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Published July 1, 2017 | Submitted + Published
Journal Article Open

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_(IR) = 10^(11)-10^(12) L⊙), (2) galaxies at z ~ 0.1-0.5 from 5MUSES (L_(IR) = 10^(10)-10^(12) L⊙), and (3) IR luminous galaxies spanning z = 0.5-3 from GOODS and Spitzer xFLS (L_(IR) > 10^(11) L⊙). All samples have Spitzermid-IR spectra, and Herschel and ground-based submillimeter imaging covering the full IR spectral energy distribution, allowing us to robustly measure L^(SF)_(IR), T_(dust), and M_(dust) for every galaxy. Despite similar infrared luminosities, z > 0.5 dusty star-forming galaxies (DSFG) have a factor of 5 higher dust masses and 5 K colder temperatures. The increase in dust mass is linked to an increase in the gas fractions with redshift, and we do not observe a similar increase in stellar mass or star formation efficiency. L^(SF)_(160)/L^(SF)_(70), a proxy for T_(dust), is strongly correlated with L^(SF)_(IR)/M_(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^(SF)_(IR)/M_(dust) or L^(SF)_(160)/L^(SF)_(70). In DSFG, the change in L^(SF)_(IR)/M_(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.

Additional Information

© 2017 The American Astronomical Society. Received 2017 January 19; revised 2017 May 19; accepted 2017 May 30; published 2017 July 5. We thank Caitlyn Casey and Gergo Popping for helpful conversations. We also thank the CANDELS collaboration for providing the visual merger classification catalogs for GOODS-N and GOODS-S. A.K., A.P., and A.S. acknowledge NASA ADAP13-0054 and NSF AAG grants AST-1312418 and AST-1313206. T.D.-S. acknowledges support from ALMA-CONICYT project 31130005 and FONDECYT regular project 1151239. The Flatiron Institute is supported by the Simons Foundation.

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Published - Kirkpatrick_2017_ApJ_843_71.pdf

Submitted - 1705.10846.pdf

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August 19, 2023
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October 26, 2023