[
{
"id": "authors:3e4gx-wt162",
"collection": "authors",
"collection_id": "3e4gx-wt162",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190521-142454869",
"type": "article",
"title": "The IRAM/GISMO 2 mm Survey in the COSMOS Field",
"author": [
{
"family_name": "Magnelli",
"given_name": "B.",
"orcid": "0000-0002-6777-6490",
"clpid": "Magnelli-B"
},
{
"family_name": "Karim",
"given_name": "A.",
"orcid": "0000-0002-8414-9579",
"clpid": "Karim-A"
},
{
"family_name": "Staguhn",
"given_name": "J.",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
},
{
"family_name": "Kov\u00e1cs",
"given_name": "A.",
"clpid": "Kov\u00e1cs-A"
},
{
"family_name": "Jim\u00e9nez-Andrade",
"given_name": "E. F.",
"orcid": "0000-0002-2640-5917",
"clpid": "Jim\u00e9nez-Andrade-E-F"
},
{
"family_name": "Casey",
"given_name": "C. M.",
"orcid": "0000-0002-0930-6466",
"clpid": "Casey-C-M"
},
{
"family_name": "Zavala",
"given_name": "J. A.",
"orcid": "0000-0002-7051-1100",
"clpid": "Zavala-J-A"
},
{
"family_name": "Schinnerer",
"given_name": "E.",
"orcid": "0000-0002-3933-7677",
"clpid": "Schinnerer-E"
},
{
"family_name": "Sargent",
"given_name": "M.",
"orcid": "0000-0003-1033-9684",
"clpid": "Sargent-M-T"
},
{
"family_name": "Aravena",
"given_name": "M.",
"orcid": "0000-0002-6290-3198",
"clpid": "Aravena-M"
},
{
"family_name": "Bertoldi",
"given_name": "F.",
"orcid": "0000-0002-1707-1775",
"clpid": "Bertoldi-F"
},
{
"family_name": "Capak",
"given_name": "P. L.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-P"
},
{
"family_name": "Riechers",
"given_name": "D. A.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
}
],
"abstract": "We present deep continuum observations at a wavelength of 2 mm centered on the COSMOS field using the Goddard IRAM Superconducting Millimeter Observer (GISMO) at the IRAM 30 m telescope. These data constitute the widest deep 2 mm survey to date, reaching a uniform \u03c3 ~ 0.23 mJy beam\u22121 sensitivity over ~250 arcmin^2 at ~24'' resolution. We detect four sources at high significance (S/N \u2265 4.4) with an expected number of false detections of 0.09 sources and five sources at 4.4 > S/N \u2265 3.7 with an expected number of false detections of 1.65 sources. Combined with deep GISMO observations in GOODS-N, we constrain the 2 mm number counts over one decade in flux density. These measurements agree with most galaxy evolution models tested here, except those with a large population of dusty star-forming galaxies at z > 7. Five GISMO sources have counterparts in (sub)millimeter catalogs available in COSMOS. Their redshifts suggest that all but one lie above z ~ 3. These four high-redshift (z > 3) galaxies have z = 3.9, SFRs ~ 400\u20131200 M \u2299 yr^(\u22121), and M_(dust) ~ 10^(9.5) M\u2299. They provide a relatively complete selection (~66%) of the most luminous (L_(IR) > 10^(12.6) L\u2299) and highest-redshift (z > 3) galaxies detected within our survey area by AzTEC at 1.1 mm. We thus conclude that 2 mm surveys favor the selection of massive, vigorously star-forming, high-redshift galaxies. This is corroborated by GISMO-C4, a source with a low false-detection probability (~6.2%), for which the absence of a (sub)millimeter counterpart supports a high-redshift origin (z \u2273 3).",
"doi": "10.3847/1538-4357/ab1912",
"issn": "1538-4357",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2019-05-20",
"series_number": "1",
"volume": "877",
"issue": "1",
"pages": "Art. No. 45"
},
{
"id": "authors:hgy5w-dty59",
"collection": "authors",
"collection_id": "hgy5w-dty59",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20151119-140541049",
"type": "article",
"title": "High radio-frequency properties and variability of brightest cluster galaxies",
"author": [
{
"family_name": "Hogan",
"given_name": "M. T.",
"clpid": "Hogan-M-T"
},
{
"family_name": "Edge",
"given_name": "A. C.",
"clpid": "Edge-A-C"
},
{
"family_name": "Geach",
"given_name": "J. E.",
"orcid": "0000-0003-4964-4635",
"clpid": "Geach-J-E"
},
{
"family_name": "Grainge",
"given_name": "K. J. B.",
"clpid": "Grainge-K-J-B"
},
{
"family_name": "Hlavacek-Larrondo",
"given_name": "J.",
"orcid": "0000-0001-7271-7340",
"clpid": "Hlavacek-Larrondo-J"
},
{
"family_name": "Hovatta",
"given_name": "T.",
"orcid": "0000-0002-2024-8199",
"clpid": "Hovatta-T"
},
{
"family_name": "Karim",
"given_name": "A.",
"orcid": "0000-0002-8414-9579",
"clpid": "Karim-A"
},
{
"family_name": "McNamara",
"given_name": "B. R.",
"clpid": "McNamara-B-R"
},
{
"family_name": "Rumsey",
"given_name": "C.",
"clpid": "Rumsey-C"
},
{
"family_name": "Russell",
"given_name": "H. R.",
"clpid": "Russell-H-R"
},
{
"family_name": "Salom\u00e9",
"given_name": "P.",
"clpid": "Salom\u00e9-P"
},
{
"family_name": "Aller",
"given_name": "H. D.",
"clpid": "Aller-H-D"
},
{
"family_name": "Aller",
"given_name": "M. F.",
"orcid": "0000-0003-2483-2103",
"clpid": "Aller-M-F"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Fabian",
"given_name": "A. C.",
"orcid": "0000-0002-9378-4072",
"clpid": "Fabian-A-C"
},
{
"family_name": "Readhead",
"given_name": "A. C. S.",
"orcid": "0000-0001-9152-961X",
"clpid": "Readhead-A-C-S"
},
{
"family_name": "Sadler",
"given_name": "E. M.",
"clpid": "Sadler-E-M"
},
{
"family_name": "Saunders",
"given_name": "R. D. E.",
"clpid": "Saunders-R-D-E"
}
],
"abstract": "We consider the high radio-frequency (15\u2013353 GHz) properties and variability of 35 brightest cluster galaxies (BCGs). These are the most core-dominated sources drawn from a parent sample of more than 700 X-ray selected clusters, thus allowing us to relate our results to the general population. We find that \u22656.0\u2009per\u2009cent of our parent sample (\u226515.1\u2009per\u2009cent if only cool-core clusters are considered) contain a radio source at 150 GHz of at least 3 mJy (\u22481\u00d710^(23) W Hz^(\u22121) at our median redshift of z \u2248 0.13). Furthermore, \u22653.4\u2009per\u2009cent of the BCGs in our parent sample contain a peaked component (Gigahertz Peaked Spectrum, GPS) in their spectra that peaks above 2 GHz, increasing to \u22658.5\u2009per\u2009cent if only cool-core clusters are considered. We see little evidence for strong variability at 15 GHz on short (week\u2013month) time-scales although we see variations greater than 20\u2009per\u2009cent at 150 GHz over six-month time frames for 4 of the 23 sources with multi-epoch observations. Much more prevalent is long-term (year\u2013decade time-scale) variability, with average annual amplitude variations greater than 1\u2009per\u2009cent at 15 GHz being commonplace. There is a weak trend towards higher variability as the peak of the GPS-like component occurs at higher frequency. We demonstrate the complexity that is seen in the radio spectra of BCGs and discuss the potentially significant implications of these high-peaking components for Sunyaev\u2013Zel'dovich cluster searches.",
"doi": "10.1093/mnras/stv1518",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2015-10-21",
"series_number": "2",
"volume": "453",
"issue": "2",
"pages": "1223-1240"
},
{
"id": "authors:ax24d-6mj06",
"collection": "authors",
"collection_id": "ax24d-6mj06",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150827-121622584",
"type": "article",
"title": "Resolving the Merging Planck Cluster PLCK G147.3-16.6 with GISMO",
"author": [
{
"family_name": "Mroczkowski",
"given_name": "T.",
"orcid": "0000-0003-3816-5372",
"clpid": "Mroczkowski-T-K"
},
{
"family_name": "Kov\u00e1cs",
"given_name": "A.",
"clpid": "Kov\u00e1cs-A"
},
{
"family_name": "Bulbul",
"given_name": "E.",
"clpid": "Bulbul-E"
},
{
"family_name": "Staguhn",
"given_name": "J.",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Clarke",
"given_name": "T. E.",
"clpid": "Clarke-T-E"
},
{
"family_name": "van Weeren",
"given_name": "R. J.",
"orcid": "0000-0002-0587-1660",
"clpid": "van-Weeren-R-J"
},
{
"family_name": "Intema",
"given_name": "H. T.",
"orcid": "0000-0002-5880-2730",
"clpid": "Intema-H-T"
},
{
"family_name": "Randall",
"given_name": "S.",
"clpid": "Randall-S-W"
}
],
"abstract": "The Planck satellite has recently completed an all-sky galaxy cluster survey exploiting the thermal Sunyaev\u2013Zel'dovich (SZ) effect to locate some of the most massive systems observable. With a median redshift of =0.22, the clusters found by Planck at z > 0.3 are proving to be exceptionally massive and/or disturbed systems. One notable Planck discovery at z = 0.645, PLCK G147.3-16.6, has an elongated core and hosts a radio halo, indicating it is likely in the process of merging. We present a 16\".5 resolution SZ observation of this high-z merger using the Goddard-IRAM Superconducting 2-Millimeter Observer, and compare it to X-ray follow-up observations with XMM-Newton. We find the SZ pressure substructure is offset from the core components seen in X-ray. We interpret this as possible line of sight temperature or density substructure due to the on-going merger.",
"doi": "10.1088/2041-8205/808/1/L6",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2015-07-20",
"series_number": "1",
"volume": "808",
"issue": "1",
"pages": "Art. No. L6"
},
{
"id": "authors:rkmyj-c3j88",
"collection": "authors",
"collection_id": "rkmyj-c3j88",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150402-140643439",
"type": "article",
"title": "Highly efficient star formation in NGC 5253 possibly from stream-fed accretion",
"author": [
{
"family_name": "Turner",
"given_name": "J. L.",
"orcid": "0000-0003-4625-2951",
"clpid": "Turner-J-L"
},
{
"family_name": "Beck",
"given_name": "S. C.",
"clpid": "Beck-S-C"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Consiglio",
"given_name": "S. M.",
"clpid": "Consiglio-S-M"
},
{
"family_name": "Ho",
"given_name": "Paul T. P.",
"clpid": "Ho-Paul-T-P"
},
{
"family_name": "Kovacs",
"given_name": "A.",
"clpid": "Kovacs-A"
},
{
"family_name": "Meier",
"given_name": "D. S.",
"orcid": "0000-0001-9436-9471",
"clpid": "Meier-D-S"
},
{
"family_name": "Zhao",
"given_name": "Jun-Hui",
"orcid": "0000-0002-1317-3328",
"clpid": "Zhao-Jun-Hui"
}
],
"abstract": "Gas clouds in present-day galaxies are inefficient at forming stars. Low star-formation efficiency is a critical parameter in galaxy evolution: it is why stars are still forming nearly 14 billion years after the Big Bang and why star clusters generally do not survive their births, instead dispersing to form galactic disks or bulges. Yet the existence of ancient massive bound star clusters (globular clusters) in the Milky Way suggests that efficiencies were higher when they formed ten billion years ago. A local dwarf galaxy, NGC 5253, has a young star cluster that provides an example of highly efficient star formation. Here we report the detection of the J = 3 2 rotational transition of CO at the location of the massive cluster. The gas cloud is hot, dense, quiescent and extremely dusty. Its gas-to-dust ratio is lower than the Galactic value, which we attribute to dust enrichment by the embedded star cluster. Its star-formation efficiency exceeds 50 per cent, tenfold that of clouds in the Milky Way. We suggest that high efficiency results from the force-feeding of star formation by a streamer of gas falling into the galaxy.",
"doi": "10.1038/nature14218",
"issn": "0028-0836",
"publisher": "Nature Publishing Group",
"publication": "Nature",
