EUSO-TA is a ground-based experiment, placed at Black Rock Mesa of the Telescope Array site as a part of the JEM-EUSO (Joint Experiment Missions for the Extreme Universe Space Observatory) program. The UV fluorescence imaging telescope with a field of view of about 10.6◦ x 10.6◦ consisting of 2304 pixels (36 Multi-Anode Photomultipliers, 64 pixels each) works with 2.5-microsecond time resolution. An experimental setup with two Fresnel lenses allows for measurements of Ultra High Energy Cosmic Rays in parallel with the TA experiment as well as the other sources like flashes of lightning, artificial signals from UV calibration lasers, meteors and stars. Stars increase counts on pixels while crossing the field of view as the point-like sources. In this work, we discuss the method for calibration of EUSO fluorescence detectors based on signals from stars registered by the EUSO-TA experiment during several campaigns. As the star position is known, the analysis of signals gives an opportunity to determine the pointing accuracy of the detector. This can be applied to space-borne or balloon-borne EUSO missions. We describe in details the method of the analysis which provides information about detector parameters like the shape of the point spread function and is the way to perform absolute calibration of EUSO cameras. © Copyright owned by the author(s).

Study of the calibration method using the stars measured by the EUSO-TA telescope

Plebaniak Z.;Barghini D.;Bertaina M.;Bisconti F.;Casolino M.;Gardiol D.;Shinozaki K.;Arnone E.;Bartocci S.;Blanc N.;Bozzo E.;Cassardo C.;Cellino A.;Cotto G.;Cremonini R.;Ferrarese S.;Franchini S.;Galeotti P.;Golzio A.;Kajino F.;Miyamoto H.;Neronov A.;Pagliaro A.;Perfetto F.;Piraino S.;Pollini A.;Scagliola A.;Suzuki M.;Vigorito C.;
2022-01-01

