Multi-wavelength SEDs of Herschel-selected Galaxies in the COSMOS Field
Abstract
We combine Herschel Photodetector Array Camera and Spectrometer and Spectral and Photometric Imaging Receiver maps of the full 2 deg^2 Cosmic Evolution Survey (COSMOS) field with existing multi-wavelength data to obtain template and model-independent optical-to-far-infrared spectral energy distributions (SEDs) for 4218 Herschel-selected sources with log(L_(IR)/L_☉) = 9.4-13.6 and z = 0.02-3.54. Median SEDs are created by binning the optical to far-infrared (FIR) bands available in COSMOS as a function of infrared luminosity. Herschel probes rest-frame wavelengths where the bulk of the infrared radiation is emitted, allowing us to more accurately determine fundamental dust properties of our sample of infrared luminous galaxies. We find that the SED peak wavelength (λpeak) decreases and the dust mass (M_(dust)) increases with increasing total infrared luminosity (L_(IR)). In the lowest infrared luminosity galaxies (log(L_(IR)/L_☉) = 10.0-11.5), we see evidence of polycyclic aromatic hydrocarbon (PAH) features (λ ~ 7-9 μm), while in the highest infrared luminosity galaxies (L_(IR) > 10^(12) L_☉) we see an increasing contribution of hot dust and/or power-law emission, consistent with the presence of heating from an active galactic nucleus (AGN). We study the relationship between stellar mass and star formation rate of our sample of infrared luminous galaxies and find no evidence that Herschel-selected galaxies follow the SFR/M_* "main sequence" as previously determined from studies of optically selected, star-forming galaxies. Finally, we compare the mid-infrared to FIR properties of our infrared luminous galaxies using the previously defined diagnostic, IR8 ≡ L_(IR)/L_8, and find that galaxies with L_(IR) ≳ 10^(11.3) L_☉ tend to systematically lie above (× 3-5) the IR8 "infrared main sequence," suggesting either suppressed PAH emission or an increasing contribution from AGN heating.
Additional Information
© 2013 American Astronomical Society. Received 2013 June 24; accepted 2013 September 27; published 2013 November 12. D. B. Sanders and C. M. Casey acknowledge the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation grant No. PHY-1066293. C. M. Casey is generously supported by a Hubble Fellowship from Space Telescope Science Institute, grant HST-HF-51268.01-A. COSMOS is based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555; also based on data collected at: the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; and the Canada–France–Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France);MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA).Attached Files
Published - 0004-637X_778_2_131.pdf
Submitted - 1310.0474v1.pdf
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Additional details
- Eprint ID
- 43229
- Resolver ID
- CaltechAUTHORS:20140106-131441483
- PHY-1066293
- NSF
- HST-HF-51268.01-A
- NASA Hubble Fellowship
- NAS 5-26555
- NASA
- Bundesministerium für Verkehr, Innovation und Technologie (BMVIT)
- ESA-PRODEX (Belgium)
- Commissariat à l'Energie Atomique (CEA)
- Deutsches Zentrum für Luft- und Raumfahrt (DLR)
- Agenzia Spaziale Italiana (ASI)
- Comisión Interministerial de Ciencia y Tecnología (CICYT)
- Canadian Space Agency (CSA)
- National Astronomical Observatories, Chinese Academy of Sciences (NAOC)
- Istituto Nazionale di Astrofisica (INAF)
- Centre National d'Études Spatiales (CNES)
- Ministerio de Ciencia Y Tecnologia (MCYT)
- Agenzia Spaziale Italiana (ASI)
- Ministerio de Ciencia e Innovación (MCINN)
- Swedish National Space Board (SNSB)
- Science and Technology Facilities Council (STFC)
- NASA
- Centre National de la Recherche Scientifique (CNRS)
- Created
-
2014-01-06Created from EPrint's datestamp field
- Updated
-
2021-11-10Created from EPrint's last_modified field
- Caltech groups
- COSMOS, Infrared Processing and Analysis Center (IPAC)