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A Controlled Study of Cold Dust Content in Galaxies from z = 0–2

Kirkpatrick, Allison and Pope, Alexandra and Sajina, Anna and Dale, Daniel A. and Díaz-Santos, Tanio and Hayward, Christopher C. and Shi, Yong and Somerville, Rachel S. and Stierwalt, Sabrina and Armus, Lee and Kartaltepe, Jeyhan S. and Kocevski, Dale D. and McIntosh, Daniel H. and Sanders, David B. and Yan, Lin (2017) A Controlled Study of Cold Dust Content in Galaxies from z = 0–2. Astrophysical Journal, 843 (1). Art. No. 71. ISSN 1538-4357.

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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.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Pope, Alexandra0000-0001-8592-2706
Sajina, Anna0000-0002-1917-1200
Dale, Daniel A.0000-0002-5782-9093
Díaz-Santos, Tanio0000-0003-0699-6083
Hayward, Christopher C.0000-0003-4073-3236
Shi, Yong0000-0002-8614-6275
Stierwalt, Sabrina0000-0002-2596-8531
Armus, Lee0000-0003-3498-2973
Kartaltepe, Jeyhan S.0000-0001-9187-3605
Sanders, David B.0000-0002-1233-9998
Yan, Lin0000-0003-1710-9339
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.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)31130005
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1151239
Simons FoundationUNSPECIFIED
Subject Keywords:galaxies: fundamental parameters – galaxies: high-redshift – galaxies: ISM – galaxies: star formation
Issue or Number:1
Record Number:CaltechAUTHORS:20170707-084101712
Persistent URL:
Official Citation:Allison Kirkpatrick et al 2017 ApJ 843 71
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78832
Deposited By: Tony Diaz
Deposited On:07 Jul 2017 17:25
Last Modified:03 Oct 2019 18:12

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