-D-A" }, { "family_name": "Schulz", "given_name": "B.", "clpid": "Schulz-B" }, { "family_name": "Shupe", "given_name": "D. L.", "orcid": "0000-0003-4401-0430", "clpid": "Shupe-David-L" }, { "family_name": "Viero", "given_name": "M. P.", "clpid": "Viero-M-P" }, { "family_name": "Xu", "given_name": "C. K.", "orcid": "0000-0002-1588-6700", "clpid": "Xu-C-Kevin" }, { "family_name": "Zemcov", "given_name": "M.", "orcid": "0000-0001-8253-1451", "clpid": "Zemcov-M" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We report the discovery of a bright (f(250 \u03bcm)>400 mJy), multiply lensed submillimeter galaxy HERMES J105751.1+573027 in Herschel/SPIRE Science Demonstration Phase data from the HerMES project. Interferometric 880 \u03bcm Submillimeter Array observations resolve at least four images with a large separation of ~9\". A high-resolution adaptive optics K_p image with Keck/NIRC2 clearly shows strong lensing arcs. Follow-up spectroscopy gives a redshift of z = 2.9575, and the lensing model gives a total magnification of \u03bc ~ 11 \u00b1 1. The large image separation allows us to study the multi-wavelength spectral energy distribution (SED) of the lensed source unobscured by the central lensing mass. The far-IR/millimeter-wave SED is well described by a modified blackbody fit with an unusually warm dust temperature, 88 \u00b1 3 K. We derive a lensing-corrected total IR luminosity of (1.43 \u00b1 0.09) \u00d7 10^(13) L_\u2609, implying a star formation rate of ~2500 M_\u2609 yr^(\u20131). However, models primarily developed from brighter galaxies selected at longer wavelengths are a poor fit to the full optical-to-millimeter SED. A number of other strongly lensed systems have already been discovered in early Herschel data, and many more are expected as additional data are collected.", "doi": "10.1088/2041-8205/732/2/L35", "issn": "2041-8205", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal Letters", "publication_date": "2011-05-10", "series_number": "2", "volume": "732", "issue": "2", "pages": "Art. No. L35" }, { "id": "authors:xs07x-yvw50", "collection": "authors", "collection_id": "xs07x-yvw50", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110518-111113979", "type": "article", "title": "The Dense Molecular Gas in the Circumnuclear Disk of NGC 1068", "author": [ { "family_name": "Kamenetzky", "given_name": "J.", "clpid": "Kamenetzky-J" }, { "family_name": "Glenn", "given_name": "J.", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Maloney", "given_name": "P. R.", "clpid": "Maloney-P-R" }, { "family_name": "Aguirre", "given_name": "J. E.", "orcid": "0000-0002-4810-666X", "clpid": "Aguirre-J-E" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Earle", "given_name": "L.", "clpid": "Earle-L" }, { "family_name": "Inami", "given_name": "H.", "orcid": "0000-0003-4268-0393", "clpid": "Inami-Hanae" }, { "family_name": "Matsuhara", "given_name": "H.", "clpid": "Matsuhara-Hideo" }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Naylor", "given_name": "B. J.", "clpid": "Naylor-B-J" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We present a 190-307 GHz broadband spectrum obtained with Z-Spec of NGC 1068 with new measurements of molecular rotational transitions. After combining our measurements with those previously published and considering the specific geometry of this Seyfert 2 galaxy, we conduct a multi-species Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+. We find that these molecules trace warm (T>100 K) gas of H_2 number densities 10^(4.2)-10^(4.9) cm^(\u20133). Our models also place strong constraints on the column densities and relative abundances of these molecules, as well as on the total mass in the circumnuclear disk. Using the uniform calibration afforded by the broad Z-Spec bandpass, we compare our line ratios to X-ray-dominated region (XDR) and photon-dominated region models. The majority of our line ratios are consistent with the XDR models at the densities indicated by the likelihood analysis, lending substantial support to the emerging interpretation that the energetics in the circumnuclear disk of NGC 1068 are dominated by accretion onto an active galactic nucleus.", "doi": "10.1088/0004-637X/731/2/83", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2011-04-20", "series_number": "2", "volume": "731", "issue": "2", "pages": "Art. No. 83" }, { "id": "authors:t48e0-xhp71", "collection": "authors", "collection_id": "t48e0-xhp71", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200221-111532581", "type": "article", "title": "Detection