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One key problem in astrophysics is understanding how and why galaxies switchoff their star formation, building the quiescent population that we observe inthe local Universe. From the GAMA and VIPERS surveys, we use spectroscopicindices to select quiescent and candidate transition galaxies. We identifypotentially rapidly transitioning post-starburst galaxies, and slowertransitioning green-valley galaxies. Over the last 8 Gyrs the quiescentpopulation has grown more slowly in number density at high masses(M$_*>10^{11}$M$_\odot$) than at intermediate masses(M$_*>10^{10.6}$M$_\odot$). There is evolution in both the post-starburst andgreen valley stellar mass functions, consistent with higher mass galaxiesquenching at earlier cosmic times. At intermediate masses(M$_*>10^{10.6}$M$_\odot$) we find a green valley transition timescale of 2.6Gyr. Alternatively, at $z\sim0.7$ the entire growth rate could be explained byfast-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 anunphysically short visibility window would be required for them to contributesignificantly to the quiescent population growth. The importance of thefast-quenching route may rapidly diminish at $z<1$. However, at high masses(M$_*>10^{11}$M$_\odot$), there is tension between the large number ofcandidate transition galaxies compared to the slow growth of the quiescentpopulation. This could be resolved if not all high mass post-starburst andgreen-valley galaxies are transitioning from star-forming to quiescent, forexample if they rejuvenate out of the quiescent population following theaccretion of gas and triggering of star formation, or if they fail tocompletely quench their star formation.

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