STAR CLUSTERS IN M31: OLD CLUSTERS WITH BAR KINEMATICS

Journal Article · Sat Jan 01 00:00:00 EST 2011 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/726/1/L9· OSTI ID:21560588

Morrison, Heather; Harding, Paul ^[1]; Caldwell, Nelson ^[2]; Schiavon, Ricardo P ^[3]; Athanassoula, E ^[4]

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1. Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106-7215 (United States)
2. Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
3. Gemini Observatory, 670 N. A'ohoku Place, Hilo, HI 96720 (United States)
4. LAM/OAMP, UMR6110, CNRS/Univ. de Provence, 38 rue Joliot Curie, 13388 Marseille 13 (France)

We analyze our accurate kinematical data for the old clusters in the inner regions of M31. These velocities are based on high signal-to-noise Hectospec data. The data are well suited for analysis of M31's inner regions because we took particular care to correct for contamination by unresolved field stars from the disk and bulge in the fibers. The metal-poor clusters show kinematics that are compatible with a pressure-supported spheroid. The kinematics of metal-rich clusters, however, argue for a disk population. In particular the innermost region (inside 2 kpc) shows the kinematics of the x{sub 2} family of bar periodic orbits, arguing for the existence of an inner Lindblad resonance in M31.

• OSTI ID: 21560588
• Journal Information: Astrophysical Journal Letters, Vol. 726, Issue 1; Other Information: DOI: 10.1088/2041-8205/726/1/L9; ISSN 2041-8205
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
GALAXIES
STAR CLUSTERS
VELOCITY