A variety of observations have shown Sgr B (G0.6 0.1) to be one of the most spectacular star-forming regions in the Galaxy. Similarly, Sgr C (G359.4 0.1) is host to sites of star formation as well as a collection of unusual non-thermal radio filaments. Using Chandra, Very Large Array, and Nobeyama Radio Observatory observations, we study the correlations between radio continuum, CS(1–0) molecular line, and X-ray emission from these sources, with a focus on the distribution of the neutral iron 6.4 keV line emission. We examine the hypothesis that such emission is evidence of past flaring from Sgr A* and present an alternative model. We also study the distribution of X-ray and radio point sources throughout these regions.
|Original language||English (US)|
|Title of host publication||Proceedings of X-Ray and Radio Connections|
|Number of pages||5|
|State||Published - 2005|