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GAMA/G10-COSMOS/3D-HST: the 0 < z < 5 cosmic star formation history, stellar-mass, and dust-mass densities

Driver, Simon P; Andrews, Stephen K; da Cunha, Elisabete; Davies, Luke J; Lagos, Claudia; Robotham, Aaron S G; Vinsen, Kevin; Wright, Angus H; Alpaslan, Mehmet; Bland-Hawthorn, Joss; Bourne, Nathan; Brough, Sarah; Bremer, Malcolm N; Cluver, Michelle; Colless, Matthew; Conselice, Christopher J; Dunne, Loretta; Eales, Steve A; Gomez, Haley; Holwerda, Benne; Hopkins, Andrew M; Kafle, Prajwal R; Kelvin, Lee S; Loveday, Jon; Liske, Jochen; Maddox, Steve J; Phillipps, Steven; Pimbblet, Kevin; Rowlands, Kate; Sansom, Anne E; Taylor, Edward; Wang, Lingyu; Wilkins, Stephen M

Authors

Simon P Driver

Stephen K Andrews

Elisabete da Cunha

Luke J Davies

Claudia Lagos

Aaron S G Robotham

Kevin Vinsen

Angus H Wright

Mehmet Alpaslan

Joss Bland-Hawthorn

Nathan Bourne

Sarah Brough

Malcolm N Bremer

Michelle Cluver

Matthew Colless

Christopher J Conselice

Loretta Dunne

Steve A Eales

Haley Gomez

Benne Holwerda

Andrew M Hopkins

Prajwal R Kafle

Lee S Kelvin

Jon Loveday

Jochen Liske

Steve J Maddox

Steven Phillipps

Kate Rowlands

Anne E Sansom

Edward Taylor

Lingyu Wang

Stephen M Wilkins



Abstract

We use the energy-balance code MAGPHYS to determine stellar and dust masses, and dust corrected star formation rates for over 200 000 GAMA galaxies, 170 000 G10-COSMOS galaxies, and 200 000 3D-HST galaxies. Our values agree well with previously reported measurements and constitute a representative and homogeneous data set spanning a broad range in stellar-mass (108-1012 M☉), dust-mass (106-109 M☉), and star formation rates (0.01-100 M☉yr-1), and over a broad redshift range (0.0 < z < 5.0). We combine these data to measure the cosmic star formation history (CSFH), the stellar-mass density (SMD), and the dust-mass density (DMD) over a 12 Gyr timeline. The data mostly agree with previous estimates, where they exist, and provide a quasi-homogeneous data set using consistent mass and star formation estimators with consistent underlying assumptions over the full time range. As a consequence our formal errors are significantly reduced when compared to the historic literature. Integrating our CSFH we precisely reproduce the SMD with an interstellar medium replenishment factor of 0.50 ± 0.07, consistent with our choice of Chabrier initial mass function plus some modest amount of stripped stellar mass. Exploring the cosmic dust density evolution, we find a gradual increase in dust density with lookback time. We build a simple phenomenological model from the CSFH to account for the dust-mass evolution, and infer two key conclusions: (1) For every unit of stellar mass which is formed 0.0065-0.004 units of dust mass is also formed. (2) Over the history of the Universe approximately 90-95 per cent of all dust formed has been destroyed and/or ejected.

Journal Article Type Article
Publication Date Apr 30, 2018
Journal Monthly notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Oxford University Press (OUP)
Peer Reviewed Peer Reviewed
Volume 475
Issue 3
Pages 2891-2935
APA6 Citation Driver, S. P., Andrews, S. K., da Cunha, E., Davies, L. J., Lagos, C., Robotham, A. S. G., …Wilkins, S. M. (2018). GAMA/G10-COSMOS/3D-HST: the 0 < z < 5 cosmic star formation history, stellar-mass, and dust-mass densities. Monthly notices, containing papers, abstracts of papers, and reports of the proceedings of the Society, 475(3), 2891-2935. doi:10.1093/mnras/stx2728
DOI https://doi.org/10.1093/mnras/stx2728
Keywords Astronomical data bases: miscellaneous; Galaxies: evolution; Galaxies: general; Galaxies: individual; Galaxies: photometry; Cosmology: observations
Publisher URL https://academic.oup.com/mnras/article/475/3/2891/4730178
Related Public URLs http://orca.cf.ac.uk/105792/
Copyright Statement This article has been accepted for publication in MNRAS ©: 2018 The authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

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Copyright Statement
This article has been accepted for publication in MNRAS ©: 2018 The authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.



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