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Title:
The orbital motion of the Arches cluster — clues on cluster formation near the galactic center
Authors:
Stolte, Andrea; Ghez, Andrea M.; Morris, Mark R.; Lu, Jessica R.; Brandner, Wolfgang; Matthews, Keith
Affiliation:
AA(UCLA, 430 Portola Plaza, Los Angeles, CA 90095-1547, USA ; 1. Physikalisches Institut, Universität Köln, Zülpicher Str. 77, 50937 Köln, Germany ), AB(UCLA, 430 Portola Plaza, Los Angeles, CA 90095-1547, USA ; Institute of Geophysics and Planetary Physics, UCLA, Los Angeles, CA 90095 ), AC(UCLA, 430 Portola Plaza, Los Angeles, CA 90095-1547, USA ), AD(UCLA, 430 Portola Plaza, Los Angeles, CA 90095-1547, USA ), AE(MPIA, Königstuhl 17, 69117 Heidelberg, Germany ), AF(Caltech Optical Observatories, California Institute of Technology, MS 320-47, Pasadena, CA 91225)
Publication:
Journal of Physics: Conference Series, Volume 131, Proceedings of "The Universe Under the Microscope - Astrophysics at High Angular Resolution", held 21-25 April 2008, in Bad Honnef, Germany. Editors: Rainer Schoedel, Andreas Eckart, Susanne Pfalzner and Eduardo Ros, pp. 012015 (2008).
Publication Date:
10/2008
Origin:
IOP
DOI:
10.1088/1742-6596/131/1/012015
Bibliographic Code:
2008JPhCS.131a2015S

Abstract

The Arches cluster is one of the most massive, young clusters in the Milky Way. Located inside the central molecular zone in the inner 200 pc of the Galactic center, it formed in one of the most extreme star-forming environments in the present-day Galaxy. Its young age of only 2.5 Myr allows us to observe the cluster despite the strong tidal shear forces in the inner Galaxy. The orbit of the cluster determines its dynamical evolution, tidal stripping, and hence its fate. We have measured the proper motion of the Arches cluster relative to the ambient field from Keck/NIRC2 LGS-AO and VLT/NAOS-CONICA NGS-AO observations taken 4.3 years earlier. When combined with the radial velocity, we derive a 3D space motion of 232 ± 30 km/s for the Arches. This motion is exceptionally large when compared to molecular cloud orbits in the GC, and places stringent constraints on the formation scenarios for starburst clusters in dense, nuclear environments.
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