Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pkas....7..231k&link_type=abstract
Publications of the Korean Astronomical Society, vol.7, no.2, p.231-253
Astronomy and Astrophysics
Astronomy
Scientific paper
A model for the distribution of stars in the disk and the spheroid of our Galaxy is reexamined from an edge-on view of the Galaxy obtained by selecting infrared sources from the IRAS Point Source Catalog. The sources are counted as a function of galactic latitude, longitude, and 12 micron apparent magnitude. The source counts are reasonably separated into the disk component and the spheroid component contributions and each of the contributions is further interpreted as a convolution of a spatial density distribution and a luminosity function based on the least-square fit method. The spatial density of the disk component has an exponential radial scale length of hr ~ 2.6 kpc and the vertical distribution follows a canonical sech2 law with a scale height hz ~ 240 pc. The distribution of the spheroid component can be represented by an oblate spheroid with an axis ratio k ~ 0.61 and a de Vaucouleurs' r^1/4 law with an effective radius of Re ~ 120 pc. The steep density gradient of the spheroid component is consistent with that of late M giants in the central bulge. The luminosity functions of the disk and the spheroid component stars resemble respectively those of the K luminosity function of disk M giants (Garwood and Jones 1986) and the bolometric luminosity function of M giants in bulge fields(Frogel et al. 1990).
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