Quenched Fractions¶

In this analysis, we also look at the quenched fractions. For the 1-halo analysis, we look at the quenched fraction of satellites around their host central galaxy, as a function of group mass.

For the 2-halo analysis, we look at the quenched fraction of centrals around other centrals, as function of their projected distance, $r_{p}$ .

We perform this statistic on three galaxy properties, i.e. specific star formation rate (sSFR), Sersic index (n), and $(g-r)$ color.