Bibcode
Zaritsky, D.; McCabe, Kelsey; Aravena, Manuel; Athanassoula, E.; Bosma, Albert; Comerón, Sébastien; Courtois, Helene M.; Elmegreen, Bruce G.; Elmegreen, Debra M.; Erroz-Ferrer, Santiago; Gadotti, Dimitri A.; Hinz, Joannah L.; Ho, Luis C.; Holwerda, Benne; Kim, Taehyun; Knapen, J. H.; Laine, Jarkko; Laurikainen, Eija; Muñoz-Mateos, Juan Carlos; Salo, Heikki; Sheth, Kartik
Referencia bibliográfica
The Astrophysical Journal, Volume 818, Issue 1, article id. 99, 11 pp. (2016).
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2
2016
Revista
Número de citas
8
Número de citas referidas
8
Descripción
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}ȯ
)\lt 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\lt
{log}({M}*/{M}ȯ )\lt 10.5 we find the
relationship can be satisfactorily described as
{T}{{N}}={({M}*/{10}6.7)}-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.