of a Population of Submillimeter-Bright, Strongly Lensed Galaxies", "author": [ { "family_name": "Negrello", "given_name": "M.", "clpid": "Negrello-M" }, { "family_name": "Hopwood", "given_name": "R." }, { "family_name": "De Zotti", "given_name": "G." }, { "family_name": "Cooray", "given_name": "A." }, { "family_name": "Verma", "given_name": "A." }, { "family_name": "Bock", "given_name": "J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Frayer", "given_name": "D. T." }, { "family_name": "Gurwell", "given_name": "M. A." }, { "family_name": "Omont", "given_name": "A." }, { "family_name": "Neri", "given_name": "R." }, { "family_name": "Dannerbauer", "given_name": "H." }, { "family_name": "Leeuw", "given_name": "L. L." }, { "family_name": "Barton", "given_name": "E." }, { "family_name": "Cooke", "given_name": "J.", "orcid": "0000-0001-5703-2108", "clpid": "Cooke-J" }, { "family_name": "Kim", "given_name": "S." }, { "family_name": "da Cunha", "given_name": "E." }, { "family_name": "Rodighiero", "given_name": "G." }, { "family_name": "Cox", "given_name": "P." }, { "family_name": "Bonfield", "given_name": "D. G." }, { "family_name": "Jarvis", "given_name": "M. J." }, { "family_name": "Serjeant", "given_name": "S." }, { "family_name": "Ivison", "given_name": "R. J." }, { "family_name": "Dye", "given_name": "S." }, { "family_name": "Aretxaga", "given_name": "I." }, { "family_name": "Hughes", "given_name": "D. H." }, { "family_name": "Ibar", "given_name": "E." }, { "family_name": "Bertoldi", "given_name": "F." }, { "family_name": "Valtchanov", "given_name": "I." }, { "family_name": "Eales", "given_name": "S." }, { "family_name": "Dunne", "given_name": "L." }, { "family_name": "Driver", "given_name": "S. P." }, { "family_name": "Auld", "given_name": "R." }, { "family_name": "Buttiglione", "given_name": "S." }, { "family_name": "Cava", "given_name": "A." }, { "family_name": "Grady", "given_name": "C. A." }, { "family_name": "Clements", "given_name": "D. L." }, { "family_name": "Dariush", "given_name": "A." }, { "family_name": "Fritz", "given_name": "J." }, { "family_name": "Hill", "given_name": "D." }, { "family_name": "Hornbeck", "given_name": "J. B." }, { "family_name": "Kelvin", "given_name": "L." }, { "family_name": "Lagache", "given_name": "G." }, { "family_name": "Lopez-Caniego", "given_name": "M." }, { "family_name": "Gonzalez-Nuevo", "given_name": "J." }, { "family_name": "Maddox", "given_name": "S." }, { "family_name": "Pascale", "given_name": "E." }, { "family_name": "Pohlen", "given_name": "M." }, { "family_name": "Rigby", "given_name": "E. E." }, { "family_name": "Robotham", "given_name": "A." }, { "family_name": "Simpson", "given_name": "C." }, { "family_name": "Smith", "given_name": "D. J. B." }, { "family_name": "Temi", "given_name": "P." }, { "family_name": "Thompson", "given_name": "M. A." }, { "family_name": "Woodgate", "given_name": "B. E." }, { "family_name": "York", "given_name": "D. G." }, { "family_name": "Aguirre", "given_name": "J. E." }, { "family_name": "Beelen", "given_name": "A." }, { "family_name": "Blain", "given_name": "A.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Baker", "given_name": "A. J." }, { "family_name": "Birkinshaw", "given_name": "M." }, { "family_name": "Blundell", "given_name": "R." }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Burgarella", "given_name": "D." }, { "family_name": "Danese", "given_name": "L." }, { "family_name": "Dunlop", "given_name": "J. S." }, { "family_name": "Fleuren", "given_name": "S." }, { "family_name": "Glenn", "given_name": "J." }, { "family_name": "Harris", "given_name": "A. I." }, { "family_name": "Kamenetzky", "given_name": "J." }, { "family_name": "Lupu", "given_name": "R. E." }, { "family_name": "Maddalena", "given_name": "R. J." }, { "family_name": "Madore", "given_name": "B. F." }, { "family_name": "Maloney", "given_name": "P. R." }, { "family_name": "Matsuhara", "given_name": "H." }, { "family_name": "Michaowski", "given_name": "M. J." }, { "family_name": "Murphy", "given_name": "E. J.", "orcid": "0000-0001-7089-7325", "clpid": "Murphy-E-J" }, { "family_name": "Naylor", "given_name": "B. J.", "clpid": "Naylor-B-J" }, { "family_name": "Nguyen", "given_name": "H.