The quenching time and timescale distribution of z~2 quiescent galaxies from precise colour distribution analysis

Understanding when and how galaxies quench their star formation is crucial for understanding the dominant physical processes at play. The spectral energy distribution (SED) of galaxies encodes significant information on their past histories: the relative importance of different physical processes influences the observed distribution of SED shapes in the galaxy population. We use a simulation based inference (SBI) approach to directly constrain the distribution of formation times, quenching times and quenching timescales within the massive galaxy population at \(z \gtrsim 2\) from their broad band photometric colour distribution at \(1.7<z<2\). We demonstrate that a simple distribution of double power-law star formation histories accurately fits the distribution of SED shapes of galaxies with \(\log_{10}(M^*/M_\odot)>10.3\). We measure a quenched galaxy fraction of \(0.24\pm0.02\), with the number density of quenched galaxies rising rapidly 2.5,Gyr after the Big Bang (\(z\lesssim2.6\)). Galaxies must quench rapidly to achieve the precise bimodal colour distribution: defining the quenching timescale as the time from peak star formation rate (\({\rm SFR_{peak}}\)) to \(0.5\,{\rm SFR_{peak}}\), the quenching timescale distribution has a mode at \(97_{-25}^{+31}\),Myr, a median of \(182\pm16\),Myr and a tail to \(\sim700\),Myr. To achieve full quiescence takes a median time of \(\sim400\),Myr. Comparing to direct number density measurements of quenched galaxies at \(z>2\) the combination of recent and rapid quenching inferred from the fossil record suggests a substantial rejuvenation and/or merger rate for quenched galaxies observed directly at \(z>3.5\).