\n
We present spatially resolved Atacama Large Millimeter/submillimeter Array Band 9 observations of the [C ii] 158 μm fine structure line from an optically selected quasar, SDSS J100038.01+020822.4 (J1000), at z = 1.8275. By utilizing [O i] 63 μm line observations from Herschel/PACS and constructing a detailed dust spectral energy distribution using Herschel and Spitzer archival imaging data, we show that the [C ii] line emission is well explained by a photodissociation region (PDR) model, in which the emission arises from the surfaces of molecular clouds exposed to far-UV radiation fields ∼5 × 103 times the local interstellar radiation field (G0). We find a factor of 30 variation in spatially resolved [C ii]/far-IR continuum across the source, which is explained by the reduced fraction of cooling via [C ii] line emission at such high far-UV field strengths. By matching the derived PDR parameters to the observed far-IR line and continuum intensities we derive cloud size scales and find that typical cloud radii in J1000 are ∼3.5 pc, perhaps indicating an interstellar medium that is highly fractured due to intense star formation activity. We model the galaxy dynamically and find that the [C ii] emission is contained within a compact, dynamically cold disk with v/σ = 6.2, consistent with the IllustrisTNG50 cosmological simulation. We also report the discovery of a companion galaxy to J1000 confirmed by the detection of [C ii] and use recently obtained JWST/NIRCam imaging of the system to argue for J1000 being an interacting system. With total stellar mass ∼ 1.5 × 1010 M\u2299 and main-component dynamical mass \u2273 1011 M\u2299, the J1000 system is a progenitor to the most massive galaxies seen in the local Universe.
\n
The PRobe far-Infrared Mission for Astrophysics (PRIMA) is under study as a potential far-IR space mission, featuring actively cooled optics, and both imaging and spectroscopic instrumentation. To fully take advantage of the low background afforded by a cold telescope, spectroscopy with PRIMA requires detectors with a noise equivalent power (NEP) better than 1×10−19 W Hz−1/2. To meet this goal, we are developing large format arrays of kinetic inductance detectors (KIDs) to work across the 25–250 μm range. Here, we present the design and characterization of a single pixel prototype detector optimized for 210 μm. The KID consists of a lens-coupled aluminum inductor-absorber connected to a niobium interdigitated capacitor to form a 2 GHz resonator. We have fabricated a small array with 28 KIDs, and we measure the performance of one of these detectors with an optical loading in the 0.01–300 aW range. At low loading, the detector achieves an NEP of 9×10−20 W Hz−1/2 at a 10 Hz readout frequency. An extrapolation of these measurements suggests this detector may remain photon noise limited at up to 20 fW of loading, offering a high dynamic range for PRIMA observations of bright astronomical sources.
",
"doi": "10.1109/tthz.2024.3454436",
"issn": "2156-342X",
"publisher": "IEEE",
"publication": "IEEE Transactions on Terahertz Science and Technology",
"publication_date": "2025-07",
"series_number": "4",
"volume": "15",
"issue": "4",
"pages": "546 - 557"
},
{
"id": "authors:qxkag-xvs52",
"collection": "authors",
"collection_id": "qxkag-xvs52",
"cite_using_url": "https://authors.library.caltech.edu/records/qxkag-xvs52",
"type": "article",
"title": "A 25-micrometer Single-Photon-Sensitive Kinetic Inductance Detector",
"author": [
{
"family_name": "Day",
"given_name": "Peter K.",
"orcid": "0000-0002-3670-9017"
},
{
"family_name": "Cothard",
"given_name": "Nicholas F.",
"orcid": "0000-0002-6151-6292"
},
{
"family_name": "Albert",
"given_name": "Christopher",
"clpid": "Albert-Christopher"
},
{
"family_name": "Foote",
"given_name": "Logan",
"orcid": "0000-0002-4162-8609",
"clpid": "Foote-Logan"
},
{
"family_name": "Kane",
"given_name": "Elijah",
"clpid": "Kane-Elijah"
},
{
"family_name": "Eom",
"given_name": "Byeong H.",
"orcid": "0000-0002-0976-0861"
},
{
"family_name": "Basu Thakur",
"given_name": "Ritoban",
"orcid": "0000-0002-3351-3078"
},
{
"family_name": "Janssen",
"given_name": "Reinier M.\u2009J.",
"orcid": "0000-0001-9122-9668"
},
{
"family_name": "Beyer",
"given_name": "Andrew",
"orcid": "0000-0002-1045-1652"
},
{
"family_name": "Echternach",
"given_name": "Pierre M.",
"orcid": "0000-0001-9643-5110"
},
{
"family_name": "van Berkel",
"given_name": "Sven",
"orcid": "0000-0002-0088-768X"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "Steven",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Stevenson",
"given_name": "Thomas R."
},
{
"family_name": "Dabironezare",
"given_name": "Shahab",
"orcid": "0000-0002-9032-2227"
},
{
"family_name": "Baselmans",
"given_name": "Jochem J.\u2009A.",
"orcid": "0000-0002-3385-7305"
},
{
"family_name": "Glenn",
"given_name": "Jason",
"orcid": "0000-0001-7527-2017"
},
{
"family_name": "Bradford",
"given_name": "C. Matt"
},
{
"family_name": "Leduc",
"given_name": "Henry G."
}
],
"abstract": "We report measurements characterizing the performance of a kinetic inductance detector array designed for a wavelength of 25 microns and very low optical background level suitable for applications such as a far-infrared instrument on a cryogenically cooled space telescope. In a pulse-counting mode of operation at low optical flux, the detectors can resolve individual 25-micron photons. In an integrating mode, the detectors remain photon noise limited over more than 6 orders of magnitude in absorbed power from 70 zW to 200 fW, with a limiting noise equivalent power of 4.6×10−20 W Hz−1 at 1 Hz. In addition, the detectors are highly stable with flat power spectra under optical load down to 1 mHz. Operational parameters of the detector are determined including the efficiency of conversion of the incident optical power into quasiparticles in the aluminum absorbing element and the quasiparticle self-recombination constant.
