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Title: The kinematic identification of a thick stellar disc in M31
Authors: Chapman, S. C.
Irwin, M. J.
Ibata, R. A.
Rich, R. M.
Ferguson, A. M. N.
Lewis, G. F.
Tanvir, N.
Koch, A.
First Published: 21-May-2011
Publisher: Oxford University Press (OUP)
Citation: Monthly Notices of the Royal Astronomical Society , 2011, 413 (3), pp. 1548-1568
Abstract: 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[Superscript:−1]. The velocity dispersion of the thick disc is σthick= 50.8 ± 1.9 km s[Superscript:−1], greater than the value of dispersion we determine for the thin disc, σthin= 35.7 ± 1.0 km s[Superscript:−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 × 10[Superscript:10] < M[Subscript:*, thick] < 4.1 × 10[Superscript:10] M[Subscript:⊙]. 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.
DOI Link: 10.1111/j.1365-2966.2011.18238.x
ISSN: 0035-8711
eISSN: 1365-2966
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 the authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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