"publication_date": "2015-03-19",
"series_number": "7543",
"volume": "519",
"issue": "7543",
"pages": "331-333"
},
{
"id": "authors:62afg-gk992",
"collection": "authors",
"collection_id": "62afg-gk992",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160824-144504856",
"type": "article",
"title": "NuSTAR and XMM-Newton Observations of Luminous, Heavily Obscured, WISE-selected Quasars at z ~ 2",
"author": [
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Lansbury",
"given_name": "G. B.",
"orcid": "0000-0002-5328-9827",
"clpid": "Lansbury-G-B"
},
{
"family_name": "Assef",
"given_name": "R. J.",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Brandt",
"given_name": "W. N.",
"orcid": "0000-0002-0167-2453",
"clpid": "Brandt-W-N"
},
{
"family_name": "Alexander",
"given_name": "D. M.",
"orcid": "0000-0002-5896-6313",
"clpid": "Alexander-D-M"
},
{
"family_name": "Ballantyne",
"given_name": "D. R.",
"orcid": "0000-0001-8128-6976",
"clpid": "Ballantyne-D-R"
},
{
"family_name": "Balokovi\u0107",
"given_name": "M.",
"orcid": "0000-0003-0476-6647",
"clpid": "Balokovi\u0107-M"
},
{
"family_name": "Bauer",
"given_name": "F. E.",
"orcid": "0000-0002-8686-8737",
"clpid": "Bauer-F-E"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Boggs",
"given_name": "S. E.",
"orcid": "0000-0001-9567-4224",
"clpid": "Boggs-S-E"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C-R"
},
{
"family_name": "Brightman",
"given_name": "M.",
"orcid": "0000-0002-8147-2602",
"clpid": "Brightman-M"
},
{
"family_name": "Christensen",
"given_name": "F. E.",
"orcid": "0000-0001-5679-1946",
"clpid": "Christensen-F-E"
},
{
"family_name": "Comastri",
"given_name": "Andrea",
"orcid": "0000-0003-3451-9970",
"clpid": "Comastri-A"
},
{
"family_name": "Craig",
"given_name": "William W.",
"clpid": "Craig-W-W"
},
{
"family_name": "Del Moro",
"given_name": "A.",
"clpid": "Del-Moro-A"
},
{
"family_name": "Eisenhardt",
"given_name": "Peter R. M.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Gandhi",
"given_name": "P.",
"orcid": "0000-0003-3105-2615",
"clpid": "Gandhi-Poshak"
},
{
"family_name": "Griffith",
"given_name": "R. L.",
"clpid": "Griffith-R-L"
},
{
"family_name": "Hailey",
"given_name": "C. J.",
"clpid": "Hailey-C-J"
},
{
"family_name": "Harrison",
"given_name": "F. A.",
"orcid": "0000-0002-4226-8959",
"clpid": "Harrison-F-A"
},
{
"family_name": "Hickox",
"given_name": "R. C.",
"orcid": "0000-0003-1468-9526",
"clpid": "Hickox-R-C"
},
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Koss",
"given_name": "M.",
"orcid": "0000-0002-7998-9581",
"clpid": "Koss-M-J"
},
{
"family_name": "Lake",
"given_name": "S.",
"clpid": "Lake-S-E"
},
{
"family_name": "LaMassa",
"given_name": "S. M.",
"orcid": "0000-0002-5907-3330",
"clpid": "LaMassa-S-M"
},
{
"family_name": "Luo",
"given_name": "B.",
"orcid": "0000-0002-9036-0063",
"clpid": "Luo-Bin"
},
{
"family_name": "Tsai",
"given_name": "C. W.",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Urry",
"given_name": "C. M.",
"orcid": "0000-0002-0745-9792",
"clpid": "Urry-C-M"
},
{
"family_name": "Walton",
"given_name": "D. J.",
"orcid": "0000-0001-5819-3552",
"clpid": "Walton-D-J"
},
{
"family_name": "Wright",
"given_name": "D. J.",
"clpid": "Wright-D-J"
},
{
"family_name": "Wu",
"given_name": "J.",
"orcid": "0000-0001-7808-3756",
"clpid": "Wu-Jingwen"
},
{
"family_name": "Yan",
"given_name": "L.",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Zhang",
"given_name": "W. W.",
"orcid": "0000-0002-1426-9698",
"clpid": "Zhang-W-W"
}
],
"abstract": "We report on a NuSTAR and XMM-Newton program that has observed a sample of three extremely luminous, heavily obscured WISE-selected active galactic nuclei (AGNs) at z ~ 2 across a broad X-ray band (0.1 - 79 keV). The parent sample, selected to be faint or undetected in the WISE 3.4 \u03bcm (W1) and 4.6 \u03bcm (W2) bands but bright at 12 \u03bcm (W3) and 22 \u03bcm (W4), are extremely rare, with only ~1000 so-called \"W1W2-dropouts\" across the extragalactic sky. Optical spectroscopy reveals typical redshifts of z ~ 2 for this population, implying rest-frame mid-IR luminosities of \u03bdL \u03bd(6 \u03bcm) ~ 6 \u00d7 1046 erg s^-1 and bolometric luminosities that can exceed L bol ~ 1014 L_\u2299. The corresponding intrinsic, unobscured hard X-ray luminosities are L(2-10 keV) ~ 4 \u00d7 1045 erg s-1 for typical quasar templates. These are among the most AGNs known, though the optical spectra rarely show evidence of a broad-line region and the selection criteria imply heavy obscuration even at rest-frame 1.5 \u03bcm. We designed our X-ray observations to obtain robust detections for gas column densities N H <= 1024 cm-2. In fact, the sources prove to be fainter than these predictions. Two of the sources were observed by both NuSTAR and XMM-Newton, with neither being detected by NuSTAR (f 3-24 keV <~ 10-13 erg cm^(-2)s^(-1), and one being faintly detected by XMM-Newton (f 0.5-10 keV ~ 5 \u00d7 10-15 erg cm-2 s-1). A third source was observed only with XMM-Newton, yielding a faint detection (f 0.5-10 keV ~ 7 \u00d7 10-15 erg cm-2 s-1). The X-ray data imply these sources are either X-ray weak, or are heavily obscured by column densities N H >~ 1024 cm-2. The combined X-ray and mid-IR analysis seems to favor this second possibility, implying the sources are extremely obscured, consistent with Compton-thick, luminous quasars. The discovery of a significant population of heavily obscured, extremely luminous AGNs would not conform to the standard paradigm of a receding torus, in which more luminous quasars are less likely to be obscured, and instead suggests that an additional source of obscuration is present in these extreme sources.",
"doi": "10.1088/0004-637X/794/2/102",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2014-10",
"series_number": "2",
"volume": "79",
"issue": "2",
"pages": "Art No.102"
},
{
"id": "authors:s2vze-efp27",
"collection": "authors",
"collection_id": "s2vze-efp27",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20141002-141208452",
"type": "article",
"title": "Interferometric Follow-up of WISE Hyper-luminous Hot, Dust-obscured Galaxies",
"author": [
{
"family_name": "Wu",
"given_name": "Jingwen",
"orcid": "0000-0001-7808-3756",
"clpid": "Wu-Jingwen"
},
{
"family_name": "Bussmann",
"given_name": "R. Shane",
"clpid": "Bussmann-R-S"
},
{
"family_name": "Tsai",
"given_name": "Chao-Wei",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Petric",
"given_name": "Andreea",
"orcid": "0000-0003-4030-3455",
"clpid": "Petric-A-O"
},
{
"family_name": "Blain",
"given_name": "Andrew",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Eisenhardt",
"given_name": "Peter R. M.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Bridge",
"given_name": "Carrie R.",
"clpid": "Bridge-C-R"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Assef",
"given_name": "Roberto J.",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Gelino",
"given_name": "Christopher R.",
"clpid": "Gelino-C-R"
},
{
"family_name": "Moustakas",
"given_name": "Leonidas",
"orcid": "0000-0003-3030-2360",
"clpid": "Moustakas-L-A"
},
{
"family_name": "Wright",
"given_name": "Edward L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
}
],
"abstract": "The Wide-field Infrared Survey Explorer (WISE) has discovered an extraordinary population of hyper-luminous dusty galaxies that are faint in the two bluer passbands (3.4 \u03bcm and 4.6 \u03bcm) but are bright in the two redder passbands of WISE (12 \u03bcm and 22 \u03bcm). We report on initial follow-up observations of three of these hot, dust-obscured galaxies, or Hot DOGs, using the Combined Array for Research in Millimeter-wave Astronomy and the Submillimeter Array interferometer arrays at submillimeter/millimeter wavelengths. We report continuum detections at ~1.3 mm of two sources (WISE J014946.17+235014.5 and WISE J223810.20+265319.7, hereafter W0149+2350 and W2238+2653, respectively), and upper limits to CO line emission at 3 mm in the observed frame for two sources (W0149+2350 and WISE J181417.29+341224.8, hereafter W1814+3412). The 1.3 mm continuum images have a resolution of 1\"-2\" and are consistent with single point sources. We estimate the masses of cold dust are 2.0 \u00d7 10^8 M_\u2609 for W0149+2350 and 3.9 \u00d7 10^8 M_\u2609 for W2238+2653, comparable to cold dust masses of luminous quasars. We obtain 2\u03c3 upper limits to the molecular gas masses traced by CO, which are 3.3 \u00d7 10^(10) M_\u2609 and 2.3 \u00d7 10^(10) M_\u2609 for W0149+2350 and W1814+3412, respectively. We also present high-resolution, near-IR imaging with the WFC3 on the Hubble Space Telescope for W0149+2653 and with NIRC2 on Keck for W2238+2653. The near-IR images show morphological structure dominated by a single, centrally condensed source with effective radius less than 4 kpc. No signs of gravitational lensing are evident.",
"doi": "10.1088/0004-637X/793/1/8",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2014-09-20",
"series_number": "1",
"volume": "793",
"issue": "1",
"pages": "Art. No. 8"
},
{
"id": "authors:6vjmb-wmj88",
"collection": "authors",
"collection_id": "6vjmb-wmj88",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140815-140858231",
"type": "article",
"title": "The GISMO Two-millimeter Deep Field in GOODS-N",
"author": [
{
"family_name": "Staguhn",
"given_name": "Johannes G.",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
},
{
"family_name": "Kov\u00e1cs",
"given_name": "Attila",
"clpid": "Kov\u00e1cs-A"
},
{
"family_name": "Arendt",
"given_name": "Richard G.",
"orcid": "0000-0001-8403-8548",
"clpid": "Arendt-R-G"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Decarli",
"given_name": "Roberto",
"orcid": "0000-0002-2662-8803",
"clpid": "Decarli-R"
},
{
"family_name": "Dwek",
"given_name": "Eli",
"orcid": "0000-0001-8033-1181",
"clpid": "Dwek-E"
},
{
"family_name": "Fixsen",
"given_name": "Dale J.",
"clpid": "Fixsen-D-J"
},
{
"family_name": "Hilton",
"given_name": "Gene C.",
"clpid": "Hilton-G-C"
},
{
"family_name": "Irwin",
"given_name": "Kent D.",
"clpid": "Irwin-K-D"
},
{
"family_name": "Jhabvala",
"given_name": "Christine A.",
"clpid": "Jhabvala-C-A"
},
{
"family_name": "Karim",
"given_name": "Alexander",
"orcid": "0000-0002-8414-9579",
"clpid": "Karim-A"
},
{
"family_name": "Leclercq",
"given_name": "Samuel",
"clpid": "Leclercq-S"
},
{
"family_name": "Maher",
"given_name": "Stephen F.",
"clpid": "Maher-S-F"
},
{
"family_name": "Miller",
"given_name": "Timothy M.",
"clpid": "Miller-T-M"
},
{
"family_name": "Moseley",
"given_name": "S. Harvey",
"clpid": "Moseley-S-H-Jr"
},
{
"family_name": "Sharp",
"given_name": "Elmer H.",
"clpid": "Sharp-E-H"
},
{
"family_name": "Walter",
"given_name": "Fabian",
"orcid": "0000-0003-4793-7880",
"clpid": "Walter-F"
},
{
"family_name": "Wollack",
"given_name": "Edward J.",
"orcid": "0000-0002-7567-4451",
"clpid": "Wollack-E-J"
}
],
