Variations in the dust emissivity index, β, within and between galaxies, are evidence that the chemistry and physics of dust must vary on large scales, although the nature of the physical and/or chemical variations is still unknown. In this paper we estimate values of β and dust temperature for a sample of 109 dusty star-forming galaxies (DSFGs) over the range, 2<z<6. We compare the results obtained with both an optically-thin model and a general opacity model, finding that our estimates of β are similar between the models but our estimates of dust temperature are not. We find no evidence of a change in β with redshift, with a median value of β=1.96 for the optically-thin model with a confidence interval (16 - 84%) of 1.67 to 2.35 for the population. Using simulations, we estimate the measurement errors from our procedure and show that the variation of β in the population results from intrinsic variations in the properties of the dust in DSFGs. At a fixed far-infrared luminosity, we find no evidence for a change in dust temperature, Tdust, with redshift. After allowing for the effects of correlated measurement errors, we find an inverse correlation between β and Tdust in DSFGs, for which there is also evidence in low-redshift galaxies.
@article{arxiv.2402.05182,
title = {Little evolution of dust emissivity in bright infrared galaxies from $2 < z < 6$},
author = {B. A. Ward and S. A. Eales and R. J. Ivison and V. Arumugam},
journal= {arXiv preprint arXiv:2402.05182},
year = {2024}
}