The star HD 36665 (B1e), which lies behind the old supernova remnant S147, has been observed with the IUE satellite. High-velocity interstellar absorption components of Fe II, Mg I, Mg II, Al II, C II and Si II were detected (|Vₗsr = -73 km s⁻¹|) which originate in gas associated with the remnant. No such high-velocity lines were observed in the IUE spectrum of HD 40111 (B1 Ib) which is offset from the remnant. The high-velocity ultraviolet lines, together with new ground-based observations of high-velocity Ca II in HD 36665, have been analysed to determine column densities and to estimate the physical conditions in the high-velocity gas. The estimated level of depletions in the high-velocity gas is somewhat less than that normally observed in low-velocity interstellar gas, suggesting that sputtering of grains has occurred in the shock front of the supernova remnant.
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Phillips et al. (1981) studied this question.