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Popescu", "given_name": "C." }, { "family_name": "Rawlings", "given_name": "S." }, { "family_name": "Rigopoulou", "given_name": "D." }, { "family_name": "Scott", "given_name": "D." }, { "family_name": "Scott", "given_name": "K. S." }, { "family_name": "Seibert", "given_name": "M." }, { "family_name": "Smail", "given_name": "I." }, { "family_name": "Tuffs", "given_name": "R. J." }, { "family_name": "Vieira", "given_name": "J. D.", "clpid": "Vieira-J-D" }, { "family_name": "van der Werf", "given_name": "P. P." }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "Gravitational lensing is a powerful astrophysical and cosmological probe and is particularly valuable at submillimeter wavelengths for the study of the statistical and individual properties of dusty star-forming galaxies. However, the identification of gravitational lenses is often time-intensive, involving the sifting of large volumes of imaging or spectroscopic data to find few candidates. We used early data from the Herschel Astrophysical Terahertz Large Area Survey to demonstrate that wide-area submillimeter surveys can simply and easily detect strong gravitational lensing events, with close to 100% efficiency.", "doi": "10.1126/science.1193420", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "2010-11-05", "series_number": "6005", "volume": "330", "issue": "6005", "pages": "800-804" }, { "id": "authors:t5akv-mvr98", "collection": "authors", "collection_id": "t5akv-mvr98", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091104-144315878", "type": "article", "title": "The Warm Molecular Gas around the Cloverleaf Quasar", "author": [ { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Aguirre", "given_name": "J. E.", "orcid": "0000-0002-4810-666X", "clpid": "Aguirre-J-E" }, { "family_name": "Aikin", "given_name": "R.", "clpid": "Aikin-R" }, { "family_name": "Bock", "given_name": "J. J.", "orcid": "0000-0002-5710-5212", "clpid": "Bock-J-J" }, { "family_name": "Earle", "given_name": "L.", "clpid": "Earle-L" }, { "family_name": "Glenn", "given_name": "J.", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "family_name": "Inami", "given_name": "H.", "orcid": "0000-0003-4268-0393", "clpid": "Inami-Hanae" }, { "family_name": "Maloney", "given_name": "P. R.", "clpid": "Maloney-P-R" }, { "family_name": "Matsuhara", "given_name": "H.", "clpid": "Matsuhara-Hideo" }, { "family_name": "Naylor", "given_name": "B. J.", "clpid": "Naylor-B-J" }, { "family_name": "Nguyen", "given_name": "H. T.", "clpid": "Nguyen-Hien-Trong" }, { "family_name": "Zmuidzinas", "given_name": "J.", "orcid": "0000-0002-3330-5439", "clpid": "Zmuidzinas-J" } ], "abstract": "We present the first broadband \u03bb = 1 mm spectrum toward the z = 2.56 Cloverleaf quasar, obtained with Z-Spec, a grating spectrograph on the 10.4 m Caltech Submillimeter Observatory. The 190-305 GHz observation band corresponds to the rest frame 272-444 \u03bcm, and we measure the dust continuum as well as all four transitions of carbon monoxide (CO) lying in this range. The power-law dust emission, F_\u03bd = 14 mJy(\u03bd/240 GHz)^(3.9) is consistent with the published continuum measurements. The CO J = 6 \u2192 5, J = 8 \u2192 7, and J = 9 \u2192 8 measurements are the first, and now provide the highest-J CO information in this source. Our measured CO intensities are very close to the previously published interferometric measurements of J = 7 \u2192 6, and we use all available transitions and our ^(13)CO upper limits to constrain the physical conditions in the Cloverleaf molecular gas disk. We find a large mass (2-50 \u00d7 10^9 M_\u2299) of highly excited gas with thermal pressure nT > 10^6 K cm^(\u20133). The ratio of the total CO cooling to the far-IR dust emission exceeds that in the local dusty galaxies, and we investigate the potential heating sources for this bulk of warm molecular gas. We conclude that both UV photons and X-rays likely contribute, and discuss implications for a top-heavy stellar initial mass function arising in the X-ray-irradiated starburst. Finally, we present tentative identifications of other species in the spectrum, including a possible detection of the H_2O 2_(0,2) \u2192 1_(1,1) transition at \u03bb_(rest) = 303 \u03bcm.", "doi": "10.1088/0004-637X/705/1/112", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2009-11-01", "series_number": "1", "volume": "705", "issue": "1", "pages": "112-122" }, { "id": "authors:v86b9-x6291", "collection": "authors", "collection_id": "v86b9-x6291", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180207-161040152", "type": "article", "title": "Direct