J/ApJ/818/99 Globular cluster populations in S4G galaxies. II. (Zaritsky+, 2016)
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., Sheth K.
<Astrophys. J., 818, 99 (2016)>
=2016ApJ...818...99Z 2016ApJ...818...99Z (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, IR ; Clusters, globular
Keywords: galaxies: evolution; galaxies: star clusters: general;
galaxies: stellar content
Abstract:
Using 3.6 and 4.5µm 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 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.
Description:
As in Paper I (Zaritsky+, 2015, J/ApJ/799/159), the parent sample is
the S4G sample, which currently consists of 2352 galaxies (Sheth et
al. 2010, J/PASP/122/1397). We provide and analyze images of these
galaxies obtained with the Spitzer Space Telescope and its Infrared
Array Camera (IRAC).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 57 73 Globular cluster population properties
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See also:
J/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)
J/ApJS/217/32 : S4G galaxy morphologies in the CVRHS system (Buta+, 2015)
J/MNRAS/447/1531 : HI data collection update (Courtois+, 2015)
J/ApJ/799/159 : Globular cluster pop. in S4G galaxies (Zaritsky+, 2015)
J/A+A/569/A91 : Optical imaging for S4G (Knapen+, 2014)
J/AJ/147/134 : Tully-Fisher relation for S4G galaxies (Zaritsky+, 2014)
J/ApJ/781/12 : Morphologies of galaxies from Spitzer (Holwerda+, 2014)
J/MNRAS/444/3015 : Morphologies of S4G galaxies (Laine+, 2014)
J/ApJ/772/135 : 3.6um surface brightness from S4G (Zaritsky+, 2013)
J/ApJ/772/82 : A catalog of globular cluster systems (Harris+, 2013)
J/MNRAS/428/389 : SLUGGS globular clusters in early-type gal. (Pota+, 2013)
J/AJ/143/87 : IRAC photometry of massive M31 GCs (Barmby+, 2012)
J/MNRAS/414/2005 : Cosmic flows observations (Courtois+, 2011)
J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Gal. (Sheth+, 2010)
J/AJ/139/1871 : Kinematics of globulars in NGC 5128 (Woodley+, 2010)
J/AJ/105/1762 : Globular clusters around NGC 1399 (Ostrov+ 1993)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Galaxy name
13- 17 F5.2 mag DM [30.1/32.4] Galaxy distance modulus
19- 20 I2 --- TT [-1/10] Galaxy T-Type (1)
22- 25 F4.1 mag [3.6] [9.9/17.3] Spitzer/IRAC 3.6um apparent
AB magnitude (2)
27- 30 F4.1 mag [4.5] [10.3/17.5] Spitzer/IRAC 4.5um apparent
AB magnitude (2)
32- 34 I3 --- N50 [2/684] Number of clusters within 50kpc (3)
36- 39 I4 10-9Msun TN [0/4433] Specific cluster frequency
per mass (4)
41- 44 I4 10-9Msun e_TN [0/1549] Downward uncertainty on TN
46- 49 I4 10-9Msun E_TN [5/1969] Upward uncertainty on TN
51- 55 F5.2 [pc-2] Back [-6/-4.2] Logarithm of background level (5)
57 I1 --- Q Quality flag (1=good; 0=poor) (6)
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Note (1): From the compilation of Buta et al. (2015, J/ApJS/217/32).
Note (2): As measured by Munoz-Mateos et al. (2015ApJS..219....3M 2015ApJS..219....3M).
Note (3): Derived from best fit model of fixed power-law slope.
Intended to represent total number of clusters.
Note (4): The specific frequency relative to the galaxy's stellar mass (TN)
corresponding to N50 in units of number per 109M☉ (as
introduced by Zepf & Ashman 1993MNRAS.264..611Z 1993MNRAS.264..611Z)
Note (5): Clusters per projected area.
Note (6): Defined by whether the data extend sufficiently over the radial
range of interest to provide a robust constraint on the fitted models.
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History:
From electronic version of the journal
References:
Zaritsky et al. Paper I. 2015ApJ...799..159Z 2015ApJ...799..159Z Cat. J/ApJ/799/159
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 29-Apr-2016