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.
Email comments, questions to