Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-25T15:40:57.647Z Has data issue: false hasContentIssue false
  • English
  • Français

Do maser stars trace a rotating Galactic bar?

Published online by Cambridge University Press:  01 March 2007

H. J. Habing
H. J. Habing*
Affiliation:
Leiden Observatory, the Netherlands email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

I have analyzed the radial velocities in two large samples of maser stars that cover the Galactic plane from l = +40deg to l = −40deg through the Galactic Centre. I compare a diagram of longitude versus radial velocity as observed with a diagram obtained from the calculation of orbits in a simple, but realistic potential containing a weak, rotating bar. Almost all stars belong to the Galactic disk but there is a small sample with high velocities close to the Galactic Centre and in the so-called forbidden quadrants. These velocities cannot be explained by a combination of pure Galactic rotation and a modest dispersion in velocity. An acceptable explanation is one in which the stars of this small sample move up and down a rotating Galactic bar.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 356 - 360
Copyright
Copyright © International Astronomical Union 2008

References

Binney, J., & Tremaine, S. 1987, Galactic Dynamics (Princeton University Press)Google Scholar
Garcia-Hernandez, D. A., Garcia-Lario, P., Plez, B., Manchado, A., D'Antona, F., Lub, J., & Habing, H. J. 2007, A&A 462, 711Google Scholar
Habing, H., Sevenster, M., Messineo, M., van der Ven, G., & Kuijken, K. 2006, A&A, 458, 151Google Scholar