Constraints on Quenching of Z ≲ 2 Massive Galaxies from the Evolution of the Average Sizes of Star-forming and Quenched Populations in COSMOS

April 2017 • 2017ApJ...839...71F

Authors • Faisst, A. L. • Carollo, C. M. • Capak, P. L. • Tacchella, S. • Renzini, A. • Ilbert, O. • McCracken, H. J. • Scoville, N. Z.

Abstract • We use >9400 {log}(m/{M}_⊙ )> 10 quiescent and star-forming galaxies at z ≲ 2 in COSMOS/UltraVISTA to study the average size evolution of these systems, with focus on the rare ultra-massive population at {log}(m/{M}_⊙ )> 11.4. The large 2 square degree survey area delivers a sample of ∼400 such ultra-massive systems. Accurate sizes are derived using a calibration based on high-resolution images from the Hubble Space Telescope. We find that at these very high masses, the size evolution of star-forming and quiescent galaxies is almost indistinguishable in terms of normalization and power-law slope. We use this result to investigate possible pathways of quenching massive m > M* galaxies at z < 2. We consistently model the size evolution of quiescent galaxies from the star-forming population by assuming different simple models for the suppression of star formation. These models include an instantaneous and delayed quenching without altering the structure of galaxies and a central starburst followed by compaction. We find that instantaneous quenching reproduces the observed mass-size relation of massive galaxies at z > 1 well. Our starburst+compaction model followed by individual growth of the galaxies by minor mergers is preferred over other models without structural change for {log}(m/{M}_⊙ )> 11.0 galaxies at z > 0.5. None of our models is able to meet the observations at m > M* and z < 1 without significant contribution of post-quenching growth of individual galaxies via mergers. We conclude that quenching is a fast process in galaxies with m ≥ 10¹¹ M _⊙, and that major mergers likely play a major role in the final steps of their evolution.

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• SIMBAD http://simbad.u-strasbg.fr/simbo.pl?bibcode=2017ApJ...839...71F
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• PREPRINT http://arxiv.org/abs/1703.09234
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• ELECTR https://doi.org/10.3847%2F1538-4357%2Faa697a