",
"doi": "10.1103/physrevx.14.041005",
"issn": "2160-3308",
"publisher": "American Physical Society",
"publication": "Physical Review X",
"publication_date": "2024-10/2024-12",
"series_number": "4",
"volume": "14",
"issue": "4",
"pages": "041005"
},
{
"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: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: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:vzaxe-6yy92",
"collection": "authors",
"collection_id": "vzaxe-6yy92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20171113-134819826",
"type": "article",
"title": "Interstellar medium conditions in z ~ 0.2 Lyman-break analogs",
"author": [
{
"family_name": "Contursi",
"given_name": "A.",
"clpid": "Contursi-A"
},
{
"family_name": "Baker",
"given_name": "A. J.",
"clpid": "Baker-A-J"
},
{
"family_name": "Berta",
"given_name": "S.",
"orcid": "0000-0002-0320-1532",
"clpid": "Berta-S"
},
{
"family_name": "Magnelli",
"given_name": "B.",
"orcid": "0000-0002-6777-6490",
"clpid": "Magnelli-B"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Verma",
"given_name": "A.",
"clpid": "Verma-A"
},
{
"family_name": "Nielbock",
"given_name": "M.",
"clpid": "Nielbock-M"
},
{
"family_name": "Gr\u00e1cia Carpio",
"given_name": "J.",
"clpid": "Gr\u00e1cia-Carpio-J"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Davies",
"given_name": "R.",
"clpid": "Davies-R"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653",
"clpid": "Genzel-Reinhard"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Herrera-Camus",
"given_name": "R.",
"orcid": "0000-0002-2775-0595",
"clpid": "Herrera-Camus-R"
},
{
"family_name": "Janssen",
"given_name": "A.",
"clpid": "Janssen-A"
},
{
"family_name": "Poglitsch",
"given_name": "A.",
"clpid": "Poglitsch-A"
},
{
"family_name": "Sternberg",
"given_name": "A.",
"clpid": "Sternberg-A"
},
{
"family_name": "Tacconi",
"given_name": "L. J.",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
}
],
"abstract": "We present an analysis of far\u2013infrared (FIR) [CII] and [OI] fine structure line and continuum observations obtained with Herschel/PACS, and ^(12)CO(1\u20130) observations obtained with the IRAM Plateau de Bure Interferometer, of Lyman-break analogs (LBAs) at z ~ 0.2. The principal aim of this work is to determine the typical interstellar medium (ISM) properties of z ~ 1\u22122 main sequence (MS) galaxies, with stellar masses between 10^(9.5) and 10^(11)M\u2299, which are currently not easily detectable in all these lines even with ALMA and NOEMA. We perform PDR modeling and apply different infared diagnostics to derive the main physical parameters of the far-infrared (FIR)-emitting gas and dust and we compare the derived ISM properties to those of galaxies on and above the MS at different redshifts. We find that the ISM properties of LBAs are quite extreme (low gas temperature and high density and thermal pressure) with respect to those found in local normal spirals and more active local galaxies. LBAs have no [CII] deficit despite having the high specific star formation rates (sSFRs) typical of starbursts. Although LBAs lie above the local MS, we show that their ISM properties are more similar to those of high-redshift MS galaxies than of local galaxies above the main sequence. This data set represents an important reference for planning future ALMA [CII] observations of relatively low-mass MS galaxies at the epoch of the peak of the cosmic star formation.",
"doi": "10.1051/0004-6361/201730609",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2017-10",
"volume": "606",
"pages": "Art. No. A86"
},
{
"id": "authors:cya4b-jvt86",
"collection": "authors",
"collection_id": "cya4b-jvt86",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170213-154850887",
"type": "article",
"title": "CO-Dark Star Formation and Black Hole Activity in 3C 368 at z = 1.131: Coeval Growth of Stellar and Supermassive Black Hole Masses",
"author": [
{
"family_name": "Lamarche",
"given_name": "C.",
"clpid": "Lamarche-C"
},
{
"family_name": "Stacey",
"given_name": "G.",
"clpid": "Stacey-G"
},
{
"family_name": "Brisbin",
"given_name": "D.",
"orcid": "0000-0002-4795-419X",
"clpid": "Brisbin-D"
},
{
"family_name": "Ferkinhoff",
"given_name": "C.",
"clpid": "Ferkinhoff-C"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Nikola",
"given_name": "T.",
"clpid": "Nikola-T"
},
{
"family_name": "Riechers",
"given_name": "D.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Sharon",
"given_name": "C. E.",
"orcid": "0000-0002-6250-5608",
"clpid": "Sharon-C-E"
},
{
"family_name": "Spoon",
"given_name": "H.",
"orcid": "0000-0002-8712-369X",
"clpid": "Spoon-H-W-W"
},
{
"family_name": "Vishwas",
"given_name": "A.",
"clpid": "Vishwas-A"
}
],
"abstract": "We present the detection of four far-infrared fine-structure oxygen lines, as well as strong upper limits for the CO(2\u20131) and [N ii] 205 \u03bcm lines, in 3C 368, a well-studied radio-loud galaxy at z = 1.131. These new oxygen lines, taken in conjunction with previously observed neon and carbon fine-structure lines, suggest a powerful active galactic nucleus (AGN), accompanied by vigorous and extended star formation. A starburst dominated by O8 stars, with an age of ~6.5 Myr, provides a good fit to the fine-structure line data. This estimated age of the starburst makes it nearly concurrent with the latest episode of AGN activity, suggesting a link between the growth of the supermassive black hole and stellar population in this source. We do not detect the CO(2\u20131) line, down to a level twelve times lower than the expected value for star-forming galaxies. This lack of CO line emission is consistent with recent star formation activity if the star-forming molecular gas has low metallicity, is highly fractionated (such that CO is photodissociated throughout much of the clouds), or is chemically very young (such that CO has not yet had time to form). It is also possible, although we argue it is unlikely, that the ensemble of fine-structure lines is emitted from the region heated by the AGN.",
