Modeling of spectroscopic astronomical observations

Details Modeling of spectroscopic astronomical observations Modeling of spectroscopic astronomical observations

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994spie.2198.1105f&link_type=abstract

Proc. SPIE Vol. 2198, p. 1105-1115, Instrumentation in Astronomy VIII, David L. Crawford; Eric R. Craine; Eds.

Astronomy and Astrophysics

Astronomy

Scientific paper

We have constructed a computer model for the simulation of spectroscopic astronomical observations of point sources. The aim is to help the observer to plan scientific and calibration exposures, to select the most suitable spectrographic parameters, to predict S/N ratios, and to test data reduction algorithms. The model, which was developed in the IRAF/STSDAS environment in the frame of the Russia / Ukraine / Italy / Germany cooperation for the SPECTRUM UV mission, is rather general and includes the whole chain: Telescope-Spectrograph-Detector. The database required to run the program consists of: (a) monochromatic PSF's of the telescope; (b) monochromatic PSF's of the spectrograph; (c) detector characteristics (pixel size, RON, gain, DC); (d) monochromatic throughputs of each system component. The input of the program is: (a) an observing mode (e.g. slit size, resolution, wavelength range, etc.); (b) the exposure time; (c) the sky background; (d) an input spectrum template. The output of the program is: (a) a 2D image containing the spectrum as it is recorded on the detector; (b) an estimate of the S/N ratio computed by taking into account also the photon noise. Examples of the application of the program to a Rowland mounting spectrograph is presented.

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