HD 62542: Probing the Bare, Dense Core of an Interstellar Cloud

Details HD 62542: Probing the Bare, Dense Core of an Interstellar Cloud HD 62542: Probing the Bare, Dense Core of an Interstellar Cloud

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004hst..prop10164w&link_type=abstract

HST Proposal ID #10164

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Hst Proposal Id #10164 Ism

Scientific paper

The line of sight to HD 62542 is remarkable for its unusual UV extinction, high column densities of various molecules, and apparent dearth of diffuse atomic gas. The main interstellar cloud appears to be a small, dense {n_H 500-1000 cm^-3}, molecular knot whose more diffuse outer layers have been stripped away by stellar winds and shocks. As such, it provides an ideal venue for investigating the properties of dense, molecular gas -- with minimal confusion from any associated diffuse gas. We propose to obtain high resolution, moderately high S/N STIS spectra of C I, CO and its isotopomers, C_2, C II, O I, and many other atomic species. Those data will be used to compare various diagnostics of the physical conditions {e.g., C I and O I fine structure excitation, CO and C_2 rotational excitation}, to determine the relative abundances of the various CO isotopomers {fractionation}, and to determine the depletions of various elements in dense gas {the predicted severe depletions have likely been masked by associated diffuse gas in other cases}. Understanding the fractionation and excitation of CO in this relatively simple case will aid in understanding its behavior in other more complex regions {important because CO and its isotopomers are often used to trace and characterize molecular gas when H_2 cannot be measured}.

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