[ { "id": "authors:ybfrc-xt968", "collection": "authors", "collection_id": "ybfrc-xt968", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-091050517", "type": "book_section", "title": "Cosmic Evolution of a Sample of Infrared Luminous Galaxies", "book_title": "Sky surveys: protostars to protogalaxies: proceedings of a Conference in Honor of Gerry Neugebauer", "author": [ { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Barrientos", "given_name": "L. F.", "clpid": "Barrientos-L-F" }, { "family_name": "Hacking", "given_name": "P.", "clpid": "Hacking-P-B" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" } ], "contributor": [ { "family_name": "Soifer", "given_name": "Baruch T.", "clpid": "Soifer-B-T" } ], "abstract": "A sample of faint, southern-hemisphere 60 \u03bcm sources\n(f_(60) > 100mJy) detected as part of the IRAS Additional Observations has been used, in conjunction with CCD imaging, to produce a list of faint infrared galaxies. Redshifts of this sample of galaxies can be compared\nwith model predictions for several evolutionary scenarios; the comparisons show an excess of galaxies at higher redshifts (z > 0.1) compared with the predictions of models which assume no evolution of the infrared-galaxy luminosity function.", "isbn": "0-937707-62-7", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1993-01", "pages": "111-114" }, { "id": "authors:e2xse-ws114", "collection": "authors", "collection_id": "e2xse-ws114", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150107-122328736", "type": "article", "title": "Ground-Based Near-Infrared Imaging Observations of Venus During the Galileo Encounter", "author": [ { "family_name": "Crisp", "given_name": "D.", "orcid": "0000-0002-4573-9998", "clpid": "Crisp-D" }, { "family_name": "McMuldroch", "given_name": "S.", "clpid": "McMuldroch-S" }, { "family_name": "Stephens", "given_name": "S. K.", "clpid": "Stephens-S-K" }, { "family_name": "Sinton", "given_name": "W. M.", "clpid": "Sinton-W-M" }, { "family_name": "Ragent", "given_name": "B.", "clpid": "Ragent-B" }, { "family_name": "Hodapp", "given_name": "K. W.", "orcid": "0000-0003-0786-2140", "clpid": "Hodapp-K-W" }, { "family_name": "Probst", "given_name": "R. G.", "clpid": "Probst-R-G" }, { "family_name": "Doyle", "given_name": "L. R.", "clpid": "Doyle-L-R" }, { "family_name": "Allen", "given_name": "D. A.", "clpid": "Allen-D-A" }, { "family_name": "Elias", "given_name": "J.", "clpid": "Elias-J-H" } ], "abstract": "Near-infrared images of Venus, obtained from a global network of ground-based observatories during January and February 1990, document the morphology and motions of the night-side near-infrared markings before, during, and after the Galileo Venus encounter. A dark cloud extended halfway around the planet at low latitudes (>\u00b140\u00b0) and persisted throughout the observing program. It had a rotation period of 5.5 \u00b1 0.15 days. The remainder of this latitude band was characterized by small-scale (400 to 1000 kilometers) dark and bright markings with rotation periods of 7.4 \u00b1 1 days. The different rotation periods for the large dark cloud and the smaller markings suggests that they are produced at different altitudes. Mid-latitudes (\u00b140\u00b0 to 60\u00b0) were usually occupied by bright east-west bands. The highest observable latitudes (\u00b160\u00b0 to 70\u00b0) were always dark and featureless, indicating greater cloud opacity. Maps of the water vapor distribution show no evidence for large horizontal gradients in the lower atmosphere of Venus.", "doi": "10.1126/science.253.5027.1538", "issn": "0036-8075", "publisher": "American Association for the Advancement of Science", "publication": "Science", "publication_date": "1991-09-27", "series_number": "5027", "volume": "253", "issue": "5027", "pages": "1538-1541" }, { "id": "authors:vd8f3-vtd08", "collection": "authors", "collection_id": "vd8f3-vtd08", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170920-104648151", "type": "article", "title": "Carbon stars at high Galactic latitude", "author": [ { "family_name": "Bothun", "given_name": "Greg", "clpid": "Bothun-G" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "MacAlpine", "given_name": "G.", "clpid": "MacAlpine-G" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Mould", "given_name": "J. R.", "orcid": "0000-0003-3820-1740", "clpid": "Mould-J-R" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Reid", "given_name": "I. N.", "clpid": "Reid-I-N" } ], "abstract": "Photometry