"doi": "10.3847/1538-4357/836/1/123",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2017-02-10",
"series_number": "1",
"volume": "836",
"issue": "1",
"pages": "Art. No. 123"
},
{
"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: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:nkkds-vkw66",
"collection": "authors",
"collection_id": "nkkds-vkw66",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151119-110743148",
"type": "article",
"title": "A Deep Herschel/Pacs Observation of CO(40-39) in NGC 1068: A Search for the Molecular Torus",
"author": [
{
"family_name": "Janssen",
"given_name": "A. W.",
"clpid": "Janssen-A-W"
},
{
"family_name": "Bruderer",
"given_name": "S.",
"clpid": "Bruderer-S"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Contursi",
"given_name": "A.",
"clpid": "Contursi-A"
},
{
"family_name": "Davies",
"given_name": "R.",
"clpid": "Davies-R"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Poglitsch",
"given_name": "A.",
"clpid": "Poglitsch-A"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653",
"clpid": "Genzel-Reinhard"
},
{
"family_name": "Graci\u00e1-Carpio",
"given_name": "J.",
"clpid": "Graci\u00e1-Carpio-J"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Tacconi",
"given_name": "L.",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Gonz\u00e1lez-Alfonso",
"given_name": "E.",
"clpid": "Gonz\u00e1lez-Alfonso-E"
},
{
"family_name": "Sternberg",
"given_name": "A.",
"clpid": "Sternberg-A"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Verma",
"given_name": "A.",
"clpid": "Verma-A"
},
{
"family_name": "Burtscher",
"given_name": "L.",
"clpid": "Burtscher-L"
}
],
"abstract": "Emission from high-J CO lines in galaxies has long been proposed as a tracer of X-ray dominated regions (XDRs) produced by active galactic nuclei (AGNs). Of particular interest is the question of whether the obscuring torus, which is required by AGN unification models, can be observed via high-J CO cooling lines. Here we report on the analysis of a deep Herschel/PACS observation of an extremely high-J CO transition (40-39) in the Seyfert 2 galaxy NGC 1068. The line was not detected, with a derived 3\u03c3 upper limit of 2 x 10^(-17) W m^(-2. We apply an XDR model in order to investigate whether the upper limit constrains the properties of a molecular torus in NGC 1068. The XDR model predicts the CO spectral line energy distributions for various gas densities and illuminating X-ray fluxes. In our model, the CO(40-39) upper limit is matched by gas with densities of ~10^6-10^7 cm^(-3), located at 1.6\u20135 pc from the AGN, with column densities of at least 10^(25) cm^(-2). At such high column densities, however, dust absorbs most of the CO(40-39) line emission at \u03bb = 65.69 \u00b5m. Therefore, even if NGC 1068 has a molecular torus that radiates in the CO(40-39) line, the dust can attenuate the line emission to below the PACS detection limit. The upper limit is thus consistent with the existence of a molecular torus in NGC 1068. In general, we expect that the CO(40-39) is observable in only a few AGN nuclei (if at all), because of the required high gas column density, and absorption by dust.",
"doi": "10.1088/0004-637X/811/2/74",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-10-01",
"series_number": "2",
"volume": "811",
"issue": "2",
"pages": "Art. No. 74"
},
{
"id": "authors:9mnz3-awf97",
"collection": "authors",
"collection_id": "9mnz3-awf97",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150805-095549737",
"type": "article",
"title": "Band-9 ALMA Observations of the [N II] 122 \u03bcm Line and FIR Continuum in Two High-z Galaxies",
"author": [
{
"family_name": "Ferkinhoff",
"given_name": "Carl",
"clpid": "Ferkinhoff-C"
},
{
"family_name": "Brisbin",
"given_name": "Drew",
"orcid": "0000-0002-4795-419X",
"clpid": "Brisbin-D"
},
{
"family_name": "Nikola",
"given_name": "Thomas",
"clpid": "Nikola-T"
},
{
"family_name": "Stacey",
"given_name": "Gordon",
"clpid": "Stacey-G-J"
},
{
"family_name": "Sheth",
"given_name": "Kartik",
"orcid": "0000-0002-5496-4118",
"clpid": "Sheth-K"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "Steve",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Falgarone",
"given_name": "Edith",
"clpid": "Falgarone-E"
}
],
"abstract": "We present Atacama Large Millimeter Array (ALMA) observations of two high-redshift systems (SMMJ02399-0136 at z_1 ~ 2.8 and the Cloverleaf QSO at z_1 ~ 2.5) in their rest-frame 122 \u03bcm continuum (\u03bdsky ~ 650 GHz, \u03bbsky ~ 450 \u03bcm) and [N ii] 122 \u03bcm line emission. The continuum observations with a synthesized beam of ~0.\"25 resolve both sources and recover the expected flux. The Cloverleaf is resolved into a partial Einstein ring, while SMMJ02399-0136 is unambiguously separated into two components: a point source associated with an active galactic nucleus and an extended region at the location of a previously identified dusty starburst. We detect the [N ii] line in both systems, though significantly weaker than our previous detections made with the first generation z (Redshift) and Early Universe Spectrometer. We show that this discrepancy is mostly explained if the line flux is resolved out due to significantly more extended emission and longer ALMA baselines than expected. Based on the ALMA observations we determine that \u226575% of the total [N ii] line flux in each source is produced via star formation. We use the [N ii] line flux that is recovered by ALMA to constrain the N/H abundance, ionized gas mass, hydrogen- ionizing photon rate, and star formation rate. In SMMJ02399-0136 we discover it contains a significant amount (~1000 M_\u2299 yr^(\u22121)) of unobscured star formation in addition to its dusty starburst and argue that SMMJ02399-0136 may be similar to the Antennae Galaxies (Arp 244) locally. In total these observations provide a new look at two well-studied systems while demonstrating the power and challenges of Band-9 ALMA observations of high-z systems.",
