The Proper Motion of the Arches Cluster: Cluster Membership and Understanding the Origin of Massive Young Clusters near the Galactic Center

Details The Proper Motion of the Arches Cluster: Cluster Membership and Understanding the Origin of Massive Young Clusters near the Galactic Center The Proper Motion of the Arches Cluster: Cluster Membership and Understanding the Origin of Massive Young Clusters near the Galactic Center

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...20925406s&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #254.06; Bulletin of the American Astronomical Society,

Physics

Optics

Scientific paper

High-precision astrometry achieved with current AO systems, and in particular with laser guide star assisted adaptive optics (LGS-AO) enables proper motion studies of distant star clusters in great detail. We present data of the Arches cluster, which is in close projected distance to the Galatic Center (GC). We compare observations obtained with Keck/NIRC2 LGS-AO with natural guide star VLT/NAOS-CONICA data of the starburst cluster taken 4 years earlier. On the 4 year baseline, we observe a mean relative motion of the Arches cluster of 6 +/- 2 mas/yr with respect to the bulge field population. The uncertainty of 2 mas is dominated by the centroiding uncertainties of the natural guide star observations. While previous determinations of the stellar mass function were limited to statistical field subtraction, which is difficult due to the large variation of the stellar background population and extinction towards the Galactic center, we are now able to distinguish cluster members individually on the basis of their proper motion. In this contribution, we present the proper motion result of the Arches cluster. The large relative motion of the cluster with respect to its immediate environment suggests that the Arches has not formed locally where it is observed today.

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