literature
Literature
Authors
Jobs
Seminars
Conferences
DataBETA

Mass models of the Milky Way

Dec, 1996
10 pages
Published in:
  • Mon.Not.Roy.Astron.Soc. 294 (1998) 429
e-Print:
DOI:
Report number:
  • OUTP-96-06A
View in:
pdf
reference search359 citations

Citations per year

1997200420112018202405101520
Abstract: (arXiv)
A parameterized model of the mass distribution within the Milky Way is fitted to the available observational constraints. The most important single parameter is the ratio of the scale length R_d* of the stellar disk to R0. The disk and bulge dominate v_c(R) at R> R0. For example, changing the disk slightly from an exponential surface-density profile significantly changes the form of v_c(R) at R >> R0, where the disk makes a negligible contribution to v_c. Moreover, minor changes in the constraints can cause the halo to develop a deep hole at its centre that is not physically plausible. These problems call into question the proposition that flat rotation curves arise because galaxies have physically distinct halos rather than outwards-increasing mass-to-light ratios. The mass distribution of the Galaxy and the relative importance of its various components will remain very uncertain until more observational data can be used to constrain mass models. Data that constrain the Galactic force field at z > R and at R > R0 are especially important.
Note:
  • 10 pages, LaTeX, mn.sty, 5 .ps figures, accepted by MNRAS major revision involving new cepheid & hipparcos data