"abstract": "We present deep continuum observations using the GISMO camera at a wavelength of 2 mm centered on the Hubble Deep Field in the GOODS-N field. These are the first deep field observations ever obtained at this wavelength. The 1\u03c3 sensitivity in the innermost ~4' of the 7' diameter map is ~135\u2009\u03bcJy beam^(\u22121), a factor of three higher in flux/beam sensitivity than the deepest available SCUBA 850\u2009\u03bcm observations, and almost a factor of four higher in flux/beam sensitivity than the combined MAMBO/AzTEC 1.2 mm observations of this region. Our source extraction algorithm identifies 12 sources directly, and another 3 through correlation with known sources at 1.2 mm and 850\u2009\u03bcm. Five of the directly detected GISMO sources have counterparts in the MAMBO/AzTEC catalog, and four of those also have SCUBA counterparts. HDF850.1, one of the first blank-field detected submillimeter galaxies, is now detected at 2 mm. The median redshift of all sources with counterparts of known redshifts is med(z) = 2.91\u00b10.94. Statistically, the detections are most likely real for five of the seven 2 mm sources without shorter wavelength counterparts, while the probability for none of them being real is negligible.",
"doi": "10.1088/0004-637X/790/1/77",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2014-07-20",
"series_number": "1",
"volume": "790",
"issue": "1",
"pages": "Art. No. 77"
},
{
"id": "authors:bbnxv-nf248",
"collection": "authors",
"collection_id": "bbnxv-nf248",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140731-131829349",
"type": "article",
"title": "Dust Formation, Evolution, and Obscuration Effects in the Very High-redshift Universe",
"author": [
{
"family_name": "Dwek",
"given_name": "Eli",
"orcid": "0000-0001-8033-1181",
"clpid": "Dwek-E"
},
{
"family_name": "Staguhn",
"given_name": "Johannes",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
},
{
"family_name": "Arendt",
"given_name": "Richard G.",
"orcid": "0000-0001-8403-8548",
"clpid": "Arendt-R-G"
},
{
"family_name": "Kovacks",
"given_name": "Attila",
"clpid": "Kovacs-A"
},
{
"family_name": "Su",
"given_name": "Ting",
"clpid": "Su-Ting"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
}
],
"abstract": "The evolution of dust at redshifts z \u2273 9, and consequently the dust properties, differs greatly from that in the local universe. In contrast to the local universe, core collapse supernovae (CCSNe) are the only source of thermally condensed dust. Because of the low initial dust-to-gas mass ratio, grain destruction rates are low, so that CCSNe are net producers of interstellar dust. Galaxies with large initial gas mass or high mass infall rate will therefore have a more rapid net rate of dust production compared to galaxies with lower gas mass, even at the same star formation rate. The dust composition is dominated by silicates, which exhibit a strong rise in the UV opacity near the Lyman break. This \"silicate-UV break\" may be confused with the Lyman break, resulting in a misidentification of a galaxy's photometric redshift. In this Letter we demonstrate these effects by analyzing the spectral energy distribution of MACS1149-JD, a lensed galaxy at z = 9.6. A potential 2 mm counterpart of MACS1149-JD has been identified with GISMO. While additional observations are required to corroborate this identification, we use this possible association to illustrate the physical processes and the observational effects of dust in the very high-redshift universe.",
"doi": "10.1088/2041-8205/788/2/L30",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2014-06-20",
"series_number": "2",
"volume": "788",
"issue": "2",
"pages": "Art. No. L30"
},
{
"id": "authors:bvb6j-ypz92",
"collection": "authors",
"collection_id": "bvb6j-ypz92",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140117-134052510",
"type": "article",
"title": "WISE J233237.05\u2013505643.5: A Double-peaked, Broad-lined Active Galactic Nucleus with a Spiral-shaped Radio Morphology",
"author": [
{
"family_name": "Tsai",
"given_name": "Chao-Wei",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Emonts",
"given_name": "Bjorn",
"clpid": "Emonts-B"
},
{
"family_name": "Barrows",
"given_name": "R. Scott",
"orcid": "0000-0002-6212-7328",
"clpid": "Barrows-R-S"
},
{
"family_name": "Assef",
"given_name": "Roberto J.",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Norris",
"given_name": "Ray P.",
"orcid": "0000-0002-4597-1906",
"clpid": "Norris-R-P"
},
{
"family_name": "Einsenhardt",
"given_name": "Peter R. M.",
"clpid": "Einsenhardt-P-R-M"
},
{
"family_name": "Lonsdale",
"given_name": "Carol",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-C-J"
},
{
"family_name": "Blain",
"given_name": "Andrew W.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Wu",
"given_name": "Jingwen",
"orcid": "0000-0001-7808-3756",
"clpid": "Wu-Jingwen"
},
{
"family_name": "Stalder",
"given_name": "Brian",
"clpid": "Stalder-B"
},
{
"family_name": "Stubbs",
"given_name": "Christopher W.",
"orcid": "0000-0003-0347-1724",
"clpid": "Stubbs-C-W"
},
{
"family_name": "High",
"given_name": "F. William",
"clpid": "High-F-W"
},
{
"family_name": "Li",
"given_name": "K. L.",
"clpid": "Li-Kelin"
},
{
"family_name": "Kong",
"given_name": "Albert K. H.",
"orcid": "0000-0002-5105-344X",
"clpid": "Kong-Albert-K-H"
}
],
"abstract": "We present radio continuum mapping, optical imaging, and spectroscopy of the newly discovered double-peaked, broad-lined active galactic nucleus (AGN) WISE J233237.05\u2013505643.5 at redshift z = 0.3447. This source exhibits an FR-I and FR-II hybrid morphology, characterized by a bright core, jet, and Doppler-boosted lobe structures in Australian Telescope Compact Array continuum maps at 1.5, 5.6, and 9 GHz. Unlike most FR-II objects, W2332\u20135056 is hosted by a disk-like galaxy. The core has a projected 5'' linear radio feature that is perpendicular to the curved primary jet, hinting at unusual and complex activity within the inner 25 kpc. The multi-epoch, optical-near-IR photometric measurements indicate significant variability over a 3-20 yr baseline from the AGN component. Gemini South optical data show unusual double-peaked emission-line features: the centroids of the broad-lined components of H\u03b1 and H\u03b2 are blueshifted with respect to the narrow lines and host galaxy by ~3800 km s^(\u20131). We examine possible cases that involve single or double supermassive black holes in the system and discuss the required future investigations to disentangle the mysterious nature of this system.",
"doi": "10.1088/0004-637X/779/1/41",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2013-12-10",
"series_number": "1",
"volume": "779",
"issue": "1",
"pages": "Art. No. 41"
},
{
"id": "authors:y5kxj-g4897",
"collection": "authors",
"collection_id": "y5kxj-g4897",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140106-094902432",
"type": "article",
"title": "WISE detections of known QSOs at redshifts greater than six",
"author": [
{
"family_name": "Blain",
"given_name": "Andrew W.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Assef",
"given_name": "Roberto",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Tsai",
"given_name": "Chao-Wei",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Eisenhardt",
"given_name": "Peter",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Bridge",
"given_name": "Carrie",
"clpid": "Bridge-C-R"
},
{
"family_name": "Benford",
"given_name": "Dominic",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Jarrett",
"given_name": "Tom",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Cutri",
"given_name": "Roc",
"orcid": "0000-0002-0077-2305",
"clpid": "Cutri-R-M"
},
{
"family_name": "Petty",
"given_name": "Sara",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Wu",
"given_name": "Jingwen",
"orcid": "0000-0001-7808-3756",
"clpid": "Wu-Jingwen"
},
{
"family_name": "Wright",
"given_name": "Edward L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
}
],
"abstract": "We present WISE All-Sky mid-infrared (IR) survey detections of 55% (17/31) of the known QSOs at z > 6 from a range of surveys: the SDSS, the CFHT-LS, FIRST, Spitzer, and UKIDSS. The WISE catalog thus provides a substantial increase in the quantity of IR data available for these sources: 17 are detected in the WISE W1 (3.4 \u03bcm) band, 16 in W2 (4.6 \u03bcm), 3 in W3 (12 \u03bcm), and 0 in W4 (22 \u03bcm). This is particularly important with Spitzer in its warm-mission phase and no faint follow-up capability at wavelengths longward of 5 \u03bcm until the launch of James Webb Space Telescope (JWST). WISE thus provides a useful tool for understanding QSOs found in forthcoming large-area optical/IR sky surveys using PanSTARRS, SkyMapper, VISTA, DES, and LSST. The rest-UV properties of the WISE-detected and the WISE-non-detected samples differ: the detections have brighter i/z-band magnitudes and redder rest-UV colors. This suggests that a more aggressive hunt for very high redshift QSOs by combining WISE W1 and W2 data with red, observed optical colors could be effective at least for a subset of dusty candidate QSOs. Stacking the WISE images of the WISE-non-detected QSOs indicates that they are, on average, significantly fainter than the WISE-detected examples, and are thus not narrowly missing detection in the WISE catalog. The WISE catalog detection of three of our sample in the W3 band indicates that their mid-IR flux can be detected individually, although there is no stacked W3 detection of sources detected in W1 but not W3. Stacking analyses of WISE data for large active galactic nucleus samples will be a useful tool, and high-redshift QSOs of all types will be easy targets for JWST.",
"doi": "10.1088/0004-637X/778/2/113",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2013-12-01",
"series_number": "2",
"volume": "778",
"issue": "2",
"pages": "Art. No. 113"
},
{
"id": "authors:p8hmn-b3584",
"collection": "authors",
"collection_id": "p8hmn-b3584",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20131011-105108149",
"type": "article",
"title": "UV-bright Nearby Early-type Galaxies Observed in the Mid-infrared: Evidence for a Multi-stage Formation History by Way of WISE and GALEX Imaging",
"author": [
{
"family_name": "Petty",
"given_name": "S. M.",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Neill",
"given_name": "J. D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Blain",
"given_name": "A. W.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Farrah",
"given_name": "D. G.",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-D"
},
{
"family_name": "Rich",
"given_name": "R. M.",
"orcid": "0000-0003-0427-8387",
"clpid": "Rich-R-M"
},
{
"family_name": "Tsai",
"given_name": "C.-W.",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Bridge",
"given_name": "C. R.",
"clpid": "Bridge-C-R"
},
{
"family_name": "Lake",
"given_name": "S. E.",
"clpid": "Lake-S-E"
},
{
"family_name": "Masci",
"given_name": "F. J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Wright",
"given_name": "E. L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
}
],
