This tool calculates the expected counts and signal to noise for a
point source using the APF spectrograph. The throughput measurements
are from a 8 by 8 arcsecond aperture. The data are from September of
2015.
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 APF, the slit depends on which Decker is
used.
The output data are given in units of per pixel.