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A model of the galaxy for star counts in the infrared

Published online by Cambridge University Press:  07 August 2017

R.P. Ortiz  and
J.R.D. Lépine
R.P. Ortiz
Affiliation:
Instituto Astronômico e Geofísico Universidade de SÃo Paulo P.O. Box 9638, CEP 01065 SÃo Paulo, Brazil
J.R.D. Lépine
Affiliation:
Instituto Astronômico e Geofísico Universidade de SÃo Paulo P.O. Box 9638, CEP 01065 SÃo Paulo, Brazil

Extract

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We constructed a model for the Galaxy to reproduce near-infrared (J, H, K, bands) and mid-infrared 12 and 25 micron IRAS bands source counts for a given direction and sensitivity of detection. The Galaxy is conceived as being formed by two populations: a disk, with different scale heights for each spectral type, and a de Vaucouleurs spheroid. The interstellar extinction is considered to be proportional to the amount of gas along the line of sight; both neutral (HI) and molecular (H2) components were taken into account, using the HI density distribution of Burton & Gordon (1978) and the CO density distribution of Sanders et al.(1984) and Gordon & Burton (1976).

Type
Poster Papers
Information
Symposium - International Astronomical Union , Volume 149: The Stellar populations of Galaxies , 1992 , pp. 465
Copyright
Copyright © Kluwer 

References

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