Inverted-conical light guide for crosstalk reduction in tightly-packed scintillator matrix and MAPMT assembly

Chang, Yuhua; Chen, C. R.; Chen, P.; Huang, J. J.; Huang, M. A.; Liu, T. C.; Nam, J. W.; Wang, M. Z.; Bogomolov, V. V.; Brandt, S.; Budtz-Jørgensen, Carl; Castro-Tirado, A. J.; Choi, Hanshin; Connell, P.; Eyles, C. J.; Jeong, S.; Kim, J. E.; Kim, M. B.; Kim, S. W.; Lee, J.; Lim, H.; Min, Kyoung Wook; Panasyuk, M. I.; Park, I. H.; Petrov, V.; Reglero, V.; Řípa, J.; Rodrigo, J. M.; Свертилов, С. И.; Yashin, I. V.

doi:10.1016/j.nima.2014.10.037

Cited by 9 publications

(7 citation statements)

References 20 publications

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“…Therefore we can make conclusion that secondary particles can't make big effect to make clusters on UBAT detector. Gammas sometimes make clusters smaller than 3 × 3 by cross-talk effects, but because of experimental signal yield is 0.72photoelectron/keV and probability to occur cross-talk is 8% for diagonal and 29% for alongside [6], gamma can't make big cluster within UBAT's sensitive energy range from 5 keV to 200 keV .…”

Section: Discussionmentioning

confidence: 99%

Comparison cosmic ray irradiation simulation and particle beam test on UFFO Burst Alert & Trigger telescope(UBAT) detectors

Jeong

Kim

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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Section: Discussionmentioning

confidence: 99%

Comparison cosmic ray irradiation simulation and particle beam test on UFFO Burst Alert & Trigger telescope(UBAT) detectors

Jeong

Kim

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…The second data flow belongs to trigger calculation: raw data are passed to a "hit finding" or detection algorithm to remove the crosstalk that occurs when scintillation photons intrude upon neighboring MAPMT pixels, generating spurious signals. Such signals make it difficult to identify GRB coordinates via the coded mask technique; and a detailed study of mechanical crosstalk reduction is available in an excellent report by Chang et al 2015. However, to maintain simplicity in the design of the structural assembly of the MAPMT and YSO detectors, we decided to reduce crosstalk using a hit finding algorithm and through the adjustment of the threshold values for photon counting on the analog boards.…”

Section: Data Processing Unitmentioning

confidence: 99%

UBAT of UFFO/Lomonosov: The X-Ray Space Telescope to Observe Early Photons from Gamma-Ray Bursts

et al. 2017

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The Ultra-Fast Flash Observatory (UFFO) Burst Alert and Trigger Telescope (UBAT) has been designed and built for the localization of transient X-ray sources such as Gamma Ray Bursts (GRBs). As one of main instruments in the UFFO payload onboard the Lomonosov satellite (hereafter UFFO/Lomonosov), the UBAT's roles are to monitor the X-ray sky, to rapidly locate and track transient sources, and to trigger the slewing of a UV/optical telescope, namely Slewing Mirror Telescope (SMT). The SMT, a pioneering application of rapid slewing mirror technology has a line of sight parallel to the UBAT, allowing us to measure the early UV/optical GRB counterpart and study the extremely early moments of GRB evolution. To detect X-rays, the UBAT utilizes a 191.1 cm 2 scintillation detector composed of Yttrium Oxyorthosilicate (YSO) crystals, Multi-Anode Photomultiplier Tubes (MAPMTs), and associated electronics. To estimate a direction vector of a GRB source in its field of view, it employs the well-known coded aperture mask technique. All functions are written for implementation on a field programmable gate array to enable fast triggering and to run the device's imaging algorithms. The UFFO/Lomonosov satellite was launched on April 28, 2016, and is now collecting GRB observation data. In this study, we describe the UBAT's design, fabrication, integration, and performance as a GRB X-ray trigger and localization telescope, both on the ground and in space.

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“…The recorded data were processed off-line with analysis software which used a geometrical center hit-finder to eliminate the optical crosstalk caused by total reflections at the glass-vacuum (photo-cathode) interface [6]. There were 30 460 registered counts due to the background and 137 256 counts due to the source, and the area of the enabled detector pixels was 160.2 cm 2 thus giving a count rate due to the source of 4.6 cnt s −1 cm −2 .…”

Section: Pixel-to-pixel Responsementioning

confidence: 99%

“…It consists of two scientific instruments. One is the UFFO Burst Alert & Trigger telescope (UBAT) [4,5,6] which employs the coded mask technique providing X-ray/gamma-ray imaging observations in the energy range of 10 − 150 keV with half-coded field of view (FOV) 70.4 • × 70.4 • and angular resolution ≤ 10 . The second instrument is the Slewing Mirror Telescope (SMT) [7,8] with the field of view of 17 × 17 and optical/ultraviolet range of 200 − 650 nm.…”

Section: Introduction and Description Of Ubatmentioning

confidence: 99%

Testing and Performance of UFFO Burst Alert & Trigger Telescope

Řípa

Kim

Lee

et al. 2015

Proceedings of Swift: 10 Years of Discovery — PoS(SWIFT 10)

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Inverted-conical light guide for crosstalk reduction in tightly-packed scintillator matrix and MAPMT assembly

Cited by 9 publications

References 20 publications

Comparison cosmic ray irradiation simulation and particle beam test on UFFO Burst Alert & Trigger telescope(UBAT) detectors

Comparison cosmic ray irradiation simulation and particle beam test on UFFO Burst Alert & Trigger telescope(UBAT) detectors

UBAT of UFFO/Lomonosov: The X-Ray Space Telescope to Observe Early Photons from Gamma-Ray Bursts

Testing and Performance of UFFO Burst Alert & Trigger Telescope

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