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HERMES: unveiling obscured star formation – the far-infrared luminosity function of ultraviolet-selected galaxies at z ∼ 1.5

Heinis, S. and Buat, V. and Béthermin, M. and Aussel, H. and Bock, J. and Boselli, A. and Burgarella, D. and Conley, A. and Cooray, A. and Farrah, D. and Ibar, E. and Ilbert, O. and Ivison, R. J. and Magdis, G. and Marsden, G. and Oliver, S. J. and Page, M. J. and Rodighiero, G. and Roehlly, Y. and Schulz, B. and Scott, Douglas and Smith, A. J. and Viero, M. and Wang, L. and Zemcov, M. (2013) HERMES: unveiling obscured star formation – the far-infrared luminosity function of ultraviolet-selected galaxies at z ∼ 1.5. Monthly Notices of the Royal Astronomical Society, 429 (2). pp. 1113-1132. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20130613-104444434

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Abstract

We study the far-infrared and sub-millimetre properties of a sample of ultraviolet (UV) selected galaxies at z ∼ 1.5. Using stacking at 250, 350 and 500 μm from Herschel Space Observatory Spectral and Photometric Imaging Receiver (SPIRE) imaging of the Cosmological Evolution Survey (COSMOS) field obtained within the Herschel Multi-tiered Extragalactic Survey (HERMES) key programme, we derive the mean infrared (IR) luminosity as a function of both UV luminosity and slope of the UV continuum β. The IR to UV luminosity ratio is roughly constant over most of the UV luminosity range we explore. We also find that the IR to UV luminosity ratio is correlated with β. We observe a correlation that underestimates the correlation derived from low-redshift starburst galaxies, but is in good agreement with the correlation derived from local normal star-forming galaxies. Using these results we reconstruct the IR luminosity function of our UV-selected sample. This luminosity function recovers the IR luminosity functions measured from IR-selected samples at the faintest luminosities (L_(IR) ∼ 10^(11) L_⊙), but might underestimate them at the bright-end (L_(IR) ≳ 5 × 10^(11) L_⊙). For galaxies with 10^(11) < L_(IR)/L_⊙ < 10^(13), the IR luminosity function of an UV selection recovers (given the differences in IR-based estimates) 52–65 to 89–112 per cent of the star formation rate density derived from an IR selection. The cosmic star formation rate density derived from this IR luminosity function is 61–76 to 100–133 per cent of the density derived from IR selections at the same epoch. Assuming the latest Herschel results and conservative stacking measurements, we use a toy model to fully reproduce the far-IR luminosity function from our UV selection at z ∼ 1.5. This suggests that a sample around 4 mag deeper (i.e. reaching u^* ∼ 30 mag) and a large dispersion of the IR to UV luminosity ratio are required.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/sts397DOIArticle
https://arxiv.org/abs/1211.4336arXivDiscussion Paper
ORCID:
AuthorORCID
Béthermin, M.0000-0002-3915-2015
Aussel, H.0000-0002-1371-5705
Bock, J.0000-0002-5710-5212
Cooray, A.0000-0002-3892-0190
Farrah, D.0000-0003-1748-2010
Ilbert, O.0000-0002-7303-4397
Ivison, R. J.0000-0001-5118-1313
Magdis, G.0000-0002-4872-2294
Oliver, S. J.0000-0001-7862-1032
Page, M. J.0000-0002-6689-6271
Rodighiero, G.0000-0002-9415-2296
Scott, Douglas0000-0002-6878-9840
Zemcov, M.0000-0001-8253-1451
Additional Information:© 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2012 November 12. Received 2012 October 31; in original form 2012 April 5. First published online: December 13, 2012. We thank the referee for a careful reading and detailed, constructive comments which helped improving the paper. SH and VB thank the French Space Agency (CNES) for financial support. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (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, UKSA (UK); and NASA (USA). We thank the COSMOS collaboration for sharing data used in this paper. The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM, http://hedam. oamp.fr/HerMES), operated by CeSAM and hosted by the Laboratoire d’Astrophysique de Marseille.
Funders:
Funding AgencyGrant Number
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
NASAUNSPECIFIED
Subject Keywords: methods: statistical galaxies: luminosity function infrared: galaxies ultraviolet: galaxies
Issue or Number:2
Record Number:CaltechAUTHORS:20130613-104444434
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130613-104444434
Official Citation:S. Heinis, V. Buat, M. Béthermin, H. Aussel, J. Bock, A. Boselli, D. Burgarella, A. Conley, A. Cooray, D. Farrah, E. Ibar, O. Ilbert, R. J. Ivison, G. Magdis, G. Marsden, S. J. Oliver, M. J. Page, G. Rodighiero, Y. Roehlly, B. Schulz, Douglas Scott, A. J. Smith, M. Viero, L. Wang, and M. Zemcov HerMES: unveiling obscured star formation – the far-infrared luminosity function of ultraviolet-selected galaxies at z ∼ 1.5 MNRAS (February 21, 2013) Vol. 429 1113-1132 first published online December 13, 2012 doi:10.1093/mnras/sts397
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:38943
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:13 Jun 2013 18:20
Last Modified:09 Mar 2020 13:19

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