The galactic spheroid

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Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...265..730b&link_type=abstract

Astrophysical Journal, Part 1, vol. 265, Feb. 15, 1983, p. 730-747.

Astronomy and Astrophysics

Astrophysics

204

Galactic Structure, Milky Way Galaxy, Spheroids, Star Distribution, Astronomical Photometry, Galactic Rotation, Stellar Luminosity

Scientific paper

Analytic approximations and numerical simulations are used to derive the characteristic behavior of star counts in a galactic spheroidal population, whose visible stars' stellar luminosity function is obtainable for galactocentric distances between about 4 and 12 kpc from star count observations above 30 deg galactic latitude. The total densities of stars and of mass in the spheroid at the solar position are evaluated using different assumed luminosity functions, in order to extrapolate the measured values to a wider range of absolute magnitudes. The upper limits to the frequency of intermediate population stars are derived for the absolute visual magnitude range of 5-8. If such stars occur in either a flat disk with a scale height of 3 kpc or a spheroid with an ellipticity of 0.5, their local surface density is less than 1.8 times that of the spheroid.

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