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The core of the Canis Major galaxy as traced by Red Clump stars | | M. Bellazzini
; R. Ibata
; N. Martin
; G.F. Lewis
; B. Conn
; M.J. Irwin
; | | Date: |
22 Apr 2005 | | Subject: | astro-ph | | Affiliation: | INAF-OA Bologna), R. Ibata (Obs. Strasbourg), N. Martin (Obs. Strasbourg), G.F. Lewis (Sidney Un.), B. Conn (Sidney Un.), M.J. Irwin (Cambridge Un. | | Abstract: | The recently-discovered stellar system in Canis Major is analysed using He-burning Red Clump stars as tracers. We find that the main body of the system has an integrated absolute magnitude M_V=-14.1 +/- 0.9, a central surface brightness mu_{V,0}=24.0 +/- 0.7 and a line-of-sight profile peaked at D_{sun}=7.2 +/- 1.0 kpc with Half Width at Half Maximum ~2.0 kpc, in excellent agreement with the results obtained with widely different tracers (M giants and Main Sequence stars) in previous analyses. The mean distance to the main body of Canis Major is observed to increase with increasing Galactic longitude, from D_{sun} = 6.3 kpc at l = 225 deg, to D_{sun} = 9.3 kpc at l = 265 deg, in good agreement with the predictions of our more recent N-body simulation that models CMa as a dwarf galaxy being accreted in a planar orbit onto the disc of the Milky Way. We confirm that the Canis Major system has all the characteristics of the relic of a dwarf galaxy seen in front of a large-scale overdensity that we detect all over the region of Galaxy considered in this study (220 deg <= l<= 320 deg, with a strong maximum around l=290 deg and b>= -5 deg) that is identified as the stellar component of the Galactic Warp. We also address a recent claim that Canis Major is on the outskirts of a larger ``Argo’’ structure centred at l = 290 deg. Our analysis shows that the stellar populations in the latter are distributed over a very large distance range along the line of sight, and do not give rise to a narrow peak in density in this direction, contrary to what is observed in Canis Major. This suggests that the Argo structure is likely due to Galactic asymmetries such as the Warp. | | Source: | arXiv, astro-ph/0504494 | | Services: | Forum | Review | PDF | Favorites | |
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