scholarly journals Near-intrinsic energy resolution for 30–662keV gamma rays in a high pressure xenon electroluminescent TPC

2013 ◽  
Vol 708 ◽  
pp. 101-114 ◽  
Author(s):  
V. Álvarez ◽  
F.I.G.M. Borges ◽  
S. Cárcel ◽  
J. Castel ◽  
S. Cebrián ◽  
...  
Keyword(s):  
High Pressure ◽  
Energy Resolution ◽  
Gamma Rays ◽  
Intrinsic Energy

Energy Resolution and Non-proportionality of Scintillation Detectors

2007 ◽  
Vol 1038 ◽  
Author(s):  
Marek Moszynski
Keyword(s):  
Liquid Nitrogen ◽  
Energy Resolution ◽  
Gamma Rays ◽  
Avalanche Photodiodes ◽  
Intrinsic Property ◽  
Liquid Nitrogen Temperature ◽  
Scintillation Detectors ◽  
Crucial Importance ◽  
Light Pulses ◽  
Intrinsic Energy

AbstractThe limitation of energy resolution of scintillation detectors are discussed with a special emphasis on non-proportionality response of scintillators to gamma rays and electrons, which is of crucial importance to an intrinsic energy resolution of the crystals. Examples of the study carried out with different crystals and particularly those of tests of undoped NaI and CsI at liquid nitrogen temperature with the light readout by avalanche photodiodes are presented suggesting strongly that the non-proportionality of the halide crystals are not their intrinsic property. Moreover, the influence of slow components of the light pulses on energy resolution and non-proportionality are discussed.

An ISPA-camera for gamma rays with improved energy resolution

1997 ◽  
Vol 44 (5) ◽  
pp. 1747-1752 ◽  
Author(s):  
D. Puertolas ◽  
D. Piedigrossi ◽  
H. Leutz ◽  
T. Gys ◽  
F. De Notaristefani ◽  
...  
Keyword(s):  
Energy Resolution ◽  
Gamma Rays

Usage of polarization approximation for the estimation of scintillator intrinsic energy resolution

2010 ◽  
Vol 45 (3-6) ◽  
pp. 258-261 ◽  
Author(s):  
A.N. Vasil'ev ◽  
I.A. Markov ◽  
A.S. Zakharov
Keyword(s):  
Energy Resolution ◽  
Intrinsic Energy

scholarly journals Secondary gamma rays excited by the passage of neutrons through matter

1935 ◽  
Vol 150 (871) ◽  
pp. 637-668 ◽  
Keyword(s):  
High Pressure ◽  
Gamma Rays ◽  
Alpha Particle ◽  
Ionization Chamber ◽  
Gamma Ray ◽  
Beta Particle ◽  
Nuclear Excitation ◽  
Ionization Chambers ◽  
Scattering Material ◽  
Pass Through

It is well known that the absorption of neutrons in their passage through matter is due to nuclear collisions, and not appreciably to interaction with extranuclear electrons. A collision of a neutron with a nucleus may result in the scattering of the neutron, or in the disintegration of the nucleus. The experiments of Feather and of Harkins, Gans, and Newson§ have shown that several light elements, C, N, O, F, Ne are disintegrated, the mechanism probably being absorption of the neutron and emission of an alpha particle. Fermi|| has reported that a variety of elements when bombarded by neutrons show the phenomenon of induced radioactivity, emitting beta rays. He suggests that the disintegration process takes place usually by absorption of a neutron and emission of an alpha particle or proton, the resulting nucleus being an unstable radio element, transforming into a stable body by emission of a beta particle. The experiments here to be described show that when neutrons pass through various substances, gamma rays are produced. The origin of this radiation has not definitely been established; nuclear excitation appears to be the most plausible explanation in most cases. 2—Experimental Method The general method consisted in measuring the ionization current produced by a Po + Be source (usually of about 10-15 millicuries) placed above a high pressure ionization chamber, and observing the increased ionization when a block of scattering material was placed immediately above the source. A correction was applied for the diminution of the natural effect caused by the scatterer. The increase in ionization amounted usually to 2-3%, and thus to obtain even a rough measurement of the effect, accurate measurements of the ionization currents were required. For this reason the high pressure ionization chamber was usually used in preference to the counter, since measurements to one part in a thousand are impracticable with the latter. The ionization method has, however, the disadvantage that both gamma rays and neutrons are detected. To distinguish between the two radiations, two similar ionization chambers were used, one containing argon at a pressure of 90 atmospheres, the other hydrogen at about 60 atmospheres. The former is more sensitive to gamma radiation, the latter to neutrons. The ionization chambers were of steel and had cylindrical walls 1 cm thick; the radiations entered through the roofs of the chambers, which were 2·5 cm thick. The inside dimensions were 16 cm high and 12 cm diameter, with a 2-cm diameter central electrode. Collecting potentials of 250-500 volts were used. Measurements were made by a balance method and followed standard practice. From the measurements of ionization currents in argon and hydrogen estimates may be made of the neutron ( n ) and gamma ray (γ) intensities separately. The method by which this is achieved is described in § 11.

scholarly journals High intrinsic energy resolution photon number resolving detectors

2013 ◽  
Vol 103 (4) ◽  
pp. 041107 ◽  
Author(s):  
L. Lolli ◽  
E. Taralli ◽  
C. Portesi ◽  
E. Monticone ◽  
M. Rajteri
Keyword(s):  
Energy Resolution ◽  
Photon Number ◽  
Intrinsic Energy

scholarly journals Revealing x-ray and gamma ray temporal and spectral similarities in the GRB 190829A afterglow

Science ◽  
2021 ◽  
Vol 372 (6546) ◽  
pp. 1081-1085
Author(s):  
◽  
H. Abdalla ◽  
F. Aharonian ◽  
F. Ait Benkhali ◽  
E. O. Angüner ◽  
...  
Keyword(s):  
Gamma Rays ◽  
Gamma Ray ◽  
High Energy ◽  
X Ray ◽  
Photon Index ◽  
Very High Energy ◽  
Stereoscopic System ◽  
Very High ◽  
Intrinsic Energy

Gamma-ray bursts (GRBs), which are bright flashes of gamma rays from extragalactic sources followed by fading afterglow emission, are associated with stellar core collapse events. We report the detection of very-high-energy (VHE) gamma rays from the afterglow of GRB 190829A, between 4 and 56 hours after the trigger, using the High Energy Stereoscopic System (H.E.S.S.). The low luminosity and redshift of GRB 190829A reduce both internal and external absorption, allowing determination of its intrinsic energy spectrum. Between energies of 0.18 and 3.3 tera–electron volts, this spectrum is described by a power law with photon index of 2.07 ± 0.09, similar to the x-ray spectrum. The x-ray and VHE gamma-ray light curves also show similar decay profiles. These similar characteristics in the x-ray and gamma-ray bands challenge GRB afterglow emission scenarios.

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