Oka, T.; Hasegawa, T.; White, G. J.; Sato, F.; Tsuboi, M. and Miyazaki, A.
Due to copyright restrictions, this file is not available for public download
|Google Scholar:||Look up in Google Scholar|
We observed CO J = 1–0 and HCN J = 1–0 line emission toward a high-velocity, compact molecular cloud, CO 0.02–0.02, near the center of our Galaxy, using the Nobeyama Millimeter Array (NMA). A CO velocityintegrated map with a resolution of 4:003 2:004 shows two oval clumps with sizes of 0.8 pc. These clumps are seperated by 1.2 pc, being located at the eastern and southwestern peripheries of the CO0.02–0.02 cloud. The overall distribution of HCN emission coincides with that taken with the Nobeyama 45m telescope. The HCN velocity integrated map with a resolution of 6:001 3:004 shows two prominent peaks in the cloud center. Both NMA maps at VLSR 110km1 show an arc-shaped edge in the southeast, which may correspond to the edge of the 'emission cavity' found in the CO J = 3–2 integrated-intesity map. We also noticed a faint radio continuum 'arc' that encircles the bulk of the CO0.02–0.02 cloud. These results support the notion that CO0.02–0.02 has been accelerated, heated, and compressed in a series of supernova shocks that ccurred within the last (3–5)104 yr. We suggest that a massive compact cluster with an age of 10–30Myr is responsible for the formation of the CO0.02–0.02 cloud.
|Item Type:||Journal Article|
|Copyright Holders:||2008 Astronomical Society of Japan|
|Academic Unit/Department:||Science > Physical Sciences|
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Tracy Bartlett|
|Date Deposited:||30 Nov 2010 16:38|
|Last Modified:||23 Jan 2011 17:29|
|Share this page:|