Probing star formation and ISM properties using galaxy disk inclination

Astronomy and Astrophysics, vol. 662, pp. A26

Abstract

Attenuation by dust severely impacts our ability to obtain unbiased observations of galaxies, especially as the amount and wavelength dependence of the attenuation varies with the stellar mass M*, inclination i, and other galaxy properties. In this study, we used the attenuation – inclination models in ultraviolet, optical, and near-infrared bands designed by Tuffs and collaborators to investigate the average global dust properties in galaxies as a function of M*, the stellar mass surface density μ*, the star-formation rate SFR, the specific star-formation rate sSFR, the star-formation main-sequence offset dMS, and the star-formation rate surface density ΣSFR at redshifts z ∼ 0 and z ∼ 0.7. We used star-forming galaxies from the Sloan Digital Sky Survey (∼20 000) and Galaxy And Mass Assembly (∼2000) to form our low-z sample at 0.04 < z < 0.1 and star-forming galaxies from Cosmological Evolution Survey (∼2000) for the sample at 0.6 < z < 0.8. We found that galaxies at z ∼ 0.7 have a higher optical depth τBf and clumpiness F than galaxies at z ∼ 0. The increase in F hints that the stars of z ∼ 0.7 galaxies are less likely to escape their birth cloud, which might indicate that the birth clouds are larger. We also found that τBf increases with M* and μ*, independent of the sample and therefore redshift. We found no clear trends in τBf or F with the SFR, which could imply that the dust mass distribution is independent of the SFR. In turn, this would imply that the balance of dust formation and destruction is independent of the SFR. Based on an analysis of the inclination dependence of the Balmer decrement, we found that reproducing the Balmer line emission requires not only a completely optically thick dust component associated with star-forming regions, as in the standard model, but an extra component of an optically thin dust within the birth clouds. This new component implies the existence of dust inside H II regions that attenuates the Balmer emission before it escapes through gaps in the birth cloud and we found it is more important in high-mass galaxies. These results will inform our understanding of dust formation and dust geometry in star-forming galaxies across redshift.

Authors 8

1. Stefan van der Giessen Aachen Leiden Observatory

   Leiden University · Universidad de Granada · Ghent University · Leiden Observatory

   Affiliation as printed

   Dept. Fisica Teorica y del Cosmos, Universidad de Granada, Granada, Spain

   Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands

   Sterrenkundig Observatorium, Ghent University, Krijgslaan 281 – S9, 9000 Gent, Belgium

2. S. K. Leslie Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands

3. Brent A Groves

   Australian National University · The University of Western Australia · Mount Stromlo Observatory · International Centre for Radio Astronomy Research

   Affiliation as printed

   International Centre for Radio Astronomy Research, The University of Western Australia, 7 Fairway, Crawley, WA 6009, Australia

   Research School of Astronomy and Astrophysics, Australian National University, Mt Stromlo Observatory, Weston Creek, ACT 2611, Australia

4. Jacqueline Hodge Aachen Leiden Observatory

   Leiden University · Leiden Observatory

   Affiliation as printed

   Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands

5. Cristina C. Popescu

   University of Lancashire

   Affiliation as printed

   Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK

6. M. Sargent

   University of Sussex · International Space Science Institute

   Affiliation as printed

   Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UK

   International Space Science Institute (ISSI), Hallerstrasse 6, 3012 Bern, Switzerland

7. Eva Schinnerer

   Max Planck Institute for Astronomy

   Affiliation as printed

   Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany

8. R. J. Tuffs

   Max Planck Institute for Nuclear Physics

   Affiliation as printed

   Max-Plank Institute for Nuclear Physics (MPIK), Saupfercheckweg 1, 69117 Heidelberg, Germany