Observations of HC3N Toward the SGR B2 Molecular Cloud

Details Observations of HC3N Toward the SGR B2 Molecular Cloud Observations of HC3N Toward the SGR B2 Molecular Cloud

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998jkas...31..117m&link_type=abstract

Journal of the Korean Astronomical Society, vol. 31, no. 2, pp. 117-125

Astronomy and Astrophysics

Astronomy

Ism: Abundances, Ism: Individual (Sgr B2), Ism: Molecules

Scientific paper

We have observed the 10-9 transitions of HC3N and its 13C substitutes (H13CCCN, HC13CCN, and HCC13CN), and the vibrationally excited 12-11 (v_7 = 1) HC3N transition toward the Sgr B2 molecular cloud. The observed HC3N emission shows an elongated shape around the Principal Cloud (~4.5 pc in R.A. X 7.4 pc in Decl.). The optically thin H13CCCN line peaks around the (N) core and we derive the total column density N(H13CCCN) = 4 X 10^13 cm^(-2) at this position. Toward the 2' N cloud which shows the peculiar chemistry, the HC3N lines show enhancements compared to the extended envelope. The shocks of the 2' N may have resulted in the enhancement of HC3N. The hot component of HC3N is strongly concentrated around the (N) core and its HPW is ~0.9 pc in diameter. We derive the lower limit of the abundance ratio N(HC3N)/N(H13CCCN) to be larger than 40 in most regions except the (M) and (N) cores. The fractionation of 13C at this region may not be as effective as previously reported.

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