FIR LINE EMISSION FROM GALACTIC HIGH-LATITUDE CLOUDS

> in this proposal, more time is being requested for rstark.coolline we propose to take deep lws02 observations of the cii 157.7 mu line, as well as medium resolution wavelength range lws01 scans necessary to analyze existing data of the oi 63.2 mu line in a sample of well studied highlatitude cirrus clouds. most of these clouds have already been observed using lws02. however, the need to defringe the medium resolution line spectrum observations requires rather longer wavelength observations than originally anticipated. the fringing has strongest impact at 63.2 microns. without defringing, the oi spectra cannot be interpreted. at 158 microns the fringing pattern has a longer period and is less disturbing. the results so far show that cii emission in quiescent cirrus clouds is weak and ubiquitous. higher s/n lws02 cii spectra are necessary to investigate the variation in each cloud as well as among the clouds, and to separate the contribution from the diffuse ionized interstellar medium along the line of sight. the lws observations will provide a direct tool to study the carbon chemistry: cii> ci > co, and the cooling by oi and cii. the primary target of our sample is the hd 210121 (g056) cloud. this is one of the best characterized quiescent highlatitude clouds to date. the other high priority clouds g22829 and g23028 are cometary cirrus clouds which are connected by their tails. the latter two have very peculiar hi, co, and fir properties. their 60/100 mu brightness ratio is one of the highest known among cirrus. they are thought to be shocked by the same collision, and to be at present in a different stage of shock completion. the cooling lines will provide unique information on the physical/chemical state and the differences between quiscent and truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]