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The Evolution of Interstellar Medium Mass Probed by Dust Emission: ALMA Observations at z = 0.3-2

Scoville, N. and Aussel, H. and Sheth, K. and Scott, K. S. and Sanders, D. and Ivison, R. J. and Pope, A. and Capak, P. and Vanden Bout, P. and Manohar, S. and Kartaltepe, J. and Robertson, B. and Lilly, S. (2014) The Evolution of Interstellar Medium Mass Probed by Dust Emission: ALMA Observations at z = 0.3-2. Astrophysical Journal, 783 (2). Art. No. 84. ISSN 0004-637X. doi:10.1088/0004-637X/783/2/84.

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The use of submillimeter dust continuum emission to probe the mass of interstellar dust and gas in galaxies is empirically calibrated using samples of local star-forming galaxies, Planck observations of the Milky Way, and high-redshift submillimeter galaxies. All of these objects suggest a similar calibration, strongly supporting the view that the Rayleigh-Jeans tail of the dust emission can be used as an accurate and very fast probe of the interstellar medium (ISM) in galaxies. We present ALMA Cycle 0 observations of the Band 7 (350 GHz) dust emission in 107 galaxies from z = 0.2 to 2.5. Three samples of galaxies with a total of 101 galaxies were stellar-mass-selected from COSMOS to have M* ≃ 10^(11) M☉: 37 at z ~ 0.4, 33 at z ~ 0.9, and 31 at z = 2. A fourth sample with six infrared-luminous galaxies at z = 2 was observed for comparison with the purely mass-selected samples. From the fluxes detected in the stacked images for each sample, we find that the ISM content has decreased by a factor ~6 from 1 to 2 × 10^(10) M☉ at both z = 2 and 0.9 down to ~2 × 10^9 M☉ at z = 0.4. The infrared-luminous sample at z = 2 shows a further ~4 times increase in M_(ISM) compared with the equivalent non-infrared-bright sample at the same redshift. The gas mass fractions are ~2% ± 0.5%, 12% ± 3%, 14% ± 2%, and 53% ± 3% for the four subsamples (z = 0.4, 0.9, and 2 and infrared-bright galaxies).

Item Type:Article
Related URLs:
URLURL TypeDescription Paper DOIArticle
Scoville, N.0000-0002-0438-3323
Aussel, H.0000-0002-1371-5705
Sheth, K.0000-0002-5496-4118
Sanders, D.0000-0002-1233-9998
Ivison, R. J.0000-0001-5118-1313
Pope, A.0000-0001-8592-2706
Capak, P.0000-0003-3578-6843
Kartaltepe, J.0000-0001-9187-3605
Lilly, S.0000-0002-6423-3597
Additional Information:© 2014 The American Astronomical Society. Received 2013 September 25; accepted 2014 January 13; published 2014 February 20. We thank the referee for a number of useful suggestions. We also thank Zara Scoville for proofreading the manuscript and Andreas Schruba for helpful comments. The Aspen Center for Physics is acknowledged for hospitality during the initial writing of this paper; NSF grant 1066293 is also acknowledged. K.S.S. and K.S. are supported by the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA# 2011.0.00097.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
National Radio Astronomy ObservatoryUNSPECIFIED
Subject Keywords:dust, extinction; evolution; galaxies: ISM; galaxies: starburst
Issue or Number:2
Record Number:CaltechAUTHORS:20140617-081753735
Persistent URL:
Official Citation:The Evolution of Interstellar Medium Mass Probed by Dust Emission: ALMA Observations at z = 0.3-2 N. Scoville et al. 2014 ApJ 783 84
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46296
Deposited By: Tony Diaz
Deposited On:17 Jun 2014 18:40
Last Modified:10 Nov 2021 17:23

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