Can dry merging explain the size evolution of early-type galaxies?
C. Nipoti (1), T. Treu (2), M.W. Auger (2), A.S. Bolton (3) ((1), Bologna University, (2) UCSB, (3) IfA/Hawaii)

TL;DR
This study uses N-body simulations to evaluate if dry mergers can explain the observed size growth of early-type galaxies, finding that they are insufficient unless extreme fine tuning occurs.
Contribution
It demonstrates that dry mergers alone cannot account for the size evolution of early-type galaxies without fine tuning, challenging previous explanations.
Findings
Dry mergers increase galaxy size and velocity dispersion with stellar mass as M^(1.09) and M^(0.07).
Dry mergers cannot fully explain the observed size evolution of ETGs.
Present-day ETGs likely assembled less than 45% of their mass via dry mergers.
Abstract
The characteristic size of early-type galaxies (ETGs) of given stellar mass is observed to increase significantly with cosmic time, from redshift z>2 to the present. A popular explanation for this size evolution is that ETGs grow through dissipationless ("dry") mergers, thus becoming less compact. Combining N-body simulations with up-to-date scaling relations of local ETGs, we show that such an explanation is problematic, because dry mergers do not decrease the galaxy stellar-mass surface-density enough to explain the observed size evolution, and also introduce substantial scatter in the scaling relations. Based on our set of simulations, we estimate that major and minor dry mergers increase half-light radius and projected velocity dispersion with stellar mass (M) as M^(1.09+/-0.29) and M^(0.07+/-0.11), respectively. This implies that: 1) if the high-z ETGs are indeed as dense as…
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