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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742503.0, MPI für Astronomie / Publikationen_mpia
A stellar overdensity associated with the Small Magellanic Cloud
Authors:Pieres, A.; Santiago, B. X.; Drlica-Wagner, A.; Bechtol, K.; Marel, R. P. v. d.; Besla, G.; Martin, N. F.; Belokurov, V.; Gallart, C.; Martinez-Delgado, D.; Marshall, J.; Nöel, N. E. D.; Majewski, S. R.; Cioni, M.-R.; 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. F.; Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Annis, J.; Benoit-Lévy, A.; Rosell, A. C.; Kind, M. C.; 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.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:Monthly Notices of the Royal Astronomical Society
Volume:468
Start Page:1349
End Page:1360
Audience:Not Specified
Abstract / Description:We report the discovery of a stellar overdensity 8° 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 ∼ 6° × 2°. It has an absolute magnitude of MV ≅ -7.7, rh = 2.1 kpc, and μV(r < rh) = 31.2 mag arcsec-2. We estimate a stellar mass of ∼105 M, 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 I 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.
Free Keywords:galaxies: interactions; Magellanic Clouds
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711
URL:http://adsabs.harvard.edu/abs/2017MNRAS.468.1349P
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