"doi": "10.1088/0004-637X/806/2/260",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-06-20",
"series_number": "2",
"volume": "806",
"issue": "2",
"pages": "Art. No. 260"
},
{
"id": "authors:4s38e-sr373",
"collection": "authors",
"collection_id": "4s38e-sr373",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150515-125149162",
"type": "article",
"title": "High-J CO Sleds in Nearby Infrared Bright Galaxies Observed By Herschel/PACS",
"author": [
{
"family_name": "Mashian",
"given_name": "N.",
"clpid": "Mashian-N"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Sternberg",
"given_name": "A.",
"clpid": "Sternberg-A"
},
{
"family_name": "Janssen",
"given_name": "A.",
"clpid": "Janssen-A"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Contursi",
"given_name": "A.",
"clpid": "Contursi-A"
},
{
"family_name": "Gonz\u00e1lez-Alfonso",
"given_name": "E.",
"clpid": "Gonz\u00e1lez-Alfonso-E"
},
{
"family_name": "Gracia-Carpio",
"given_name": "J.",
"clpid": "Gracia-Carpio-J"
},
{
"family_name": "Poglitsch",
"given_name": "A.",
"clpid": "Poglitsch-A"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Davies",
"given_name": "R.",
"clpid": "Davies-R"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653",
"clpid": "Genzel-Reinhard"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Tacconi",
"given_name": "L.",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
},
{
"family_name": "Verma",
"given_name": "A.",
"clpid": "Verma-A"
},
{
"family_name": "Weiss",
"given_name": "A.",
"orcid": "0000-0003-4678-3939",
"clpid": "Weiss-Axel"
},
{
"family_name": "Polisensky",
"given_name": "E.",
"clpid": "Polisensky-E"
},
{
"family_name": "Nikola",
"given_name": "T.",
"clpid": "Nikola-T"
}
],
"abstract": "We report the detection of far-infrared (FIR) CO rotational emission from nearby active galactic nuclei (AGNs) and starburst galaxies, as well as several merging systems and Ultra-Luminous Infrared Galaxies (ULIRGs). Using the Herschel Photodetector Array Camera and Spectrometer (PACS), we have detected transitions in the J_(upp) = 14\u201330 range. The PACS CO data obtained here provide the first reference of well-sampled FIR extragalactic CO spectral line energy distributions (SLEDs) for this range. We find a large range in the overall SLED shape, even among galaxies of similar type, demonstrating the uncertainties in relying solely on high-J CO diagnostics to characterize the excitation source of a galaxy. Combining our data with low-J line intensities taken from the literature, we present a CO ratio\u2013ratio diagram and discuss its value in distinguishing excitation sources and physical properties of the molecular gas. The position of a galaxy on such a diagram is less a signature of its excitation mechanism, than an indicator of the presence of warm, dense molecular gas. We then quantitatively analyze the CO emission from a subset of the detected sources with single-component and two-component large velocity gradient (LVG) radiative transfer models to fit the CO SLEDs. From these fits we derive the molecular gas mass and the corresponding CO-to-H_2 conversion factor, \u0251_(CO), for each respective source. For the ULIRGs we find \u03b1 values in the canonical range 0.4\u2013 5M_\u2299 (K km s^(\u22121) pc^2)^(\u22121), while for the other objects, \u03b1 varies between 0.2 and 14. Finally, we compare our best-fit LVG model results with previous studies of the same galaxies and comment on any differences.",
"doi": "10.1088/0004-637X/802/2/81",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-04-01",
"series_number": "2",
"volume": "802",
"issue": "2",
"pages": "Art. No. 81"
},
{
"id": "authors:91b78-4x825",
"collection": "authors",
"collection_id": "91b78-4x825",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150316-124557171",
"type": "article",
"title": "High-lying OH Absorption, [C_(II)] Deficits, and Extreme L_(FIR)/M_(H2) Ratios in Galaxies",
"author": [
{
"family_name": "Gonz\u00e1lez-Alfonso",
"given_name": "E",
"clpid": "Gonz\u00e1lez-Alfonso-E"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Graci\u00e1-Carpio",
"given_name": "J.",
"clpid": "Graci\u00e1-Carpio-J"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Mel\u00e9ndez",
"given_name": "M.",
"clpid": "Mel\u00e9ndez-M"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Poglitsch",
"given_name": "A.",
"clpid": "Poglitsch-A"
},
{
"family_name": "Aalto",
"given_name": "S.",
"orcid": "0000-0002-5828-7660",
"clpid": "Aalto-Susanne"
},
{
"family_name": "Falstad",
"given_name": "N.",
"clpid": "Falstad-N"
},
{
"family_name": "Spoon",
"given_name": "H. W. W.",
"orcid": "0000-0002-8712-369X",
"clpid": "Spoon-H-W-W"
},
{
"family_name": "Farrah",
"given_name": "D.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Blasco",
"given_name": "A.",
"clpid": "Blasco-A"
},
{
"family_name": "Henkel",
"given_name": "C.",
"clpid": "Henkel-Christian"
},
{
"family_name": "Contursi",
"given_name": "A.",
"clpid": "Contursi-A"
},
{
"family_name": "Verma",
"given_name": "A.",
"clpid": "Verma-A"
},
{
"family_name": "Spaans",
"given_name": "M.",
"clpid": "Spaans-M"
},
{
"family_name": "Smith",
"given_name": "H. A.",
"clpid": "Smith-H-A"
},
{
"family_name": "Ashby",
"given_name": "M. L. N.",
"orcid": "0000-0002-3993-0745",
"clpid": "Ashby-M-L-N"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Garc\u00eda-Burillo",
"given_name": "S.",
"clpid": "Garc\u00eda-Burillo-S"
},
{
"family_name": "Mart\u00edn-Pintado",
"given_name": "J.",
"clpid": "Mart\u00edn-Pintado-J"
},
{
"family_name": "van der Werf",
"given_name": "P.",
"orcid": "0000-0001-5434-5942",
"clpid": "van-der-Werf-P-P"
},
{
"family_name": "Meijerink",
"given_name": "R.",
"clpid": "Meijerink-R"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653",
"clpid": "Genzel-Reinhard"
}
],
