Absolute Proper Motion of the Canis Major Dwarf Galaxy Candidate

Details Absolute Proper Motion of the Canis Major Dwarf Galaxy Candidate Absolute Proper Motion of the Canis Major Dwarf Galaxy Candidate

2005-08-10

arxiv.org/abs/astro-ph/0508247v1

Astrophys.J.631:L49-L52,2005

Astronomy and Astrophysics

Astrophysics

12 pages, 3 figures, accepted for publication in ApJ Letters

Scientific paper

10.1086/497027

We have measured the absolute proper motion of the candidate Canis Major dwarf galaxy (CMa) at $(l,b) = (240\arcdeg, -8\arcdeg)$. Likely main-sequence stars in CMa have been selected from a region in the color-magnitude diagram that has very little contamination from known Milky Way components. We obtain $\mu_{l} cos b = -1.47 \pm 0.37$ and $\mu_{b} = -1.07 \pm 0.38$ mas yr$^{-1}$, on the ICRS system via Hipparcos stars. Together with the radial velocity of 109 km s$^{-1}$, and the assumed distance of 8 kpc, these results imply a space motion of $(\Pi, \Theta, W) = (-5 \pm 12, 188 \pm 10, -49 \pm 15)$ km s$^{-1}$. While CMa has in-plane rotation similar to the mean of thick disk stars, it shows significant $(3\sigma)$ motion perpendicular to the disk, and differs even more $(7\sigma)$ from that expected for the Galactic warp. The $W$ velocity lends support to the argument that the CMa overdensity is part of a satellite galaxy remnant.

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