PICsIT: the high-energy detection plane of the IBIS instrument onboard INTEGRAL

1996 ◽  
Author(s):  
Claudio Labanti ◽  
Guido Di Cocco ◽  
Giuseppe Malaguti ◽  
Alessandro Mauri ◽  
Elio Rossi ◽  
...  
Keyword(s):  
Energy Detection ◽  
High Energy ◽  
Detection Plane

Prospects for High Energy Detection of Microquasars with the AGILE and GLAST Gamma‐Ray Telescopes

2007 ◽  
Author(s):  
Patrizia Santolamazza ◽  
Carlotta Pittori ◽  
Francesco Verrecchia
Keyword(s):  
Gamma Ray ◽  
Energy Detection ◽  
High Energy ◽  
Gamma Ray Telescopes

The use of Schottky CdTe detectors for high-energy astronomy: application to the detection plane of the instrument SVOM/ECLAIRs

2014 ◽  
Author(s):  
G. Nasser ◽  
O. Godet ◽  
J.-L. Atteia ◽  
C. Amoros ◽  
D. Barret ◽  
...  
Keyword(s):  
High Energy ◽  
Detection Plane

scholarly journals INTEGRAL high energy detection of the transient IGR J11321–5311

2007 ◽  
Vol 468 (1) ◽  
pp. L21-L24 ◽  
Author(s):  
V. Sguera ◽  
A. Bazzano ◽  
A. J. Bird ◽  
A. B. Hill ◽  
A. J. Dean ◽  
...  
Keyword(s):  
Energy Detection ◽  
High Energy

scholarly journals e- discrimination at high energy in the JUNO detector

2019 ◽  
Vol 209 ◽  
pp. 01011
Author(s):  
Giulio Settanta ◽  
Stefano Maria Mari ◽  
Cristina Martellini ◽  
Paolo Montini
Keyword(s):  
Neutrino Oscillation ◽  
Liquid Scintillator ◽  
Detection Threshold ◽  
Atmospheric Neutrino ◽  
Neutrino Flux ◽  
Cosmic Ray ◽  
Energy Detection ◽  
High Energy ◽  
Low Energy ◽  
Temporal Behaviour

Cosmic Ray and neutrino oscillation physics can be studied by using atmospheric neutrinos. JUNO (Jiangmen Underground Neutrino Observatory) is a large liquid scintillator detector with low energy detection threshold and excellent energy resolution. The detector performances allow the atmospheric neutrino oscillation measurements. In this work, a discrimination algorithm for different reaction channels of neutrino-nucleon interactions in the JUNO liquid scintillator, in the GeV/sub-GeV energy region, is presented. The atmospheric neutrino flux is taken as reference, considering $\mathop {{v_\mu }}\limits^{( - )} $ and $\mathop {{v_e}}\limits^{( - )} $. The different temporal behaviour of the classes of events have been exploited to build a timeprofile-based discrimination algorithm. The results show a good selection power for $\mathop {{v_e}}\limits^{( - )} $ CC events, while the $\mathop {{v_\mu }}\limits^{( - )} $ CC component suffers of an important contamination from NC events at low energy, which is under study. Preliminary results are presented.

Luminescence and cathodoluminescent properties of monoclinic Y2WO6 co-doped with Dy-Bi

2017 ◽  
Vol 31 (24) ◽  
pp. 1750182 ◽  
Author(s):  
Peiju Hu ◽  
Wei Zhang ◽  
Zhengfa Hu ◽  
Zuyong Feng ◽  
Lun Ma ◽  
...  
Keyword(s):  
Light Emission ◽  
Energy Detection ◽  
High Energy ◽  
Effect Of Temperature ◽  
Solid State Method ◽  
X Ray ◽  
Light Excitation ◽  
Promising Application ◽  
Resistance Stability ◽  
Co Doped

Dy-Bi co-doped yttrium tungstate crystal materials were synthesized by high temperature solid-state method. To reveal the photoluminescence features and properties of the samples, some measurements have been taken. It turned out that different Bi[Formula: see text] concentrations play obvious influence in emission performance, and show visible light emission under ultraviolet light excitation. Besides, the effect of temperature on phase structure of samples has also been studied here. Superhigh X-ray luminescence of the phosphors exhibited the promising application in the field of high energy detection. The X-ray irradiation crystal resistance stability of the phosphors has also been investigated through the subsequent testing of XRD and spectra.

scholarly journals A Brewster route to Cherenkov detectors

2021 ◽  
Vol 12 (1) ◽  
Author(s):  
Xiao Lin ◽  
Hao Hu ◽  
Sajan Easo ◽  
Yi Yang ◽  
Yichen Shen ◽  
...  
Keyword(s):  
Refractive Index ◽  
Incident Angle ◽  
Photon Number ◽  
Visible Spectrum ◽  
High Energy ◽  
Particle Identification ◽  
Cherenkov Detectors ◽  
Host Materials ◽  
Detection Plane ◽  
Filtering Effect

