Statistics of galaxy mergers: bridging the gap between theory and observation

TL;DR

This study uses cosmological simulations and semi-analytical models to analyze galaxy merger statistics up to redshift 10, revealing discrepancies with other models and observations, and providing new fitting formulas for merger timescales.

Contribution

It offers the first comprehensive analysis of galaxy merger rates and close pair fractions up to high redshift, including new fitting formulas for merger timescales and detailed comparisons with observations.

Findings

Merger rates decline rapidly for high-mass galaxies at low redshift.

Predicted merger rates increase then turn over with redshift, conflicting with some models.

Close pair fractions depend on maximum projected separation as r_max^1.32.

Abstract

We present a study of galaxy mergers up to $z=10$ using the Planck Millennium cosmological dark matter simulation and the {\tt GALFORM} semi-analytical model of galaxy formation. Utilising the full ($800$ Mpc)$^3$ volume of the simulation, we studied the statistics of galaxy mergers in terms of merger rates and close pair fractions. We predict that merger rates begin to drop rapidly for high-mass galaxies ($M_*>10^{11.3}-10^{10.5}$ $M_\odot$ for $z=0-4$), as a result of the exponential decline in the galaxy stellar mass function. The predicted merger rates increase and then turn over with increasing redshift, by $z=3.5$, in disagreement with hydrodynamical simulations and semi-empirical models. In agreement with most other models and observations, we find that close pair fractions flatten or turn over at some redshift (dependent on the mass selection). We conduct an extensive comparison of close pair fractions, and highlight inconsistencies among models, but also between different observations. We provide a fitting formula for the major merger timescale for close galaxy pairs, in which the slope of the stellar mass dependence is redshift dependent. This is in disagreement with previous theoretical results that implied a constant slope. Instead we find a weak redshift dependence only for massive galaxies ($M_*>10^{10}$ M$_\odot$): in this case the merger timescale varies approximately as $M_*^{-0.55}$. We find that close pair fractions and merger timescales depend on the maximum projected separation as $r_\mathrm{max}^{1.32}$. This is in agreement with observations of small-scale clustering of galaxies, but is at odds with the linear dependence on projected separation that is often assumed.