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D.J. Helfand, A. Fallon (Columbia University), R.H. Becker (UC Davis & IGPP), U. Giveon (UC Davis), R.L. White (STScI)
We are in the process of constructing a deep, high-resolution, multiwavelength image of the Galactic plane in the first quadrant. Observations with the Very Large Array in the B, C, and D configurations have been added to single dish data in order to obtain an image at 20cm with a sensitivity of ~2mJy and a dynamic range of 500:1. In addition, 90cm data have been obtained, and a comparison with archival 6cm images has been conducted. Portions of this region have also been covered with the imaging instruments on XMM-Newton in the 0.3-12 keV band; archival data from ASCA have also been examined. Finally, we have undertaken a detailed comparison of the radio data with mid-IR images from the MSX mission. Hundreds of new HII regions and dozens of supernova remnant candidates are apparent in the 13 degrees of longitude covered to date. We will present a preliminary analysis of the HII-region flux density distribution, and will describe the utility of this survey for a variety of projects ranging from a determination of a quantitative star formation rate for the Galaxy, the discovery of young supernova remnants, and the improvement of the model for the free-electron distribution in the plane which is essential is characterizing the pulsar population.
This work is supported under grant AST-02-06055 from the NSF.
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.