Volume 440, Number 2, September III 2005
|Page(s)||523 - 530|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||01 September 2005|
Constraints on the halo density profile using HI flaring in the outer Galaxy
Department of Physics, Indian Institute of Science, Bangalore 560012, India e-mail: firstname.lastname@example.org
Accepted: 3 June 2005
The observed flaring of HI disk in the outer region of galaxies has been used in the past to determine the shape of the dark matter halo. Previous studies based on this concept suggest a slightly oblate halo (axis ratio ~0.8) for our Galaxy. We reinvestigate this problem by calculating the HI scaleheight in the outer Galaxy to a larger radial distance, and by studying its dependence on the shape and the density profile of the halo. We find that a simple isothermal infinite halo of any shape- oblate or prolate, is not able to account for the observed flaring. Instead we show that a spherical halo with density falling faster than isothermal halo in the outer region provides a better fit to the observed HI flaring as well as the observed rotation curve of our Galaxy. These halos have about 95% of their mass within a few hundreds of kpc for kpc and km s-1, the central density and core radius can be constrained to the range pc-3 and kpc. Our claim for such “finite-sized” spherical halos is supported by recent literature on numerical simulation studies of halo formation as well as analyses of SDSS data.
Key words: galaxies: ISM / galaxies: kinematics and dynamics / galaxies: structure / galaxies: halos
© ESO, 2005
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