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For refcode 2001AJ....121.1482B:
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Copyright by American Astronomical Society. Reproduced by permission
2001AJ....121.1482B THE M31 GLOBULAR CLUSTER LUMINOSITY FUNCTION PAULINE BARMBY AND JOHN P. HUCHRA Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; pbarmby@cfa.harvard.edu, huchra@cfa.harvard.edu AND JEAN P. BRODIE Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064; brodie@ucolick.org Received 2000 June 4; accepted 2000 November 28 ABSTRACT We combine our compilation of photometry of M31 globular clusters and probable cluster candidates with new near-infrared photometry for 30 objects. Using these data we determine the globular cluster luminosity function (GCLF) in multiple filters for the M31 halo clusters. We find a GCLF peak and dispersion V_0_^0^ = 16.84 +/- 0.11, {sigma}_t_ = 0.93 +/- 0.13 (Gaussian {sigma} = 1.20 +/- 0.14), consistent with previous results. The halo GCLF peak colors (e.g., B_0_^0^ - V_0_^0^) are consistent with the average cluster colors. We also measure V-band GCLF parameters for several other subsamples of the M31 globular cluster population. The inner third of the clusters have a GCLF peak significantly brighter than that of the outer clusters ({DELTA}V^0^ ~ 0.5 mag). Dividing the sample by both galactocentric distance and metallicity, we find that the GCLF also varies with metallicity, as the metal-poor clusters are on average 0.36 mag fainter than the metal-rich clusters. Our modeling of the catalog selection effects suggests that they are not the cause of the measured GCLF differences, but a more complete, less contaminated M31 cluster catalog is required for confirmation. Our results imply that dynamical destruction is not the only factor causing variation in the M31 GCLF: metallicity, age, and cluster initial mass function may also be important. Key words: galaxies: individual (M31)-galaxies: star clusters -globular clusters: general
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