GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies⋆
1 Aix-Marseille Université, CNRS – LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
2 Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstr. 25/8, 6020 Innsbruck, Austria
3 University of the Western Cape, Private Bag X17, 7535 Bellville, Cape Town, South Africa
4 University of Crete, Department of Physics and Institute of Theoretical & Computational Physics, 71003 Heraklion, Greece
5 IESL/Foundation for Research & Technology-Hellas, 71110 Heraklion, Greece
6 Observatoire de Paris, LERMA (CNRS: UMR 8112), 61 Av. de l’Observatoire, 75014 Paris, France
7 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris Diderot, CE-Saclay, 91191 Gif-sur-Yvette, France
8 Smithsonian Astrophysical Observatory, 60 Garden St., Cambridge, MA 02138, USA
9 National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA
10 Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK
11 Department of Physics and Astronomy, University of California, Riverside, 900 University Avenue, Riverside, 92521 California, USA
12 Spitzer Science Center, California Institute of Technology, Pasadena, CA, 91125, USA
Received: 13 April 2012
Accepted: 14 June 2012
Context. Dust attenuation in galaxies is poorly known, especially at high redshift. And yet the amount of dust attenuation is a key parameter to deduce accurate star formation rates from ultraviolet (UV) rest-frame measurements. The wavelength dependence of the dust attenuation is also of fundamental importance to interpret the observed spectral energy distributions (SEDs) and to derive photometric redshifts or physical properties of galaxies.
Aims. We want to study dust attenuation at UV wavelengths at high redshift, where the UV is redshifted to the observed visible light wavelength range. In particular, we search for a UV bump and related implications for dust attenuation determinations.
Methods. We use photometric data in the Chandra Deep Field South (CDFS), obtained in intermediate and broad band filters by the MUSYC project, to sample the UV rest-frame of 751 galaxies with 0.95 < z < 2.2. When available, infrared (IR) Herschel/PACS⋆⋆ data from the GOODS-Herschel project, coupled with Spitzer/MIPS measurements, are used to estimate the dust emission and to constrain dust attenuation. The SED of each source is fit using the CIGALE code. The amount of dust attenuation and the characteristics of the dust attenuation curve are obtained as outputs of the SED fitting process, together with other physical parameters linked to the star formation history.
Results. The global amount of dust attenuation at UV wavelengths is found to increase with stellar mass and to decrease as UV luminosity increases. A UV bump at 2175 Å is securely detected in 20% of the galaxies, and the mean amplitude of the bump for the sample is similar to that observed in the extinction curve of the LMC supershell region. This amplitude is found to be lower in galaxies with very high specific star formation rates, and 90% of the galaxies exhibiting a secure bump are at z < 1.5. The attenuation curve is confirmed to be steeper than that of local starburst galaxies for 20% of the galaxies. The large dispersion found for these two parameters describing the attenuation law is likely to reflect a wide diversity of attenuation laws among galaxies. The relations between dust attenuation, IR-to-UV flux ratio, and the slope of the UV continuum are derived for the mean attenuation curve found for our sample. Deviations from the average trends are found to correlate with the age of the young stellar population and the shape of the attenuation curve.
Key words: galaxies: high-redshift / galaxies: ISM / galaxies: starburst / ultraviolet: galaxies / dust, extinction
Table of multi-colour photometry for the 751 galaxies is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/545/A141
© ESO, 2012