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Detailed Properties of Populous Clusters in the Large Magellanic Cloud

Citation

Grocholski, AJ and Sarajedini, A and Cole, AA and Geisler, D and Olsen, KAG and Tiede, GP and Smith, VV and Mancone, CL, Detailed Properties of Populous Clusters in the Large Magellanic Cloud, Stellar Populations as Building Blocks of Galaxies, 10-16 December, 2006, La Palma, Spain, pp. 227-230. ISBN 0521863503 (2006) [Non Refereed Conference Paper]

Abstract

We present results from a series of projects aimed at better understanding the ages, velocities, metallicities, and distances of populous clusters in the LMC. Using FORS2 on the VLT, we obtained near-infrared spectra for more than 200 stars in 28 LMC clusters, which span a large range of ages and metallicities. The strong absorption lines of the Ca II triplet are used to calculate cluster velocities and abundances. We determine cluster ages through main sequence fitting of theoretical isochrones to deep optical photometry using a combination of published photometry, VLT FORS2 images and archival HST WFPC2 images. As shown by Grocholski & Sarajedini, a cluster¡¯s age and [Fe/H] can be used to predict the K-band luminosity of core helium burning red clump (RC) stars in that cluster. Using ISPI on the CTIO 4m telescope, we imaged 17 LMC clusters in the J− and K−bands, with the resulting photometry reaching ¡­0.5 mag below the RC. We combine the measured apparent RC magnitudes with the predicted absolute values to determine absolute distances to each of these clusters and thereby probe the structure of the LMC as traced by its intermediate-age clusters.

Item Details

Item Type:Non Refereed Conference Paper
Keywords:galaxies: star clusters, Magellanic Clouds, stars: distances, stars: abundances
Research Division:Physical Sciences
Research Group:Astronomical and Space Sciences
Research Field:Galactic Astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding Knowledge
Objective Field:Expanding Knowledge in the Physical Sciences
Author:Cole, AA (Dr Andrew Cole)
ID Code:71108
Year Published:2006
Deposited By:Physics
Deposited On:2011-07-07
Last Modified:2011-07-07
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