This tool calculates the expected signal to noise for a point source
using the LRIS spectrograph.
The input spectrum is one of the templates normalized by the
specified AB or Vega magnitude in the specified filter. A flat
template means that the flux is distributed as either flat in
frequency or the spectrum of Vega. The total flux of the object
specified by the user will be reduced to account for slit losses
based on the specified slit width, height, and seeing. The target is
assumed to be a point source with a PSF FWHM as specified by the
seeing parameter.
The output data are given in units of per pixel.