The physical and chemical state of a dense core in the high-latitude cloud MCLD 123.5 + 24.9

Details The physical and chemical state of a dense core in the high-latitude cloud MCLD 123.5 + 24.9 The physical and chemical state of a dense core in the high-latitude cloud MCLD 123.5 + 24.9

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...264..195g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 264, no. 1, p. 195-202.

Astronomy and Astrophysics

Astrophysics

22

Abundance, Interstellar Chemistry, Interstellar Matter, Molecular Clouds, Astronomical Spectroscopy, Carbon Monoxide, Electron Transitions, Formaldehyde, Hydrocyanic Acid, Line Spectra

Scientific paper

We present observations of a dense core in the translucent high-latitude cloud MCLD 123.5 + 24.9 in the (J = 1 -0) transitions of (C13) O, C (O-18), HCO (+), H(C-13)O(+), HCN, in the C(O-18) (J = 2 -1) and the NH3 (J,K) = (1,1) and (2,2) transitions. The core is extended and shows significant substructure in all transitions even at the highest angular resolution, corresponding to 0.04 pc at an adopted distance of 200 pc. The HCO+ and C(O-18) emission are similar in extent and corresponds to an equivalent radius of 0.07 pc, the region of the ammonia emission is smaller and has an equivalent radius of 0.04 pc. From the ammonia observations we derive an upper limit for the kinetic temperature of 15 K, the lower limit from CO observations is 6 K. The C(O-18) abundance for MCLD 123.5 + 24.9 is normal, X(C(O-18) is about 1.4 x 10 exp -7; the abundances of HCO + and NH3 relative to H2 are likely to be lower by an order of magnitude compared to corresponding values for typical dark clouds, the abundance of HCN is comparable e.g., to L134N. We find X(HNC)/X(HCN) = 0.8 +/- 0.1, which is typical for low temperature chemistry.

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