An Investigation of the Canis Major Over-Density

Details An Investigation of the Canis Major Over-Density An Investigation of the Canis Major Over-Density

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.1401p&link_type=abstract

American Astronomical Society, AAS Meeting #211, #14.01; Bulletin of the American Astronomical Society, Vol. 39, p.759

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Using 2MASS colors, Martin et al. (2004) uncovered evidence for a remnant dwarf galaxy in Canis Major, in the form of an over-density of M-giant stars. The spatial distribution of the M-giants indicate an extended, and likely disrupted, group of stars extending over roughly 30 degrees of the sky. Alternative explanations of the origin of this over-density invoke the warp of the Galactic disk or other sub-structure of the Milky Way (Momany et al. (2004, 2006), Lopez-Corredoira (2006)). We present new color-magnitude diagrams for various fields near the center of the over-density, obtained at McDonald Observatory and Cerro Tololo Inter-American Observatory. We also obtained spectra at McDonald Observatory of a preliminary sample of blue plume stars selected from the photometry. I present kinematic results.

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