and kinematics are presented for a sample of objective prism selected carbon stars towards the north and south Galactic poles. Distances are determined by fitting the infrared colors to a giant branch. If these stars are like the carbon stars seen in dwarf spheroidal galaxies, the median distance of the sample is 28 kpc. If they are more like the carbon stars found recently in the Galactic bulge, they may be only half as distant. The surface density of carbon stars as a function of distance is remarkably consistent with an R^(1/4) density profile for the Galactic halo. This density profile can be traced to \u2248 15 scale radii and fills a volume similar to that occupied by globular clusters. The data yield an effective\nradius of either 7.0 or 3.5 kpc depending on choice of distance scale. The velocity dispersion of the sample is 96 + 12 km/s. A kinematic model in which vertical velocity dispersion is independent of height above the Galactic plane seems in best accord with the data.", "doi": "10.1086/115844", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1991-06", "series_number": "6", "volume": "101", "issue": "6", "pages": "2220-2228" }, { "id": "authors:gxnbq-by374", "collection": "authors", "collection_id": "gxnbq-by374", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-101536812", "type": "article", "title": "The near-infrared variability of a sample of optically selected quasars", "author": [ { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" } ], "abstract": "A complete sample of 108 optically selected quasars, the Palomar-Green quasars, has been studied at near-infrared wavelengths over an average time base of about 6 yr; in some cases the time base extends to 20 yr. The measurements show that about half the quasars have a high probability of having varied, but that half show little evidence of variability, in sharp contrast to published studies indicating that most quasars vary on comparable timescales at optical wavelengths. The maximum amplitude of variation is less than 1 mag and generally near 0.5 mag. During variations, the near-infrared colors are\nalmost constant. The more luminous quasars show a smaller mean probability of having varied in the time frame of the study than the less-luminous quasars. The majority of the quasars with flat radio spectra have a high probability of having varied. Among those quasars that have a high probability of having varied, the rate is fairly independent of the time interval between the observations after the first year. The quasar 3C 273 shows definite variations at 10.1 \u00b5m which preclude the emission being\nthermal emission from heated dust grains for that quasar. The observations of the other quasars cannot be used to differentiate uniquely between thermal and nonthermal emission mechanisms.", "doi": "10.1086/115040", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1989-04", "series_number": "4", "volume": "97", "issue": "4", "pages": "957-977" }, { "id": "authors:5ekjh-vss11", "collection": "authors", "collection_id": "5ekjh-vss11", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-135109214", "type": "article", "title": "Multifrequency observation of the optically violent variable quasar 3C 446", "author": [ { "family_name": "Bregman", "given_name": "J. N.", "clpid": "Bregman-J-N" }, { "family_name": "Glassgold", "given_name": "A. E.", "clpid": "Glassgold-A-E" }, { "family_name": "Huggins", "given_name": "P. J.", "clpid": "Huggins-P-J" }, { "family_name": "Kinney", "given_name": "A. L.", "clpid": "Kinney-A-L" }, { "family_name": "McHardy", "given_name": "I.", "clpid": "McHardy-I-M" }, { "family_name": "Webb", "given_name": "J. R.", "clpid": "Webb-J-R" }, { "family_name": "Pollock", "given_name": "J. T.", "clpid": "Pollock-J-T" }, { "family_name": "Leacock", "given_name": "R. J.", "clpid": "Leacock-R-J" }, { "family_name": "Smith", "given_name": "A. G.", "clpid": "Smith-A-G" }, { "family_name": "Pica", "given_name": "A. J.", "clpid": "Pica-A-J" }, { "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": "Hodge", "given_name": "P. E.", "clpid": "Hodge-P-E" }, { "family_name": "Miller", "given_name": "J. S.", "clpid": "Miller-J-S" }, { "family_name": "Stephens", "given_name": "S. A.", "clpid": "Stephens-S-A" }, { "family_name": "Dent", "given_name": "W. A.", "clpid": "Dent-W-A" }, { "family_name": "Balonek", "given_name": "T. J.", "clpid": "Balonek-T-J" }, { "family_name": "Barvainis", "given_name": "R.", "clpid": "Barvainis-R" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Impey", "given_name": "C. D.", "clpid": "Impey-C-D" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Wisniewski", "given_name": "W. Z.", "clpid": "Wisniewski-W-Z" } ], "abstract": "Extensive