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A stellar overdensity associated with the Small Magellanic Cloud

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A stellar overdensity associated with the Small Magellanic Cloud

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Título A stellar overdensity associated with the Small Magellanic Cloud
Autor Pieres, Adriano
Santiago, Basilio Xavier
Drlica-Wagner, Alex
Bechtol, Keith
Marel, Roeland Paul van der
Besla, Gurtina
Martin, Nicolas F.
Belokurov, Vasily
Gallart, Carme
Martínez-Delgado, David
Marshall, Jennifer L.
Nöel, N. E. D.
Majewski, Steven Raymond
Cioni, Maria-Rosa L.
Li, T. S.
Hartley, William
Luque Canaza, Elmer Fidel
Conn, Blair Campbell
Walker, Alistair
Balbinot, Eduardo
Stringfellow, Guy S.
Olsen, Knut A. G.
Nidever, D.L.
Costa, Luiz N. da
Ogando, Ricardo L.C.
Maia, Marcio Antonio Geimba
Fausti Neto, Angelo
Abbott, Timothy M. C.
Abdalla, Filipe B.
Allam, Sahar S.
Annis, James T.
Benoit-Lévy, Aurélien
Carnero Rosell, Aurelio
Carrasco Kind, Matías
Carretero Palacios, Jorge
Cunha, Carlos Eduardo
D'Andrea, Christopher B.
Desai, S.
Diehl, H. Thomas
Doel, Peter
Flaugher, Brenna
Fosalba Vela, Pablo
García-Bellido, Juan
Gruen, Daniel
Gruendl, Robert A.
Gschwend, Julia de Figueiredo
Gutierrez, Gaston R.
Honscheid, K.
James, David J.
Kuehn, Kyler
Kuropatkin, Nikolay P.
Menanteau, Felipe
Miquel, Ramon
Plazas Malagón, Andrés Alejandro
Romer, Anita K.
Sako, Mari
Sanchez-Alvaro, Eusebio
Scarpine, Victor Emanuel
Schubnell, Michael
Sevilla Noarbe, Ignacio
Smith, Robert Christopher
Soares-Santos, Marcelle
Sobreira, Flávia
Suchyta, Eric
Swanson, Molly E. C.
Tarle, Gregory
Tucker, Douglas L.
Wester, William Carl
Abstract 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 theMAGellanic 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 HI 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.
Contido em Monthly notices of the Royal Astronomical Society. Oxford. Vol. 468, no. 2 (June 2017), p. 1349-1360
Assunto Formacao de estrelas
Mapeamentos astronômicos
Pequena Nuvem de Magalhães
[en] Galaxies: interactions
[en] Magellanic Clouds
Origem Estrangeiro
Tipo Artigo de periódico
URI http://hdl.handle.net/10183/169027
Arquivos Descrição Formato
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