"abstract": "Herschel/PACS observations of 29 local (ultra)luminous infrared galaxies, including both starburst and active galactic nucleus (AGN) dominated sources as diagnosed in the mid-infrared/optical, show that the equivalent width of the absorbing OH 65 \u03bcm \u03a0_(3/2) J = 9/2-7/2 line (W_(eq)(OH65)) with lower level energy E_(low) \u2248 300 K, is anticorrelated with the [C II]158 \u03bcm line to far-infrared luminosity ratio, and correlated with the far-infrared luminosity per unit gas mass and with the 60-to-100 \u03bcm far-infrared color. While all sources are in the active L_(IR)/M_(H2) > 50L_\u2609/M_\u2609 mode as derived from previous CO line studies, the OH65 absorption shows a bimodal distribution with a discontinuity at L_(FIR)/M_(H2) \u2248 100 L_\u2609/M_\u2609. In the most buried sources, OH65 probes material partially responsible for the silicate 9.7 \u03bcm absorption. Combined with observations of the OH 71 \u03bcm \u03a0_(1/2) J = 7/2-5/2 doublet (E_(low) \u2248 415 K), radiative transfer models characterized by the equivalent dust temperature, T_(dust), and the continuum optical depth at 100 \u03bcm, \u03c4_(100), indicate that strong [C_(II)]158 \u03bcm deficits are associated with far-IR thick (\u03c4_(100) \u2273 0.7, N_H \u2273 10^(24) cm^(\u20132)), warm (T_(dust) \u2273 60 K) structures where the OH 65 \u03bcm absorption is produced, most likely in circumnuclear disks/tori/cocoons. With their high L_(FIR)/M_(H2) ratios and columns, the presence of these structures is expected to give rise to strong [C_(II)] deficits. W_(eq)(OH65) probes the fraction of infrared luminosity arising from these compact/warm environments, which is \u2273 30%-50% in sources with high W_(eq)(OH65). Sources with high W_(eq)(OH65) have surface densities of both L_(IR) and M_(H2) higher than inferred from the half-light (CO or UV/optical) radius, tracing coherent structures that represent the most buried/active stage of (circum)nuclear starburst-AGN co-evolution.",
"doi": "10.1088/0004-637X/800/1/69",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-02-10",
"series_number": "1",
"volume": "800",
"issue": "1",
"pages": "Art. No. 69"
},
{
"id": "authors:2y44n-3vg04",
"collection": "authors",
"collection_id": "2y44n-3vg04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150227-113602734",
"type": "article",
"title": "Strong C^+ Emission in Galaxies at z ~ 1-2: Evidence for Cold Flow Accretion Powered Star Formation in the Early Universe",
"author": [
{
"family_name": "Brisbin",
"given_name": "Drew",
"orcid": "0000-0002-4795-419X",
"clpid": "Brisbin-D"
},
{
"family_name": "Ferkinhoff",
"given_name": "Carl",
"clpid": "Ferkinhoff-C"
},
{
"family_name": "Nikola",
"given_name": "Thomas",
"clpid": "Nikola-T"
},
{
"family_name": "Parshley",
"given_name": "Stephen",
"clpid": "Parshley-S-C"
},
{
"family_name": "Stacey",
"given_name": "Gordon J.",
"clpid": "Stacey-G-J"
},
{
"family_name": "Spoon",
"given_name": "Henrik",
"orcid": "0000-0002-8712-369X",
"clpid": "Spoon-H"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "Steven",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Verma",
"given_name": "Aprajita",
"clpid": "Verma-A"
}
],
"abstract": "We have recently detected the [C II] 157.7 \u03bcm line in eight star-forming galaxies at redshifts 1 to 2 using the redshift (z) Early Universe Spectrometer (ZEUS). Our sample targets star formation dominant sources detected in PAH emission. This represents a significant addition to [C II] observations during the epoch of peak star formation. We have augmented this survey with observations of the [O I] 63 \u03bcm line and far infrared photometry from the PACS and SPIRE Herschel instruments as well as Spitzer IRS spectra from the literature showing PAH features. Our sources exhibit above average gas heating efficiency, many with both [O I]/FIR and [C II]/FIR of ~1% or more. The relatively strong [C II] emission is consistent with our sources being dominated by star formation powered photo-dissociation regions, extending to kiloparsec scales. We suggest that the star formation mode in these systems follows a Schmidt-Kennicutt law similar to local systems, but at a much higher rate due to molecular gas surface densities 10-100 times that of local star-forming systems. The source of the high molecular gas surface densities may be the infall of neutral gas from the cosmic web. In addition to the high [C II]/FIR values, we also find high [C II]/PAH ratios and, in at least one source, a cool dust temperature. This source, SWIRE 4-5, bears a resemblance in these diagnostics to shocked regions of Stephan's Quintet, suggesting that another mode of [C II] excitation in addition to normal photoelectric heating may be contributing to the observed [C II] line.",
"doi": "10.1088/0004-637X/799/1/13",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2015-01-20",
"series_number": "1",
"volume": "799",
"issue": "1",
"pages": "Art. No. 13"
},
{
"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:2mzxq-56m69",
"collection": "authors",
"collection_id": "2mzxq-56m69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140428-104758132",
"type": "article",
"title": "Massive molecular outflows and evidence for AGN feedback from CO observations",
"author": [
{
"family_name": "Cicone",
"given_name": "C.",
"orcid": "0000-0003-0522-6941",
"clpid": "Cicone-C"
},
{
"family_name": "Maiolino",
"given_name": "R.",
"clpid": "Maiolino-R"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Graci\u00e1-Carpio",
"given_name": "J.",
"clpid": "Graci\u00e1-Carpio-J"
},
{
"family_name": "Feruglio",
"given_name": "C.",
"clpid": "Feruglio-C"
},
{
"family_name": "Neri",
"given_name": "R.",
"orcid": "0000-0002-7176-4046",
"clpid": "Neri-Roberto"
},
{
"family_name": "Aalto",
"given_name": "S.",
"orcid": "0000-0002-5828-7660",
"clpid": "Aalto-Susanne"
},
{
"family_name": "Davies",
"given_name": "R.",
"clpid": "Davies-R"
},
{
"family_name": "Fiore",
"given_name": "F.",
"clpid": "Fiore-F"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Garc\u00eda-Burillo",
"given_name": "S.",
"clpid": "Garc\u00eda-Burillo-S"
},
{
"family_name": "Gonz\u00e1lez-Alfonso",
"given_name": "E.",
"clpid": "Gonz\u00e1lez-Alfonso-E"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Piconcelli",
"given_name": "E.",
