Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/26462
Title: The kinematic footprints of five stellar streams in Andromeda's halo
Authors: Chapman, S. C.
Irwin, M.
Collins, M.
Trethewey, D.
McConnachie, A.
Peñarrubia, J.
Ibata, R.
Koch, A.
Rich, R. M.
Letarte, B.
Martin, N.
Lewis, G. F.
Ferguson, A.
Huxor, A.
Tanvir, N.
First Published: 11-Nov-2008
Publisher: Royal Astronomical Society (RAS)
Citation: Monthly Notices of the Royal Astronomical Society, 2008, 390 (4), pp. 1437-1452
Abstract: We present a spectroscopic analysis of five stellar streams (‘A’, ‘B’, ‘Cr’, ‘Cp’ and ‘D’) as well as the extended star cluster, EC4, which lies within Stream ‘C’, all discovered in the halo of M31 from our Canada–France–Hawaii Telescope/MegaCam survey. These spectroscopic results were initially serendipitous, making use of our existing observations from the DEep Imaging Multi-Object Spectrograph mounted on the Keck II telescope, and thereby emphasizing the ubiquity of tidal streams that account for ∼70 per cent of the M31 halo stars in the targeted fields. Subsequent spectroscopy was then procured in Stream ‘C’ and Stream ‘D’ to trace the velocity gradient along the streams. Nine metal-rich ([Fe/H]∼−0.7) stars at vhel=−349.5 km s−1, σv,corr∼ 5.1 ± 2.5 km s−1 are proposed as a serendipitous detection of Stream ‘Cr’, with follow-up kinematic identification at a further point along the stream. Seven metal-poor ([Fe/H]∼−1.3) stars confined to a narrow, 15 km s−1 velocity bin centred at vhel=−285.6, σv,corr= 4.3+1.7−1.4 km s−1 represent a kinematic detection of Stream ‘Cp’, again with follow-up kinematic identification further along the stream. For the cluster EC4, candidate member stars with average [Fe/H]∼−1.4, are found at vhel=−282 suggesting it could be related to Stream ‘Cp’. No similarly obvious cold kinematic candidate is found for Stream ‘D’, although candidates are proposed in both of two spectroscopic pointings along the stream (both at ∼−400 km s−1). Spectroscopy near the edge of Stream ‘B’ suggests a likely kinematic detection at vhel∼−330, σv,corr∼ 6.9 km s−1, while a candidate kinematic detection of Stream ‘A’ is found (plausibly associated to M33 rather than M31) with vhel∼−170, σv,corr= 12.5 km s−1. The low dispersion of the streams in kinematics, physical thickness and metallicity makes it hard to reconcile with a scenario whereby these stream structures as an ensemble are related to the giant southern stream. We conclude that the M31 stellar halo is largely made up of multiple kinematically cold streams.
DOI Link: 10.1111/j.1365-2966.2008.13703.x
ISSN: 0035-8711
eISSN: 1365-2966
Links: http://hdl.handle.net/2381/26462
http://mnras.oxfordjournals.org/content/390/4/1437
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 ©: 2008 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

Files in This Item:
File Description SizeFormat 
MNRAS-2008-Chapman-1437-52.pdfPublished (publisher PDF) 4.57 MBAdobe PDFView/Open


Items in LRA are protected by copyright, with all rights reserved, unless otherwise indicated.