On the signal-to-noise ratio in IUE high-dispersion spectra

Details On the signal-to-noise ratio in IUE high-dispersion spectra On the signal-to-noise ratio in IUE high-dispersion spectra

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apjs...71..387l&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 71, Oct. 1989, p. 387-406.

Astronomy and Astrophysics

Astrophysics

17

Data Reduction, High Dispersion Spectrographs, Noise Reduction, Signal To Noise Ratios, Ultraviolet Spectra, Algorithms, Amplitude Distribution Analysis, Background Noise, Iue, Quantitative Analysis, Random Noise, Tables (Data)

Scientific paper

An observational and data reduction technique for fixed pattern noise (FPN) and random noise (RN) in fully extracted IUE high-dispersion spectra is described in detail, along with actual empirical values of signal-to-noise ratio (S/N) achieved. A co-addition procedure, involving SWP and LWR cameras observations of the same spectrum at different positions in the image format, provides a basis to disentangle FPN from RN, allowing each average amplitude, within a given wavelength interval, to be estimated as a function of average flux number. Empirical curves, derived with the noise algorithm, make it possible to estimate the S/N in individual spectra at the wavelengths investigated. The average S/N at the continuum level in well-exposed stellar spectra varies from 10 to 20, for the orders analyzed, depending on position in the spectral format. The co-addition procedure yields an improvement in S/N by factors ranging from 2.3 to 2.9. Direct measurements of S/N in narrow, line-free wavelength intervals of individual and co-added spectra for weak-lined stars yield comparable, or in some cases somewhat higher, S/N values and improvement factors.

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