Detection Spectroscopy in the 350\u03bcm Window: SPIFI on the JCMT", "author": [ { "family_name": "Stacey", "given_name": "G. J.", "clpid": "Stacey-G-J" }, { "family_name": "Nikola", "given_name": "T.", "clpid": "Nikola-T" }, { "family_name": "Bradford", "given_name": "C. M.", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Hall", "given_name": "L.", "clpid": "Hall-L" }, { "family_name": "Unger", "given_name": "S.", "clpid": "Unger-S-J" }, { "family_name": "Savage", "given_name": "M.", "clpid": "Savage-M" }, { "family_name": "Davidson", "given_name": "J. A.", "clpid": "Davidson-J-A" }, { "family_name": "Bolatto", "given_name": "A. D.", "orcid": "0000-0002-5480-5686", "clpid": "Bolatto-A-D" }, { "family_name": "Jackson", "given_name": "J. M.", "orcid": "0000-0002-3466-6164", "clpid": "Jackson-James-M" } ], "abstract": "We present the results from our first observing runs with the South Pole Imaging Fabry-Perot Inteferometer (SPIFI). SPIFI is a direct detection imaging spectrometer for use in the submillimeter - the first of its kind. SPIFI employs a 5 \u00d7 5 element array of bolometers as its focal plane, and uses two Fabry-Perot in series as its resolution achieving devices. To date, SPIFI has had 5 observing runs on the 15 meter James Clerk Maxwell Telescope (JCMT), three of which were entirely weathered out. During the two good runs, we obtained fully sampled maps in the 370 \u03bcm [CI] fine structure line and 372 \u03bcm CO(7\u21926) rotational line of the Galactic Center and the nuclei of several infrared bright galaxies. We present the results, and preliminary analysis of the data obtained for several of these sources below. To date, we have only used SPIFI in the 350 \u03bcm telluric window, but SPIFI can also access the 450 and 600 \u03bcm windows available to the JCMT, and the far-IR 200 \u03bcm window available to the NSF's 1.7 m AST/RO telescope at the South Pole. SPIFI is fully described in [1,2,9].", "doi": "10.1051/eas:2002111", "issn": "1633-4760", "publisher": "EDP Sciences", "publication": "EAS Publications Series", "publication_date": "2002-09-25", "volume": "4", "pages": "419-419" }, { "id": "authors:6ny7v-t8x94", "collection": "authors", "collection_id": "6ny7v-t8x94", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BRAao02", "type": "article", "title": "SPIFI: a Direct-Detection Imaging Spectrometer for Submillimeter Wavelengths", "author": [ { "family_name": "Bradford", "given_name": "C. Matt", "orcid": "0000-0001-5261-7094", "clpid": "Bradford-C-M" }, { "family_name": "Stacey", "given_name": "Gordon J.", "clpid": "Stacey-G-J" }, { "family_name": "Swain", "given_name": "Mark R.", "orcid": "0000-0002-0919-4468", "clpid": "Swain-M-R" }, { "family_name": "Nikola", "given_name": "Thomas", "clpid": "Nikola-T" }, { "family_name": "Bolatto", "given_name": "Alberto D.", "orcid": "0000-0002-5480-5686", "clpid": "Bolatto-A-D" }, { "family_name": "Jackson", "given_name": "James M.", "orcid": "0000-0002-3466-6164", "clpid": "Jackson-James-M" }, { "family_name": "Savage", "given_name": "Maureen L.", "clpid": "Savage-M-L" }, { "family_name": "Davidson", "given_name": "Jacqueline A.", "clpid": "Davidson-J-A" }, { "family_name": "Ade", "given_name": "Peter A. R.", "orcid": "0000-0002-5127-0401", "clpid": "Ade-P-A-R" } ], "abstract": "The South Pole Imaging Fabry-Perot Interferometer (SPIFI) is the first instrument of its kind -a direct-detection imaging spectrometer for astronomy in the submillimeter band. SPIFI 's focal plane is a square array of 25 silicon bolometers cooled to 60 mK; the spectrometer consists of two cryogenic scanning Fabry-Perot interferometers in series with a 60-mK bandpass filter. The instrument operates in the short submillimeter windows (350 and 450 \u03bcm) available from the ground, with spectral resolving power selectable between 500 and 10,000. At present, SPIFI's sensitivity is within a factor of 1.5-3 of the photon background limit, comparable with the best heterodyne spectrometers. The instrument 's large bandwidth and mapping capability provide substantial advantages for specific astrophysical projects, including deep extragalactic observations. We present the motivation for and design of SPIFI and its operational characteristics on the telescope.", "issn": "0003-6935", "publisher": "Optical Society of America", "publication": "Applied Optics", "publication_date": "2002-05-01", "series_number": "13", "volume": "41", "issue": "13", "pages": "2561-2574" } ]