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Author
Pieres, A.Santiago, B. X.
Drlica-Wagner, A.
Bechtol, K.
Marel, R. P. van der
Besla, G.
Martin, N. F.
Belokurov, V.
Gallart, C.
Martinez-Delgado, D.
Marshall, J.
Nöel, N. E. D.
Majewski, Steven R.
Cioni, M.-R. L.
Li, T. S.
Hartley, W.
Luque, E.
Conn, B. C.
Walker, A. R.
Balbinot, E.
Stringfellow, G. S.
Olsen, K. A. G.
Nidever, D.
da Costa, L. N.
Ogando, R.
Maia, M.
Neto, A. Fausti
Abbott, T. M. C.
Abdalla, F. B.
Allam, S.
Annis, J.
Benoit-Lévy, A.
Rosell, A. Carnero
Kind, M. Carrasco
Carretero, J.
Cunha, C. E.
D'Andrea, C. B.
Desai, S.
Diehl, H. T.
Doel, P.
Flaugher, B.
Fosalba, P.
García-Bellido, J.
Gruen, D.
Gruendl, R. A.
Gschwend, J.
Gutierrez, G.
Honscheid, K.
James, D.
Kuehn, K.
Kuropatkin, N.
Menanteau, F.
Miquel, R.
Plazas, A. A.
Romer, A. K.
Sako, M.
Sanchez, E.
Scarpine, V.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Tucker, D. L.
Wester, W.
Affiliation
Univ Arizona, Steward ObservIssue Date
2017-06
Metadata
Show full item recordPublisher
OXFORD UNIV PRESSCitation
A stellar overdensity associated with the Small Magellanic Cloud 2017, 468 (2):1349 Monthly Notices of the Royal Astronomical SocietyRights
© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We report the discovery of a stellar overdensity 8 degrees north of the centre of the Small Magellanic Cloud (SMC; Small Magellanic Cloud Northern Over-Density; SMCNOD), using data from the first 2 yr of the Dark Energy Survey (DES) and the first year of the MAGellanic SatelLITEs Survey (MagLiteS). The SMCNOD is indistinguishable in age, metallicity and distance from the nearby SMC stars, being primarily composed of intermediate-age stars (6 Gyr, Z=0.001), with a small fraction of young stars (1 Gyr, Z=0.01). The SMCNOD has an elongated shape with an ellipticity of 0.6 and a size of similar to 6 degrees x 2 degrees. It has an absolute magnitude of M-V congruent to -7.7, r(h) = 2.1 kpc, and mu v(r < r(h)) = 31.2 mag arcsec(-2). We estimate a stellar mass of similar to 10(5) M-circle dot, following a Kroupa mass function. The SMCNOD was probably removed from the SMC disc by tidal stripping, since it is located near the head of the Magellanic Stream, and the literature indicates likely recent Large Magellanic Cloud-SMC encounters. This scenario is supported by the lack of significant H-1 gas. Other potential scenarios for the SMCNOD origin are a transient overdensity within the SMC tidal radius or a primordial SMC satellite in advanced stage of disruption.ISSN
0035-87111365-2966
Version
Final published versionSponsors
European Research Council [ERC-StG-335936]; Sonderforschungsbereich 'The Milky Way System' of the German Research Foundation (DFB) [(SFB) 881]; US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the DESae974a485f413a2113503eed53cd6c53
10.1093/mnras/stx507