The spatial distribution of the LMC foreground stars.

Details The spatial distribution of the LMC foreground stars. The spatial distribution of the LMC foreground stars.

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...294...57o&link_type=abstract

Astronomy and Astrophysics 294, 57-64 (1995)

Astronomy and Astrophysics

Astrophysics

4

Galaxies: Magellanic Clouds, Galaxy: Structure, Galaxy: Abundances, Galaxy: Stellar Content

Scientific paper

Reddenings and distances of 1883 LMC foreground stars were recently derived by Oestreicher et al., taking into account metallicity effects. This large data sample allowed not only to derive a reddening map of high angular resolution, but also to calculate the distance distribution of the stars. With a scale height of (105+/-1)pc the early type stars are located in the galactic disc. A component of stars situated above the disc with a scale height of (417+/-57)pc is visible, too. So the first component belongs to old population I, the second to disc population I. The F stars of solar metallicity are also concentrated to the galactic plane, their scale height is (95+/-3)pc. When going to metal-poor stars, the scale height increases rapidly to (249+/-18)pc and (507+/-161)pc for mean metallicities of -0.6dex and -1.2dex, respectively. Thus these stars belong to disc population I or to intermediate population II. The scale height of the late type giants increases with decreasing metallicity, too. Values of (254+/-12)pc, (387+/-82)pc and (526+/-219)pc for mean metallicities of 0.0dex, -0.5dex and -1.1dex, respectively, imply, that these stars also belong to disc population I or to intermediate population II.

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