GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies

被引：160

作者：

Buat, V. ^{[1
]}

Noll, S. ^{[2
]}

Burgarella, D. ^{[1
]}

Giovannoli, E. ^{[1
,3
]}

Charmandaris, V. ^{[4
,5
,6
,7
]}

Pannella, M. ^{[8
]}

Hwang, H. S. ^{[9
]}

Elbaz, D. ^{[8
]}

Dickinson, M. ^{[10
]}

Magdis, G. ^{[11
]}

Reddy, N. ^{[12
]}

Murphy, E. J. ^{[13
]}

机构：

[1] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille UMR 7326, F-13388 Marseille, France

[2] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[3] Univ Western Cape, ZA-7535 Cape Town, South Africa

[4] Univ Crete, Dept Phys, Iraklion 71003, Greece

[5] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Greece

[6] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece

[7] Observ Paris, LERMA, CNRS UMR 8112, F-75014 Paris, France

[8] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France

[9] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA

[10] Natl Opt Astron Observ, Tucson, AZ 85719 USA

[11] Univ Oxford, Dept Phys, Oxford OX1 3RH, England

[12] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA

[13] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2012年 / 545卷

关键词：

galaxies: high-redshift; galaxies: ISM; galaxies: starburst; ultraviolet: galaxies; dust; extinction; STAR-FORMING GALAXIES; SIMILAR-TO; 2; LYMAN BREAK GALAXIES; STELLAR POPULATION SYNTHESIS; SPECTRAL ENERGY-DISTRIBUTION; FORMATION RATE DENSITY; INITIAL MASS FUNCTION; K-SELECTED GALAXIES; DEEP FIELD-SOUTH; STARBURST GALAXIES;

D O I：

10.1051/0004-6361/201219405

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 angstrom 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.

引用

页数：15

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