"orcid": "0000-0001-9095-2782",
"clpid": "Piconcelli-E"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
}
],
"abstract": "We study the properties of massive, galactic-scale outflows of molecular gas and investigate their impact on galaxy evolution. We present new IRAM PdBI CO(1\u20130) observations of local ultra-luminous infrared galaxies (ULIRGs) and quasar-hosts: a clear signature of massive and energetic molecular outflows, extending on kpc scales, is found in the CO(1\u20130) kinematics of four out of seven sources, with measured outflow rates of several 100 M_\u2299 yr^(-1). We combine these new observations with data from the literature, and explore the nature and origin of massive molecular outflows within an extended sample of 19 local galaxies. We find that starburst-dominated galaxies have an outflow rate comparable to their star formation rate (SFR), or even higher by a factor of ~2\u20134, implying that starbursts can indeed be effective in removing cold gas from galaxies. Nevertheless, our results suggest that the presence of an active galactic nucleus (AGN) can boost the outflow rate by a large factor, which is found to increase with the L_(AGN)/L_(bol) ratio. The gas depletion time scales due to molecular outflows are anti-correlated with the presence and luminosity of an AGN in these galaxies, and range from a few hundred million years in starburst galaxies down to just a few million years in galaxies hosting powerful AGNs. In quasar hosts, the depletion time scales due to the outflow are much shorter than the depletion time scales due to star formation. We estimate the outflow kinetic power and find that, for galaxies hosting powerful AGNs, it corresponds to about 5% of the AGN luminosity, as expected by models of AGN feedback. Moreover, we find that momentum rates of about 20 L_(AGN)/c are common among the AGN-dominated sources in our sample. For \"pure\" starburst galaxies, our data tentatively support models in which outflows are mostly momentum-driven by the radiation pressure from young stars onto dusty clouds. Overall, our results indicate that, although starbursts are effective in powering massive molecular outflows, the presence of an AGN may strongly enhance such outflows, and therefore have a profound feedback effect on the evolution of galaxies by efficiently removing fuel for star formation, hence quenching star formation.",
"doi": "10.1051/0004-6361/201322464",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2014-02",
"volume": "562",
"pages": "Art. No. A21"
},
{
"id": "authors:na93b-5hg39",
"collection": "authors",
"collection_id": "na93b-5hg39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140225-075642175",
"type": "article",
"title": "The Second-generation z (Redshift) and Early Universe Spectrometer. I. First-light Observation of a Highly Lensed Local-ulirg Analog at High-z",
"author": [
{
"family_name": "Ferkinhoff",
"given_name": "Carl",
"clpid": "Ferkinhoff-C"
},
{
"family_name": "Brisbin",
"given_name": "Drew",
"orcid": "0000-0002-4795-419X",
"clpid": "Brisbin-D"
},
{
"family_name": "Parshley",
"given_name": "Stephen",
"clpid": "Parshley-S-C"
},
{
"family_name": "Nikola",
"given_name": "Thomas",
"clpid": "Nikola-Thomas"
},
{
"family_name": "Stacey",
"given_name": "Gordon J.",
"clpid": "Stacey-G-J"
},
{
"family_name": "Schoenwald",
"given_name": "Justin",
"clpid": "Schoenwald-J"
},
{
"family_name": "Higdon",
"given_name": "James L.",
"orcid": "0000-0003-1397-0586",
"clpid": "Higdon-J-L"
},
{
"family_name": "Higdon",
"given_name": "Sarah J. U.",
"orcid": "0000-0002-4021-7453",
"clpid": "Higdon-S-J-U"
},
{
"family_name": "Verma",
"given_name": "Aprajita",
"clpid": "Verma-A"
},
{
"family_name": "Riechers",
"given_name": "Dominik",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "Steven",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Menten",
"given_name": "Karl M.",
"orcid": "0000-0001-6459-0669",
"clpid": "Menten-K-M"
},
{
"family_name": "G\u00fcsten",
"given_name": "Rolf",
"clpid": "G\u00fcsten-Rolf"
},
{
"family_name": "Weiss",
"given_name": "Axel",
"orcid": "0000-0003-4678-3939",
"clpid": "Weiss-Axel"
},
{
"family_name": "Irwin",
"given_name": "Kent",
"clpid": "Irwin-K-D"
},
{
"family_name": "Cho",
"given_name": "Hsiao M.",
"clpid": "Cho-Hsiao-M"
},
{
"family_name": "Niemack",
"given_name": "Michael",
"clpid": "Niemack-M"
},
{
"family_name": "Halpern",
"given_name": "Mark",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Amiri",
"given_name": "Mandana",
"clpid": "Amiri-M"
},
{
"family_name": "Hasselfield",
"given_name": "Matthew",
"clpid": "Hasselfield-M"
},
{
"family_name": "Wiebe",
"given_name": "D. V.",
"clpid": "Wiebe-D-V"
},
{
"family_name": "Ade",
"given_name": "Peter A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Tucker",
"given_name": "Carol E.",
"clpid": "Tucker-C-E"
}
],
"abstract": "We recently commissioned our new spectrometer, the second-generation z(Redshift) and Early Universe Spectrometer (ZEUS-2) on the Atacama Pathfinder Experiment telescope. ZEUS-2 is a submillimeter grating spectrometer optimized for detecting the faint and broad lines from distant galaxies that are redshifted into the telluric windows from 200 to 850 \u03bcm. It uses a focal plane array of transition-edge sensed bolometers, the first use of these arrays for astrophysical spectroscopy. ZEUS-2 promises to be an important tool for studying galaxies in the years to come because of its synergy with Atacama Large Millimeter Array and its capabilities in the short submillimeter windows that are unique in the post-Herschel era. Here, we report on our first detection of the [C II] 158 \u03bcm line with ZEUS-2. We detect the line at z ~ 1.8 from H-ATLAS J091043.1\u2013000322 with a line flux of (6.44 \u00b1 0.42) \u00d7 10^(\u201318) W m^(\u20132). Combined with its far-IR luminosity and a new Herschel-PACS detection of the [O I] 63 \u03bcm line, we model the line emission as coming from a photo-dissociation region with far-ultraviolet radiation field, G ~ 2 \u00d7 10^4 G_0, gas density, n ~ 1 \u00d7 10^3 cm^(\u20133) and size between ~0.4 and 1 kpc. On the basis of this model, we conclude that H-ATLAS J091043.1\u2013000322 is a high-redshift analog of a local ultra-luminous IR galaxy; i.e., it is likely the site of a compact starburst caused by a major merger. Further identification of these merging systems is important for constraining galaxy formation and evolution models.",
