Mass distribution in our Galaxy

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In this Subject: <a title="Transportation" href="/content/subcat;jsessionid=14vb6kmu6e63h.alice?j_subject=194&j_availability=">Transportation ,&nbsp; <a title="Astronomy" href="/content/subcat;jsessionid=14vb6kmu6e63h.alice?j_subject=226&j_availability=">Astronomy
By this author: Gerhard O.

Author: Gerhard O.

Source: Space Science Reviews, Volume 100, Numbers 1-4, January 2002 , pp. 129-138(10)

Publisher: Springer

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Abstract:

This article summarizes recent work on the luminosity and mass distribution of the galactic bulge and disk, and on the mass of the Milky Way's dark halo. A new luminosity model consistent with the COBE NIR data and the apparent magnitude distributions of bulge clump giant stars has bulge/bar length of sime 3.5 kpc, axis ratios of 1:(0.3–0.4):0.3, and short disk scale-length ( sime 2.1 kpc). Gas-dynamical flows in the potential of this model with constant M/L fit the terminal velocities in 10° le|l|le50° very well. The luminous mass distribution with this M/L is consistent with the surface density of known matter near the Sun, but still underpredicts the microlensing optical depth towards the bulge. Together, these facts argue strongly for a massive, near-maximal disk in our sim L^*, Sbc spiral galaxy. While the outer rotation curve and global mass distribution are not as readily measured as in similar spiral galaxies, the dark halo mass estimated from satellite velocities is consistent with a flat rotation curve continuing on from the luminous mass distribution.