HOCO+ toward the Galactic Center
arXiv:astro-ph/0609625 · doi:10.1093/pasj/58.6.979
Abstract
We have identified a weak thermal line U42.767, which has been detected only in the directions toward Sgr A and Sgr B2, as the HOCO+ 2_{02}--1_{01} transition. Because of the proximity of this line to the SiO maser line at 42.821 GHz (J=1-0 v=2),it was observable simultaneously in the ~43 GHz SiO maser searches at Nobeyama. From the past data of SiO maser surveys of infrared objects in the Galactic center, we created a map of emission distribution of HOCO+ in the Sgr A molecular cloud as well as maps of the 29SiO J=1-0 v=0 thermal emission and H53alpha emission. The emission distribution of HOCO+ was quite similar to the distribution of 29SiO emission. It suggests that the enhancement of the HOCO+ abundance in the galactic center is induced by shock activities which release the CO2 molecules frozen on grains into gases.
PASJ Dec. 25, 2006 issue in press
References in corpus (1)
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