optical and radio monitoring data and seven multifrequency spectra were obtained of the violently\nvariable quasar 3C 446. The monitoring data suggest a correlation between the radio and optical outbursts,\nwith the optical flare preceding the radio activity by 400-600 days. A difference in the statistical behavior of the optical and radio variability indicates that considerable processing occurs to the optical emitting plasma before it becomes radio emitting plasma. Within the radio band, outbursts proceed from high to low frequencies. An outburst in 1983 showed greater and more rapid variation in the optical than in the near-IR region. The 10-100 \u03bcm fluxes did not follow the higher frequency variation, suggesting a time delay between these spectral domains. During another time, the X-ray emission varied on a time scale of days and more rapidly than the UV or optical emission. On a time scale of weeks-months, the X-ray fluxes are well correlated with the UV-IR fluxes but not with the radio fluxes. The multifrequency data show that the flat radio spectrum turns over at 3-10 x 10^(11) Hz and the continuum steepens with frequency; \u0251(IR) = 1.1, \u0251(opt-UV) = -2 to -3. The X-ray emission lies an order of magnitude above an extrapolation of the optical-UV spectrum and has a harder spectrum. The power is primarily\nconcentrated in the submillimeter and infrared region. When the source is faint, a blue bump may be present. The flux in the Lycx line is proportional to the UV continuum flux density when the source is bright but is independent of the continuum level when the source is faint. The data suggest that the X-rays are produced by the inverse Compton process from an emitting region (10^(16) cm) smaller than but related to the synchrotron emitting UV-IR region. The characteristic size of the emitting region increases with decreasing frequency from 10^(16) (X-ray region) to 1-3 x 10^(17) cm (far IR-submillimeter region) to 10^(19)-10^(20) cm (radio region). Plasma conditions are best constrained at the frequency when the source becomes transparent, the far IR-submillimeter band, where B \u2248 3-100 G, n \u2248 40-100 cm^(-3); and the Doppler boosting factor \u03b4 \u2248 1-5.", "doi": "10.1086/166596", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1988-08-15", "series_number": "1", "volume": "331", "issue": "1", "pages": "746-763" }, { "id": "authors:p8ff1-w3e84", "collection": "authors", "collection_id": "p8ff1-w3e84", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-101508395", "type": "article", "title": "Warm ultraluminous galaxies in the IRAS survey - The transition from galaxy to quasar?", "author": [ { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" } ], "abstract": "Of 90 extragalactic objects chosen from the IRAS catalog on the basis of brightness at 60 mum and \"warm\" infrared color [f_ \u03bd(25 \u00b5m)/f_ \u03bd(60 \u00b5m) >0.2], 12 have luminosities characteristic of quasars. These 12 ultraluminous objects have Seyfert spectra, and nine of them show morphological evidence for recent collisions or mergers - they plausibly represent a transition stage between cooler ultraluminous infrared galaxies and optical quasars.", "doi": "10.1086/185155", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1988-05-15", "series_number": "2", "volume": "328", "issue": "2", "pages": "L35-L39" }, { "id": "authors:y75ns-1kt12", "collection": "authors", "collection_id": "y75ns-1kt12", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-103148522", "type": "article", "title": "Ultraluminous infrared galaxies and the origin of quasars", "author": [ { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Madore", "given_name": "B. F.", "orcid": "0000-0002-1576-1676", "clpid": "Madore-B-F" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" } ], "abstract": "An evolutionary connection between ultraluminous infrared galaxies and quasars is deduced from the observations\nof all 10 infrared galaxies with luminosities L(8-1000 \u03bcm) \u2265 10^(12) L\u2299, taken from a flux-limited sample of infrared bright galaxies. Images of the infrared galaxies show that nearly all are strongly interacting merger systems with exceptionally luminous nuclei. Millimeter-wave CO observations show that these objects typically contain 0.5-2 x 10^(10) M\u2299 of H_2. Optical spectra indicate a mixture of starburst and active galactic nucleus (AGN) energy sources, both of which are apparently fueled by the tremendous reservoir of molecular gas. It is proposed that these ultraluminous infrared galaxies represent the initial, dust-enshrouded stages of quasars. Once these nuclei shed their obscuring dust, allowing the AGN to visually dominate the decaying starburst, they become optically selected quasars. The origin of quasars through the merger of molecular gas-rich spiral galaxies can account for both the increased number of high-luminosity quasars at large redshift, when the universe was smaller and gas supplies less depleted, and the observed \"redshift-cutoff\" of quasars which represents the epoch after galaxy formation when the first collisions occur.", "doi": "10.1086/165983", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1988-02-01", "series_number": "1", "volume": "325", "issue": "1", "pages": "74-91" }, { "id": "authors:xrp5s-21z43", "collection": "authors", "collection_id": "xrp5s-21z43", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-124104509", "type": "article", "title": "The IRAS Bright Galaxy Sample. III. 1-10 \u00b5m observations and coadded IRAS data for galaxies with L_(IR) \u2a7e 10^(11) L\u2299", "author": [ { "family_name": "Carico", "given_name": "David P.", "clpid": "Carico-D-P" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" } ], "abstract": "Galaxies from the IRAS Bright Galaxy Sample with infrared luminosities L_(IR) \u2a7e 10^(11) L\u2299 have been measured at 1.3, 1.6, 2.2, 3.7, and 10 \u00b5m. In addition, coadded IRAS measurements at all four IRAS bands have been obtained. It is found that an increase in the total infrared luminosity above L_(IR) \u2a7e 10^(11) L\u2299 is correlated with increased emission from hot dust with characteristic temperatures\n~800 K contributing a substantial fraction of the 2.2 and 3.7 \u00b5m emission. This hot dust emission appears to \"turn on\" at luminosities of roughly 10^(11) L\u2299. The far-infrared emission cannot be modeled with a single dust temperature, but requires a cold (T~30-50 K) component coupled with a warmer (T\u227370 K) component. Although the relative contribution from the cold component decreases with\nincreasing luminosity, the temperature of the warmer component is independent of luminosity. The f_v (12 \u00b5m)/f_v (25 \u00b5m) ratios for the galaxies in this sample are small compared with other extragalactic objects, indicating that the radiation at 12 and 25 \u00b5m is dominated by emission from large dust grains radiating at high temperatures, rather than PAHs. The spatial distribution of the 10 \u00b5m emission\nindicates a substantial extended component for most of the galaxies in this sample, implying that star-formation\nprocesses contribute significantly to the luminosities. However, one-third of the galaxies have exponential scale sizes characteristic of compact sources, and half of the galaxies have 10 \u00b5m emission consistent with a contribution of 50% or more from a central point source.", "doi": "10.1086/114640", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1988-02", "series_number": "2", "volume": "95", "issue": "2", "pages": "356-373" }, { "id": "authors:kv5j3-92f08", "collection": "authors", "collection_id": "kv5j3-92f08", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-135108191", "type": "article", "title": "The IRAS bright galaxy sample. II - The sample and luminosity function", "author": [ { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Madore", "given_name": "B. F.", "orcid": "0000-0002-1576-1676", "clpid": "Madore-B-F" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Danielson", "given_name": "G. E.", "clpid": "Danielson-G-E" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Lonsdale", "given_name": "Carol J.", "orcid": "0000-0003-0898-406X", "clpid": "Lonsdale-C-J" }, { "family_name": "Rice", "given_name": "W. L.", "clpid": "Rice-W-L" } ], "abstract": "A complete sample of 324 extragalactic objects with 60 \u03bcm flux densities greater than 5.4 Jy has been selected from the IRAS catalogs. Only one of these objects can be classified morphologically as a Seyfert nucleus; the others are all galaxies. The median distance of the galaxies in the sample is ~ 30 Mpc, and the median luminosity vL,(60 \u03bcm) is ~ 2 x 10^(10) L_\u2609 . This infrared selected sample is much more \"infrared active\" than optically selected galaxy samples. The range in far-infrared luminosities of the galaxies in the sample is 10^8 L_\u2609 -2 x 10^(12) L_\u2609 The far-infrared luminosities of the sample galaxies appear to be independent of the optical luminosities, suggesting a separate luminosity component. As previously found, a correlation exists between 60 \u03bcm/100 \u03bcm flux density ratio and\nfar-infrared luminosity. The mass of interstellar dust required to produce the far-infrared radiation corresponds to a mass of gas of 108-10^(10) M_\u2609 for normal gas to dust ratios. This is comparable to the mass of the interstellar medium in most galaxies. The infrared luminous galaxies are found to be an important component of extraglactic objects, being the\nmost numerous objects in the local universe at luminosities L > 10^(11) L_\u2609, and producing a luminosity density of ~ that of the observed starlight in normal galaxies. Approximately 60%-80% of the far-infrared luminosity of the local universe is likely attributed to recent or ongoing star formation. If the infrared active phase (L_(FIR) > 10^(11) L_\u2609 ) is a nonrecurring event of duration less than 108 yr in galaxy evolution, then more than\n 10%, and perhaps all of the galaxies with blue luminosities greater than 10^(10) L_\u2609 must undergo such an event.", "doi": "10.1086/165536", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1987-09-01", "series_number": "1", "volume": "320", "issue": "1", "pages": "238-257" }, { "id": "authors:vwg2p-21g64", "collection": "authors", "collection_id": "vwg2p-21g64", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-140308167", "type": "book_section", "title": "Near-infrared observations of IRAS minisurvey galaxies", "author": [ { "family_name": "Carico", "given_name": "David P.", "clpid": "Carico-D-P" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Beichman", "given_name": "C.", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Persson", "given_name": "C. J.", "clpid": "Persson-C-J" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" } ], "contributor": [ { "family_name": "Persson", "given_name": "Carol J. Lonsdale", "clpid": "Persson-C-J-L" } ], "abstract": "Near infrared photometry at J, H, and K was obtained for 82 galaxies from the IRAS minisurvey. The near infrared colors of these galaxies cover a larger range in J-H and H-K than do normal field spiral galaxies, and evidence is presented of a tighter correlation between the near and far infrared emission in far infrared bright galaxies than exists between the far infrared and the visible emission. These results suggest the presence of dust in the far infrared bright galaxies, with hot dust emission contributing to the 2.2 \u00b5m emission, and extinction by dust affecting both the near infrared colors and the visible luminosities. In addition, there is some indication that the infrared emission in many of the minisurvey galaxies is coming from a strong nuclear component.", "publisher": "NASA", "publication_date": "1987-05" }, { "id": "authors:vcgq5-5ws60", "collection": "authors", "collection_id": "vcgq5-5ws60", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-143909957", "type": "book_section", "title": "Ultraluminous infrared galaxies", "author": [ { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Madore", "given_name": "B. F.", "orcid": "0000-0002-1576-1676", "clpid": "Madore-B-F" }, { "family_name": "Danielson", "given_name": "G. E.", "clpid": "Danielson-G-E" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Persson", "given_name": "C. J.", "clpid": "Persson-C-J" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" } ], "contributor": [ { "family_name": "Persson", "given_name": "Carol J. Lonsdale", "clpid": "Persson-C-J-L" } ], "abstract": "The IRAS survey of the local universe (z\u227e0.1) has revealed the existence of a class of ultraluminous infrared galaxies with L(8-1000\u03bcm) > 10^(12)L\u2299 that are slightly more numerous, and as luminous as optically selected quasars at similar redshift. Optical CCD images of these infrared galaxies show that nearly all are advanced mergers. Millimeter-wave CO (1 \u2192 0) observations indicate that these interacting systems are extremely rich in molecular gas with total H_2 masses 1-3 x 10^(10) M\u2299. Nearly all of the ultraluminous infrared galaxies show some evidence in their optical spectra for nonthermal nuclear activity. It is proposed that their infrared luminosity is powered by an embedded active nucleus and a nuclear starburst both of which are fueled by the tremendous reservoir of molecular gas. Once these merger nuclei shed their obscuring dust, allowing the AGN to visually dominate the decaying starburst, they become the optically selected quasars.", "publisher": "NASA", "publication_date": "1987-05" }, { "id": "authors:5xb5a-ve920", "collection": "authors", "collection_id": "5xb5a-ve920", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170301-145735902", "type": "article", "title": "High-spatial-resolution, near-infrared observations of ARP 220", "author": [ { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Elias", "given_name": "J.", "clpid": "Elias-J-H" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "McGill", "given_name": "J.", "clpid": "McGill-J" }, { "family_name": "Scoville", "given_name": "N.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" } ], "abstract": "High-spatial-resolution slit scans of the nucleus of Arp 220 are presented along with near-infrared photometry of the nuclear region. A single nucleus is found coincident with the strongest radio peak. The core is resolved to be on the order of 1\" (370 pc) in diameter. The photometry of the central region shows a minimum near 3.7 \u00b5m which is inconsistent with the near-infrared source being a \"classical\" nonthermal source, such as 3C 273, embedded in a dust cloud.", "doi": "10.1086/114389", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1987-05", "series_number": "5", "volume": "93", "issue": "5", "pages": "1057-1061" }, { "id": "authors:1dfgp-mw987", "collection": "authors", "collection_id": "1dfgp-mw987", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170306-084047427", "type": "article", "title": "Near-infrared observations of IRAS minisurvey galaxies", "author": [ { "family_name": "Carico", "given_name": "D. P.", "clpid": "Carico-D-P" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Beichman", "given_name": "C.", "orcid": "0000-0002-5627-5471", "clpid": "Beichman-C-A" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" } ], "abstract": "Near-infrared photometry at J, H, and K has been obtained for 82 galaxies from the IRAS minisurvey, a sample of infrared-selected galaxies. The near-infrared colors of these galaxies are similar to those of normal field spiral galaxies, but cover a larger range in J \u2014 H and H \u2014 K. There is evidence of a tighter correlation between the near- and far-infrared emission than exists between the far-infrared and the visible emission. These results suggest that hot-dust emission contributes to the 2.2 \u00b5m luminosity, and extinction by dust affects both the near-infrared colors and the visible luminosities. In addition, there is an indication that the far-infrared emission in many of the minisurvey galaxies is coming from a strong nuclear component.", "doi": "10.1086/114259", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1986-12", "series_number": "6", "volume": "92", "issue": "6", "pages": "1254-1261" }, { "id": "authors:21x5f-jsb72", "collection": "authors", "collection_id": "21x5f-jsb72", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170306-105407727", "type": "article", "title": "Infrared photometry of the nebulosity around quasars", "author": [ { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" } ], "abstract": "Measurements