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

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Date
01/01/2018
Author
Rowlands, K.
Wild, V.
Bourne, N.
Bremer, M.
Brough, S.
Driver, S. P.
Hopkins, A. M.
Owers, M. S.
Phillipps, S.
Pimbblet, K.
Sansom, A. E.
Wang, L.
Alpaslan, M.
Bland-Hawthorn, J.
Colless, M.
Holwerda, B. W.
Taylor, E. N.
Keywords
Galaxies: evolution
Galaxies: luminosity function, mass function
Galaxies: starburst
Galaxies: interactions
Galaxies: star fomation
Galaxies: statistics
QB Astronomy
QC Physics
3rd-DAS
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Abstract
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 GAMA and VIPERS surveys, we use spectroscopic indices to select quiescent and candidate transition galaxies. We identify potentially rapidly transitioning post-starburst galaxies, and slower transitioning green-valley galaxies. Over the last 8 Gyrs the quiescent population has grown more slowly in number density at high masses (M∗>1011M⊙) than at intermediate masses (M∗>1010.6M⊙). There is evolution in both the post-starburst and green valley stellar mass functions, consistent with higher mass galaxies quenching at earlier cosmic times. At intermediate masses (M∗>1010.6M⊙) we find a green valley transition timescale of 2.6 Gyr. Alternatively, at z∼0.7 the entire growth rate could be explained by fast-quenching post-starburst galaxies, with a visibility timescale of 0.5 Gyr. At lower redshift, the number density of post-starbursts 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∗>1011M⊙), 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 post-starburst 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.
Citation
Rowlands , K , Wild , V , Bourne , N , Bremer , M , Brough , S , Driver , S P , Hopkins , A M , Owers , M S , Phillipps , S , Pimbblet , K , Sansom , A E , Wang , L , Alpaslan , M , Bland-Hawthorn , J , Colless , M , Holwerda , B W & Taylor , E N 2018 , ' Galaxy And Mass Assembly (GAMA) : the mechanisms for quiescent galaxy formation at z < 1 ' , Monthly Notices of the Royal Astronomical Society , vol. 473 , no. 1 , pp. 1168-1185 . https://doi.org/10.1093/mnras/stx1903
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/stx1903
ISSN
0035-8711
Type
Journal article
Rights
© 2017, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1093/mnras/stx1903
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  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2017arXiv170707989R
URI
http://hdl.handle.net/10023/11897

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