"abstract": "In the local universe, 10% of massive elliptical galaxies are observed to exhibit a peculiar property: a substantial excess of ultraviolet emission than what is expected from their old, red stellar populations. Several origins for this ultraviolet excess (UVX) have been proposed including a population of hot young stars and a population of old, blue horizontal branch or extended horizontal branch (BHB or EHB) stars that have undergone substantial mass loss from their outer atmospheres. We explore the radial distribution of UVX in a selection of 49 nearby E/S0-type galaxies by measuring their extended photometry in the UV through mid-infrared (mid-IR) with the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the Wide-field Infrared Survey Explorer (WISE). We compare UV/optical and UV/mid-IR colors with the Flexible Stellar Population Synthesis models, which allow for the inclusion of EHB stars. We find that combined WISE mid-IR and GALEX UV colors are more effective in distinguishing models than optical colors, and that the UV/mid-IR combination is sensitive to the EHB fraction. There are strong color gradients, with the outer radii bluer than the inner half-light radii by ~1 mag. This color difference is easily accounted for with an increase in the BHB fraction of 0.25 with radius. We estimated that the average ages for the inner and outer radii are 7.0 \u00b1 0.3 Gyr, and 6.2 \u00b1 0.2 Gyr, respectively, with the implication that the outer regions are likely to have formed ~1 Gyr after the inner regions. Additionally, we find that metallicity gradients are likely not a significant factor in the color difference. The separation of color between the inner and outer regions, which agrees with a specific stellar population difference (e.g., higher EHB populations), and the ~0.5\u20132 Gyr age difference suggests multi-stage formation. Our results are best explained by inside-out formation: rapid star formation within the core at early epochs (>4 Gyr ago) and at least one later stage starburst event coinciding with z ~ 1.",
"doi": "10.1088/0004-6256/146/4/77",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2013-10",
"series_number": "4",
"volume": "146",
"issue": "4",
"pages": "Art. No. 77"
},
{
"id": "authors:t8x5r-vej40",
"collection": "authors",
"collection_id": "t8x5r-vej40",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120604-084501850",
"type": "article",
"title": "A New Population of High-z, Dusty Ly\u03b1 Emitters and Blobs Discovered by WISE: Feedback Caught in the Act?",
"author": [
{
"family_name": "Bridge",
"given_name": "Carrie R.",
"clpid": "Bridge-C-R"
},
{
"family_name": "Blain",
"given_name": "Andrew",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Borys",
"given_name": "Colin J. K.",
"clpid": "Borys-C-J-K"
},
{
"family_name": "Petty",
"given_name": "Sara M.",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Eisenhardt",
"given_name": "Peter",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Farrah",
"given_name": "Duncan",
"orcid": "0000-0003-1748-2010",
"clpid": "Farrah-Duncan"
},
{
"family_name": "Griffith",
"given_name": "Roger L.",
"clpid": "Griffith-R-L"
},
{
"family_name": "Jarrett",
"given_name": "Tom",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Lonsdale",
"given_name": "Carol",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Stanford",
"given_name": "Spencer A.",
"clpid": "Stanford-S-A"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Tsai",
"given_name": "Chao-Wei",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Wright",
"given_name": "Edward L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
},
{
"family_name": "Wu",
"given_name": "Jingwen",
"orcid": "0000-0001-7808-3756",
"clpid": "Wu-Jingwen"
}
],
"abstract": "By combining data from the NASA Wide-field Infrared Survey Explorer (WISE) mission with optical spectroscopy from the W. M. Keck telescope, we discover a mid-IR color criterion that yields a 78% success rate in identifying rare, typically radio-quiet, 1.6 \u227e z \u227e 4.6 dusty Ly\u03b1 emitters (LAEs). Of these, at least 37% have emission extended on scales of 30-100 kpc and are considered Ly\u03b1 \"blobs\" (LABs). The objects have a surface density of only ~0.1 deg^(\u20132), making them rare enough that they have been largely missed in deep, small area surveys. We measured spectroscopic redshifts for 92 of these galaxies, and find that the LAEs (LABs) have a median redshift of 2.3 (2.5). The WISE photometry coupled with data from Herschel (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) reveals that these galaxies are in the Hyper Luminous IR galaxy regime (L IR \u2273 10^(13)-10^(14) L_\u2609) and have warm colors. They are typically more luminous and warmer than other dusty, z ~ 2 populations such as submillimeter-selected galaxies and dust-obscured galaxies. These traits are commonly associated with the dust being illuminated by intense active galactic nucleus activity. We hypothesize that the combination of spatially extended Ly\u03b1, large amounts of warm IR-luminous dust, and rarity (implying a short-lived phase) can be explained if the galaxies are undergoing brief, intense \"feedback\" transforming them from an extreme dusty starburst/QSO into a mature galaxy.",
"doi": "10.1088/0004-637X/769/2/91",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2013-06-01",
"series_number": "2",
"volume": "769",
"issue": "2",
"pages": "Art. No. 91"
},
{
"id": "authors:vkj8x-hp913",
"collection": "authors",
"collection_id": "vkj8x-hp913",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20130115-090532935",
"type": "article",
"title": "Extending the Nearby Galaxy Heritage with WISE: First Results from the WISE Enhanced Resolution Galaxy Atlas",
"author": [
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Tsai",
"given_name": "C. W.",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Petty",
"given_name": "S.",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Cluver",
"given_name": "M. E.",
"orcid": "0000-0002-9871-6490",
"clpid": "Cluver-M-E"
},
{
"family_name": "Assef",
"given_name": "Roberto J.",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C-R"
},
{
"family_name": "Donoso",
"given_name": "E.",
"clpid": "Donoso-E"
},
{
"family_name": "Eisenhardt",
"given_name": "P.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Koribalski",
"given_name": "B.",
"clpid": "Koribalski-B-S"
},
{
"family_name": "Lake",
"given_name": "S.",
"clpid": "Lake-S"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Seibert",
"given_name": "M.",
"orcid": "0000-0002-1143-5515",
"clpid": "Seibert-M"
},
{
"family_name": "Sheth",
"given_name": "K.",
"orcid": "0000-0002-5496-4118",
"clpid": "Sheth-K"
},
{
"family_name": "Stanford",
"given_name": "S. Adam",
"clpid": "Stanford-S-A"
},
{
"family_name": "Wright",
"given_name": "E.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
}
],
"abstract": "The Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at mid-infrared wavelengths 3.4 \u03bcm, 4.6 \u03bcm, 12 \u03bcm, and 22 \u03bcm. The mission was primarily designed to extract point sources, leaving resolved and extended sources, for the most part, unexplored. Accordingly, we have begun a dedicated WISE Enhanced Resolution Galaxy Atlas (WERGA) project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we demonstrate the first results of the WERGA project for a sample of 17 galaxies, chosen to be of large angular size, diverse morphology, and covering a range in color, stellar mass, and star formation. It includes many well-studied galaxies, such as M 51, M 81, M 87, M 83, M 101, and IC 342. Photometry and surface brightness decomposition is carried out after special super-resolution processing, achieving spatial resolutions similar to that of Spitzer Infrared Array Camera. The enhanced resolution method is summarized in the first paper of this two-part series. In this second work, we present WISE, Spitzer, and Galaxy Evolution Explorer (GALEX) photometric and characterization measurements for the sample galaxies, combining the measurements to study the global properties. We derive star formation rates using the polycyclic aromatic hydrocarbon sensitive 12 \u03bcm (W3) fluxes, warm-dust sensitive 22 \u03bcm (W4) fluxes, and young massive-star sensitive ultraviolet (UV) fluxes. Stellar masses are estimated using the 3.4 \u03bcm (W1) and 4.6 \u03bcm (W2) measurements that trace the dominant stellar mass content. We highlight and showcase the detailed results of M 83, comparing the WISE/Spitzer results with the Australia Telescope Compact Array H I gas distribution and GALEX UV emission, tracing the evolution from gas to stars. In addition to the enhanced images, WISE's all-sky coverage provides a tremendous advantage over Spitzer for building a complete nearby galaxy catalog, tracing both stellar mass and star formation histories. We discuss the construction of a complete mid-infrared catalog of galaxies and its complementary role of studying the assembly and evolution of galaxies in the local universe.",
"doi": "10.1088/0004-6256/145/1/6",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2013-01",
"series_number": "1",
"volume": "145",
"issue": "1",
"pages": "Art. No. 6"
},
{
"id": "authors:x5876-ezy31",
"collection": "authors",
"collection_id": "x5876-ezy31",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121031-103418816",
"type": "article",
"title": "Submillimeter Follow-up of WISE-selected Hyperluminous Galaxies",
"author": [
{
"family_name": "Wu",
"given_name": "Jingwen",
"orcid": "0000-0001-7808-3756",
"clpid": "Wu-Jingwen"
},
{
"family_name": "Tsai",
"given_name": "Chao-Wei",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Sayers",
"given_name": "Jack",
"orcid": "0000-0002-8213-3784",
"clpid": "Sayers-Jack"
},
{
"family_name": "Benford",
"given_name": "Dominic",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Bridge",
"given_name": "Carrie",
"clpid": "Bridge-C-R"
},
{
"family_name": "Blain",
"given_name": "Andrew",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Eisenhardt",
"given_name": "Peter R. M.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Petty",
"given_name": "Sara",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Assef",
"given_name": "Roberto",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Bussmann",
"given_name": "Shane",
"clpid": "Bussmann-S"
},
{
"family_name": "Comerford",
"given_name": "Julia M.",
"orcid": "0000-0001-8627-4907",
"clpid": "Comerford-J-M"
},
{
"family_name": "Cutri",
"given_name": "Roc",
"orcid": "0000-0002-0077-2305",
"clpid": "Cutri-R-M"
},
{
"family_name": "Evans",
"given_name": "Neal J., II",
"orcid": "0000-0001-5175-1777",
"clpid": "Evans-N-J-II"
},
{
"family_name": "Griffith",
"given_name": "Roger",
"clpid": "Griffith-R-L"
},
{
"family_name": "Jarrett",
"given_name": "Thomas",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Lake",
"given_name": "Sean",
"clpid": "Lake-S"
},
{
"family_name": "Lonsdale",
"given_name": "Carol",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Rho",
"given_name": "Jeonghee",
"orcid": "0000-0003-3643-839X",
"clpid": "Rho-Jeonghee"
},
{
"family_name": "Stanford",
"given_name": "S. Adam",
"clpid": "Stanford-S-A"
},
{
"family_name": "Weiner",
"given_name": "Benjamin",
"clpid": "Weiner-B-J"
},
{
"family_name": "Wright",
"given_name": "Edward L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (∼1000 all-sky) population of galaxies at high redshift (peaks at z = 2–3), which are faint or undetected by WISE at 3.4 and 4.6 μm, yet are clearly detected at 12 and 22 μm. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350–850 μm, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 μm, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60–120 K using a single-temperature model. Their infrared luminosities are well over 1013 L\u2609. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.