of the nebulosity around quasars have been carried out in the near-infrared. The colors of the host galaxies found in these observations are consistent with those of normal galaxies. The luminosities are also similar to those of normal galaxies but are slightly brighter than average.", "doi": "10.1086/163606", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1985-11-01", "volume": "298", "pages": "275-280" }, { "id": "authors:gdw23-nwe97", "collection": "authors", "collection_id": "gdw23-nwe97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170320-161626343", "type": "article", "title": "Type I supernovae in the infrared and their use as distance indicators", "author": [ { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" } ], "abstract": "New infrared data for 11 Type I supernovae are presented. These results, when combined with other published data for Type I supernovae, show that the light curves fall into two well-defined groups. The first more common type - Type Ia - shows strong, variable, unexplained absorption at 1.2 \u03bcm and probably at 3.5 \u03bcm, while the second type - Type Ib - shows no such absorption and a slower decline after maximum. The light curves of the Type Ia supernovae appear to have a dispersion in color and absolute magnitude of \u00b10.2 mag or less, making them potentially valuable for distance determination within the Local Supercluster.", "doi": "10.1086/163456", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1985-09-15", "volume": "296", "pages": "379-389" }, { "id": "authors:9s9pm-k3w58", "collection": "authors", "collection_id": "9s9pm-k3w58", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170306-084047122", "type": "article", "title": "A 2.2-\u00b5m search for variable galactic plane radio sources", "author": [ { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Matthews", "given_name": "K.", "clpid": "Matthews-K" } ], "abstract": "A search for infrared counterparts of some of the variable galactic plane radio sources identified by Gregory and Taylor has yielded two detections. Of these, one is of the star LSI + 61\u00b0303, already identified by Gregory et al. as the counterpart of GT 0236 + 610, while the other, GT 2100 + 468, appears to be a heavily obscured object which may be either galactic or extragalactic.", "doi": "10.1086/113825", "issn": "0004-6256", "publisher": "American Astronomical Society", "publication": "Astronomical Journal", "publication_date": "1985-07", "series_number": "7", "volume": "90", "issue": "7", "pages": "1188-1190" }, { "id": "authors:kfe5k-8qy61", "collection": "authors", "collection_id": "kfe5k-8qy61", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190531-091631781", "type": "article", "title": "Bolometric luminosities and infrared properties of carbon stars in the Magellanic Clouds and the Galaxy", "author": [ { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Frogel", "given_name": "Jay A.", "clpid": "Frogel-J-A" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" }, { "family_name": "Elias", "given_name": "Jonathan H.", "clpid": "Elias-J-H" } ], "abstract": "Broad band J, H, K photometry and narrow band CO and H_2O indices have been obtained for 89 luminous red stars in the Large Magellanic Cloud (LMC) and 21 in the Small Magellanic Cloud (SMC), chosen largely from the sample of Blanco, McCarthy, and Blanco. Most are known to be carbon stars, and their infrared properties are compared with new observations of 33 galactic carbon stars. The bolometric luminosity distributions of an unbiased sample of Magellanic Cloud carbon stars are compared with those predicted from evolutionary calculations by Renzini and Voli for double shell burning stars undergoing He shell flashes. The observed and theoretical distributions disagree markedly: nearly all the observed stars have lower luminosities than even the faintest\ntheoretical carbon star. \n\nIn addition, we find many fewer than expected high luminosity stars with initial mass greater than 3 M_\u2299. Possible explanations for this include a steep initial mass function for intermediate mass stars, a star formation rate significantly higher in the past than at present, or a neglected physical effect, such as underestimation of the importance of mass loss. Nevertheless, it appears that