Observations and modeling of infrared and millimeter molecular lines towards GL2591

Details Observations and modeling of infrared and millimeter molecular lines towards GL2591 Observations and modeling of infrared and millimeter molecular lines towards GL2591

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ap%26ss.224..181n&link_type=abstract

Astrophysics and Space Science, Volume 224, Issue 1-2, pp. 181-184

Astronomy and Astrophysics

Astrophysics

Abundances, Molecular, Infrared

Scientific paper

We have observed C2H2 and HCN rovibrational transitions near 13µm in absorption against GL2591. We also have observed rotational transitions at 0.6-3 mm of CS, HCN, H2CO, and HCO+. Analysis of the rotational lines, which arise in the extended cloud around the source, shows that no single density model can explain all the data. Models with density and temperature gradients do much better; in particular models withn(r) αr -1.5 can reproduce the observed pattern of emission line strengths. The abundances show significant depletion compared to models of gas-phase chemistry. The rovibrational data were analyzed in comparison to the absorption line analysis of CO by Mitchellet al. (1989). Our data are consistent with the C2H2 and HCN absorption arising in the same warm (200 K) and hot (1010 K) components seen in CO, but we see little evidence for the cold (38 K) component seen in CO. The rovibrational lines from higher states (J ≥ 21) indicate that the hot HCN deviates from LTE, leading to a density of about 3 × 107 cm-3. Comparison of the two data sets shows that the rovibrational absorption of HCN, rather than arising in the extended envelope, must come from a region with a small angular extent. A model in which early-time gas phase abundances are preserved on grain mantles and released at high temperature can explain the data.

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