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Galaxy And Mass Assembly (GAMA) : The mechanisms for quiescent galaxy formation at z<1

Wang, L.; Wild, V.; Sansom, A. E.; Phillipps, S.; Owers, M. S.; Hopkins, A. M.; Driver, S. P.; Brough, S.; Bremer, M.; Pimbblet, K.; Alpaslan, M.; Bland-Hawthorn, J.; Bourne, N.; Bremer, M N; Brough, Sarah; Colless, M.; Driver, Simon; Holwerda, B. W.; Hopkins, Andrew; Owers, Matt; Phillipps, Steven; Rowlands, K.; Sansom, Anne; Taylor, E. N.; Wang, Lingyu; Wild, Vivienne


L. Wang

V. Wild

A. E. Sansom

S. Phillipps

M. S. Owers

A. M. Hopkins

S. P. Driver

S. Brough

M. Bremer

M. Alpaslan

J. Bland-Hawthorn

N. Bourne

M N Bremer

Sarah Brough

M. Colless

Simon Driver

B. W. Holwerda

Andrew Hopkins

Matt Owers

Steven Phillipps

K. Rowlands

Anne Sansom

E. N. Taylor

Lingyu Wang

Vivienne Wild


© 2016 The Authors. One key problem in astrophysics is understanding how and why galaxies switch off their star formation, building the quiescent population that we observe in the local Universe. From the Galaxy And Mass Assembly and VIsible MultiObject Spectrograph Public Extragalactic Redshift surveys, we use spectroscopic indices to select quiescent and candidate transition galaxies.We identify potentially rapidly transitioning post-starburst (PSB) galaxies and slower transitioning green-valley galaxies. Over the last 8Gyr, the quiescent population has grown more slowly in number density at high masses (M * > 10 11 M ⊙ ) than at intermediate masses (M * > 10 10.6 M ⊙ ). There is evolution in both the PSB and green-valley stellar mass functions, consistent with higher mass galaxies quenching at earlier cosmic times.At intermediatemasses (M * > 10 10.6 M ⊙ ), we find a green-valley transition time-scale of 2.6 Gyr. Alternatively, at z ~ 0.7, the entire growth rate could be explained by fast-quenching PSB galaxies, with a visibility time-scale of 0.5 Gyr. At lower redshift, the number density of PSBs is so low that an unphysically short visibility window would be required for them to contribute significantly to the quiescent population growth. The importance of the fast-quenching route may rapidly diminish at z < 1. However, at high masses (M * > 10 11 M ⊙ ), there is tension between the large number of candidate transition galaxies compared to the slow growth of the quiescent population. This could be resolved if not all high-mass PSB and green-valley galaxies are transitioning from star forming to quiescent, for example if they rejuvenate out of the quiescent population following the accretion of gas and triggering of star formation, or if they fail to completely quench their star formation.

Publication Date Jan 1, 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 473
Issue 1
Pages 1168-1185
Institution Citation Wild, V., Bremer, M., Brough, S., Driver, S. P., Hopkins, A. M., Owers, M. S., …Wild, V. (2018). Galaxy And Mass Assembly (GAMA) : The mechanisms for quiescent galaxy formation at z<1. Monthly notices, containing papers, abstracts of papers, and reports of the proceedings of the Society, 473(1), 1168-1185.
Keywords Galaxies: evolution, Galaxies: luminosity function, Mass function, Galaxies: starburst, Galaxies: interactions, Galaxies: star formation, Galaxies: statistics
Publisher URL
Copyright Statement © 2017 The Authors
Additional Information Copy of an article published in: Monthly notices of the Royal Astronomical Society, 2018, v.473, issue 1.


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