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Session 58 - Future of Antarctic Astrophysics.
Display session, Wednesday, June 10
We have imaged the CO 4-3 line, the dominant coolant of the dense molecular interstellar medium, from the Galactic Center region, between l=-3 to 4 degrees and b= -1 to 1 degrees. We detect bright CO 4-3 emission from the well-known Galactic Center clouds Sgr A, Sgr B, Sgr C, and Sgr D. We compare the CO 4-3 intensities with CO 1-0, C18O 1-0, HCN 1-0, and HCO+ 1-0 from the literature to infer excitation conditions. The CO 4-3 traces fairly warm, dense gas with opacities near unity. We also detect CO 4-3 absorption at V= 0 km/s along the line of sight toward the Galactic Center.
This research was supported in part by the National Science Foundation under a cooperative agreement with the Center for Astrophysical Research in Antarctica (CARA), grant number NSF OPP 89-20223. CARA is a National Science Foundation Science and Technology Center.
Program listing for Wednesday