The quenching time and timescale distribution of z 2 quiescent galaxies from precise colour distribution analysis
astro-ph.GA
Submitted: 2026-06-04
Updated: 2026-09-09
Comments: Published in the Open Journal of Astrophysics. Bayesian Analysis of Galaxy PopUlations with Spectra (BAGPUS) code is available at https://github.com/SEDMORPH/bagpus
Code: https://github.com/SEDMORPH/bagpus
Project page: https://sbi-dev.github.io/sbi/v0.23.3
License: http://creativecommons.org/licenses/by/4.0/
The gist: Understanding when and how galaxies quench their star formation is crucial for understanding the dominant physical processes at play.
Terminology
Abstract
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 > 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 log10(M*/Msol)>10.3. We measure a quenched galaxy fraction of 0.24+/-0.02, with the number density of quenched galaxies rising rapidly 2.5Gyr after the Big Bang (z< 2.6). Galaxies must quench rapidly to achieve the precise bimodal colour distribution: defining the quenching timescale as the time from peak star formation rate (SFR peak) -> 0.5xSFR peak, the quenching timescale distribution has a mode at 97-25+31Myr, a median of 182+/-16Myr and a tail to 700Myr. To achieve full quiescence takes a median time of 400Myr. 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.
Sources
- DeepDive: Tracing the early quenching pathways of massive quiescent galaxies at $z>3$ from their star-formation histories and chemical abundances
- PANORAMIC: The Dawn of Massive Quiescent Galaxies I. Number Density and Cosmic Variance from 1000 arcmin squared NIRCam Imaging
- Spatially resolved star-formation histories of local post-starburst galaxies: Starburst and quenching spatial patterns consistent with recent mergers
- Winding Back the Clock: Recent Star Formation Histories of Massive Quiescent Galaxies Are Consistent With Their Rapid Number Density Evolution Since $\mathbf{z\sim7}$
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