2021/07/31 by Filip Huško, Cedric G. Lacey, Carlton M. Baugh · 1 citation
Physics and Astronomy · #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stab3324
Accepted for publication in MNRAS
arxiv created 2021/11/15 · arxiv updated 2021/12/17
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_*>1011.3-1010.5 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_*>1010 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 rmax1.32. 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.