Data Set Overview : This dataset is comprised of asteroid flux data measured in 26 filters using the McCord dual beam photometer. Of the 26 filters used for the full dataset, a maximum of 24 were used for any one measurement. The wavelength range covered is from 0.32 to 1.08 micrometers.  Processing Level Id : 3 Software Flag : N Processing Start Time : 1975 Processing Stop Time : 1984   Parameters : Sampling Parameter Name : WAVELENGTH Data Set Parameter Name : FLUX RATIO Minimum Sampling Parameter : 0.330000 Maximum Sampling Parameter : 1.100000 Data Set Parameter Unit : DIMENSIONLESS Noise Level : 2.000000 Sampling Parameter Unit : MICROMETER   Data : FLUX RATIO is defined as the ratio of two measured photon fluxes from a photometric or spectrometric instrument. For instance, the ratio of the measured spectrum of a target relative to the measured spectrum of a calibration standard will yield a value that is a flux ratio. This parameter is dimensionless.   Ancillary Data :  Atmospheric Conditions ---------------------- An estimate of the quality of the observing conditions for each night of observing is given in the original papers, Chapman (1972) [CHAPMAN1972], Chapman and Gaffey (1979) [CHAPMAN&GAFFEY1979A] [CHAPMAN&GAFFEY1979B] and McFadden et al. (1984) [MCFADDENETAL1984].  Calibration Standard -------------------- The data are calibrated to flux ratio (asteroid/inferred sun) with reference to a set of standard stars. During the observation sessions, the standard stars are observed both to determine extinction corrections in each filter and as color standards. Many of the standard stars used are A- or B- Oke/Hayes standard stars and others of the solar type.

Confidence Level Overview : Acquisition of the 24 data points takes time; thus, a 24-point spectrum can be affected by the varying light curve of the asteroid, as well as by the changing sky conditions and instrument stability. In most, but not all, cases, data were co-added from numerous rapid rotations of the filter wheel. Uncertainties in the relative calibration between stars and Alpha Lyrae may contribute an uncertainty of up to 2% in the visible and 4% in the infrared bands. It is believed that this uncertainty is larger than other systematic errors in the data.