Massive Stars in the Arches Cluster

December 2002 • 2002ApJ...581..258F

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

Abstract • We present and use new spectra and narrowband images, along with previously published broadband 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 (W-R) stars; are some of the most massive stars known, having M_init>100M_solar and have prodigious winds, M>10^-5 M_solar yr^-1, that are enriched with helium and nitrogen; with these identifications, the Arches cluster contains about 5% of all known W-R stars in the Galaxy. We find an upper limit to the velocity dispersion of 22 km s^-1, implying an upper limit to the cluster mass of 7×10⁴ M_solar within a radius of 0.23 pc; we also estimate the bulk heliocentric velocity of the cluster to be v_{cluster,solar}~+95 km s^-1. Taken together, these results suggest that the Arches cluster was formed in a short, but massive, burst of star formation about 2.5+/-0.5 Myr ago, from a molecular cloud that is no longer present. The cluster happens to be approaching and ionizing the surface of a background molecular cloud, thus producing the thermal arched filaments. We estimate that the cluster produces 4×10⁵¹ ionizing photons s^-1, more than enough to account for the observed thermal radio flux from the nearby cloud, 3×10⁴⁹ ionizing photons s^-1. Commensurately, it produces 10^7.8 L_solar in total luminosity, providing the heating source for the nearby molecular cloud, L_cloud~10⁷ L_solar. These interactions between a cluster of hot stars and a wayward molecular cloud are similar to those seen in the ``Quintuplet/Sickle'' region. The small spread of formation times for the known young clusters in the Galactic center and the relative lack of intermediate-age stars (τ_age=10^7.0-10^7.3 yr) suggest that the Galactic center has recently been host to a burst of star formation. Finally, we have made new identifications of near-infrared sources that are counterparts to recently identified X-ray and radio sources. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.

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Harry Teplitz

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