The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.
The kinematic identification of a thick stellar disc in M31
Article first published online: 1 MAR 2011
© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS
Monthly Notices of the Royal Astronomical Society
Volume 413, Issue 3, pages 1548–1568, May 2011
How to Cite
Collins, M. L. M., Chapman, S. C., Ibata, R. A., Irwin, M. J., Rich, R. M., Ferguson, A. M. N., Lewis, G. F., Tanvir, N. and Koch, A. (2011), The kinematic identification of a thick stellar disc in M31. Monthly Notices of the Royal Astronomical Society, 413: 1548–1568. doi: 10.1111/j.1365-2966.2011.18238.x
Based on observations obtained with MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii.
- Issue published online: 11 MAY 2011
- Article first published online: 1 MAR 2011
- Accepted 2010 December 17. Received 2010 December 17; in original form 2010 October 25
- stars: kinematics and dynamics;
- galaxies: abundances;
- galaxies: evolution;
- Local Group;
- galaxies: spiral;
- galaxies: structure
We present the first characterization of a thick-disc component in the Andromeda galaxy (M31) using kinematic data from the DEIMOS instrument on Keck II. Using 21 fields in the south-west of the galaxy, we measure the lag of this component with respect to the thin disc, as well as the dispersion, metallicity and scalelength of the component. We find an average lag between the two components of 〈Δv〉= 46.0 ± 3.9 km s−1. The velocity dispersion of the thick disc is σthick= 50.8 ± 1.9 km s−1, greater than the value of dispersion we determine for the thin disc, σthin= 35.7 ± 1.0 km s−1. The thick disc is more metal poor than the thin disc, with [Fe/H]spec=−1.0 ± 0.1 compared with [Fe/H]spec=−0.7 ± 0.05 for the thin disc. We measure a radial scalelength of the thin and thick discs of hr= 7.3 ± 1.0 and 8.0 ± 1.2 kpc, respectively. From this, we infer scaleheights for both discs of 1.1 ± 0.2 and 2.8 ± 0.6 kpc, both of which are approximately two to three times larger than those observed in the Milky Way. We estimate a mass range for the thick-disc component of 2.4 × 1010 < M*, thick < 4.1 × 1010 M⊙. This value provides a useful constraint on possible formation mechanisms, as any proposed method for forming a thick disc must be able to heat (or deposit) at least this amount of material.