Abundances and Physical Conditions in the Low and Intermediate Velocity Gas Toward Mu Columbae

Details Abundances and Physical Conditions in the Low and Intermediate Velocity Gas Toward Mu Columbae Abundances and Physical Conditions in the Low and Intermediate Velocity Gas Toward Mu Columbae

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7538s&link_type=abstract

HST Proposal ID #7538

Physics

Hst Proposal Id #7538 Interstellar Matter

Scientific paper

The interstellar path to the O9.5 V star Mu Columbae {l=237degrees, b=-27degrees; d=1100 pc, z=-485 pc} intercepts several clouds of differing physical conditions. The lowest velocity clouds sampled are typical of warm diffuse clouds, while the higher velocity components appear to be examples of shocked-processed clouds, as evidenced by their enhanced gas phase abundances. Copernicus observations measured OVI absorption, thus also providing evidence that hot gas exists along this sightline. During the post-COSTAR orbital verification program, an extremely rich, high quality data set was obtained for Mu Col with the GHRS echelle gratings. This extensive data set represents the most complete observations of any interstellar path, including that towards Zeta Ophiuchi. We will analyze these 3.5 km s^-1 resolution data to derive important information about the patterns of elemental abundances in the warm neutral medium of the Galaxy, the shock destruction of interstellar grains in intermediate velocity clouds and the origin of highly ionized disk gas. The abundances measured for the principal diffuse cloud at V_mathrm LSR=3 olinebreak km s^-1 will provide the fundamental reference data for gas-phase elemental abundances in the low-density warm interstellar medium of the Galaxy and will be an important complement to the well studied dense cloud abundances towards Zeta Oph.

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