We obtained new UBV photometry and spectroscopy of Blue Plume ( BP ) stars near the center of the Canis Major Over-Density ( CMa ) .
We combined analyses of color-color diagrams with a new comparison of the hydrogen Balmer-line profile to the reddening-free Q parameter to improve the reddening and extinction estimates for this low-latitude , differentially reddened , area of the sky .
Results of our stellar parameter analysis for B/A spectral type stars associated with the BP show that the majority of the stars have main-sequence surface gravities placing them at an average heliocentric distance of < D > = 6.0 \pm 2.7 kpc .
This distance is more consistent with membership in the intervening Perseus spiral arm and strongly suggests that the BP stars are not associated with the other stellar populations previously reported to make up the CMa .
This result casts serious doubt on the proposed dwarf galaxy origin for the CMa .