This dataset consists of reflectance spectra of small lunar areas measured in 120 spectral channels from 0.62 to 2.6 micrometers using the McCord circular-variable-filter (CVF) near-infrared photometer. A small aperture allows light from the selected lunar area to pass through the CVF and onto the detector. Each spectral channel is obtained sequentially as the CVF is rotated. Data were acquired using the 2.2 m telescope on Mauna Kea, Hawaii. All spectra have been scaled to a given wavelength. Spectral resolution varies somewhat from run to run. The first half of the CVF produces data at approximately twice the spectral resolution as the second half; data points where the two sections of the CVF were joined are unreliable. All data were acquired as relative reflectance spectra and were calibrated to scaled reflectance data using a directional-hemispheric (diffuse) spectrum of Apollo 16 soil acquired by J. B. Adams. See McCord et al., 1981 [MCCORDETAL1981] and Pieters, 1986 [PIETERS1986] for more detail on the instrument and calibration procedures.  Data files are named according to the scheme Hknnnn. H stands for Hawaii. The k represents the original archive tape on which the data were stored, and is related to the year of observation, as follows:  8 - 1978 9 - 1978 A - 1980 B - 1981 C - 1981 D - 1982 E - 1983.  The last four digits are the sequential number of the file on the original archive tape.

Acquisition of the 120 data points takes a few minutes; thus, a 120-point spectrum can be affected by the accuracy of guiding on the Moon as well as changing sky conditions and instrument stability. In most cases, several independent runs of data taken in sequence were averaged. Error bars are the standard deviation of this average and only refer to the repeatability of the measurement under these conditions.