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HOCO+ toward the galactic center

机译：HOCO +朝向银河系中心

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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 similar to 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 (SiO)-Si-29 J = 1-0 v = 0 thermal emission and H53 alpha emission. The emission distribution of HOCO+ was quite similar to that of (SiO)-Si-29 emission. This suggests that an enhancement of the HOCO+ abundance in the galactic center is induced by shock activities, which release CO2 molecules frozen on grains into gases.
机译：我们已经确定了一条弱热线U42.767，它仅在朝向Sgr A和Sgr B2的方向上被检测到，作为HOCO + 2（02）-1（01）的转变。由于这条线在42.821 GHz（J = 1-0 v = 2）处接近SiO maser线，因此在类似于Nobeyama的43 GHz SiO maser搜索中可以同时观察到。根据银河中心红外物体的SiO maser调查的过去数据，我们创建了Sgr A分子云中HOCO +的发射分布图以及（SiO）-Si-29 J = 1-0 v的图= 0热辐射和H53α辐射。 HOCO +的发射分布与（SiO）-Si-29的发射分布非常相似。这表明，激波活动导致银河中心HOCO +丰度的增加，激波活动将冻结在谷物上的CO2分子释放到气体中。

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