Number Density Distribution of Satellite Galaxies around Massive Central Galaxies in CLAUDS + HSC at 0:3 < z < 0:9
Speaker: Mr. Lingjian Chen (SMU)
Time: August 19, 2019 - 1:00 PM
Location: Atrium 305
Satellite galaxies around massive central galaxies can provide important information forenvironmental effect of galaxy evolution in groups or clusters. In this paper, we selected thousands of massive (log(Mcen) > 11.15) central galaxies using 20 square degree deep (iAB = 27) imaging data from Subaru-HSCSSP and CFHT-CLAUDS at 0.3 < z < 0.9 and investigated radial number density distribution of the satellite galaxies around them with appropriate corrections applied. We found that the number density of satellites can be described by the NFW profile at large projected radii from central but deviate from it in inner regions (within 100 kpc). We also found that redshift evolution of number density enhances number density in inner regions more significantly than outer regions. We found that central mass does not have a strong effect on slope of radial distribution of satellites, only the total number of satellites is different for different central masses. Galaxy conformity signal was found when separating star-forming and quiescent centrals. By dividing the satellite galaxy sample, we found that low massive satellite galaxies (9.5 < log(Msat) < 10.2) have more significant deviation from the NFW profile in inner regions than high mass satellites (log(Msat) > 10.2). Additionally, we compared our satellite distribution with IllustrisTNG simulation. Our results support the satellite population formation scenario in which the specific shape of the distribution is related to migration
of satellites, which involves various environmental effects such as dynamical friction and the tidal stripping.