Simulation study for the proposed wide field-of-view gamma-ray detector array ALTO
Gorde:
| Argitaratua izan da: | arXiv.org (Aug 3, 2017), p. n/a |
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| Egile nagusia: | |
| Beste egile batzuk: | , |
| Argitaratua: |
Cornell University Library, arXiv.org
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| Gaiak: | |
| Sarrera elektronikoa: | Citation/Abstract Full text outside of ProQuest |
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| LEADER | 00000nab a2200000uu 4500 | ||
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| 001 | 2075723031 | ||
| 003 | UK-CbPIL | ||
| 022 | |a 2331-8422 | ||
| 035 | |a 2075723031 | ||
| 045 | 0 | |b d20170803 | |
| 100 | 1 | |a Thoudam, Satyendra | |
| 245 | 1 | |a Simulation study for the proposed wide field-of-view gamma-ray detector array ALTO | |
| 260 | |b Cornell University Library, arXiv.org |c Aug 3, 2017 | ||
| 513 | |a Working Paper | ||
| 520 | 3 | |a ALTO is a wide field-of-view air shower detector array for very-high-energy (VHE) gamma-ray astronomy, proposed to be installed in the Southern Hemisphere at an altitude of about 5.1 km above sea level. The array will use water Cherenkov detectors, as in the HAWC observatory, but combined with scintillator detectors, to detect air showers induced by VHE gamma rays in the atmosphere. It is being designed to attain a lower energy threshold, better energy and angular resolution, and improved sensitivity. The array will consist of about 1250 small-sized (3.6 m diameter) detector units distributed over a circular area of about 160 m in diameter. Each detector unit will consist of a water Cherenkov detector and a liquid scintillation detector underneath which will preferentially identify muons, facilitating the background (cosmic ray) rejection, thereby improving the sensitivity. The background rejection will be further enhanced by the close-packed arrangement and the small size of the detectors which will allow a fine sampling of air-shower footprints at the ground. In this contribution, we present the Monte-Carlo simulation of the experiment performed using CORSIKA and GEANT4 simulation packages. The expected performance of the array in terms of reconstruction accuracies of the shower core and arrival direction, as well as preliminary estimate of the trigger energy threshold after preliminary selection cuts for a point-like gamma-ray source are presented. | |
| 653 | |a Cosmic rays | ||
| 653 | |a Sensors | ||
| 653 | |a Gamma rays | ||
| 653 | |a Cerenkov counters | ||
| 653 | |a Detectors | ||
| 653 | |a Sea level | ||
| 653 | |a High energy astronomy | ||
| 653 | |a Astronomy | ||
| 653 | |a Rejection | ||
| 653 | |a Sensitivity | ||
| 653 | |a Cosmic ray showers | ||
| 653 | |a Angular resolution | ||
| 653 | |a Southern Hemisphere | ||
| 653 | |a Gamma ray detectors | ||
| 653 | |a Scintillation counters | ||
| 653 | |a Arrays | ||
| 653 | |a Background radiation | ||
| 653 | |a Computer simulation | ||
| 653 | |a Muons | ||
| 653 | |a Field of view | ||
| 653 | |a Monte Carlo simulation | ||
| 700 | 1 | |a Becherini, Yvonne | |
| 700 | 1 | |a Punch, Michael | |
| 773 | 0 | |t arXiv.org |g (Aug 3, 2017), p. n/a | |
| 786 | 0 | |d ProQuest |t Engineering Database | |
| 856 | 4 | 1 | |3 Citation/Abstract |u https://www.proquest.com/docview/2075723031/abstract/embedded/H09TXR3UUZB2ISDL?source=fedsrch |
| 856 | 4 | 0 | |3 Full text outside of ProQuest |u http://arxiv.org/abs/1708.01059 |