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arXiv · astro-ph/0208145

Massive Stars in the Arches Cluster

Donald F. Figer·Francisco Najarro·Diane Gilmore·Mark Morris·Sungsoo S. Kim·Eugene Serabyn·Ian S. McLean·Andrea M. Gilbert·James R. Graham·James E. Larkin·N. A. Levenson·Harry I. Teplitz
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Abstract

We present and use new spectra and narrow-band images, along with previously published broad-band images, of stars in the Arches cluster to extract photometry, astrometry, equivalent width, and velocity information. The data are interpreted with a wind/atmosphere code to determine stellar temperatures, luminosities, mass-loss rates, and abundances. We have doubled the number of known emission-line stars, and we have also made the first spectroscopic identification of the main sequence for any population in the Galactic Center. We conclude that the most massive stars are bona-fide Wolf-Rayet (WR) stars and are some of the most massive stars known, having M_{initial} > 100 Msun, and prodigious winds, Mdot > 10^{-5} Msun yr^{-1}, that are enriched with helium and nitrogen; with these identifications, the Arches cluster contains about 5% of all known WR stars in the Galaxy. We find an upper limit to the velocity dispersion of 22 kms^{-1}, implying an upper limit to the cluster mass of 7(10^4) Msun within a radius of 0.23 pc; we also estimate the bulk heliocentric velocity of the cluster to be v_{cluster,odot} approximately +95 kms^{-1}.

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Donald F. Figer, Francisco Najarro, Diane Gilmore, Mark Morris, Sungsoo S. Kim, Eugene Serabyn, Ian S. McLean, Andrea M. Gilbert, James R. Graham, James E. Larkin, N. A. Levenson, Harry I. Teplitz. 2002-08-07. Massive Stars in the Arches Cluster. https://doi.org/10.1086/344154

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