Signal-to-noise ratios in IUE SWP-LO spectra of chromospheric emission-line sources

Details Signal-to-noise ratios in IUE SWP-LO spectra of chromospheric emission-line sources Signal-to-noise ratios in IUE SWP-LO spectra of chromospheric emission-line sources

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990pasp..102.1420a&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 102, Dec. 1990, p. 1420-1432.

Astronomy and Astrophysics

Astronomy

7

Chromosphere, Emission Spectra, Iue, Signal To Noise Ratios, Stellar Spectra, Astronomical Spectroscopy, Cosmic Rays, Image Processing, Random Noise

Scientific paper

The short-wavelength-prime (SWP) detector of the International Ultraviolet Explorer should operate near the photon-counting limit, but the noise levels in flat-field images are several times higher. The exaggerated noise can be traced to the incomplete removal of the pixel-to-pixel granularity of the television frames by the prevailing spectral image processing system. An empirical noise model for the current-epoch photometric linearization strategy and one for a hypothetical processing system that achieves complete flat fielding of the raw images are derived. A formula is then proposed to predict the signal-to-noise ratio in the measured flux of an emission line (possibly superimposed on a smooth continuum) in an IUE low-dispersion (5 A resolution) far-ultraviolet (1150 A-1950 A) spectrum as recorded with the SWP camera. For illustration, the formula is specialized to the important C IV 1549 A feature of F-K stars. The S/N relation permits one to determine sensitivity limits, upper limits in faint exposures, and optimum exposure times.

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