Physical Conditions Near High Galactic Latitude Molecular Clouds

Details Physical Conditions Near High Galactic Latitude Molecular Clouds Physical Conditions Near High Galactic Latitude Molecular Clouds

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6723b&link_type=abstract

HST Proposal ID #6723

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Hst Proposal Id #6723 Interstellar Medium

Scientific paper

Ultra high resolution observations (R ~ 10^6) of the highlatitude stars HD 28497, HD 89688, HD 141569 and HD 151741,show complex NaI (D1 and D2) and Ca II K interstellarabsorption line profiles. Due to their location near highgalactic latitude molecular clouds, these stars are well-suited background sources for detailed spectroscopic studiesof molecular clouds as well as gas in the near halo. Theoptical data show that the column densities are low and theclouds are well resolved with a wide range of physicalconditions, making these rich and important sightlines forultraviolet studies. We would like to study the distributionand physical characteristics of the neutral (HI), ionized(HII) and highly ionized (hot) gas associated with theindividual absorbing components observed in the NaI and CaIIabsorption line profiles. HST GHRS spectra of the interstellarabsorption lines of MgI, CI, SiII, FeII, MgII, CrII, ZnII,SiIV, CIV and NV will allow us to trace the extent of theneutral, ionized and hot gas and will be used to estimatekinetic temperatures, electron densities, pressures, thedepletions of the various elements in the HI gas, and thecomposition of the grains. Further, these observations willdetermine if high galactic latitude molecular clouds areindeed embedded in the hot local interstellar medium assuggested by X-ray observations and how the physicalconditions in these clouds differ from other diffuseinterstellar clouds.

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