the hypothesis that He shell flashes lead to a dredge-up of carbon into the envelope, which results in a carbon star, can be maintained, if dredging occurs after fewer shell flashes than are predicted by presently available stellar evolutionary calculations. \n\nThe colors and indices of the late M giants in the LMC field are similar to those of late M giants in the Galaxy. \n\nThe narrow band infrared data are interpreted qualitatively in terms of the effects of molecular band absorption, which also strongly influences the infrared broad band colors of carbon stars. The small differences in the color-color relationships of the SMC and LMC samples are consistent with the differences in heavy metal abundance between the LMC, SMC, and Galaxy.", "doi": "10.1086/159308", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1981-10-15", "volume": "249", "pages": "481-503" }, { "id": "authors:y3nkg-9yh57", "collection": "authors", "collection_id": "y3nkg-9yh57", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190529-161904668", "type": "book_section", "title": "Observed Bolometric Luminosities of Carbon Stars", "book_title": "Physical Processes in Red Giants", "author": [ { "family_name": "Frogel", "given_name": "Jay A.", "clpid": "Frogel-J-A" }, { "family_name": "Cohen", "given_name": "Judith G.", "orcid": "0000-0002-8039-4673", "clpid": "Cohen-J-G" }, { "family_name": "Persson", "given_name": "S. E.", "clpid": "Persson-S-E" }, { "family_name": "Elias", "given_name": "Jonathan H.", "clpid": "Elias-J-H" } ], "contributor": [ { "family_name": "Iben", "given_name": "Icko, Jr.", "clpid": "Iben-I-Jr" }, { "family_name": "Renzini", "given_name": "Alvio", "clpid": "Renzini-A" } ], "abstract": "To the best of our knowledge, most carbon stars are cool stars on their second ascent of the giant branch, i.e. the asymptotic giant branch. By some means they have mixed nuclear processed, carbon enriched material to their surfaces and probably have luminosities that are greater than those that mark the termination point of first time evolution up the giant branch, i.e. the location of the core helium flash. Observational and theoretical evidence for this picture may be found in Iben and Truran (1978), Renzini and Voli (1980), Scalo (1976), Richer, Olander and Westerlund (1979), and earlier references these authors cite.", "doi": "10.1007/978-94-009-8492-9_15", "isbn": "9789400984943", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication_date": "1981", "pages": "159-164" }, { "id": "authors:g92a9-yew70", "collection": "authors", "collection_id": "g92a9-yew70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170303-153446123", "type": "article", "title": "Far-infrared observations of IRC + 10216", "author": [ { "family_name": "Campbell", "given_name": "M. P.", "clpid": "Campbell-M-P" }, { "family_name": "Harvey", "given_name": "P. M.", "clpid": "Harvey-P-M" }, { "family_name": "Hoffmann", "given_name": "W. F.", "clpid": "Hoffmann-W-F" }, { "family_name": "Elias", "given_name": "J. H.", "clpid": "Elias-J-H" }, { "family_name": "Neugebauer", "given_name": "G.", "clpid": "Neugebauer-G" }, { "family_name": "Gezari", "given_name": "D. Y.", "clpid": "Gezari-D-Y" }, { "family_name": "Westbrook", "given_name": "W. E.", "clpid": "Westbrook-W-E" }, { "family_name": "Hudson", "given_name": "H. S.", "orcid": "0000-0001-5685-1283", "clpid": "Hudson-H-S" }, { "family_name": "Soifer", "given_name": "B. T.", "orcid": "0000-0002-8112-1132", "clpid": "Soifer-B-T" }, { "family_name": "Werner", "given_name": "M. W.", "clpid": "Werner-M-W" } ], "abstract": "Broad-band photometric observations of IRC + 10216 in five wavelength intervals from 50 to 1000 \u03bc are reported. The observed radiation is interpreted as thermal emission from dust in the extended molecular cloud heated by the compact 2-20 \u03bc source as the core of the cloud. The shape of the 50-1000 \u03bc spectrum suggests that the emissivity of the dust particles varies approximately as \u03bb^(-1) over this spectral interval. The mass of dust inferred from the far-infrared emission is comparable with the mass of heavy molecules in the cloud.", "doi": "10.1086/154619", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "1976-09-01", "series_number": "1", "volume": "208", "issue": "1", "pages": "396-398" } ]