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The evolution of compact massive quiescent and starforming galaxies derived from the Rₑ-Rₕ and Mₛₜₐᵣ-Mₕ relations
L. Zanisi, F. Shankar, H. Fu, A. Rodriguez-Puebla, V. Avila-Reese, A. Faisst, E. Daddi, L. Boco, A. Lapi, M. Giavalisco, P. Saracco, F. Buitrago, M. Huertas-Company, A. Puglisi, A. Dekel
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The mean size ( effective radius Rₑ) of Massive Galaxies (MGs, Mₛₜₐᵣ>10^(11.2)M_⊙) is observed to increase steadily with cosmic time. It is still unclear whether this trend originates from the size growth of individual galaxies (via, e.g., mergers and/or AGN feedback) or from the inclusion of larger galaxies entering the selection at later epochs (progenitor bias). We here build a data-driven, flexible theoretical framework to probe the structural evolution of MGs. We assign galaxies to dark matter haloes via stellar mass-halo mass (SMHM) relations with varying high-mass slopes and scatters σ_(SMHM) in stellar mass at fixed halo mass, and assign sizes to galaxies using an empirically-motivated, constant and linear relationship between Rₑ and the host dark matter halo radius Rₕ. We find that: 1) the fast mean size growth of MGs is well reproduced independently of the shape of the input SMHM relation; 2) the numbers of compact MGs grow steadily until z≳2 and fall off at lower redshifts, suggesting a lesser role of progenitor bias at later epochs; 3) a time-independent scatter σ_(SMHM) is consistent with a scenario in which compact starforming MGs transition into quiescent MGs in a few $10^8$yr with a negligible structural evolution during the compact phase, while a scatter increasing at high redshift implies significant size growth during the starforming phase. A robust measurement of the size function of MGs at high redshift can set strong constraints on the scatter of the SMHM relation and, by extension, on models of galaxy evolution.
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