Astrophys. J., 818, 99 (2016/February-2)
Globular cluster populations: results including S4G late-type galaxies.
ZARITSKY D., McCABE K., ARAVENA M., ATHANASSOULA E., BOSMA A., COMERON S., COURTOIS H.M., ELMEGREEN B.G., ELMEGREEN D.M., ERROZ-FERRER S., GADOTTI D.A., HINZ J.L., HO L.C., HOLWERDA B., KIM T., KNAPEN J.H., LAINE J., LAURIKAINEN E., MUNOZ-MATEOS J.C., SALO H. and SHETH K.
Abstract (from CDS):
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_☉ < 10, 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 TNfamilies. 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 TNif they have converted a larger proportion of their baryons into stars.
galaxies: evolution - galaxies: star clusters: general - galaxies: stellar content
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<Available at CDS (J/ApJ/818/99): table1.dat>
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