[Previous] | [Session 84] | [Next]
R. Simon, J.M. Jackson, D.P. Clemens, T.M. Bania, M. Kolpak (BU), M.H. Heyer (UMASS)
The Milky Way Galactic Ring Survey (GRS) exploits the new 16 element array receiver SEQUOIA on the FCRAO 14m telescope to map molecular gas in the First Galactic Quadrant with unprecedented sensitivity (0.2 -- 0.4 K), angular resolution (45''), and spectral resolution (0.2 km/s). Unlike previous molecular line surveys, we achieve the full resolution of our telescope. Moreover, we use both a column density (13CO 1-0) and a volume density tracer (CS 2-1) to image molecular clouds and cloud cores in the inner Galaxy, especially in the ``5 kpc ring,'' the Milky Way's dominant star-forming structure. The GRS will ultimately provide a unique database for the study of cloud structure, Galactic structure, the interstellar medium, and star formation.
Here we present results for the Galactic Ring Survey's first two square degrees, from l=44.5 to 46.5 degrees and b=-0.5 to 0.5 degrees. We display integrated intensity images of both 13CO and CS and compare the GRS to previous molecular line surveys. We also outline the plans to complete the GRS in the next few years.
The Galactic Ring Survey is supported by NSF grant AST-9800334.
If the author provided an email address or URL for general inquiries, it is a
s follows:
http://carp.bu.edu/grs/