Modeling Star counts in the Monoceros stream and the Galactic anti-centre

Details Modeling Star counts in the Monoceros stream and the Galactic anti-centre Modeling Star counts in the Monoceros stream and the Galactic anti-centre

2010-11-10

arxiv.org/abs/1011.2405v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

11 pages, 4 figures, accepted to be published in A&A

Scientific paper

There is a continued debate as to the form of the outer disc of the Milky Way galaxy, which has important implications for its formation. Stars are known to exist at a galacto-centric distance of at least 20 kpc. However, there is much debate as to whether these stars can be explained as being part of the disc or whether another extra galactic structure, the so called Monoceros ring/stream, is required. To examine the outer disc of the Galaxy toward the anti-centre to determine whether the star counts can be explained by the thin and thick discs alone. Using Sloan star counts and extracting the late F and early G dwarfs it is possible to directly determine the density of stars out to a galacto-centric distance of about 25 kpc. These are then compared with a simple flared disc model. A flared disc model is shown to reproduce the counts along the line of sights examined, if the thick disc does not have a sharp cut off. The flare starts at a Galacto-centric radius of 16 kpc and has a scale length of 4.5+/-1.5 kpc. Whilst the interpretation of the counts in terms of a ring/stream cannot be definitely discounted, it does not appear to be necessary, at least along the lines of sight examined towards the anti centre.

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