Probing star formation and ISM properties using galaxy disk inclination

I. Evolution in disk opacity since z ~ 0.7

¹ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
e-mail: leslie@mpia.de
² Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UK
³ Research School of Astronomy and Astrophysics, Australian National University, Canberra ACT 2611, Australia
⁴ INAF-Osservatorio Astronomico di Bologna, via Gobetti 93/3, 40129 Bologna, Italy
⁵ Observatoire de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland
⁶ Faculty of Science University of Zagreb, Bijenička c. 32, 10002 Zagreb, Croatia

Received: 7 November 2017
Accepted: 22 December 2017

Abstract

Disk galaxies at intermediate redshift (z ~ 0.7) have been found in previous work to display more optically thick behaviour than their local counterparts in the rest-frame B-band surface brightness, suggesting an evolution in dust properties over the past ~6 Gyr. We compare the measured luminosities of face-on and edge-on star-forming galaxies at different wavelengths (Ultraviolet (UV), mid-infrared (MIR), far-infrared (FIR), and radio) for two well-matched samples of disk-dominated galaxies: a local Sloan Digital Sky Survey (SDSS)-selected sample at z ~ 0.07 and a sample of disks at z ~ 0.7 drawn from Cosmic Evolution Survey (COSMOS). We have derived correction factors to account for the inclination dependence of the parameters used for sample selection. We find that typical galaxies are transparent at MIR wavelengths at both redshifts, and that the FIR and radio emission is also transparent as expected. However, reduced sensitivity at these wavelengths limits our analysis; we cannot rule out opacity in the FIR or radio. Ultra-violet attenuation has increased between z ~ 0 and z ~ 0.7, with the z ~ 0.7 sample being a factor of ~3.4 more attenuated. The larger UV attenuation at z ~ 0.7 can be explained by more clumpy dust around nascent star-forming regions. There is good agreement between the fitted evolution of the normalisation of the SFR_UV versus 1 − cos(i) trend (interpreted as the clumpiness fraction) and the molecular gas fraction/dust fraction evolution of galaxies found out to z < 1.