"doi": "10.1088/0004-637X/780/2/142",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2014-01-10",
"series_number": "2",
"volume": "780",
"issue": "2",
"pages": "Art. No. 142"
},
{
"id": "authors:nd361-jnm05",
"collection": "authors",
"collection_id": "nd361-jnm05",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131104-082047378",
"type": "article",
"title": "Fast Molecular Outflows in Luminous Galaxy Mergers: Evidence for Quasar Feedback from Herschel",
"author": [
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Mel\u00e9ndez",
"given_name": "M.",
"clpid": "Mel\u00e9ndez-M"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Gracia-Carpio",
"given_name": "J.",
"clpid": "Gracia-Carpio-J"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Gonz\u00e1lez-Alfonso",
"given_name": "E.",
"clpid": "Gonz\u00e1lez-Alfonso-E"
},
{
"family_name": "Contursi",
"given_name": "A.",
"clpid": "Contursi-A"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Poglitsch",
"given_name": "A.",
"clpid": "Poglitsch-A"
},
{
"family_name": "Davies",
"given_name": "R.",
"clpid": "Davies-R"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653",
"clpid": "Genzel-Reinhard"
},
{
"family_name": "Tacconi",
"given_name": "L.",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
},
{
"family_name": "de Jong",
"given_name": "J. A.",
"clpid": "de-Jong-J-A"
},
{
"family_name": "Sternberg",
"given_name": "A.",
"clpid": "Sternberg-A"
},
{
"family_name": "Netzer",
"given_name": "H.",
"clpid": "Netzer-H"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Verma",
"given_name": "A.",
"clpid": "Verma-A"
},
{
"family_name": "Rupke",
"given_name": "D. S. N.",
"clpid": "Rupke-D-S-N"
},
{
"family_name": "Maiolino",
"given_name": "R.",
"clpid": "Maiolino-R"
},
{
"family_name": "Teng",
"given_name": "S. H.",
"clpid": "Teng-S-H"
},
{
"family_name": "Polisensky",
"given_name": "E.",
"clpid": "Polisensky-E"
}
],
"abstract": "We report the results from a systematic search for molecular (OH 119 \u03bcm) outflows with Herschel/PACS in a sample of 43 nearby (z < 0.3) galaxy mergers, mostly ultraluminous infrared galaxies (ULIRGs) and QSOs. We find that the character of the OH feature (strength of the absorption relative to the emission) correlates with that of the 9.7 \u03bcm silicate feature, a measure of obscuration in ULIRGs. Unambiguous evidence for molecular outflows, based on the detection of OH absorption profiles with median velocities more blueshifted than \u201350 km s^(\u20131), is seen in 26 (70%) of the 37 OH-detected targets, suggesting a wide-angle (~145\u00b0) outflow geometry. Conversely, unambiguous evidence for molecular inflows, based on the detection of OH absorption profiles with median velocities more redshifted than +50 km s^(\u20131), is seen in only four objects, suggesting a planar or filamentary geometry for the inflowing gas. Terminal outflow velocities of ~\u20131000 km s^(\u20131) are measured in several objects, but median outflow velocities are typically ~\u2013200 km s^(\u20131). While the outflow velocities show no statistically significant dependence on the star formation rate, they are distinctly more blueshifted among systems with large active galactic nucleus (AGN) fractions and luminosities [log(L_(AGN)/L_\u2609) \u2265 11.8 \u00b1 0.3]. The quasars in these systems play a dominant role in driving the molecular outflows. However, the most AGN dominated systems, where OH is seen purely in emission, show relatively modest OH line widths, despite their large AGN luminosities, perhaps indicating that molecular outflows subside once the quasar has cleared a path through the obscuring material.",
"doi": "10.1088/0004-637X/776/1/27",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2013-10-10",
"series_number": "1",
"volume": "776",
"issue": "1",
"pages": "Art. No. 27"
},
{
"id": "authors:y7n84-j9208",
"collection": "authors",
"collection_id": "y7n84-j9208",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130409-152633063",
"type": "article",
"title": "Excited OH^+, H_2O^+, and H_3O^+ in NGC 4418 and Arp 220",
"author": [
{
"family_name": "Gonz\u00e1lez-Alfonso",
"given_name": "E.",
"clpid": "Gonz\u00e1lez-Alfonso-E"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Bruderer",
"given_name": "S.",
"clpid": "Bruderer-S"
},
{
"family_name": "M\u00fcller",
"given_name": "H. S. P.",
"orcid": "0000-0002-0183-8927",
"clpid": "M\u00fcller-H-S-P"
},
{
"family_name": "Graci\u00e1-Carpio",
"given_name": "J.",
"clpid": "Graci\u00e1-Carpio-J"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Poglitsch",
"given_name": "A.",
"clpid": "Poglitsch-A"
},
{
"family_name": "Feuchtgruber",
"given_name": "H.",
"clpid": "Feuchtgruber-H"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Contursi",
"given_name": "A.",
"clpid": "Contursi-A"
},
{
"family_name": "Sternberg",
"given_name": "A.",
"clpid": "Sternberg-A"
},
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Verma",
"given_name": "A.",
"clpid": "Verma-A"
},
{
"family_name": "Christopher",
"given_name": "N.",
"clpid": "Christopher-N"
},
{
"family_name": "Davies",
"given_name": "R.",
"clpid": "Davies-R"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653",
"clpid": "Genzel-Reinhard"
},
{
"family_name": "Tacconi",
"given_name": "L.",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
}
],
