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    A spatial characterization of the sagittarius dwarf galaxy tidal tails

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    Genre
    Journal Article
    Date
    2013-06-01
    Author
    Newby, M
    Cole, N
    Newberg, HJ
    Desell, T
    Magdon-Ismail, M
    Szymanski, B
    Varela, C
    Willett, B
    Yanny, B
    Subject
    catalogs
    Galaxy: halo
    Galaxy: structure
    methods: data analysis
    methods: statistical
    Permanent link to this record
    http://hdl.handle.net/20.500.12613/5960
    
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    DOI
    10.1088/0004-6256/145/6/163
    Abstract
    We measure the spatial density of F turnoff stars in the Sagittarius dwarf tidal stream, from Sloan Digital Sky Survey data, using statistical photometric parallax. We find a set of continuous, consistent parameters that describe the leading Sgr stream's position, direction, and width for 15 stripes in the north Galactic cap, and three stripes in the south Galactic cap. We produce a catalog of stars that has the density characteristics of the dominant leading Sgr tidal stream that can be compared with simulations. We find that the width of the leading (north) tidal tail is consistent with recent triaxial and axisymmetric halo model simulations. The density along the stream is roughly consistent with common disruption models in the north, but possibly not in the south. We explore the possibility that one or more of the dominant Sgr streams has been misidentified, and that one or more of the "bifurcated" pieces is the real Sgr tidal tail, but we do not reach definite conclusions. If two dwarf progenitors are assumed, fits to the planes of the dominant and "bifurcated" tidal tails favor an association of the Sgr dwarf spheroidal galaxy with the dominant southern stream and the " bifurcated" stream in the north. In the north Galactic cap, the best fit Hernquist density profile for the smooth component of the stellar halo is oblate, with a flattening parameter q = 0.53, and a scale length of r 0 = 6.73. The southern data for both the tidal debris and the smooth component of the stellar halo do not match the model fits to the north, although the stellar halo is still overwhelmingly oblate. Finally, we verify that we can reproduce the parameter fits on the asynchronous MilkyWay@home volunteer computing platform. © 2013. The American Astronomical Society. All rights reserved.
    Citation to related work
    American Astronomical Society
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    Astronomical Journal
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    ae974a485f413a2113503eed53cd6c53
    http://dx.doi.org/10.34944/dspace/5942
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