A controlled study of cold dust content in galaxies from $z=0-2$

Abstract

At $z=1-3$, the formation of new stars is dominated by dusty galaxies whose far-IR emission indicates they contain colder dust than local galaxies of a similar luminosity. We explore the reasons for the evolving IR emission of similar galaxies over cosmic time using: 1) Local galaxies from GOALS $(L_{\mathrm{IR}}=10^{11}-10^{12}{L}_{\odot })$; 2) Galaxies at $z\sim 0.1-0.5$ from the 5MUSES ($L_{\mathrm{IR}}=10^{10}-10^{12}{L}_{\odot }$); 3) IR luminous galaxies spanning $z=0.5-3$ from GOODS and Spitzer xFLS ($L_{\mathrm{IR}}>10^{11}{L}_{\odot }$). All samples have Spitzer mid-IR spectra, and Herschel and ground-based submillimeter imaging covering the full IR spectral energy distribution, allowing us to robustly measure $L_{\mathrm{IR}}^{\mathrm{SF}}$, $T_{\mathrm{dust}}$, and $M_{\mathrm{dust}}$ for every galaxy. Despite similar infrared luminosities, $z>0.5$ dusty star forming galaxies have a factor of 5 higher dust masses and 5K colder temperatures. The increase in dust mass is linked with an increase in the gas fractions with redshift, and we do not observe a similar increase in stellar mass or star formation efficiency. $L_{160}^{\mathrm{SF}}/L_{70}^{\mathrm{SF}}$, a proxy for $T_{\mathrm{dust}}$, is strongly correlated with $L_{\mathrm{IR}}^{\mathrm{SF}}/M_{\mathrm{dust}}$ independently of redshift. We measure merger classification and galaxy size for a subsample, and there is no obvious correlation between these parameters and $L_{\mathrm{IR}}^{\mathrm{SF}}/M_{\mathrm{dust}}$ or $L_{160}^{\mathrm{SF}}/L_{70}^{\mathrm{SF}}$. In dusty star forming galaxies, the change in $L_{\mathrm{IR}}^{\mathrm{SF}}/M_{\mathrm{dust}}$ can fully account for the observed colder dust temperatures, suggesting that any change in the spatial extent of the interstellar medium is a second order effect.

arXiv commentAccepted for publication in ApJ. 21 pages, 11 figures

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