Molecular abundance variations near our galactic center

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Millimeter-wave observations of CO, HCO+, HNCO, and SiO molecular lines toward Sgr A show that the prominent gas condensations in this region differ significantly in their chemical properties, which may be a result of gradients in the physical conditions as a function of location. HNCO and SiO observations suggest that M − 0.13 − 0.08 (the +20 km s−1 cloud) appears to consist of two different components, M − 0.13 − 0.08a and M − 0.13 − 0.08b, with LSR velocities of about +25 and +5 km s−1, respectively. The clump M − 0.13 − 0.08a (the +25 km s−1 cloud) seems to be located very close to Sgr A East and the observed enhancement of HNCO and SiO may result from the interaction with Sgr A East. The molecular gas clump M − 0.02 − 0.07 (the +50 km s−1 cloud) shows the strongest 13CO emission among the identified clouds in this region, and is the most massive condensation (3 × 105 M), but may be located closer to us than other clouds, since it appears to be chemically quiescent and shade the “inter-cloud region” where the HCO+/13CO ratio is enhanced. The −30 km s−1 component shows a similar morphology to the HCO+ enhanced “inter-cloud” region. M + 0.07 − 0.08 and M + 0.11 − 0.08 show strong HCO+ 1–0 emission, and appear to consist of one cloud (the HCO+ cloud) in this observation. The HCO+/13CO abundance ratio is enhanced by a factor of 2–3 toward this HCO+ cloud and the inter-cloud region between l = 0.1° and 0° near to Sgr A East, compared to other clouds observed in this region. This relative enhancement of HCO+ is thought to result from interaction with Sgr A East.







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