Applying Filter Functions to Spectra Using the Cubic Spline Method

Details Applying Filter Functions to Spectra Using the Cubic Spline Method Applying Filter Functions to Spectra Using the Cubic Spline Method

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...201.9107m&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #91.07; Bulletin of the American Astronomical Society, Vol. 34, p.1257

Astronomy and Astrophysics

Astronomy

Scientific paper

Spectra taken with a CCD are first reduced to one dimension and calibrated using IRAF specred functionality. A Perl computer program was then developed to apply filters of any type to these spectra. The value of the transmission as a function of wavelength for a particular filter is determined using a cubic spline method. From the FITS header, the pixel to wavelength correspondence is derived from the IRAF World Coordinate System. The transmission function is then applied to each pixel value as per its corresponding wavelength. The output image is then a calibrated, reduced, and filtered spectrum.

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