The Cool Atomic and Molecular Medium: Spectroscopy of the b5 Molecular Cloud Halo

Details The Cool Atomic and Molecular Medium: Spectroscopy of the b5 Molecular Cloud Halo The Cool Atomic and Molecular Medium: Spectroscopy of the b5 Molecular Cloud Halo

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.5895w&link_type=abstract

HST Proposal ID #5895

Computer Science

Hst Proposal Id #5895 Interstellar Medium

Scientific paper

The cool atomic and molecular medium (CAMM) plays a pivotal role in the evolution of the ISM, shielding dense clouds from ionizing radiation and providing formation sites for simple molecules. Yet, observations of this component have been hampered by observational difficulties. For optical and UV absorption line studies, the problem is one of sampling: lines of sight to the brightest stars often miss the CAMM, usually found near dense, obscuring clouds. The present proposal uses the GHRS to target three stars near B5, a quiescent molecular cloud lying well below the Galactic Plane. We have carried out a program of supporting observations of B5, including full maps of radio wavelength CO and HI, and absorption line studies at HI (21 cm) and at optical wavelengths (CH, CH+ and CaII). Even in the quiescent B5, velocity offsets between the lines of different molecular and atomic species suggest that the atomic medium participates in (or is a result of?) active flows. The GHRS will provide the spectral resolution necessary to resolve the kinematics, along with the sensitivity required to target stars lying near B5. Wavelength settings are for CI, CO and C2. Together these spectral lines will yield gas pressure and density and information needed to understand the cloud structure, kinematics and chemical processes.

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