A brief description of the spectra is given below.
The spectra are described in somewhat more detail in the
paper "Spectroscopy of Brown Dwarf Candidates in the Rho Oph
Molecular Core", by Wilking, Greene, & Meyer (1999, AJ, v117, 
469; WGM99).  *Note that the ascii spectra have been recalibrated
in wavelength since WGM99 and were used in the analysis
presented by Wilking et al. (2004, AJ, v127,1131).*

All of the spectra were taken at NASA's IRTF with the NSFCAM 
grism in the K band using the HKL Grism, the 0.3 arcsec/pixel
scale and the 0.6 arcsec slit.  The spectra have a resolution
R of ~300.  Before extraction, the spectra were sky-subtracted
and divided by a flat-field.  After extraction, the spectra 
were divided by a telluric standard of spectral type  B9V to
A2V which was observed at the same airmass very close in time.
The final spectra were normalized to one.  To restore the true
continuum shape one must multiply the spectra by an A0V star
continuum, i.e., a ~10,000 K blackbody.

The data are stored as x,y pairs with x = wavelength in angstroms
and y = relative flux in arbitrary units.  The spectra have been
trimmed to show the highest quality spectral region from 2.0 - 
2.5 microns.  The apparent emission feature at Br gamma (21700 
angstroms) is an artifact of the division by the telluric 
standard.

You may contact Bruce Wilking (bwilking@umsl.edu) or 
Tom Greene (tgreene@mail.arc.nasa.gov) for further
information.  We would appreciate it if you let us know if
you make use of these spectra for classification.

This research is supported in part by the National Science 
Foundation.