TY - JOUR
T1 - GLOBULAR CLUSTER POPULATIONS
T2 - RESULTS INCLUDING S4G LATE-TYPE GALAXIES
AU - Zaritsky, Dennis
AU - McCabe, Kelsey
AU - Aravena, Manuel
AU - Athanassoula, E.
AU - Bosma, Albert
AU - Comerón, Sébastien
AU - Courtois, Helene M.
AU - Elmegreen, Bruce G.
AU - Elmegreen, Debra M.
AU - Erroz-Ferrer, Santiago
AU - Gadotti, Dimitri A.
AU - Hinz, Joannah L.
AU - Ho, Luis C.
AU - Holwerda, Benne
AU - Kim, Taehyun
AU - Knapen, Johan H.
AU - Laine, Jarkko
AU - Laurikainen, Eija
AU - Muñoz-Mateos, Juan Carlos
AU - Salo, Heikki
AU - Sheth, Kartik
N1 - Funding Information:
D.Z. acknowledges financial support from NASA ADAP NNX12AE27G. K.M. acknowledges support through a NASA Spacegrant undergraduate research fellowship. L.C.H. acknowledges support from the Kavli Foundation, Peking University, and the Chinese Academy of Science through grant No. XDB09030102 (Emergence of Cosmological Structures) from the Strategic Priority Research Program. J.H.K. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant number AYA2013-41243-P. K.Sheth, J.C. Mu?oz-Mateos, and T. Kim gratefully acknowledge support from the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. E.A. and A.B. acknowledge financial support from the CNES (Centre National d''Etudes Spatiales?France). We also acknowledge support from the People Programme (Marie Curie Actions) of the European Union''s Seventh Framework Programme FP7/ 2007-2013/ under REA grant agreement number PITN-GA-2011-289313 to the DAGAL network. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.
Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/2/10
Y1 - 2016/2/10
N2 - 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.
AB - 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.
KW - galaxies: evolution
KW - galaxies: star clusters: general
KW - galaxies: stellar content
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U2 - 10.3847/0004-637X/818/1/99
DO - 10.3847/0004-637X/818/1/99
M3 - Article
AN - SCOPUS:84959186426
VL - 818
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 99
ER -