Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-25T10:57:40.512Z Has data issue: false hasContentIssue false
  • English
  • Français

Analysis of HST CMDs of 15 intermediate-age LMC clusters: self-consistent physical parameters and 3D distribution

Published online by Cambridge University Press:  01 December 2006

L. O. Kerber ,
B. X. Santiago  and
E. Brocato
L. O. Kerber
Affiliation:
IAG/USP, São Paulo, Brazil email: [email protected]
B. X. Santiago
Affiliation:
IF/UFRGS, Porto Alegre, Brazil
E. Brocato
Affiliation:
INAF-OAC, Teramo, Italy
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We analysed HST/WFPC2 colour-magnitude diagrams (CMDs) from 15 populous Large Magellanic Cloud (LMC) stellar clusters with ages between ∼0.3 Gyr and ∼3 Gyr. These (V, B-V) CMDs are photometrically homogeneous and reach typically V ∼22. Accurate and self-consistent physical parameters (age, metallicity, distance modulus and reddening) were extracted for each cluster by comparing the observed CMDs with synthetic ones. These determinations were made by means of simultaneous statistical comparison of MS fiducial lines and red clump position, offering objective and robust criteria to determine the best models. In general, the best models show a satisfactory fit to the data, adequately constraining the physical parameters of each cluster. The inferred spatial distribution of these clusters is roughly aligned with the LMC disk. The set of ages and metallicities homogeneously derived here can be used to calibrate integrated light studies applied to distant galaxies.

Keywords

galaxies: star clustersMagellanic CloudsHertzsprung-Russell diagram
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S241: Stellar Populations as Building Blocks of Galaxies , December 2006 , pp. 353 - 354
Copyright
Copyright © International Astronomical Union 2007

References

Brocato, E., Di, Carlo, E. & Menna, G. 2001, A&A, 374, 523Google Scholar
Geisler, D., Bica, E., Dottori, H. et al. , 1997, AJ, 114, 1920CrossRefGoogle Scholar
Grocholski, A.J., Cole, A.A., Sarajedini, A., Geisler, D. & Smith, V.V. 2006, AJ, 132, 1630CrossRefGoogle Scholar
Kerber, L., Santiago, B. & Brocato, E., 2007, A&A, 462, 139Google Scholar
Nikolaev, S., Drake, A.J., Keller, S.C. et al. , 2004, ApJ, 601, 260CrossRefGoogle Scholar
Olszewski, E.W., Schommer, R.A., Suntzeff, N.B. & Harris, H. 1991, AJ, 101, 515CrossRefGoogle Scholar
Olszewski, E.W., Suntzeff, N.B. & Mateo, M. 1996, ARA&A, 34, 511Google Scholar