Testing population synthesis models with globular cluster colors
| dc.creator | Barmby, Pauline | |
| dc.creator | Huchra, John P. | |
| dc.date | 2000-01-06 | |
| dc.date.accessioned | 2026-07-07T06:18:54Z | |
| dc.date.available | 2026-07-07T06:18:54Z | |
| dc.description | We have measured an extensive set of UBVRIJHK colors for M31 globular clusters [Barmby et al. 2000]. We compare the predicted simple stellar population colors of three population synthesis models to the intrinsic colors of Galactic and M31 globular clusters. The best-fitting models fit the cluster colors very well -- the weighted mean color offsets are all < 0.05 mag. The most significant offsets between model and data are in the U and B passbands; these are not unexpected and are likely due to problems with the spectral libraries used by the models. The metal-rich clusters ([Fe/H] > -0.8) are best fit by young (8 Gyr) models, while the metal-poor clusters are best fit by older (12--16 Gyr) models. If this range of globular cluster ages is correct, it implies that conditions for cluster formation must have existed for a substantial fraction of the galaxies' lifetimes. | |
| dc.description | To appear in ApJ Letters; 8 pages including 3 figures and 1 table | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0001087 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0001087 | |
| dc.identifier | Astrophys.J. 531 (2000) L29 | |
| dc.identifier | doi:10.1086/312511 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/94898 | |
| dc.subject | Astrophysics | |
| dc.title | Testing population synthesis models with globular cluster colors | |
| dc.type | text |