The infrared compactness-temperature relation for quiescent and starburst galaxies^*

¹ Astrophysics Group, Blackett Laboratory, Imperial College, Prince Consort Road, London SW7 2AZ, UK e-mail: p.chanial@imperial.ac.uk
² Laboratoire Galaxies, Etoiles, Physique et Instrumentation, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France
³ Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 avenue Charles André, 69230 Saint-Genis Laval, France; CNRS, UMR 5574; École Normale Supérieure de Lyon, Lyon, France
⁴ Service d'Astrophysique, DAPNIA, DSM, CEA-Saclay, Orme des Merisiers, Bât. 709, 91191 Gif-sur-Yvette, France
⁵ Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France; CNRS, UMR 7095; Université Pierre & Marie Curie, Paris, France

Received: 22 July 2005
Accepted: 6 October 2006

Abstract

Context. IRAS observations show the existence of a correlation between the infrared luminosity L_IR and dust temperature T_d in star-forming galaxies, in which larger L_IR leads to higher dust temperature. The L_IR–T_d relation is commonly seen as reflecting the increase in dust temperature in galaxies with higher star formation rate (SFR). Even though the correlation shows a significant amount of dispersion, a unique relation has been commonly used to construct spectral energy distributions (SEDs) of galaxies in distant universe studies, such as source number counting or photometric redshift determination.

Aims.In this work, we introduce a new parameter, namely the size of the star-forming region and lay out the empirical and modelled relation between the global parameters L_IR , T_d and of IR-bright non-AGN galaxies.

Methods.IRAS 60-to-100 μm color is used as a proxy for the dust temperature and the 1.4 GHz radio contiuum (RC) emission for the infrared spatial distribution. The analysis has been carried out on two samples. The first one is made of the galaxies from the 60 μm flux-limited IRAS Revised Bright Galaxy Samples (RBGS) which have a reliable RC size estimate from the VLA follow-ups of the IRAS Bright Galaxy Samples. The second is made of the sources from the 170 μm ISOPHOT Serendipity Sky Survey (ISOSSS) which are resolved by the NRAO VLA Sky Survey (NVSS) or by the Faint Images of the Radio Sky at Twenty-cm survey (FIRST).

Results.We show that the dispersion in the L_IR–T_d diagram can be reduced to a relation between the infrared surface brightness and the dust temperature, a relation that spans 5 orders of magnitude in surface brightness.

Conclusions. We explored the physical processes giving rise to the –T_d relation, and show that it can be derived from the Schmidt law, which relates the star formation rate to the gas surface density.