This tool calculates the expected signal to noise for a point source using the KAST spectrograph. Currently, the user can only select two grisms, two dichroics and one grating. As more data on the throughput of the instrument become available, more options will be added.
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. For KAST the slit is 120 arcseconds in length.
The output data are given in units of per pixel.
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