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.