Top left: the blue spectrum of B275 in M 17 shown next to B main-sequence-star spectra (Gray & Corbally 2009). Bottom left: the 1st and 2nd overtone CO emission bands. Zero velocity corresponds to the first component in the series (at 2294 and 1558 nm, respectively). Right: a sample of the emission line profiles in the spectrum of B275. The Ca ii triplet lines and O i 845 nm are superposed on hydrogen Paschen series absorption lines. The flux of the Hα line is scaled down by a factor 5; the structure near the peak is a remnant of the nebular-line subtraction.