A sensitive continuum analysis method for gamma ray spectra

Author(s):  
Alakh N. Thakur ◽  
James R. Arnold
1975 ◽  
Vol 125 (4) ◽  
pp. 507-523 ◽  
Author(s):  
Nobuo Sasamoto ◽  
Kinji Koyama ◽  
Shun-Ichi Tanaka

Author(s):  
Susan E. Haywood

Gamma-ray spectra containing peaks that are too close in energy for deconvolution to be done accurately are best analyzed by a library-based method. However, a library-based analysis done with a large library may result an unacceptable number of false positives being reported. A normal working library suitable for analyzing environmental samples containing unknown materials may have over 1000 peaks, many of which are too close for deconvolution to be done accurately. A program has been written that uses a library-based analysis method that reduces the reporting of false positives, while retaining the ability to identify isotopes accurately from a large range of possibilities. In addition, the peak area calculation has been improved by allowing the energy calibration to be a free parameter in the fit of individual multiplets. This peak area improvement can result in a change of activity of several percent for some nuclides. In some cases, shifting the multiplet position can reduce false positives by identifying a peak in the multiplet as an unknown rather than associating it with a nuclide. One spectrum showed a marked peak activity improvement when the calibration was allowed to shift even though the the average error in the original calibration was 0.08%. Results obtained from a study on the identification of uranium decay products are presented.


2019 ◽  
Vol 322 (3) ◽  
pp. 1299-1303
Author(s):  
Takuto Kudo ◽  
Kazuhiko Ninomiya ◽  
Patrick Strasser ◽  
Kentaro Terada ◽  
Yosuke Kawai ◽  
...  

2008 ◽  
Vol 4 (S252) ◽  
pp. 333-338
Author(s):  
Wei Wang

AbstractGamma-ray line emission from radioactive decay of 60Fe provides constraints on nucleosynthesis in massive stars and supernovae. We detect the γ-ray lines from 60Fe decay at 1173 and 1333 keV using three years of data from the spectrometer SPI on board INTEGRAL. The average flux per line is (4.4 ± 0.9) × 10−5 ph cm−2 s−1 rad−1 for the inner Galaxy region. Deriving the Galactic 26Al gamma-ray line flux with using the same set of observations and analysis method, we determine the flux ratio of 60Fe/26Al gamma-rays as 0.15 ± 0.05. We discuss the implications of these results for the widely-held hypothesis that 60Fe is synthesized in core-collapse supernovae, and also for the closely-related question of the precise origin of 26Al in massive stars.


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