Probing star formation and ISM properties using galaxy disk inclination I: Evolution in disk opacity since $z\sim0.7$

TL;DR

This study compares galaxy disk inclination effects at different wavelengths between local and $z\,\sim0.7$ galaxies, revealing increased UV attenuation and dust clumpiness evolution over 6 Gyr.

Contribution

It provides new correction factors for inclination effects and demonstrates increased UV attenuation and dust clumpiness at intermediate redshift.

Findings

UV attenuation increased by a factor of ~3.4 from $z\sim0$ to $z\sim0.7$

Galaxies are transparent at MIR, FIR, and radio wavelengths at both redshifts

Clumpy dust around star-forming regions explains UV attenuation evolution.

Abstract

Disk galaxies at intermediate redshift ($z\sim0.7$) 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 $\sim$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 $z\sim0.07$ and a sample of disks at $z\sim0.7$ 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 $z\sim0$ and $z\sim0.7$, with the $z\sim0.7$ sample being a factor of $\sim$3.4 more attenuated. The larger UV attenuation at $z\sim0.7$ 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$_{\text{UV}}$ versus 1-cos(i) trend (interpreted as the clumpiness fraction) and the molecular gas fraction/dust fraction evolution of galaxies found out to $z<1$.