Major Merging History in CANDELS. I. Evolution of the Incidence of Massive Galaxy-Galaxy Pairs from z=3 to z~0

Abstract

The rate of major galaxy-galaxy merging is theoretically predicted to steadily increase with redshift during the peak epoch of massive galaxy development ($1\le z\le 3$). We use close-pair statistics to objectively study the incidence of massive galaxies (stellar $M_1\ge 2\times 10^{10}{M}_{\odot }$) hosting major companions ($1\le M_1/M_2\le 4$; i.e., $<$4:1) at six epochs spanning $0<z<3$. We select companions from a nearly complete, mass-limited ($\ge 5\times 10^9{M}_{\odot }$) sample of 23,696 galaxies in the five CANDELS fields and the SDSS. Using $5-50$ kpc projected separation and close redshift proximity criteria, we find that the major companion fraction $f_{\mathrm{mc}}(z)$ based on stellar mass-ratio (MR) selection increases from 6% ($z\sim 0$) to 16% ($z\sim 0.8$), then turns over at $z\sim 1$ and decreases to 7% ($z\sim 3$). Instead, if we use a major F160W flux ratio (FR) selection, we find that $f_{\mathrm{mc}}(z)$ increases steadily until $z=3$ owing to increasing contamination from minor (MR$>$4:1) companions at $z>1$. We show that these evolutionary trends are statistically robust to changes in companion proximity. We find disagreements between published results are resolved when selection criteria are closely matched. If we compute merger rates using constant fraction-to-rate conversion factors ($C_{\mathrm{merg},\mathrm{pair}}=0.6$ and $T_{\mathrm{obs},\mathrm{pair}}=0.65\mathrm{Gyr}$), we find that MR rates disagree with theoretical predictions at $z>1.5$. Instead, if we use an evolving $T_{\mathrm{obs},\mathrm{pair}}(z)\propto (1+z{)}^{-2}$ from Snyder et al., our MR-based rates agree with theory at $0<z<3$. Our analysis underscores the need for detailed calibration of $C_{\mathrm{merg},\mathrm{pair}}$ and $T_{\mathrm{obs},\mathrm{pair}}$ as a function of redshift, mass and companion selection criteria to better constrain the empirical major merger history.

27 pages, 15 figures, 5 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society Main Journal

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