Taehyun Kim, Kartik Sheth, et al.
ApJ
Using 3.6 and 4.5 μm images of 73 late-type, edge-on galaxies from the S4G survey, we compare the richness of the globular cluster populations of these galaxies to those of early-type galaxies that we measured previously. In general, the galaxies presented here fill in the distribution for galaxies with lower stellar mass, M∗, specifically log(M∗/M⊙, overlap the results for early-type galaxies of similar masses, and, by doing so, strengthen the case for a dependence of the number of globular clusters per 109M⊙ of galaxy stellar mass, TN, on M∗. For 8.5 < log(M∗/M⊙ < 10.5 we find the relationship can be satisfactorily described as TN=(M∗/106.7)-0.56 when M∗ is expressed in solar masses. The functional form of the relationship is only weakly constrained, and extrapolation outside this range is not advised. Our late-type galaxies, in contrast to our early types, do not show the tendency for low-mass galaxies to split into two TN families. Using these results and a galaxy stellar mass function from the literature, we calculate that, in a volume-limited, local universe sample, clusters are most likely to be found around fairly massive galaxies (M∗ ∼ 1010.8M⊙) and present a fitting function for the volume number density of clusters as a function of parent-galaxy stellar mass. We find no correlation between TN and large-scale environment, but we do find a tendency for galaxies of fixed M∗ to have larger TN if they have converted a larger proportion of their baryons into stars.
Taehyun Kim, Kartik Sheth, et al.
ApJ
Bonita De Swardt, Kartik Sheth, et al.
ApJ
Dennis Zaritsky, Heikki Salo, et al.
ApJ
Mauricio Cisternas, Dimitri A. Gadotti, et al.
ApJ