High-resolution and sensitive near-infrared spectroscopy is often limi
ted by the ability to correct the atmospheric transmission. The simple
division of the object spectrum by the spectrum of a nearby star turn
s out to be unsatisfactory because of the stellar features in the latt
er. We show how to measure the atmospheric transmission with a nearby
early GV or late FV star, and to correct for the stellar features by m
eans of the (atmospheric-transmission-corrected) solar spectrum. (C) 1
995 American Astronomical Society.