The M31 Globular Cluster Luminosity Function

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dc.creatorBarmby, P.
dc.creatorHuchra, J. P.
dc.creatorBrodie, J. P.
dc.date2000-11-28
dc.date.accessioned2026-07-07T06:18:55Z
dc.date.available2026-07-07T06:18:55Z
dc.descriptionWe combine our compilation of photometry of M31 globular cluster 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 of 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 brigher than that of the outer clusters (delta V =~ 0.5mag). Dividing the sample by both galacticentric 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 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.
dc.descriptionAJ, in press. 36 pages, including 7 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0011522
dc.identifierhttp://arxiv.org/abs/astro-ph/0011522
dc.identifierAstrophys.J. 121 (2001) 1482
dc.identifierdoi:10.1086/319389
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/94899
dc.subjectAstrophysics
dc.titleThe M31 Globular Cluster Luminosity Function
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