Satellites around MW analogs from SAGA II

We use archival GALEX UV imaging as a star formation indicator for the SAGA-II sample and derive star formation rates (SFRs) to compare with those from APOSTLE and Auriga. We compare our detection rates from the NUV and FUV bands to the SAGA-II H{alpha} detections and find that they are broadly consistent with over 85% of observed satellites detected in all three tracers.

We apply the same spatial selection criteria used around SAGA-II hosts to select satellites around the MW-like hosts in APOSTLE and Auriga. We find very good overall agreement in the derived SFRs for the star-forming satellites as well as the number of star-forming satellites per host in observed and simulated samples. However, the number and fraction of quenched satellites in the SAGA-II sample are significantly lower than those in APOSTLE and Auriga below a stellar mass of M_*_~10^8^M_{sun}_, even when the SAGA-II incompleteness and interloper corrections are included.