S2COSMOS: Evolution of gas mass with redshift using dust emission

Creators: Millard, Jenifer S.; Eales, Stephen A.; Smith, M. W. L.; Gomez, H. L.; Małek, K.; Simpson, J. M.; Peng, Y.; Sawicki, M.; Beeston, R. A.; Bunker, Andrew; Ao, Y.; Babul, A.; Ho, L. C.; Hwang, Ho Seong; Michałowski, M. J.; Scoville, N.; Shim, H.; Toba, Y.

Abstract

We investigate the evolution of the gas mass fraction for galaxies in the COSMOS field using submillimetre emission from dust at 850 μm. We use stacking methodologies on the 850 μm S2COSMOS map to derive the gas mass fraction of galaxies out to high redshifts, 0 ≤ z ≤ 5, for galaxies with stellar masses of 10^(9.5) < M∗ (M⊙) < 10^(11.75)⁠. In comparison to previous literature studies we extend to higher redshifts, include more normal star-forming galaxies (on the main sequence), and also investigate the evolution of the gas mass fraction split by star-forming and passive galaxy populations. We find our stacking results broadly agree with scaling relations in the literature. We find tentative evidence for a peak in the gas mass fraction of galaxies at around z ∼ 2.5–3, just before the peak of the star formation history of the Universe. We find that passive galaxies are particularly devoid of gas, compared to the star-forming population. We find that even at high redshifts, high stellar mass galaxies still contain significant amounts of gas.

Additional Information

© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2020 February 27. Received 2020 February 27; in original form 2019 October 10. Published: 03 March 2020. We thank Luke Davies and Simon Driver for providing the MAGPHYS data set on which this study is based. We thank Pieter De Vis for providing average gas fraction measurements for local galaxies. We thank Ian Smail for his comments at several stages of paper development, and also the anonymous referee for their comments and suggestions – both parties ultimately improved this manuscript. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan; Academia Sinica Institute of Astronomy and Astrophysics; the Korea Astronomy and Space Science Institute; the Operation, Maintenance and Upgrading Fund for Astronomical Telescopes and Facility Instruments, budgeted from the Ministry of Finance (MOF) of China and administrated by the Chinese Academy of Sciences (CAS), as well as the National Key R&D Program of China (No. 2017YFA0402700). Additional funding support is provided by the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada (ST/M007634/1, ST/M003019/1, ST/N005856/1). The James Clerk Maxwell Telescope has historically been operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and the Netherlands Organization for Scientific Research and data from observations undertaken during this period of operation is used in this manuscript. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. The data used in this work were taken as part of Program ID M16AL002. JSM, HLG, and RAB acknowledge support from the European Research Council (ERC) in the form of Consolidator Grant COSMICDUST (ERC-2014-CoG-647939). KM has been supported by the National Science Centre (grant UMO-2013/09/D/ST9/04030). YP acknowledges National Key R&D Program of China Grant 2016YFA0400702 and National Science Foundation of China (NSFC) Grant No. 11773001. LCH was supported by the NSFC (11721303, 11991052) and the National Key R&D Program of China (2016YFA0400702). MJM acknowledges the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208.

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