The COS Calibration Pipeline

Details The COS Calibration Pipeline The COS Calibration Pipeline

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21113503h&link_type=abstract

American Astronomical Society, AAS Meeting #211, #135.03; Bulletin of the American Astronomical Society, Vol. 39, p.972

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Scientific paper

The COS calibration pipeline (CALCOS) includes three main components: basic calibration, wavelength calibration, and spectral extraction. Calibration of modes using the far ultraviolet (FUV) and near ultraviolet (NUV) detectors share a common structure, although the individual reference files differ and there are some additional steps for the FUV channel. The pipeline is designed to calibrate data acquired in either ACCUM or time-tag mode.
The basic calibration includes pulse-height filtering and geometric correction for FUV, and flat-field, deadtime, and Doppler correction for both detectors.
Wavelength calibration can be done either by using separate lamp exposures or by taking several short lamp exposures concurrently with a science exposure. For time-tag data, the latter mode ("tagflash") will allow better correction of potential drift of the spectrum on the detector.
One-dimensional spectra will be extracted and saved in a FITS binary table. Separate columns will be used for the flux-calibrated spectrum, error estimate, and the associated wavelengths.
CALCOS is written in Python, with some functions in C. It is similar in style to other HST pipeline code in that it uses an association table to specify which files to be included, and the calibration steps to be performed and the reference files to use are specified by header keywords.
Currently, in conjunction with the Instrument Definition Team (led by J. Green), the ground-based reference files are being refined, delivered, and tested with the pipeline.

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