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Shuji Deguchi, Atsushi Miyazaki, Young Chol Minh, HOCO+ toward the Galactic Center, Publications of the Astronomical Society of Japan, Volume 58, Issue 6, 25 December 2006, Pages 979–986, https://doi.org/10.1093/pasj/58.6.979
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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 |$\mathrm{HOCO}^{+} 2_{02} \hbox{--}1_{01}$| transition. Because of the proximity of this line to the SiO maser line at 42.821 GHz (|$J = 1 \hbox{--} 0 v = 2$|), it was observable simultaneously in |$\sim 43 \,\mathrm{GHz}$| 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 |$\mathrm{HOCO}^{+}$| in the Sgr A molecular cloud as well as maps of the |${{29\atop} \mathrm{SiO}} J = 1 \hbox{--} 0 v=0$| thermal emission and H53|$\alpha$| emission. The emission distribution of |$\mathrm{HOCO}^{+}$| was quite similar to that of |${{29\atop} \mathrm{SiO}}$| emission. This suggests that an enhancement of the |$\mathrm{HOCO}^{+}$| abundance in the galactic center is induced by shock activities, which release |$\mathrm{CO}_2$| molecules frozen on grains into gases.
