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.
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