",
"doi": "10.1088/0004-637X/756/1/96",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2012-09-01",
"series_number": "1",
"volume": "756",
"issue": "1",
"pages": "Art. No. 96"
},
{
"id": "authors:r0etj-a9w74",
"collection": "authors",
"collection_id": "r0etj-a9w74",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121030-134258087",
"type": "article",
"title": "The First Hyper-luminous Infrared Galaxy Discovered by WISE",
"author": [
{
"family_name": "Eisenhardt",
"given_name": "Peter R. M.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Wu",
"given_name": "Jingwen",
"orcid": "0000-0001-7808-3756",
"clpid": "Wu-Jingwen"
},
{
"family_name": "Tsai",
"given_name": "Chao-Wei",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Assef",
"given_name": "Roberto",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Benford",
"given_name": "Dominic",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Blain",
"given_name": "Andrew",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bridge",
"given_name": "Carrie",
"clpid": "Bridge-C-R"
},
{
"family_name": "Condon",
"given_name": "J. J.",
"orcid": "0000-0003-4724-1939",
"clpid": "Condon-J-J"
},
{
"family_name": "Cushing",
"given_name": "Michael C.",
"orcid": "0000-0001-7780-3352",
"clpid": "Cushing-M-C"
},
{
"family_name": "Cutri",
"given_name": "Roc",
"orcid": "0000-0002-0077-2305",
"clpid": "Cutri-R-M"
},
{
"family_name": "Evans",
"given_name": "Neal J., II",
"orcid": "0000-0001-5175-1777",
"clpid": "Evans-N-J-II"
},
{
"family_name": "Gelino",
"given_name": "Chris",
"clpid": "Gelino-C-R"
},
{
"family_name": "Griffith",
"given_name": "Roger L.",
"clpid": "Griffith-R-L"
},
{
"family_name": "Grillmair",
"given_name": "Carl J.",
"orcid": "0000-0003-4072-169X",
"clpid": "Grillmair-C-J"
},
{
"family_name": "Jarrett",
"given_name": "Tom",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Lonsdale",
"given_name": "Carol J.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Masci",
"given_name": "Frank J.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Mason",
"given_name": "Brian S.",
"clpid": "Mason-B-S"
},
{
"family_name": "Petty",
"given_name": "Sara",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Sayers",
"given_name": "Jack",
"orcid": "0000-0002-8213-3784",
"clpid": "Sayers-Jack"
},
{
"family_name": "Stanford",
"given_name": "S. A.",
"clpid": "Stanford-S-A"
},
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Wright",
"given_name": "Edward L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
}
],
"abstract": "We report the discovery by the Wide-field Infrared Survey Explorer (WISE) of the z = 2.452 source WISE J181417.29+341224.9, the first hyperluminous source found in the WISE survey. WISE 1814+3412 is also the prototype for an all-sky sample of ∼1000 extremely luminous \"W1W2-dropouts\" (sources faint or undetected by WISE at 3.4 and 4.6 μm and well detected at 12 or 22 μm). The WISE data and a 350 μm detection give a minimum bolometric luminosity of 3.7 × 1013 L\u2609, with ∼1014 L\u2609 plausible. Follow-up images reveal four nearby sources: a QSO and two Lyman break galaxies (LBGs) at z = 2.45, and an M dwarf star. The brighter LBG dominates the bolometric emission. Gravitational lensing is unlikely given the source locations and their different spectra and colors. The dominant LBG spectrum indicates a star formation rate ∼300 M\u2609 yr−1, accounting for \u2272 10% of the bolometric luminosity. Strong 22 μm emission relative to 350 μm implies that warm dust contributes significantly to the luminosity, while cooler dust normally associated with starbursts is constrained by an upper limit at 1.1 mm. Radio emission is ∼10 times above the far-infrared/radio correlation, indicating an active galactic nucleus (AGN) is present. An obscured AGN combined with starburst and evolved stellar components can account for the observations. If the black hole mass follows the local MBH–bulge mass relation, the implied Eddington ratio is \u2273 4. WISE 1814+3412 may be a heavily obscured object where the peak AGN activity occurred prior to the peak era of star formation.
",
"doi": "10.1088/0004-637X/755/2/173",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2012-08-20",
"series_number": "2",
"volume": "755",
"issue": "2",
"pages": "Art. No. 173"
},
{
"id": "authors:8gckr-m6b29",
"collection": "authors",
"collection_id": "8gckr-m6b29",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120827-101936774",
"type": "article",
"title": "Constructing a WISE High Resolution Galaxy Atlas",
"author": [
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Tsai",
"given_name": "C. W.",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Petty",
"given_name": "S.",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Cluver",
"given_name": "M.",
"orcid": "0000-0002-9871-6490",
"clpid": "Cluver-M-E"
},
{
"family_name": "Assef",
"given_name": "Roberto J.",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Bridge",
"given_name": "C.",
"clpid": "Bridge-C-R"
},
{
"family_name": "Donoso",
"given_name": "E.",
"clpid": "Donoso-E"
},
{
"family_name": "Eisenhardt",
"given_name": "P.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Fowler",
"given_name": "J.",
"clpid": "Fowler-J"
},
{
"family_name": "Koribalski",
"given_name": "B.",
"clpid": "Koribalski-B-S"
},
{
"family_name": "Lake",
"given_name": "S.",
"clpid": "Lake-S"
},
{
"family_name": "Neill",
"given_name": "James D.",
"orcid": "0000-0002-0466-1119",
"clpid": "Neill-J-D"
},
{
"family_name": "Seibert",
"given_name": "M.",
"orcid": "0000-0002-1143-5515",
"clpid": "Seibert-M"
},
{
"family_name": "Sheth",
"given_name": "K.",
"orcid": "0000-0002-5496-4118",
"clpid": "Sheth-K"
},
{
"family_name": "Stanford",
"given_name": "S.",
"clpid": "Stanford-S"
},
{
"family_name": "Wright",
"given_name": "E.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
}
],
"abstract": "After eight months of continuous observations, the Wide-field Infrared Survey Explorer (WISE) mapped the entire sky at 3.4 \u03bcm, 4.6 \u03bcm, 12 \u03bcm, and 22 \u03bcm. We have begun a dedicated WISE High Resolution Galaxy Atlas project to fully characterize large, nearby galaxies and produce a legacy image atlas and source catalog. Here we summarize the deconvolution techniques used to significantly improve the spatial resolution of WISE imaging, specifically designed to study the internal anatomy of nearby galaxies. As a case study, we present results for the galaxy NGC 1566, comparing the WISE enhanced-resolution image processing to that of Spitzer, Galaxy Evolution Explorer, and ground-based imaging. This is the first paper in a two-part series; results for a larger sample of nearby galaxies are presented in the second paper.",
"doi": "10.1088/0004-6256/144/2/68",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2012-08",
"series_number": "2",
"volume": "144",
"issue": "2",
"pages": "Art. No. 68"
},
{
"id": "authors:zyqzh-sb430",
"collection": "authors",
"collection_id": "zyqzh-sb430",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120724-083652733",
"type": "article",
"title": "Mid-infrared Selection of Active Galactic Nuclei with the Wide-Field Infrared Survey Explorer. I. Characterizing WISE-selected Active Galactic Nuclei in COSMOS",
"author": [
{
"family_name": "Stern",
"given_name": "Daniel",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Assef",
"given_name": "Roberto J.",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Blain",
"given_name": "Andrew",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Cutri",
"given_name": "Roc",
"orcid": "0000-0002-0077-2305",
"clpid": "Cutri-R-M"
},
{
"family_name": "Dey",
"given_name": "Arjun",
"orcid": "0000-0002-4928-4003",
"clpid": "Dey-A"
},
{
"family_name": "Einsenhardt",
"given_name": "Peter R. M.",
"clpid": "Einsenhardt-P-R-M"
},
{
"family_name": "Griffith",
"given_name": "Roger L.",
"clpid": "Griffith-R-L"
},
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Lake",
"given_name": "Sean",
"clpid": "Lake-S"
},
{
"family_name": "Masci",
"given_name": "Frank",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Petty",
"given_name": "Sara",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Stanford",
"given_name": "S. A.",
"clpid": "Stanford-S-A"
},
{
"family_name": "Tsai",
"given_name": "Chao-Wei",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Wright",
"given_name": "E. L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
},
{
"family_name": "Yan",
"given_name": "Lin",
"orcid": "0000-0003-1710-9339",
"clpid": "Yan-Lin"
},
{
"family_name": "Harrison",
"given_name": "Fiona",
"orcid": "0000-0002-4226-8959",
"clpid": "Harrison-F-A"
},
{
"family_name": "Madsen",
"given_name": "Kristin",
"orcid": "0000-0003-1252-4891",
"clpid": "Madsen-K-K"
}
],
"abstract": "The Wide-field Infrared Survey Explorer (WISE) is an extremely capable and efficient black hole finder. We present a simple mid-infrared color criterion, W1 \u2013 W2 \u2265 0.8 (i.e., [3.4]\u2013[4.6] \u22650.8, Vega), which identifies 61.9 \u00b1 5.4 active galactic nucleus (AGN) candidates per deg^2 to a depth of W2 ~ 15.0. This implies a much larger census of luminous AGNs than found by typical wide-area surveys, attributable to the fact that mid-infrared selection identifies both unobscured (type 1) and obscured (type 2) AGNs. Optical and soft X-ray surveys alone are highly biased toward only unobscured AGNs, while this simple WISE selection likely identifies even heavily obscured, Compton-thick AGNs. Using deep, public data in the COSMOS field, we explore the properties of WISE-selected AGN candidates. At the mid-infrared depth considered, 160 \u03bcJy at 4.6 \u03bcm, this simple criterion identifies 78% of Spitzer mid-infrared AGN candidates according to the criteria of Stern et al. and the reliability is 95%. We explore the demographics, multiwavelength properties and redshift distribution of WISE-selected AGN candidates in the COSMOS field.",
