Cosmic component of the background counting rate of a scintillation detector

1981 ◽  
Vol 51 (5) ◽  
pp. 745-746
Author(s):  
I. F. Lukashin
Keyword(s):  
Scintillation Detector ◽  
Counting Rate ◽  
Background Counting Rate ◽  
Background Counting

Principal components of the background counting rate of a large scintillation detector

1980 ◽  
Vol 49 (1) ◽  
pp. 475-479
Author(s):  
Yu. V. Sivintsev ◽  
G. A. Nezhdanov ◽  
E. L. Koval'chuk ◽  
K. V. Voronin ◽  
S. P. Pugachev
Keyword(s):  
Principal Components ◽  
Scintillation Detector ◽  
Counting Rate ◽  
Background Counting Rate ◽  
Background Counting

scholarly journals Study of Background Pulse Spectrum of an LSC System

Radiocarbon ◽  
1989 ◽  
Vol 31 (03) ◽  
pp. 342-351 ◽  
Author(s):  
Sigurđur A Einarsson ◽  
Páll Theodórsson
Keyword(s):  
Counting Rate ◽  
Liquid Scintillation ◽  
Collection Efficiency ◽  
Pulse Height ◽  
Pulse Height Spectrum ◽  
Light Collection ◽  
Background Counting Rate ◽  
Proportional Counters ◽  
Background Counting ◽  
Made In

Important advances have been made in reducing the background counting rate of gas proportional counters for14C dating through detailed and systematic study of the background components. Until recently, limited work has been reported on the study of the background of liquid scintillation counters (LSC). During the last few years, commercial systems with greatly reduced background have been introduced. It is shown that the best gas proportional counters and LSC have similar backgrounds for the same amount of sample material. Similar results with less effort may be expected with more detailed and fundamental knowledge of the components of the background of LSC. We report the results of a study of one photomultiplier LSC system where we research all parameters of importance: light collection efficiency, absorbed energy per photo-electron, pulse height spectrum and background counting rate.

An attempt to detect the positronium Lyman alpha spectral line

1963 ◽  
Vol 272 (1350) ◽  
pp. 363-370 ◽  
Keyword(s):  
Automatic System ◽  
Counting Rate ◽  
Optical Radiation ◽  
Optical Signal ◽  
Radioactive Source ◽  
Inert Gases ◽  
Background Counting Rate ◽  
Lyman Alpha ◽  
Negative Results ◽  
Background Counting

The possibility of optical radiation from the 2 p states of positronium is discussed, and an experimental attempt to detect the positronium Lyman α line is described. Photomultipliers were used in the attempted detection. Initially filters, and later a quartz monochromator, were employed as the dispersive elements. Positrons from a radioactive source were stopped in various inert gases, and the total optical signal was recorded by counting circuitry with an automatic system that eliminated background and sensitivity variations. It was estimated that if 1 in 1000 of the positrons stopped in the gas gave rise to a Lyman α emission, then a signal would have been obtained which would be about four times the observed standard deviation in the background counting rate. This peak was not observed, although light from excitation of the target gas was detected. These results are compared with the findings of other workers, and the possible reasons for these negative results are examined.

scholarly journals Parameters of a Radiocarbon Installation

Radiocarbon ◽  
1996 ◽  
Vol 38 (2) ◽  
pp. 375-384 ◽  
Author(s):  
Vladimir Z. Khait
Keyword(s):  
Measurement Errors ◽  
Counting Rate ◽  
Counting Efficiency ◽  
Additional Measurement ◽  
Laboratory Installation ◽  
Background Counting Rate ◽  
Poisson Statistics ◽  
Destabilizing Factors ◽  
Two Parameters ◽  
Background Counting

I aim to define instrumental parameters of a radiocarbon laboratory installation whereby one can estimate its precision and a maximum age up to which its measuring results are reliable. The commonly accepted factor of merit (FM) relates the precision of measurement to Poisson statistics. Unlike the FM, the proposed parameters show the extent to which a 14C laboratory is affected by destabilizing factors that could cause additional measurement errors. Assuming that all destabilizing factors produce either a change in counting efficiency or additional fluctuations of the background counting rate, I have derived two parameters for consideration.

scholarly journals Sudden changes in the intensity of high energy X-rays from Sco X-1

1970 ◽  
Vol 37 ◽  
pp. 104-106
Author(s):  
P. C. Agrawal ◽  
S. Biswas ◽  
G. S. Gokhale ◽  
V. S. Iyengar ◽  
P. K. Kunte ◽  
...  
Keyword(s):  
Counting Rate ◽  
High Energy ◽  
Field Of View ◽  
X Rays ◽  
Background Counting Rate ◽  
X Ray ◽  
The North ◽  
Residual Atmosphere ◽  
Flux Gate ◽  
Background Counting

In this note we wish to report briefly the observation of sudden changes in the intensity of Sco X-1 by a factor of about 3 recorded in the energy interval 29.9–52.3 keV on December 22, 1968 between 04 h 27 m and 05 h 53 m UT. The observation was made with an X-ray telescope flown in a balloon from Hyderabad, India. The balloon was launched at 0200 hr UT and reached the ceiling of 7.5 g/cm2 of residual atmosphere at 0435 hr UT. The X-ray telescope consisted of a NaI(T1) crystal with an area of 97.3 cm2 and thickness 4 mm, surrounded by both active and passive collimators. The telescope was mounted on an oriented platform which was programmed to look in four specified directions successively, of azimuths, Φ=0°, 110°, 180° and 310° (Φ=0° being North and Φ=90°, West), spending about 4 min in each direction during a cycle of period of about 16 min. The axis of the telescope was inclined at an angle of 32° with respect to the zenith. A pair of crossed flux gate magnetometers provided information every 8.2 sec on the azimuth of the telescope. The pulse heights from the X-ray detector were sorted into several channels extending from 10 to 120 keV. An Am241 source came into the field of view of the telescope once in 15 min for about 30 sec to provide in-flight calibration of the detector. The meridian transit of Sco X-1 was at 0454 hr UT. Just before the balloon reached the ceiling Sco X-1 was in the field of view of the telescope for 3 min and 41 sec. After the balloon reached ceiling, Sco X-1 was in the field of view of the telescope on five occasions between 0443 and 0553 hr UT. During the last observation, however, the balloon had lost altitude by about 1 g/cm2. The excess counts due to Sco X-1 were obtained by subtracting the counting rates corresponding to the North direction which did not include any known X-ray sources. The observation on Sco X-1 in the 1st cycle was made while the balloon was still ascending and consequently the interposed grammage was changing from 10.5 to 9.7 g/cm2. However, for the energy range under consideration, the change in the background counting rate was not significant and there cannot be any doubt regarding the genuineness of the excess counts recorded.

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