Abstract

EUSO-TA is a ground-based experiment, placed at Black Rock Mesa of the Telescope Array site as a part of the JEM-EUSO (Joint Experiment Missions for the Extreme Universe Space Observatory) program. The UV fluorescence imaging telescope with a field of view of about 10.6◦ x 10.6◦ consisting of 2304 pixels (36 Multi-Anode Photomultipliers, 64 pixels each) works with 2.5-microsecond time resolution. An experimental setup with two Fresnel lenses allows for measurements of Ultra High Energy Cosmic Rays in parallel with the TA experiment as well as the other sources like flashes of lightning, artificial signals from UV calibration lasers, meteors and stars. Stars increase counts on pixels while crossing the field of view as the point-like sources. In this work, we discuss the method for calibration of EUSO fluorescence detectors based on signals from stars registered by the EUSO-TA experiment during several campaigns. As the star position is known, the analysis of signals gives an opportunity to determine the pointing accuracy of the detector. This can be applied to space-borne or balloon-borne EUSO missions. We describe in details the method of the analysis which provides information about detector parameters like the shape of the point spread function and is the way to perform absolute calibration of EUSO cameras. © Copyright owned by the author(s).
2022
37 th International Cosmic Ray Conference (ICRC 2021)
Berlin
July 12th – 23rd, 2021
395
1
12
https://www.scopus.com/inward/record.uri?eid=2-s2.0-85145552432&partnerID=40&md5=bdf9f25e9a5f6b38f71da09f9db9987f
Calibration; Cosmic rays; Cosmology; Fluorescence imaging; Gamma rays; Optical transfer function; Pixels; Signal detection; Telescopes; Calibration method; Field of views; Fluorescence imaging; Fresnel lens; Ground based; Multianode photo multipliers; Space observatories; Telescope arrays; Time-resolution; UV Fluorescence; Stars
Plebaniak Z.; Przybylak M.; Barghini D.; Bertaina M.; Bisconti F.; Casolino M.; Gardiol D.; Lipiec R.; Piotrowski L.W.; Shinozaki K.; Szabelski J.; Abdellaoui G.; Abe S.; Adams J.H.; Ahriche A.; Allard D.; Alonso G.; Anchordoqui L.; Anzalone A.; Arnone E.; Asano K.; Attallah R.; Attoui H.; Ave Pernas M.; Bacholle S.; Baláz J.; Bakiri M.; Yashin I.V.; Bartocci S.; Battisti M.; Bayer J.; Beldjilali B.; Belenguer T.; Belkhalfa N.; Bellotti R.; Belov A.; Benmessai K.; Yonetoku D.; Bertone P.; Biermann P.L.; Yoshida S.; Blaksley C.; Blanc N.; Blin-Bondil S.; Bobik P.; Bogomilov M.; Bozzo E.; Briz S.; Bruno A.; Caballero K.S.; Cafagna F.; Cambie G.; Campana D.; Capdevielle J.-N.; Capel F.; Caramete A.; Caramete L.; Carlson P.; Caruso R.; Yano H.; Cassardo C.; Castellina A.; Catalano O.; Cellino A.; Cerny K.; Chikawa M.; Chiritoi G.; Christl M.J.; Colalillo R.; Conti L.; Cotto G.; Crawford H.J.; Cremonini R.; Creusot A.; de Castro Gónzalez A.; de la Taille C.; del Peral L.; Diaz Damian A.; Diesing R.; Djakonow A.; Djemil T.; Ebersoldt A.; Ebisuzaki T.; Engel R.; Eliasson L.; Eser J.; Fenu F.; Fernández-González S.; Ferrarese S.; Fillapatos G.; Fornaro C.; Fouka M.; Franceschi A.; Franchini S.; Fuglesang C.; Fujii T.; Fukushima M.; Galeotti P.; García-Ortega E.; Young R.; Garipov G.; Gascón E.; Genci J.; Golzio A.; González Alvarado C.; Gorodetzky P.; Green A.; Guarino F.; Guzmán A.; Hachisu Y.; Haungs A.; Hernández Carretero J.; Hulett L.; Ikeda D.; Inoue N.; Inoue S.; Isgrò F.; Itow Y.; Jammer T.; Jeong S.; Joven E.; Judd E.G.; Jochum J.; Kajino F.; Kajino T.; Kalli S.; Kaneko I.; Karadzhov Y.; Kasztelan M.; Katahira K.; Kawai K.; Kawasaki Y.; Kedadra A.; Khales H.; Khrenov B.A.; Kungel V.; Kim Jeong-Sook; Kim Soon-Wook; Kleifges M.; Klimov P.A.; Kolev D.; Kreykenbohm I.; Krizmanic J.F.; Królik K.; Kurihara Y.; Kusenko A.; Kuznetsov E.; Lahmar H.; Lakhdari F.; Licandro J.; López Campano L.; López Martínez F.; Mackovjak S.; Mahdi M.; Mandat D.; Marcelli L.; Marcos J.L.; Marszał W.; Martín Y.; Martinez O.; Mase K.; Matev R.; Matthews J.N.; Mebarki N.; Medina-Tanco G.; Menshikov A.; Merino A.; Meseguer J.; Meyer S.S.; Mimouni J.; Miyamoto H.; Mizumoto Y.; Monaco A.; Morales de los Ríos J.A.; Mastafa M.; Nagataki S.; Naitamor S.; Napolitano T.; Neronov A.; Nomoto K.; Nonaka T.; Ogawa T.; Ogio S.; Ohmori H.; Olinto A.V.; Osteria G.; Otte A.N.; Pagliaro A.; Painter W.; Panasyuk M.I.; Panico B.; Parizot E.; Park I.H.; Pastircak B.; Paul T.; Pech M.; Pérez-Grande I.; Perfetto F.; Peter T.; Picozza P.; Pindado S.; Zotov M.Yu.; Piraino S.; Plebanlak Z.; Pollini A.; Popescu E.M.; Prevete R.; Prévôt G.; Prieto H.; Puehlhofer G.; Putis M.; Reardon P.; Reyes M.; Ricci M.; Rodríguez Frías M.D.; Romero Matamala O.F.; Ronga F.; Rusinov I.; Sabau M.D.; Saccá G.; Sáez Cano G.; Sagawa H.; Sahnoune Z.; Saito A.; Sakaki N.; Salazar H.; Sanchez Balanzar J.C.; Sánchez J.L.; Santangelo A.; Sanz-Andrés A.; Sanz Palomino M.; Saprykin O.; Sarazin F.; Sato M.; Scagliola A.; Schanz T.; Schieler H.; Schovanek P.; Scotti V.; Serra M.; Sharakin S.; Shimizu H.M.; Zgura I.S.; Shirahama T.; Soriano J.F.; Sotgiu A.; Stan I.; Strharský I.; Sugiyama N.; Supanitsky D.; Suzuki M.; Zuccarello F.; Tajima N.; Tajima T.; Takahashi Y.; Takeda M.; Takizawa Y.; Talai M.C.; Zuccaro Marchi A.; Tenzer C.; Thomas S.B.; Tibolla O.; Tkachev L.; Tomida T.; Tone N.; Toscano S.; Traïche M.; Tsenov R.; Tsunesada Y.; Tsuno K.; Turriziani S.; Uchihori Y.; Vaduvescu O.; Valdés-Galicia J.F.; Vallania P.; Valore L.; Vankova L.; Venters T.; Vigorito C.; Villaseñor L.; Vlcek B.; von Ballmoos P.; Vrabel M.; Wada S.; Watanabe J.; Watts J.; Weber M.; Weigand Muñoz R.; Weindl A.; Wiencke L.; Wille M.; Wilms J.; Yamamoto T.; Yang J.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2318/1929330
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