Number density distribution of satellite galaxies around massive central galaxies in CLAUDS + HSC at 0.3 < z < 0.9

Abstract

Satellite galaxies around massive central galaxies can provide important information about galactic environmental effect. In this thesis, we selected thousands of massive (log(M_cen/M_☉) &gt; 11.15) central galaxies using wide and deep imaging data at 0.3 &lt; z &lt; 0.9 and investigated radial number density distribution of the satellites. The distribution of satellites can be described by the NFW profile at large projected radii but deviates from it in inner regions (within &sim;100 kpc). We found that low-massive satellite galaxies (9.5 &lt; log(M_sat/M_☉) &lt; 10.2) have more significant deviation from the NFW than high-mass (log(M_sat/M_☉) &gt; 10.2). For central galaxy dependence, we found galaxy conformity signal and that the number of satellites increases with central mass. Redshift evolution enhances number density in inner regions more significantly than in outer regions. We propose that shape of the satellite distribution is related to migration, involving effects such as dynamical friction and tidal stripping. We compared our results with the IllustrisTNG simulation.