"doi": "10.1088/0004-637X/753/1/30",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2012-07-01",
"series_number": "1",
"volume": "753",
"issue": "1",
"pages": "Art. No. 30"
},
{
"id": "authors:j8vwb-fsw88",
"collection": "authors",
"collection_id": "j8vwb-fsw88",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120130-115037613",
"type": "article",
"title": "Wide-field Infrared Survey Explorer Observations of the Evolution of Massive Star-forming Regions",
"author": [
{
"family_name": "Koenig",
"given_name": "X. P.",
"clpid": "Koenig-X-P"
},
{
"family_name": "Leisawitz",
"given_name": "D. T.",
"clpid": "Leisawitz-D-T"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Rebull",
"given_name": "L. M.",
"orcid": "0000-0001-6381-515X",
"clpid": "Rebull-L-M"
},
{
"family_name": "Padgett",
"given_name": "D. L.",
"orcid": "0000-0001-5334-5107",
"clpid": "Padgett-D-L"
},
{
"family_name": "Assef",
"given_name": "R. J.",
"orcid": "0000-0002-9508-3667",
"clpid": "Assef-R-J"
}
],
"abstract": "We present the results of a mid-infrared survey of 11 outer Galaxy massive star-forming regions and 3 open clusters with data from the Wide-field Infrared Survey Explorer (WISE). Using a newly developed photometric scheme to identify young stellar objects and exclude extragalactic contamination, we have studied the distribution of young stars within each region. These data tend to support the hypothesis that latter generations may be triggered by the interaction of winds and radiation from the first burst of massive star formation with the molecular cloud material leftover from that earlier generation of stars. We dub this process the \"fireworks hypothesis\" since star formation by this mechanism would proceed rapidly and resemble a burst of fireworks. We have also analyzed small cutout WISE images of the structures around the edges of these massive star-forming regions. We observe large (1-3 pc size) pillar and trunk-like structures of diffuse emission nebulosity tracing excited polycyclic aromatic hydrocarbon molecules and small dust grains at the perimeter of the massive star-forming regions. These structures contain small clusters of emerging Class I and Class II sources, but some are forming only a single to a few new stars.",
"doi": "10.1088/0004-637X/744/2/130",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2012-01-10",
"series_number": "2",
"volume": "744",
"issue": "2",
"pages": "130"
},
{
"id": "authors:avp8j-z4002",
"collection": "authors",
"collection_id": "avp8j-z4002",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111014-150442996",
"type": "article",
"title": "First Detections of the [N II] 122 \u03bcm Line at High Redshift: Demonstrating the Utility of the Line for Studying Galaxies in the Early Universe",
"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-Thomas"
},
{
"family_name": "Parshley",
"given_name": "Stephen C.",
"clpid": "Parshley-S-C"
},
{
"family_name": "Stacey",
"given_name": "Gordon J.",
"clpid": "Stacey-G-J"
},
{
"family_name": "Phillips",
"given_name": "Thomas G.",
"clpid": "Phillips-T-G"
},
{
"family_name": "Falgarone",
"given_name": "Edith",
"clpid": "Falgarone-E"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Staguhn",
"given_name": "Johannes G.",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
},
{
"family_name": "Tucker",
"given_name": "Carol E.",
"clpid": "Tucker-C-E"
}
],
"abstract": "We report the first detections of the [N II] 122 \u03bcm line from a high-redshift galaxy. The line was strongly (>6\u03c3) detected from SMMJ02399\u20130136, and H1413+117 (the Cloverleaf QSO) using the Redshift (z) and Early Universe Spectrometer on the Caltech Submillimeter Observatory. The lines from both sources are quite bright with line to far-infrared (FIR) continuum luminosity ratios that are ~7.0 \u00d7 10^(\u20134) (Cloverleaf) and 2.1 \u00d7 10^(\u20133) (SMMJ02399). With ratios 2-10 times larger than the average value for nearby galaxies, neither source exhibits the line-to-continuum deficits seen in nearby sources. The line strengths also indicate large ionized gas fractions, ~8%-17% of the molecular gas mass. The [O III]/[N II] line ratio is very sensitive to the effective temperature of ionizing stars and the ionization parameter for emission arising in the narrow-line region (NLR) of an active galactic nucleus (AGN). Using our previous detection of the [O III] 88 \u03bcm line, the [O III]/[N II] line ratio for SMMJ02399\u20130136 indicates that the dominant source of the line emission is either stellar H II regions ionized by O9.5 stars, or the NLR of the AGN with ionization parameter log(U) = \u20133.3 to \u20134.0. A composite system, where 30%-50% of the FIR lines arise in the NLR also matches the data. The Cloverleaf is best modeled by a superposition of ~200 M82-like starbursts accounting for all of the FIR emission and 43% of the [N II] line. The remainder may come from the NLR. This work demonstrates the utility of the [N II] and [O III] lines in constraining properties of the ionized medium.",
"doi": "10.1088/2041-8205/740/1/L29",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2011-10-10",
"series_number": "1",
"volume": "740",
"issue": "1",
"pages": "Art. No. L29"
},
{
"id": "authors:gqy2e-kc451",
"collection": "authors",
"collection_id": "gqy2e-kc451",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110908-113958497",
"type": "article",
"title": "Star and Dust Formation Activities in AzTEC-3, a Starburst Galaxy at z = 5.3",
"author": [
{
"family_name": "Dwek",
"given_name": "Eli",
"orcid": "0000-0001-8033-1181",
"clpid": "Dwek-E"
},
{
"family_name": "Staguhn",
"given_name": "Johannes G.",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
},
{
"family_name": "Arendt",
"given_name": "Richard G.",
"orcid": "0000-0001-8403-8548",
"clpid": "Arendt-R-G"
},
{
"family_name": "Capak",
"given_name": "Peter L.",
"orcid": "0000-0003-3578-6843",
"clpid": "Capak-P"
},
{
"family_name": "Kovacs",
"given_name": "Attila",
"clpid": "Kovacs-A"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Fixsen",
"given_name": "Dale",
"clpid": "Fixsen-D-J"
},
{
"family_name": "Karim",
"given_name": "Alexander",
"orcid": "0000-0002-8414-9579",
"clpid": "Karim-A"
},
{
"family_name": "Leclercq",
"given_name": "Samuel",
"clpid": "Leclercq-S"
},
{
"family_name": "Maher",
"given_name": "Stephen F.",
"clpid": "Maher-S-F"
},
{
"family_name": "Moseley",
"given_name": "Samuel H.",
"clpid": "Moseley-S-H"
},
{
"family_name": "Schinnerer",
"given_name": "Eva",
"orcid": "0000-0002-3933-7677",
"clpid": "Schinnerer-E"
},
{
"family_name": "Sharp",
"given_name": "Elmer H.",
"clpid": "Sharp-E-H"
}
],
"abstract": "Analyses of high-redshift ultraluminous infrared (IR) galaxies traditionally use the observed optical to submillimeter spectral energy distribution (SED) and estimates of the dynamical mass as observational constraints to derive the star formation rate (SFR), the stellar mass, and age of these objects. An important observational constraint neglected in the analysis is the mass of dust giving rise to the IR emission. In this paper we add this constraint to the analysis of AzTEC-3. Adopting an upper limit to the mass of stars and a bolometric luminosity for this object, we construct different stellar and chemical evolutionary scenarios, constrained to produce the inferred dust mass and observed luminosity before the associated stellar mass exceeds the observational limit. We use the P\u00c9GASE population synthesis code and a chemical evolution model to follow the evolution of the galaxy's SED and its stellar and dust masses as a function of galactic age for seven different stellar initial mass functions (IMFs). We find that the model with a Top Heavy IMF provided the most plausible scenario consistent with the observational constraints. In this scenario the dust formed over a period of ~200 Myr, with an SFR of ~500 M_\u2609 yr^(\u20131). These values for the age and SFR in AzTEC-3 are significantly higher and lower, respectively, from those derived without the dust mass constraint. However, this scenario is not unique, and others cannot be completely ruled out because of the prevailing uncertainties in the age of the galaxy, its bolometric luminosity, and its stellar and dust masses. A robust result of our models is that all scenarios require most of the radiating dust mass to have been accreted in molecular clouds. Our new procedure highlights the importance of a multiwavelength approach, and of the use of dust evolution models in constraining the age and the star formation activity and history in galaxies.",
"doi": "10.1088/0004-637X/738/1/36",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2011-09-01",
"series_number": "1",
"volume": "738",
"issue": "1",
"pages": "Art. No. 36"
},
{
"id": "authors:772nn-hy784",
"collection": "authors",
"collection_id": "772nn-hy784",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110712-133958408",
"type": "article",
"title": "The Spitzer-WISE Survey of the Ecliptic Poles",
"author": [
{
"family_name": "Jarrett",
"given_name": "T. H.",
"orcid": "0000-0002-4939-734X",
"clpid": "Jarrett-T-H"
},
{
"family_name": "Cohen",
"given_name": "M.",
"clpid": "Cohen-Martin"
},
{
"family_name": "Masci",
"given_name": "F.",
"orcid": "0000-0002-8532-9395",
"clpid": "Masci-F-J"
},
{
"family_name": "Wright",
"given_name": "E.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
},
{
"family_name": "Stern",
"given_name": "D.",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Blain",
"given_name": "A.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Carey",
"given_name": "S.",
"orcid": "0000-0002-0221-6871",
"clpid": "Carey-S-J"
},
{
"family_name": "Cutri",
"given_name": "R. M.",
"orcid": "0000-0002-0077-2305",
"clpid": "Cutri-R-M"
},
{
"family_name": "Eisenhardt",
"given_name": "P.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Lonsdale",
