Astrophys. J., 799, 159 (2015/February-1)
Globular cluster populations: first results from S4G early-type galaxies.
ZARITSKY D., ARAVENA M., ATHANASSOULA E., BOSMA A., COMERON S., ELMEGREEN B.G., ERROZ-FERRER S., GADOTTI D.A., HINZ J.L., HO L.C., HOLWERDA B., KNAPEN J.H., LAINE J., LAURIKAINEN E., MUNOZ-MATEOS J.C., SALO H. and SHETH K.
Abstract (from CDS):
Using 3.6 µm images of 97 early-type galaxies, we develop and verify methodology to measure globular cluster populations from the S4G survey images. We find that (1) the ratio, TN, of the number of clusters, NCL, to parent galaxy stellar mass, M*, rises weakly with M* for early-type galaxies with M*> 1010 M☉when we calculate galaxy masses using a universal stellar initial mass function (IMF) but that the dependence of TNon M*is removed entirely once we correct for the recently uncovered systematic variation of IMF with M*; and (2) for M*< 1010 M☉, there is no trend between NCLand M*, the scatter in TNis significantly larger (approaching two orders of magnitude), and there is evidence to support a previous, independent suggestion of two families of galaxies. The behavior of NCLin the lower-mass systems is more difficult to measure because these systems are inherently cluster-poor, but our results may add to previous evidence that large variations in cluster formation and destruction efficiencies are to be found among low-mass galaxies. The average fraction of stellar mass in clusters is ∼0.0014 for M*> 1010 M☉ and can be as large as ∼0.02 for less massive galaxies. These are the first results from the S4G sample of galaxies and will be enhanced by the sample of early-type galaxies now being added to S4G and complemented by the study of later-type galaxies within S4G.
galaxies: evolution - galaxies: formation - galaxies: star clusters: general - galaxies: stellar content
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<Available at CDS (J/ApJ/799/159): table1.dat>
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