Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26as..113..167b&link_type=abstract
Astronomy and Astrophysics Supplement, v.113, p.167
Astronomy and Astrophysics
Astrophysics
9
Gamma Rays: Observations, X-Rays: General, Methods: Data Analysis
Scientific paper
Estimating an incident spectrum from observed count rates is generally a complex problem, because the solution is unstable with respect to the measurement errors. When information about the signal is available, one can simply proceed by "model-fitting"; the spectrum is modelled, leading to a solution which depends on a few parameters only. In general, this method does not allow to introduce the number of degrees of freedom required for a complete description of the entire structure in the signal. Because the solution does not have the appropriate number of degrees of freedom, this simplification leads to false confidence limits on the signal. That is why deconvolution methods must be used, and these methods differ from the previous ones in the way that each point of the unknown incident spectrum is a parameter. We compare the performances of various spectral deconvolution methods for data measured by X-and gamma-ray detectors. In our study, the data are the count rates, related to an incident spectrum by a complex transfer function. The signal-to-noise ratios are small, and the dynamic range of the incident spectrum is very large leading to a tricky problem. Most deconvolution methods work best when the signal-to-noise ratios are fairly large, e.g. 3σ detection in each energy channel. When detection per channel becomes small, only methods which impose some constraints on the range and shape of the spectrum remain performant.
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