Semi-theoretical density profiles for late-type giants along the galactic radius through the sun

Details Semi-theoretical density profiles for late-type giants along the galactic radius through the sun Semi-theoretical density profiles for late-type giants along the galactic radius through the sun

Feb 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26as...35..249s&link_type=abstract

Astronomy and Astrophysics Supplement Series, vol. 35, Feb. 1979, p. 249-251. Research supported by the Schweizerischer Nationa

Astronomy and Astrophysics

Astrophysics

1

Astronomical Photometry, Galactic Structure, Giant Stars, Late Stars, Star Distribution, Density Distribution, Milky Way Galaxy, Monte Carlo Method, Spirals

Scientific paper

An empirical (zero-dispersion) space-density function is derived for late-type giants in four low-latitude fields in the anticenter direction and one such field in the direction of the Galactic center. The combined empirical density function obtained is complete between 3 kpc in the direction of the Galactic center and 5.4 kpc in the anticenter direction. The density results are corrected for nonzero dispersion by a simple Monte Carlo calculation of semitheoretical density profiles on the basis of assumed Gaussian luminosity functions for dispersions of + or - 0.25, 0.5, and 1.0 mag. The density profile for a dispersion of + or - 0.5 mag indicates a monotonic space-density decrease in the anticenter direction, an apparent accumulation of giants between the sun and the inner edge of the -I spiral arm in the direction of the Galactic center, and a possible second increase in the space density of late-type giants beginning at about 3 kpc from the sun toward the Galactic center.

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