A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. A target acquisition should probably be performed before doing spectroscopy or coronography with STIS or COS. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. This is a resubmission with one orbit per visit based on Patricia Royle's suggestion that it is easier to schedule that way than as 3 orbits per visit. No other changes. Target confirmation was done with the tool, but a better check was a recent HST [O III] image. There are no bright stars here. 1698209305 ----- Attempting Submission 2 (Wed Sep 06 21:26:24 GMT 2023) ----- The targets are exteneded SNR filaments, and the normal acquistion procedures are not appropriate. We are aware of the difficulties with calibration of extended targets. Dust Destruction in Supernova Remnant Shock Waves Supernova remnant shock waves dominate the destruction of interstellar dust, but the observational constraints on the destruction efficiency are poor. This is partly due to incomplete knowledge of the shock parameters and partly to inadequate observations, especially in the UV. We propose to obtain accurate fractions of the dust destroyed in 6 radiative shocks in the Cygnus Loop for which the shock wave parameters -- shock speed, preshock density and magnetic field -- are accurately known. We will use the COS UV spectra to measure the gas phase abundances of C, O and Si. Oxygen is nearly undepleted in the preshock gas, while C and Si are locked up in grains until the grains are destroyed. We will obtain COS FUV spectra of 6 positions in the Cygnus Loop with the G140L grating. Each spectrum will be a 1 orbit exposure. There are no restrictions on roll angle. The emission is diffuse, so no peakup should be attempted. John Raymond has been modeling supernova remnant shock waves and observing them at UV, optical, IR and X-ray wavelengths for many years. He recently led two analyses of shocks in the western Cygnus Loop, deriving accurate shock speeds, densities and magnetic fields. He will modify his code to account for gradual liberation of C and Si from grains as the shocked gas cools. Jon Slavin is an expert on the large-scale structure of supernova remnants, their interaction with dense clouds, and the destruction of dust grains in shocks. His models include detailed calculations of grain trajectories in the downstream magnetic field and the destruction of grains in evolving supernova shocks. Most recently he has modeled the evolution of supernova-formed dust grains during the remnant evolution starting from their natal ejecta knots until they reach the interstellar medium. 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