Modeling the Milky Way in the infrared

Details Modeling the Milky Way in the infrared Modeling the Milky Way in the infrared

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pasp...99..453g&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 99, June 1987, p. 453-460. NASA-supported research.

Astronomy and Astrophysics

Astronomy

48

Astronomical Models, Galactic Structure, Infrared Astronomy, Milky Way Galaxy, Star Distribution, Infrared Astronomy Satellite, Solar Neighborhood

Scientific paper

The spatial distribution of stars in the Milky Way is modeled using an exponential disk with the addition of a de Vaucouleurs spheroid. The model is compared to 2 - 2.5 μm star counts and surface-brightness data and to IRAS 12 μm source counts. With an R1/4spheroid and R0/Re ≡ 3, the model fits the data inside 10° from the Galactic center fairly well but is too extended in latitude, suggesting the bulge is flattened by approximately 4:1. Extrapolation of this bulge component to the solar neighborhood yields a local spheroid-to-disk population ratio of 1:150, well above the accepted value. Comparison of the model with IRAS 12 μm source counts was limited by the uncertainty in the stellar population sampled at 12 μm by IRAS. However, the data are consistent with a flattened bulge.

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