"given_name": "C.",
"orcid": "0000-0003-0898-406X",
"clpid": "Lonsdale-Carol-J"
},
{
"family_name": "Mainzer",
"given_name": "A.",
"clpid": "Mainzer-A-K"
},
{
"family_name": "Marsh",
"given_name": "K.",
"clpid": "Marsh-K"
},
{
"family_name": "Padgett",
"given_name": "D.",
"orcid": "0000-0001-5334-5107",
"clpid": "Padgett-D-L"
},
{
"family_name": "Petty",
"given_name": "S.",
"orcid": "0000-0003-0624-3276",
"clpid": "Petty-Sara-M"
},
{
"family_name": "Ressler",
"given_name": "M.",
"clpid": "Ressler-M"
},
{
"family_name": "Skrutskie",
"given_name": "M.",
"clpid": "Skrutskie-M-F"
},
{
"family_name": "Stanford",
"given_name": "S.",
"clpid": "Stanford-S-A"
},
{
"family_name": "Surace",
"given_name": "J.",
"orcid": "0000-0001-7291-0087",
"clpid": "Surace-J-A"
},
{
"family_name": "Tsai",
"given_name": "C. W.",
"orcid": "0000-0002-9390-9672",
"clpid": "Tsai-Chao-Wei"
},
{
"family_name": "Wheelock",
"given_name": "S.",
"clpid": "Wheelock-S"
},
{
"family_name": "Yan",
"given_name": "D. L.",
"clpid": "Yan-D-L"
}
],
"abstract": "We have carried out a survey of the north and south ecliptic poles, EP-N and EP-S, respectively, with the Spitzer Space Telescope and the Wide-field Infrared Survey Explorer (WISE). The primary objective was to cross-calibrate WISE with the Spitzer and Midcourse Space Experiment (MSX) photometric systems by developing a set of calibration stars that are common to these infrared missions. The ecliptic poles were continuous viewing zones for WISE due to its polar-crossing orbit, making these areas ideal for both absolute and internal calibrations. The Spitzer IRAC and MIPS imaging survey covers a complete area of 0.40 deg^2 for the EP-N and 1.28 deg^2 for the EP-S. WISE observed the whole sky in four mid-infrared bands, 3.4, 4.6, 12, and 22 \u03bcm, during its eight-month cryogenic mission, including several hundred ecliptic polar passages; here we report on the highest coverage depths achieved by WISE, an area of ~1.5 deg^2 for both poles. Located close to the center of the EP-N, the Sy-2 galaxy NGC 6552 conveniently functions as a standard calibrator to measure the red response of the 22 \u03bcm channel of WISE. Observations from Spitzer-IRAC/MIPS/IRS-LL and WISE show that the galaxy has a strong red color in the mid-infrared due to star-formation and the presence of an active galactic nucleus (AGN), while over a baseline >1 year the mid-IR photometry of NGC 6552 is shown to vary at a level less than 2%. Combining NGC 6552 with the standard calibrator stars, the achieved photometric accuracy of the WISE calibration, relative to the Spitzer and MSX systems, is 2.4%, 2.8%, 4.5%, and 5.7% for W1 (3.4 \u03bcm), W2 (4.6 \u03bcm), W3 (12 \u03bcm), and W4 (22 \u03bcm), respectively. The WISE photometry is internally stable to better than 0.1% over the cryogenic lifetime of the mission. The secondary objective of the Spitzer-WISE Survey was to explore the poles at greater flux-level depths, exploiting the higher angular resolution Spitzer observations and the exceptionally deep (in total coverage) WISE observations that potentially reach down to the confusion limit of the survey. The rich Spitzer and WISE data sets were used to study the Galactic and extragalactic populations through source counts, color-magnitude and color-color diagrams. As an example of what the data sets facilitate, we have separated stars from galaxies, delineated normal galaxies from power-law-dominated AGNs, and reported on the different fractions of extragalactic populations. In the EP-N, we find an AGN source density of ~260 deg^(\u20132) to a 12 \u03bcm depth of 115 \u03bcJy, representing 15% of the total extragalactic population to this depth, similar to what has been observed for low-luminosity AGNs in other fields.",
"doi": "10.1088/0004-637X/735/2/112",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2011-07-10",
"series_number": "2",
"volume": "735",
"issue": "2",
"pages": "Art. No. 112"
},
{
"id": "authors:my4sy-c1e04",
"collection": "authors",
"collection_id": "my4sy-c1e04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110728-134923707",
"type": "article",
"title": "CO(1-0) in z \u2273 4 Quasar Host Galaxies: No Evidence for Extended Molecular Gas Reservoirs",
"author": [
{
"family_name": "Riechers",
"given_name": "Dominik A.",
"orcid": "0000-0001-9585-1462",
"clpid": "Riechers-D-A"
},
{
"family_name": "Walter",
"given_name": "Fabian",
"orcid": "0000-0003-4793-7880",
"clpid": "Walter-F"
},
{
"family_name": "Carilli",
"given_name": "Christopher L.",
"orcid": "0000-0001-6647-3861",
"clpid": "Carilli-C-L"
},
{
"family_name": "Knudsen",
"given_name": "Kirsten K.",
"orcid": "0000-0002-7821-8873",
"clpid": "Knudsen-K-K"
},
{
"family_name": "Lo",
"given_name": "K. Y.",
"clpid": "Lo-K-Y"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Staguhn",
"given_name": "Johannes G.",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
},
{
"family_name": "Hunter",
"given_name": "Todd R.",
"orcid": "0000-0001-6492-0090",
"clpid": "Hunter-T-R"
},
{
"family_name": "Bertoldi",
"given_name": "Frank",
"orcid": "0000-0002-1707-1775",
"clpid": "Bertoldi-F"
},
{
"family_name": "Henkel",
"given_name": "Christian",
"clpid": "Henkel-Christian"
},
{
"family_name": "Menten",
"given_name": "Karl M.",
"orcid": "0000-0001-6459-0669",
"clpid": "Menten-K-M"
},
{
"family_name": "Weiss",
"given_name": "Axel",
"orcid": "0000-0003-4678-3939",
"clpid": "Weiss-Axel"
},
{
"family_name": "Yun",
"given_name": "Min S.",
"orcid": "0000-0001-7095-7543",
"clpid": "Yun-Min-S"
},
{
"family_name": "Scoville",
"given_name": "Nick Z.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
}
],
"abstract": "We present ^(12)CO(J = 1 \u2192 0) observations of the high-redshift quasi-stellar objects (QSOs) BR 1202-0725 (z = 4.69), PSS J2322+1944 (z = 4.12), and APM 08279+5255 (z = 3.91) using the NRAO Green Bank Telescope (GBT) and the MPIfR Effelsberg 100 m telescope. We detect, for the first time, the CO ground-level transition in BR 1202-0725. For PSS J2322+1944 and APM 08279+5255, our observations result in line fluxes that are consistent with previous NRAO Very Large Array (VLA) observations, but they reveal the full line profiles. We report a typical lensing-corrected velocity-integrated intrinsic ^(12)CO(J = 1 \u2192 0) line luminosity of L'_(CO) = 5 \u00d7 10^(10) K km s^(-1) pc^2 and a typical total H_2 mass of M(H_2) = 4 \u00d7 10^(10) M_\u2609 for the sources in our sample. The CO/FIR luminosity ratios of these high-z sources follow the same trend as seen for low-z galaxies, leading to a combined solution of log L_(FIR) = (1.39 \u00b1 0.05) log L_(CO) - 1.76. It has previously been suggested that the molecular gas reservoirs in some quasar host galaxies may exhibit luminous, extended ^(12)CO(J = 1 \u2192 0) components that are not observed in the higher J CO transitions. Using the line profiles and the total intensities of our observations and large velocity gradient (LVG) models based on previous results for higher J CO transitions, we derive that emission from all CO transitions is described well by a single gas component in which all molecular gas is concentrated in a compact nuclear region. Thus, our observations and models show no indication of a luminous extended, low surface brightness molecular gas component in any of the high-redshift QSOs in our sample. If such extended components exist, their contribution to the overall luminosity is limited to at most 30%.",
"doi": "10.1086/507014",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2006-10-20",
"series_number": "2",
"volume": "650",
"issue": "2",
"pages": "604-613"
},
{
"id": "authors:bnx7t-ddh18",
"collection": "authors",
"collection_id": "bnx7t-ddh18",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110216-102922057",
"type": "article",
"title": "350 \u03bcm dust emission from high-redshift quasars",
"author": [
{
"family_name": "Beelen",
"given_name": "Alexandre",
"clpid": "Beelen-A"
},
{
"family_name": "Cox",
"given_name": "Pierre",
"orcid": "0000-0003-2027-8221",
"clpid": "Cox-Pierre"
},
{
"family_name": "Benford",
"given_name": "Dominic J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Dowell",
"given_name": "C. Darren",
"clpid": "Dowell-C-D"
},
{
"family_name": "Kov\u00e1cs",
"given_name": "Attila",
"clpid": "Kov\u00e1cs-A"
},
{
"family_name": "Bertoldi",
"given_name": "Frank",
"orcid": "0000-0002-1707-1775",
"clpid": "Bertoldi-F"
},
{
"family_name": "Omont",
"given_name": "Alain",
"orcid": "0000-0002-4721-3922",
"clpid": "Omont-A"
},
{
"family_name": "Carilli",
"given_name": "Chris L.",
"orcid": "0000-0001-6647-3861",
"clpid": "Carilli-C-L"
}
],
"abstract": "We report detections of six high-redshift (1.8 \u2264 z \u2264 6.4), optically luminous, radio-quiet quasars at 350 \u03bcm, using the SHARC II bolometer camera at the Caltech Submillimeter Observatory. Our observations double the number of high-redshift quasars for which 350 \u03bcm photometry is available. By combining the 350 \u03bcm measurements with observations at other submillimeter/millimeter wavelengths, for each source we have determined the temperature of the emitting dust (ranging from 40 to 60 K) and the far-infrared luminosity [(0.6-2.2) \u00d7 10^(13) L\u2299]. The combined mean spectral energy distribution of all high-redshift quasars with two or more rest-frame far-infrared photometric measurements is best fit with a graybody with temperature of 47 \u00b1 3 K and a dust emissivity power-law spectral index of \u03b2 = 1.6 \u00b1 0.1. This warm dust component is a good tracer of the starburst activity of the quasar host galaxy. The ratio of the far-infrared to radio luminosities of infrared-luminous, radio-quiet high-redshift quasars is consistent with that found for local star-forming galaxies.",
"doi": "10.1086/500636",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2006-05-10",
"series_number": "2",
"volume": "642",
"issue": "2",
