Fabry-Perot Absorption Line Spectroscopy of the Galactic Bar

Details Fabry-Perot Absorption Line Spectroscopy of the Galactic Bar Fabry-Perot Absorption Line Spectroscopy of the Galactic Bar

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4801r&link_type=abstract

American Astronomical Society Meeting 208, #48.01; Bulletin of the American Astronomical Society, Vol. 38, p.123

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Scientific paper

There is substantial evidence now for the presence of a bar in the Milky Way. The signature of the Galactic bar should be found in kinematic distortions of the stellar velocity field in the central regions of the Galaxy, since the orbits are not circular, but rather elongated streams around the bar. The existing radial velocity sample is very sparse (100 - 200 stars), and hence, not sufficient to put strong constraints on the properties of the bar. More importantly these measurements were done in Baade’s window and other fields close to l = 0°. A much stronger dynamical signature of the bar ought to be apparent away from l = 0°.We use Fabry-Perot absorption line spectroscopy to measure radial velocities of over 3000 stars in the Milky Way bar. This sample is an order of magnitude larger than the current stellar kinematic data,and hence, will significantly improve the constraints on the properties of the Galactic bar like its orientation, length and shape. Our measurements were done at l = ± 5°, where the bar’s dynamical signature is stronger. Here we expect to see a two-component velocity distribution from approaching and receding velocities of the stars in the bar. In addition, we will be able to provide a constraint on the disk to halo mass ratio by determining the pattern speed of the bar.We acknowledge funding by the National Science Foundation.

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