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dc.contributor.authorSimon, Josh D.pt_BR
dc.contributor.authorLi, T. S.pt_BR
dc.contributor.authorDrlica-Wagner, Alexpt_BR
dc.contributor.authorBechtol, Keithpt_BR
dc.contributor.authorMarshall, Jennifer L.pt_BR
dc.contributor.authorJames, David J.pt_BR
dc.contributor.authorWang, M.pt_BR
dc.contributor.authorStrigari, Louis E.pt_BR
dc.contributor.authorBalbinot, Eduardopt_BR
dc.contributor.authorKuehn, Kylerpt_BR
dc.contributor.authorWalker, Alistairpt_BR
dc.contributor.authorAbbott, Timothy M. C.pt_BR
dc.contributor.authorAllam, Sahar S.pt_BR
dc.contributor.authorAnnis, James T.pt_BR
dc.contributor.authorBenoit-Lévy, Aurélienpt_BR
dc.contributor.authorBrooks, D.pt_BR
dc.contributor.authorBuckley-Geer, Elizabethpt_BR
dc.contributor.authorBurke, David Lylept_BR
dc.contributor.authorCarnero Rosell, Aureliopt_BR
dc.contributor.authorCarrasco Kind, Matíaspt_BR
dc.contributor.authorCarretero Palacios, Jorgept_BR
dc.contributor.authorCunha, Carlos Eduardopt_BR
dc.contributor.authorD'Andrea, Christopher B.pt_BR
dc.contributor.authorCosta, Luiz N. dapt_BR
dc.contributor.authorDePoy, Darren L.pt_BR
dc.contributor.authorDesai, S.pt_BR
dc.contributor.authorDoel, Peterpt_BR
dc.contributor.authorFernandez, Enriquept_BR
dc.contributor.authorFlaugher, Brennapt_BR
dc.contributor.authorFrieman, Joshua A.pt_BR
dc.contributor.authorGarcía-Bellido, Juanpt_BR
dc.contributor.authorGaztañaga, Enriquept_BR
dc.contributor.authorGoldstein, Daniel Abrahampt_BR
dc.contributor.authorGruen, Danielpt_BR
dc.contributor.authorGutierrez, Gaston R.pt_BR
dc.contributor.authorKuropatkin, Nikolay P.pt_BR
dc.contributor.authorMaia, Marcio Antonio Geimbapt_BR
dc.contributor.authorMartini, Paulpt_BR
dc.contributor.authorMenanteau, Felipept_BR
dc.contributor.authorMiller, Christopher J.pt_BR
dc.contributor.authorMiquel, Ramonpt_BR
dc.contributor.authorNeilsen, Eric H.pt_BR
dc.contributor.authorNord, Brian Dennispt_BR
dc.contributor.authorOgando, Ricardo L.C.pt_BR
dc.contributor.authorPlazas Malagón, Andrés Alejandropt_BR
dc.contributor.authorRomer, Anita K.pt_BR
dc.contributor.authorRykoff, Elipt_BR
dc.contributor.authorSanchez-Alvaro, Eusebiopt_BR
dc.contributor.authorSantiago, Basilio Xavierpt_BR
dc.contributor.authorScarpine, Victor Emanuelpt_BR
dc.contributor.authorSchubnell, Michaelpt_BR
dc.contributor.authorSevilla Noarbe, Ignaciopt_BR
dc.contributor.authorSmith, Robert Christopherpt_BR
dc.contributor.authorSobreira, Fláviapt_BR
dc.contributor.authorSuchyta, Ericpt_BR
dc.contributor.authorSwanson, Molly E. C.pt_BR
dc.contributor.authorTarle, Gregorypt_BR
dc.contributor.authorWhiteway, L.pt_BR
dc.contributor.authorYanny, Brianpt_BR
dc.contributor.authorDES Collaborationpt_BR
dc.date.accessioned2017-10-20T02:26:24Zpt_BR
dc.date.issued2017pt_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.urihttp://hdl.handle.net/10183/169601pt_BR
dc.description.abstractWe present Magellan/IMACS spectroscopy of the recently discovered Milky Way satellite TucanaIII (Tuc III). We identify 26 member stars in TucIII from which we measure a mean radial velocity of vhel=−102.3±0.4 (stat.)±2.0(sys.) km s-1, a velocity dispersion of - 0.1+0.1 0.7 km s-1, and a mean metallicity of = - - [Fe/H] 2.42+0.08 0.07. The upper limit on the velocity dispersion is σ<1.5 km s-1 at 95.5%confidence, and the corresponding upper limit on the mass within the half-light radius of TucIII is 9.0×104Me. We cannot rule out mass-to-light ratios as large as 240Me/Le for TucIII, but much lower mass-to-light ratios that would leave the system baryon-dominated are also allowed. We measure an upper limit on the metallicity spread of the stars in TucIII of 0.19dex at 95.5% confidence. TucIII has a smaller metallicity dispersion and likely a smaller velocity dispersion than any known dwarf galaxy, but a larger size and lower surface brightness than any known globular cluster. Its metallicity is also much lower than those of the clusters with similar luminosity. We therefore tentatively suggest that TucIII is the tidally stripped remnant of a dark matter-dominated dwarf galaxy, but additional precise velocity and metallicity measurements will be necessary for a definitive classification. If TucIII is indeed a dwarf galaxy, it is one of the closest external galaxies to the Sun. Because of its proximity, the most luminous stars in TucIII are quite bright, including one star at V=15.7 that is the brightest known member star of an ultra-faint satellite.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofThe astrophysical journal. Bristol. Vol. 838, no. 1 (Mar. 2017), 11, 14 p.pt_BR
dc.rightsOpen Accessen
dc.subjectDark matteren
dc.subjectGaláxiaspt_BR
dc.subjectMatéria escurapt_BR
dc.subjectGalaxies: dwarfen
dc.subjectGalaxies: individual (Tucana III)en
dc.subjectComposicao estelarpt_BR
dc.subjectMetalicidadept_BR
dc.subjectGalaxies: stellar contenten
dc.subjectLocal groupen
dc.subjectVia lácteapt_BR
dc.subjectStars: abundancesen
dc.titleNearest neighbor : the low-mass Milky Way satellite Tucana IIIpt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb001044743pt_BR
dc.type.originEstrangeiropt_BR


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