We continue our empirical study of the emission line flux originating in the cool (T ∼ 104 K) gas that populates the halos of galaxies and their environments. Specifically, we present results obtained for a sample of nearly half a million individual galaxies, groups, and clusters of galaxies, intersected by more than two million SDSS lines of sight at projected separations of up to a quarter of the virial radius. Adopting simple power law relationships between the circumgalactic (CGM) cool gas fraction and either the halo or stellar mass, we present expressions for the CGM cool gas fraction as a function of either halo or stellar mass, fcool(Mh) = (0.25+0−0..0706) × (Mh/1012M)(−0.39+0 −0 . . 06 07) or fcool(M∗) = (0.28+0−0..0706) × (M∗/1010.0M)(−0.33±0.06). Where we can compare, our results are consistent with previous constraints from absorption line studies, our own previous emission line work, and simulations. The cool gas can be the dominant baryonic CGM component, comprising a fraction as high as > 90% of halo gaseous baryons, in low mass halos, Mh ∼ 1010.5M, and a minor fraction, < 5%, in groups and clusters, Mh > 1014M.
|Original language||English (US)|
|State||Published - Nov 5 2019|
ASJC Scopus subject areas