"abstract": "We report on Herschel/PACS observations of absorption lines of OH^+, H_2O^+ and H_3O^+ in NGC 4418 and Arp 220. Excited lines of OH^+ and H_2O^+ with E_(lower) of at least 285 and ~200 K, respectively, are detected in both sources, indicating radiative pumping and location in the high radiation density environment of the nuclear regions. Abundance ratios OH^+/H_2O^+ of 1\u22122.5 are estimated in the nuclei of both sources. The inferred OH^+ column and abundance relative to H nuclei are (0.5\u22121) \u00d7 10^(16) cm^(-2) and ~ 2\u2009\u00d7 10^(-8), respectively. Additionally, in Arp 220, an extended low excitation component around the nuclear region is found to have OH^+/H^2O^+ ~ 5\u221210. H_3O^+ is detected in both sources with N(H_3O^+) ~ (0.5\u22122)\u2009\u00d7\u200910^(16) cm^(-2), and in Arp 220 the pure inversion, metastable lines indicate a high rotational temperature of ~500 K, indicative of formation pumping and/or hot gas. Simple chemical models favor an ionization sequence dominated by H^+ \u2192 O^+ \u2192 OH^+ \u2192 H_2O^+ \u2192 H_3O^+, and we also argue that the H^+ production is most likely dominated by X-ray/cosmic ray ionization. The full set of observations and models leads us to propose that the molecular ions arise in a relatively low density (\u227310^4 cm^(-3)) interclump medium, in which case the ionization rate per H nucleus (including secondary ionizations) is \u03b6 > 10^(-13) s^(-1), a lower limit that is several\u2009\u00d7\u200910^2 times the highest current rate estimates for Galactic regions. In Arp 220, our lower limit for \u03b6 is compatible with estimates for the cosmic ray energy density inferred previously from the supernova rate and synchrotron radio emission, and also with the expected ionization rate produced by X-rays. In NGC 4418, we argue that X-ray ionization due to an active galactic nucleus is responsible for the molecular ion production.",
"doi": "10.1051/0004-6361/201220466",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy and Astrophysics",
"publication_date": "2013-02",
"volume": "550",
"pages": "Art. No. A25"
},
{
"id": "authors:st55m-51985",
"collection": "authors",
"collection_id": "st55m-51985",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120905-085644068",
"type": "article",
"title": "Herschel-PACS Observations of Far-IR CO Line Emission in NGC 1068: Highly Excited Molecular Gas in the Circumnuclear Disk",
"author": [
{
"family_name": "Hailey-Dunsheath",
"given_name": "S.",
"orcid": "0000-0002-8504-7988",
"clpid": "Hailey-Dunsheath-S"
},
{
"family_name": "Sturm",
"given_name": "E.",
"clpid": "Sturm-E"
},
{
"family_name": "Fischer",
"given_name": "J.",
"orcid": "0000-0001-6697-7808",
"clpid": "Fischer-J"
},
{
"family_name": "Sternberg",
"given_name": "A.",
"clpid": "Sternberg-A"
},
{
"family_name": "Graci\u00e1-Carpio",
"given_name": "J.",
"clpid": "Graci\u00e1-Carpio-J"
},
{
"family_name": "Davies",
"given_name": "R.",
"clpid": "Davies-R"
},
{
"family_name": "Gonz\u00e1lez-Alfonso",
"given_name": "E.",
"clpid": "Gonz\u00e1lez-Alfonso-E"
},
{
"family_name": "Mark",
"given_name": "D.",
"clpid": "Mark-D"
},
{
"family_name": "Poglitsch",
"given_name": "A.",
"clpid": "Poglitsch-A"
},
{
"family_name": "Contursi",
"given_name": "A.",
"clpid": "Contursi-A"
},
{
"family_name": "Genzel",
"given_name": "R.",
"orcid": "0000-0002-2767-9653",
"clpid": "Genzel-Reinhard"
},
{
"family_name": "Lutz",
"given_name": "D.",
"orcid": "0000-0003-0291-9582",
"clpid": "Lutz-Dieter"
},
{
"family_name": "Tacconi",
"given_name": "L.",
"orcid": "0000-0002-1485-9401",
"clpid": "Tacconi-Linda-J"
},
{
"family_name": "Veilleux",
"given_name": "S.",
"orcid": "0000-0002-3158-6820",
"clpid": "Veilleux-S"
},
{
"family_name": "Verma",
"given_name": "A.",
"clpid": "Verma-A"
},
{
"family_name": "de Jong",
"given_name": "J. A.",
"clpid": "de-Jong-J-A"
}
],
"abstract": "We report the detection of far-IR CO rotational emission from the prototypical Seyfert 2 galaxy NGC 1068. Using Herschel-PACS, we have detected 11 transitions in the J_(upper) = 14-30 (E_(upper)/k_B = 580-2565 K) range, all of which are consistent with arising from within the central 10\" (700 pc). The detected transitions are modeled as arising from two different components: a moderate-excitation (ME) component close to the galaxy systemic velocity and a high-excitation (HE) component that is blueshifted by ~80 km s^(\u20131). We employ a large velocity gradient model and derive n_(H2) ~ 10^(5.6) cm^(\u20133), T_(kin) ~ 170 K, and M_(H2) ~ 10^(6.7) M_\u2609 for the ME component and n_(H2) ~ 10^(6.4) cm^(\u20133), T_(kin) ~ 570 K, and M_(H2) ~ 10^(5.6) M_\u2609 for the HE component, although for both components the uncertainties in the density and mass are \u00b1(0.6-0.9) dex. Both components arise from denser and possibly warmer gas than traced by low-J CO transitions, and the ME component likely makes a significant contribution to the mass budget in the nuclear region. We compare the CO line profiles with those of other molecular tracers observed at higher spatial and spectral resolution and find that the ME transitions are consistent with these lines arising in the ~200 pc diameter ring of material traced by H_2 1-0 S(1) observations. The blueshift of the HE lines may also be consistent with the bluest regions of this H_2 ring, but a better kinematic match is found with a clump of infalling gas ~40 pc north of the active galactic nucleus (AGN). We consider potential heating mechanisms and conclude that X-ray- or shock heating of both components is viable, while far-UV heating is unlikely. We discuss the prospects of placing the HE component near the AGN and conclude that while the moderate thermal pressure precludes an association with the ~1 pc radius H_2O maser disk, the HE component could potentially be located only a few parsecs more distant from the AGN and might then provide the N_H ~ 10^(25) cm^(\u20132) column obscuring the nuclear hard X-rays. Finally, we also report sensitive upper limits extending up to J_(upper) = 50, which place constraints on a previous model prediction for the CO emission from the X-ray obscuring torus.",
"doi": "10.1088/0004-637X/755/1/57",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2012-08-10",
"series_number": "1",
"volume": "755",
"issue": "1",
"pages": "Art. No. 57"
}
]