"pages": "694-701"
},
{
"id": "authors:j69ba-erj39",
"collection": "authors",
"collection_id": "j69ba-erj39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150114-152106998",
"type": "article",
"title": "The design and performance of the 384-element imaging submillimeter detector arrays for HAWC and SHARC II",
"author": [
{
"family_name": "Moseley",
"given_name": "S. H.",
"clpid": "Moseley-S-H"
},
{
"family_name": "Allen",
"given_name": "C. A.",
"clpid": "Allen-C-A"
},
{
"family_name": "Benford",
"given_name": "D.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Dowell",
"given_name": "C. D.",
"clpid": "Dowell-C-D"
},
{
"family_name": "Harper",
"given_name": "D. A.",
"clpid": "Harper-D-A"
},
{
"family_name": "Phillips",
"given_name": "T. G.",
"clpid": "Phillips-T-G"
},
{
"family_name": "Silverberg",
"given_name": "R. F.",
"clpid": "Silverberg-R-F"
},
{
"family_name": "Staguhn",
"given_name": "J.",
"orcid": "0000-0002-8437-0433",
"clpid": "Staguhn-J-G"
}
],
"abstract": "We report on the performance of the SHARC II detector, a 12\u00d732 array of ion implanted Si pop-up bolometers. This 384 element detector array was built as a prototype for the High Angular Resolution Widefield Camera for the Stratospheric Observatory for Infrared Astronomy. We will discuss the design process, the characterization of the detectors, and the performance of the array in the SHARC II instrument. SHARC II is now a facility instrument on the Caltech Submillimeter Observatory, providing background-limited imaging at 350 and 450 \u00b5m.",
"doi": "10.1016/j.nima.2003.11.349",
"issn": "0168-9002",
"publisher": "Elsevier",
"publication": "Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment",
"publication_date": "2004-03-11",
"series_number": "1-3",
"volume": "520",
"issue": "1-3",
"pages": "417-420"
},
{
"id": "authors:snwyh-dds35",
"collection": "authors",
"collection_id": "snwyh-dds35",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:SERao00",
"type": "article",
"title": "Dual Fabry-Perot filter for measurement of CO rotational spectra: design and application to the CO spectrum of Venus",
"author": [
{
"family_name": "Serabyn",
"given_name": "E.",
"clpid": "Serabyn-E"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Wu",
"given_name": "S.",
"clpid": "Wu-S"
},
{
"family_name": "Pardo",
"given_name": "J. R.",
"clpid": "Pardo-J-R"
}
],
"abstract": "We present the design of a harmonic resonant filter that can be used with a Fourier transform spectrometer (FTS) for simultaneous measurement of a series of lines in the CO rotational ladder. To enable studies of both broad CO absorptions in Venus and modestly red-shifted CO emission from external galaxies, relatively broad (approximately 10-30-GHz FWHM) transmission passbands are desirable. Because a single low-finesse Fabry Perot (FP) etalon has insufficient interline rejection, a dual-FP etalon was considered. Such a design provides significantly better interband rejection and somewhat more flattopped transmission spikes. A prototype filter of this type, made of two thin silicon disks spaced by an air gap, has been constructed and used with our FTS at the Caltech Submillimeter Observatory for simultaneous measurement of the four submillimeter CO transitions in the atmosphere of Venus that are accessible from the ground.",
"doi": "10.1364/AO.39.006448",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "2000-12-01",
"series_number": "34",
"volume": "39",
"issue": "34",
"pages": "6448-6452"
},
{
"id": "authors:pf8qg-mwv36",
"collection": "authors",
"collection_id": "pf8qg-mwv36",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-140130255",
"type": "article",
"title": "A Large Throughput High Resolution Fourier Transform Spectrometer for Submillimeter Applications",
"author": [
{
"family_name": "Bin",
"given_name": "M.",
"clpid": "Bin-Mei"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Gaidis",
"given_name": "M. C.",
"clpid": "Gaidis-M-C"
},
{
"family_name": "B\u00fcttgenbach",
"given_name": "T. H.",
"clpid": "B\u00fcttgenbach-T-H"
},
{
"family_name": "Zmuidzinas",
"given_name": "J.",
"orcid": "0000-0002-3330-5439",
"clpid": "Zmuidzinas-J"
},
{
"family_name": "Serabyn",
"given_name": "E.",
"clpid": "Serabyn-E"
},
{
"family_name": "Phillips",
"given_name": "T. G.",
"clpid": "Phillips-T-G"
}
],
"abstract": "We have designed and constructed a Fourier Transform Spectrometer (FTS) for the study of submillimeter-wave mixers and optical components. The FTS has a large aperture (up to 25.4 cm) and small focal ratio (as fast as f/2.5) to achieve a large throughput. It operates in the 100-3750 GHz (3.3-125 cm^(\u22121)) frequency range with a resolution of up to 75 MHz (0.0025 cm^(\u22121)). Here we discuss the design goals and provide a detailed description of the construction of the FTS. In addition, we highlight the variety of studies which have been conducted with this instrument, which include characterizing SIS mixers through both direct and heterodyne detection and measuring the properties of optical materials.",
"doi": "10.1023/A:1021709330349",
"issn": "0195-9271",
"publisher": "Springer",
"publication": "International Journal of Infrared and Millimeter Waves",
"publication_date": "1999-03",
"series_number": "3",
"volume": "20",
"issue": "3",
"pages": "383-400"
},
{
"id": "authors:n73ct-qa304",
"collection": "authors",
"collection_id": "n73ct-qa304",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170223-141455305",
"type": "article",
"title": "G34.24+0.13MM: A Deeply Embedded Proto\u2013B Star",
"author": [
{
"family_name": "Hunter",
"given_name": "T. R.",
"orcid": "0000-0001-6492-0090",
"clpid": "Hunter-T-R"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Matthews",
"given_name": "K.",
"clpid": "Matthews-K"
},
{
"family_name": "Lis",
"given_name": "D. C.",
"orcid": "0000-0002-0500-4700",
"clpid": "Lis-D-C"
},
{
"family_name": "Serabyn",
"given_name": "E.",
"clpid": "Serabyn-E"
},
{
"family_name": "Phillips",
"given_name": "T. G.",
"clpid": "Phillips-T-G"
}
],
"abstract": "By means of millimeter and submillimeter imaging, we have identified a massive protostellar object that coincides with a methanol maser and is not detectable in the continuum at centimeter wavelengths. Located 84\" (1.5 pc) southeast of the ultracompact H II (UCHII) region G34.26+0.15, the new object G34.24+0.13MM was discovered in a wide-field 350 \u03bcm continuum image obtained with the Submillimeter High Angular Resolution Camera (SHARC) at the Caltech Submillimeter Observatory (CSO). Interferometric imaging at 225.7 and 110.7 GHz continuum has determined more precisely the position and angular diameter (2\".0, or 7600 AU) of the object. No source was detected at that position in 1.2-3.7 \u03bcm imaging or 10 and 20 \u03bcm photometry. Our observations are consistent with a cool dust core with temperature ~50 K, total gas mass 100 M_\u2609, and total luminosity in the range of 1600-6300 L_\u2609. Considering the high luminosity and lack of compact radio continuum emission, we conclude that this core probably contains a deeply embedded proto-B star.",
"doi": "10.1086/311142",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "1998-02-01",
"series_number": "2",
"volume": "493",
"issue": "2",
"pages": "L97-L100"
},
{
"id": "authors:rtx14-j8t67",
"collection": "authors",
"collection_id": "rtx14-j8t67",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:WANao96",
"type": "article",
"title": "Characterization of a submillimeter high-angular-resolution camera with a monolithic silicon bolometer array for the Caltech Submillimeter Observatory",
"author": [
{
"family_name": "Wang",
"given_name": "Nina",
"clpid": "Wang-Nina"
},
{
"family_name": "Hunter",
"given_name": "T. R.",
"orcid": "0000-0001-6492-0090",
"clpid": "Hunter-T-R"
},
{
"family_name": "Benford",
"given_name": "D. J.",
"orcid": "0000-0002-9884-4206",
"clpid": "Benford-D-J"
},
{
"family_name": "Serabyn",
"given_name": "E.",
"clpid": "Serabyn-E"
},
{
"family_name": "Lis",
"given_name": "D. C.",
"orcid": "0000-0002-0500-4700",
"clpid": "Lis-D-C"
},
{
"family_name": "Phillips",
"given_name": "T. G.",
"clpid": "Phillips-T-G"
},
{
"family_name": "Moseley",
"given_name": "S. H.",
"clpid": "Moseley-S-H"
},
{
"family_name": "Bpyce",
"given_name": "K.",
"clpid": "Boyce-K"
},
{
"family_name": "Szymkowiak",
"given_name": "A.",
"clpid": "Szymkowiak-A"
},
{
"family_name": "Allen",
"given_name": "C.",
"clpid": "Allen-C"
},
{
"family_name": "Mott",
"given_name": "B.",
"clpid": "Mott-B"
},
{
"family_name": "Gygax",
"given_name": "J.",
"clpid": "Gygax-J"
}
],
"abstract": "We constructed a 24-pixel bolometer camera operating in the 350- and 450-\u00b5m atmospheric windows for the Caltech Submillimeter Observatory (CSO). This instrument uses a monolithic silicon bolometer array that is cooled to approximately 300 mK by a single-shot 3 He refrigerator. First-stage amplification is provided by field-effect transistors at approximately 130 K. The sky is imaged onto the bolometer array by means of several mirrors outside the Dewar and a cold off-axis elliptical mirror inside the cryostat. The beam is defined by cold aperture and field stops, which eliminates the need for any condensing horns. We describe the instrument, present measurements of the physical properties of the bolometer array, describe the performance of the electronics and the data-acquisition system, and demonstrate the sensitivity of the instrument operating at the observatory. Approximate detector noise at 350 \u00b5m is 5 x 10^-15 W/\u221aHz, referenced to the entrance of the Dewar, and the CSO system noise-equivalent flux density is approximately 4 Jy/\u221aHz. These values are within a factor of 2.5 of the background limit.",
"doi": "10.1364/AO.35.006629",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "1996-12-01",
"series_number": "34",
"volume": "35",
"issue": "34",
"pages": "6629-6640"
}
]