Simple dynamical models of the Sagittarius dwarf galaxy

dc.creatorHelmi, Amina
dc.creatorWhite, Simon David Manton
dc.date2001
dc.date2019-10-11T14:33:00Z
dc.identifierhttp://sedici.unlp.edu.ar/handle/10915/83148
dc.identifierissn:0035-8711
dc.descriptionWe present two simple dynamical models for Sagittarius based on N-body simulations of the progressive disruption of a satellite galaxy orbiting for 12.5 Gyr within a realistic Galactic potential. In both models the satellite initially has observable properties similar to those of current outlying dwarfs; in one case it is purely stellar while in the other it is embedded in an extended massive halo. The purely stellar progenitor is a King model with a total velocity dispersion of 18.9 km s<SUP>-1</SUP>, a core radius of 0.44 kpc and a tidal radius of 3 kpc. The initial stellar distribution in the other case follows a King profile with the same core radius, a slightly larger total velocity dispersion and similar extent. Both these models are consistent with all published data on the current Sagittarius system, they match not only the observed properties of the main body of Sagittarius, but also those reported for unbound debris at larger distances.
dc.descriptionFacultad de Ciencias Astronómicas y Geofísicas
dc.formatapplication/pdf
dc.format529-536
dc.languageen
dc.rightshttp://creativecommons.org/licenses/by-nc-sa/4.0/
dc.rightsCreative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.subjectCiencias Astronómicas
dc.subjectGalaxies: individual: Sagittarius dSph
dc.subjectGalaxies: interactions
dc.subjectGalaxy: halo
dc.subjectGalaxy: structure
dc.subjectLocal group
dc.titleSimple dynamical models of the Sagittarius dwarf galaxy
dc.typeArticulo
dc.typeArticulo


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