The TIGRE gamma-ray telescope

O'Neill, T. J.; Bhattacharya, D.; Dixon, David; Polson, Matthew I. J.; White, R. S.; Zych, A. D.; Ryan, J.; McConnell, M.; Macri, J.; Samimi, J.; Akyüz, A.; Mahoney, W. M.; Varnell, L.

doi:10.1063/1.1303309

Cited by 13 publications

(6 citation statements)

References 1 publication

(1 reference statement)

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“…Toward this end, however, we have studied competing technologies that could either augment or supplant those chosen for the baseline design. These include thin Si [29,19], liquid Xe (LXe) [2][3][4], CdZnTe [37,25,30], LaBr scintillator [39], and gaseous Xe (GXe) detectors [6,12,13]. Each of these detectors possesses capabilities that could potentially improve the performance over the baseline instrument-in terms of electron tracking (thin Si, GXe), fast timing (LXe, LaBr, GXe), or room-temperature operation (CdZnTe, LaBr).…”

Section: Baseline Science Instrumentmentioning

confidence: 99%

The Advanced Compton Telescope

et al. 2006

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The Advanced Compton Telescope (ACT), the next major step in gamma-ray astronomy, will probe the fires where chemical elements are formed by enabling high-resolution spectroscopy of nuclear emission from supernova explosions. During the past two years, our collaboration has been undertaking a NASA mission concept study for ACT. This study was designed to (1) transform the key scientific objectives into specific instrument requirements, (2) to identify the most promising technologies to meet those requirements, and (3) to design a viable mission concept for this instrument. We present the results of this study, including scientific goals and expected performance, mission design, and technology recommendations.

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Section: Baseline Science Instrumentmentioning

confidence: 99%

The Advanced Compton Telescope

et al. 2006

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“…4 Compton telescopes using silicon detectors for astrophysics have been proposed and ground based prototypes have been created over a number of years. [5][6][7] All of these configurations use the silicon detectors to Compton scatter the incident gamma ray and then have a scintillation detector or high atomic number semiconductor absorber behind it. This configuration allows for complete absorption of the gamma-ray energy after a Compton scattering event in the silicon.…”

Section: Silicon Detectorsmentioning

confidence: 99%

Prototype Compton imager for special nuclear material

Wulf

Phlips

Kurfess

et al. 2006

Non-Intrusive Inspection Technologies

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Compton imagers offer a method for passive detection of nuclear material over background radiation. A prototype Compton imager has been constructed using 8 layers of silicon detectors. Each layer consists of a 2×2 array of 2 mm thick cross-strip double-sided silicon detectors with active areas of 5.7 × 5.7 cm 2 and 64 strips per side. The detectors are daisy-chained together in the array so that only 256 channels of electronics are needed to read-out each layer of the instrument. This imager is a prototype for a large, high-efficiency Compton imager that will meet operational requirements of Homeland Security for detection of shielded uranium. The instrument can differentiate between different radioisotopes using the reconstructed gamma-ray energy and can also show the location of the emissions with respect to the detector location. Results from the current instrument as well as simulations of the next generation instrument are presented.

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“…For thick wafers (≈ 500 µm [47,48,49,50,51,52]), the effective polarization asymmetry, and therefore the dilution factor, are still low because multiple scattering remains an issue. It's only if very thin wafers can be made, held and launched (≈ 150 µm [53]) that there is some hope of a sizeable sensitivity to polarization (see Figs.…”

Section: γ-Ray Polarimetry With Pairs: Techniquesmentioning

confidence: 99%

γ-Ray polarimetry with conversions to e+e− pairs: Polarization asymmetry and the way to measure it

Gros

Bernard

2017

Astroparticle Physics

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We revisit the measurement of the polarization fraction, P , and the measurement of the polarization angle of partially linearly-polarized gamma rays using their conversion to e + e − pairs in the field of a nucleus. We show that an inappropriate definition of the azimuthal angle, ϕ, used to reference the orientation of the final state degrades the precision of the measurement of P , by comparison to the optimal case where the bisector angle of the electron and of the positron momenta is used. We then focus on the lowest part of the energy spectrum, below ≈ 10 MeV, where a large part of the statistics lie for a cosmic source. We obtain the value of the polarization asymmetry, A, of pair conversion at threshold and we show that in the case where the correct expression is used for ϕ, the measured value of A tends to the limit.

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The TIGRE gamma-ray telescope

Cited by 13 publications

References 1 publication

The Advanced Compton Telescope

The Advanced Compton Telescope

Prototype Compton imager for special nuclear material

γ-Ray polarimetry with conversions to e+e− pairs: Polarization asymmetry and the way to measure it

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