A Rich Satellite Population of the NGC 4437 Group and Implications of a Magnitude Gap for Galaxy Group Assembly History

Both observations and cosmological simulations have recently shown that there is a large scatter in the number of satellites of Milky Way (MW)-like galaxies. In this study, we investigate the relation between the satellite number and galaxy group assembly history using the r-band magnitude gap (Delta m (12)) between the brightest and second-brightest galaxies as an indicator. From 20 deg(2) of the Hyper Suprime-Cam Subaru Strategic Program Wide layer, we identify 17 dwarf satellite candidates around NGC 4437, a spiral galaxy with about one-fourth of the MW stellar mass. We estimate their distances using the surface brightness fluctuation method. Then we confirm five candidates as members of the NGC 4437 group, resulting in a total of seven group members. Combining the NGC 4437 group (with Delta m (12) = 2.5 mag) with other groups in the literature, we find a stratification of the satellite number by Delta m (12) for a given host stellar mass. The satellite number for the given host stellar mass decreases as Delta m (12) increases. The same trend is found in simulated galaxy groups in the TNG50 simulation of the IllustrisTNG project. We also find that the host galaxies in groups with a smaller Delta m (12) (like NGC 4437) have assembled their halo mass more recently than those in larger gap groups, and that their stellar-to-halo mass ratios increase as Delta m (12) increases. These results show that the large scatter in the satellite number is consistent with a large range of Delta m (12), indicating diverse group assembly histories.