Galaxy And Mass Assembly (GAMA) : time-scales for galaxies crossing the green valley
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We explore the constraints that can be placed on the evolutionary time-scales for typical low-redshift galaxies evolving from the blue cloud through the green valley and on to the red sequence. We utilize galaxies from the GAMA survey with 0.1 < z < 0.2 and classify them according to the intrinsic (u* − r*) colours of their stellar populations, as determined by fits to their multiwavelength spectral energy distributions. Using these fits to also determine stellar population ages and star formation time-scales, we argue that our results are consistent with a green valley population dominated by galaxies that are simply decreasing their star formation (running out of gas) over a time-scale of 2–4 Gyr which are seen at a specific epoch in their evolution (approximately 1.6 e-folding times after their peak in star formation). If their fitted star formation histories are extrapolated forward, the green galaxies will further redden over time, until they attain the colours of a passive population. In this picture, no specific quenching event which cuts-off their star formation is required, though it remains possible that the decline in star formation in green galaxies may be expedited by internal or external forces. However, there is no evidence that green galaxies have recently changed their star formation time-scales relative to their previous longer term star formation histories.
Phillipps , S , Bremer , M N , Hopkins , A M , De Propris , R , Taylor , E N , James , P A , Davies , L J M , Cluver , M , Driver , S P , Eales , S A , Holwerda , B W , Kelvin , L S & Sansom , A E 2019 , ' Galaxy And Mass Assembly (GAMA) : time-scales for galaxies crossing the green valley ' , Monthly Notices of the Royal Astronomical Society , vol. 485 , no. 4 , pp. 5559–5572 . https://doi.org/10.1093/mnras/stz799
Monthly Notices of the Royal Astronomical Society
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz799
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