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The LMC geometry and outer stellar populations from early DES data

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The LMC geometry and outer stellar populations from early DES data

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Título The LMC geometry and outer stellar populations from early DES data
Autor Balbinot, Eduardo
Santiago, Basilio Xavier
Girardi, Leo Alberto
Pieres, Adriano
Costa, Luiz N. da
Maia, Marcio Antonio Geimba
Gruendl, Robert A.
Walker, Alistair
Yanny, Brian
Drlica-Wagner, Alex
Benoit-Lévy, Aurélien
Abbott, Timothy M. C.
Allam, Sahar S.
Annis, James T.
Bernstein, Joseph P.
Bernstein, Rebecca A.
Bertin, Emmanuel
Brooks, D.
Buckley-Geer, Elizabeth
Carnero Rosell, Aurelio
Cunha, Carlos Eduardo
DePoy, Darren L.
Desai, S.
Diehl, H. Thomas
Doel, Peter
Estrada, Juan
Evrard, August E.
Fausti Neto, Angelo
Finley, David A.
Flaugher, Brenna
Frieman, Joshua A.
Gruen, Daniel
Honscheid, K.
James, David J.
Kuehn, Kyler
Kuropatkin, Nikolay P.
Lahav, Ofer
March, Marisa Cristina
Marshall, Jennifer L.
Miller, Christopher J.
Miquel, Ramon
Ogando, Ricardo L.C.
Peoples, John
Plazas Malagón, Andrés Alejandro
Scarpine, Victor Emanuel
Schubnell, Michael
Sevilla Noarbe, Ignacio
Smith, Robert Christopher
Soares-Santos, Marcelle
Suchyta, Eric
Swanson, Molly E. C.
Tarle, Gregory
Tucker, Douglas L.
Wechsler, Risa H.
Zuntz, J.
Abstract The Dark Energy Camera has captured a large set of images as part of Science Verification (SV) for the Dark Energy Survey (DES). The SV footprint covers a large portion of the outer LargeMagellanic Cloud (LMC), providing photometry 1.5 mag fainter than the main sequence turn-off of the oldest LMC stellar population.We derive geometrical and structural parameters for various stellar populations in the LMC disc. For the distribution of all LMC stars, we find an inclination of i = −38. ◦ 14 ± 0. ◦ 08 (near side in the north) and a position angle for the line of nodes of θ0 = 129. ◦ 51 ± 0. ◦ 17. We find that stars younger than ∼4 Gyr are more centrally concentrated than older stars. Fitting a projected exponential disc shows that the scale radius of the old populations is R>4 Gyr = 1.41 ± 0.01 kpc, while the younger population has R<4 Gyr = 0.72 ± 0.01 kpc. However, the spatial distribution of the younger population deviates significantly from the projected exponential disc model. The distribution of old stars suggests a large truncation radius of Rt = 13.5 ± 0.8 kpc. If this truncation is dominated by the tidal field of the Galaxy, we find that the LMC is 24+9 −6 times less massive than the encircled Galactic mass. By measuring the Red Clump peak magnitude and comparing with the best-fitting LMC disc model, we find that the LMC disc is warped and thicker in the outer regions north of the LMC centre. Our findings may either be interpreted as a warped and flared disc in the LMC outskirts, or as evidence of a spheroidal halo component.
Contido em Monthly notices of the Royal Astronomical Society. Oxford. Vol. 449, no. 1 (May 2015), p. 1129-1145
Assunto Grande Nuvem de Magalhães
Mapeamentos astronômicos
[en] Galaxies: stellar content
[en] Magellanic clouds
[en] Stars: statistics
Origem Estrangeiro
Tipo Artigo de periódico
URI http://hdl.handle.net/10183/126981
Arquivos Descrição Formato
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