| DOI | Resolve DOI: https://doi.org/10.1093/mnras/stt2139 |
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| Author | Search for: Bate, N. F.; Search for: Conn, A. R.; Search for: McMonigal, B.; Search for: Lewis, G. F.; Search for: Martin, N. F.; Search for: McConnachie, A. W.1; Search for: Veljanoski, J.; Search for: Mackey, A. D.; Search for: Ferguson, A. M. N.; Search for: Ibata, R. A.; Search for: Irwin, M. J.; Search for: Fardal, M.; Search for: Huxor, A. P.; Search for: Babul, A. |
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| Affiliation | - National Research Council of Canada. National Science Infrastructure
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| Format | Text, Article |
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| Abstract | We undertake the first detailed analysis of the stellar population and spatial properties of a diffuse substructure in the outer halo ofM31. The South-West Cloud lies at a projected distance of ̃100 kpc from the centre of M31 and extends for at least ̃50 kpc in projection. We use Pan-Andromeda Archaeological Survey photometry of red giant branch stars to determine a distance to the South-West Cloud of 793+45 -45 kpc. The metallicity of the cloud is found to be [Fe/H] = -1.3 ± 0.1. This is consistent with the coincident globular clusters PAndAS-7 and PAndAS-8, which have metallicities determined using an independent technique of [Fe/H] = -1.35 ± 0.15. We measure a brightness for the Cloud of MV = -12.1 mag; this is ̃75 per cent of the luminosity implied by the luminosity-metallicity relation. Under the assumption that the South-West Cloud is the visible remnant of an accreted dwarf satellite, this suggests that the progenitor object was amongst M31's brightest dwarf galaxies prior to disruption. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. |
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| Publication date | 2013-12-03 |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| NPARC number | 21270876 |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 33553aa1-0da0-4892-ad87-acfa99923670 |
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| Record created | 2014-02-17 |
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| Record modified | 2020-04-22 |
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