Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....95...46i&link_type=abstract
Astronomy and Astrophysics, vol. 95, no. 1, Feb. 1981, p. 46-53.
Astronomy and Astrophysics
Astrophysics
15
Astronomical Models, Galactic Bulge, Galactic Nuclei, Galactic Rotation, Galactic Structure, Mass Distribution, Planetary Nebulae, Dynamic Stability, Gravitational Fields, Mass Ratios, Power Series
Scientific paper
Three groups of bulge mass models are examined against the distribution of galactic center planetary nebulae. It is assumed that the nebulae have no systematic orbital motion and a velocity dispersion of 134 km/sec. The power law density distribution and thickened disk models (order 0 and 2) give consistent results for the mass of the bulge at (1.1 + or - 0.2) 10 to the 10th solar masses for the inner kiloparsec. The power law models suggest a density exponent in the range 1.8 + or - 0.3, depending somewhat on the inclination and position angles of the mass distribution. The rotation curves derived from the best-fit mass models give circulate velocities that are lower than the observed H I velocities, implying that the neutral gas moves on noncircular orbits.
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