AbstractCherenkov detectors enable a valuable tool to identify high-energy particles. However, their sensitivity and momentum coverage are limited by the refractive index of host materials. Especially, identifying particles with energy above multiple gigaelectronvolts requires host materials with a near-unity refractive index, which are limited to bulky gas chambers. Overcoming this fundamental material limit is important for future particle detectors yet remains a long-standing challenge. Here, we propose a different paradigm for Cherenkov detectors that utilizes the broadband angular filter made from stacks of variable one-dimensional photonic crystals. Owing to the Brewster effect, the angular filter is transparent only to Cherenkov photons from a precise incident angle. Particle identification is achieved by mapping each Cherenkov angle to the peak-intensity position of transmitted photons in the detection plane. Such angular filtering effect, although decreases the photon number collected in the detection plane, enables the realization of a non-dispersive pseudo refractive index over the entire visible spectrum. Moreover, the pseudo refractive index can be flexibly designed to different values close to unity. Our angular-selective Brewster paradigm offers a feasible solution to implement compact and highly sensitive Cherenkov detectors especially in beam lines with a small angular divergence using regular dielectrics.

scholarly journals Improved Analysis of COMPTEL Solar Neutron Data, with Application to the 15 June 1991 Flare

2001 ◽  
Vol 203 ◽  
pp. 573-576
Author(s):  
M. P. Toner ◽  
J. M. Ryan ◽  
A. L. MacKinnon ◽  
D. Bhattacharya ◽  
K. P. Macpherson ◽  
...  
Keyword(s):  
Instrumental Response ◽  
Energy Detection ◽  
High Energy ◽  
Ion Acceleration ◽  
Energy Measurement ◽  
Response Matrix ◽  
Neutron Data ◽  
Neutron Detectors ◽  
Solar Neutron ◽  
Incomplete Model

Direct solar flare neutrons are a valuable diagnostic of high-energy ion acceleration in these events, and COMPTEL improves over all previous cosmic neutron detectors in its capacity for neutron energy measurement. Previous studies of COMPTEL neutron data have worked with an incomplete model of the instrumental response, applying energy-by-energy detection efficiencies. Here we employ statistical regularisation techniques with the full (Monte Carlo simulation derived) response matrix to produce improved estimates of neutron numbers and energy distribution. These techniques are applied to data from the well-observed 15 June 1991 flare. Our improved treatment of the instrumental response results in a reduction of 73% in total neutron numbers, compared with previously deduced values. Implications for the picture of primary ion acceleration in this flare are briefly discussed.

The E-ring: interactions with plasma and implications for its evolution

1984 ◽  
Vol 75 ◽  
pp. 599-602
Author(s):  
T.V. Johnson ◽  
G.E. Morfill ◽  
E. Grun
Keyword(s):  
Time Scale ◽  
Particle Density ◽  
High Energy ◽  
Particle Removal ◽  
Density Region ◽  
Drag Forces ◽  
Orbit Evolution ◽  
History Of ◽  
Ring Particle ◽  
Ring Material

A number of lines of evidence suggest that the particles making up the E-ring are small, on the order of a few microns or less in size (Terrile and Tokunaga, 1980, BAAS; Pang et al., 1982 Saturn meeting; Tucson, AZ). This suggests that a variety of electromagnetic and plasma affects may be important in considering the history of such particles. We have shown (Morfill et al., 1982, J. Geophys. Res., in press) that plasma drags forces from the corotating plasma will rapidly evolve E-ring particle orbits to increasing distance from Saturn until a point is reached where radiation drag forces acting to decrease orbital radius balance this outward acceleration. This occurs at approximately Rhea's orbit, although the exact value is subject to many uncertainties. The time scale for plasma drag to move particles from Enceladus' orbit to the outer E-ring is ~104yr. A variety of effects also act to remove particles, primarily sputtering by both high energy charged particles (Cheng et al., 1982, J. Geophys. Res., in press) and corotating plasma (Morfill et al., 1982). The time scale for sputtering away one micron particles is also short, 102 - 10 yrs. Thus the detailed particle density profile in the E-ring is set by a competition between orbit evolution and particle removal. The high density region near Enceladus' orbit may result from the sputtering yeild of corotating ions being less than unity at this radius (e.g. Eviatar et al., 1982, Saturn meeting). In any case, an active source of E-ring material is required if the feature is not very ephemeral - Enceladus itself, with its geologically recent surface, appears still to be the best candidate for the ultimate source of E-ring material.

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