2000NewA....5..285Z

The UV spectrum of a few reddened stars will be decomposed into two terms. One is the direct starlight, F_*,lambda^0 e^ - tau_lambda, which is the product of the flux of the star corrected for interstellar extinction, F_*,lambda^0, and of the extinction e^ - tau_lambda. The second is starlight scattered by interstellar dust into the beam of the observation. This excess of scattered starlight affects the FUV part of the spectrum (lambda < 2200 A). The combination of both terms gives the shape of the UV spectrum of a reddened star, with its characteristic depression at 2200 A.