The gSeaGen code is a GENIE-based application developed to efficiently generate high statistics samples of events, induced by neutrino interactions, detectable in a neutrino telescope. The gSeaGen code is able to generate events induced by all neutrino flavours, considering topological differences between track-type and shower-like events. Neutrino interactions are simulated taking into account the density and the composition of the media surrounding the detector. The main features of gSeaGen are presented together with some examples of its application within the KM3NeT project. Program summary: Program Title: gSeaGen CPC Library link to program files: http://dx.doi.org/10.17632/ymgxvy2br4.1 Licensing provisions: GPLv3 Programming language: C++ External routines/libraries: GENIE [1] and its external dependencies. Linkable to MUSIC [2] and PROPOSAL [3]. Nature of problem: Development of a code to generate detectable events in neutrino telescopes, using modern and maintained neutrino interaction simulation libraries which include the state-of-the-art physics models. The default application is the simulation of neutrino interactions within KM3NeT [4]. Solution method: Neutrino interactions are simulated using GENIE, a modern framework for Monte Carlo event generators. The GENIE framework, used by nearly all modern neutrino experiments, is considered as a reference code within the neutrino community. Additional comments including restrictions and unusual features: The code was tested with GENIE version 2.12.10 and it is linkable with release series 3. Presently valid up to 5 TeV. This limitation is not intrinsic to the code but due to the present GENIE valid energy range. References: [1] C. Andreopoulos at al., Nucl. Instrum. Meth. A614 (2010) 87. [2] P. Antonioli et al., Astropart. Phys. 7 (1997) 357. [3] J. H. Koehne et al., Comput. Phys. Commun. 184 (2013) 2070. [4] S. Adrián-Martínez et al., J. Phys. G: Nucl. Part. Phys. 43 (2016) 084001.

gSeaGen: The KM3NeT GENIE-based code for neutrino telescopes

Castaldi P.;Filippini F.;Fusco L. A.;Illuminati G.;Levi G.;Margiotta A.;Pellegrino C.;Spurio M.;Versari F.;
2020

Abstract

The gSeaGen code is a GENIE-based application developed to efficiently generate high statistics samples of events, induced by neutrino interactions, detectable in a neutrino telescope. The gSeaGen code is able to generate events induced by all neutrino flavours, considering topological differences between track-type and shower-like events. Neutrino interactions are simulated taking into account the density and the composition of the media surrounding the detector. The main features of gSeaGen are presented together with some examples of its application within the KM3NeT project. Program summary: Program Title: gSeaGen CPC Library link to program files: http://dx.doi.org/10.17632/ymgxvy2br4.1 Licensing provisions: GPLv3 Programming language: C++ External routines/libraries: GENIE [1] and its external dependencies. Linkable to MUSIC [2] and PROPOSAL [3]. Nature of problem: Development of a code to generate detectable events in neutrino telescopes, using modern and maintained neutrino interaction simulation libraries which include the state-of-the-art physics models. The default application is the simulation of neutrino interactions within KM3NeT [4]. Solution method: Neutrino interactions are simulated using GENIE, a modern framework for Monte Carlo event generators. The GENIE framework, used by nearly all modern neutrino experiments, is considered as a reference code within the neutrino community. Additional comments including restrictions and unusual features: The code was tested with GENIE version 2.12.10 and it is linkable with release series 3. Presently valid up to 5 TeV. This limitation is not intrinsic to the code but due to the present GENIE valid energy range. References: [1] C. Andreopoulos at al., Nucl. Instrum. Meth. A614 (2010) 87. [2] P. Antonioli et al., Astropart. Phys. 7 (1997) 357. [3] J. H. Koehne et al., Comput. Phys. Commun. 184 (2013) 2070. [4] S. Adrián-Martínez et al., J. Phys. G: Nucl. Part. Phys. 43 (2016) 084001.
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Aiello S.; Albert A.; Garre S.A.; Aly Z.; Ameli F.; Andre M.; Androulakis G.; Anghinolfi M.; Anguita M.; Anton G.; Ardid M.; Aublin J.; Bagatelas C.; Barbarino G.; Baret B.; Basegmez du Pree S.; Bendahman M.; Berbee E.; van den Berg A.M.; Bertin V.; Biagi S.; Biagioni A.; Bissinger M.; Boettcher M.; Boumaaza J.; Bouta M.; Bouwhuis M.; Bozza C.; Branzas H.; Bruchner M.; Bruijn R.; Brunner J.; Buis E.; Buompane R.; Busto J.; Calvo D.; Capone A.; Carretero V.; Castaldi P.; Celli S.; Chabab M.; Chau N.; Chen A.; Cherubini S.; Chiarella V.; Chiarusi T.; Circella M.; Cocimano R.; Coelho J.A.B.; Coleiro A.; Molla M.C.; Coniglione R.; Corredoira I.; Coyle P.; Creusot A.; Cuttone G.; D'Onofrio A.; Dallier R.; De Palma M.; Di Palma I.; Diaz A.F.; Diego-Tortosa D.; Distefano C.; Domi A.; Dona R.; Donzaud C.; Dornic D.; Dorr M.; Drouhin D.; Durocher M.; Eberl T.; van Eijk D.; El Bojaddaini I.; Elsaesser D.; Enzenhofer A.; Rosello V.E.; Fermani P.; Ferrara G.; Filipovic M.D.; Filippini F.; Franco A.; Fusco L.A.; Gabella O.; Gal T.; Soto A.G.; Garufi F.; Gatelet Y.; Geisselbrecht N.; Gialanella L.; Giorgio E.; Gozzini S.R.; Gracia R.; Graf K.; Grasso D.; Grella G.; Guderian D.; Guidi C.; Hallmann S.; Hamdaoui H.; van Haren H.; Heijboer A.; Hekalo A.; Hernandez-Rey J.J.; Hofestadt J.; Huang F.; Ibnsalih W.I.; Illuminati G.; James C.W.; de Jong M.; de Jong P.; Jung B.J.; Kadler M.; Kalaczynski P.; Kalekin O.; Katz U.F.; Chowdhury N.R.K.; van der Knaap F.; Koffeman E.N.; Kooijman P.; Kouchner A.; Kreter M.; Kulikovskiy V.; Lahmann R.; Larosa G.; Le Breton R.; Leonardi O.; Leone F.; Leonora E.; Levi G.; Lincetto M.; Lindsey Clark M.; Lipreau T.; Lonardo A.; Longhitano F.; Lopez-Coto D.; Maderer L.; Manczak J.; Mannheim K.; Margiotta A.; Marinelli A.; Markou C.; Martin L.; Martinez-Mora J.A.; Martini A.; Marzaioli F.; Mastroianni S.; Mazzou S.; Melis K.W.; Miele G.; Migliozzi P.; Migneco E.; Mijakowski P.; Miranda L.S.; Modebadze Z.; Mollo C.M.; Morganti M.; Moser M.; Moussa A.; Muller R.; Musumeci M.; Nauta L.; Navas S.; Nicolau C.A.; O Fearraigh B.; Organokov M.; Orlando A.; Papalashvili G.; Papaleo R.; Pastore C.; Paun A.M.; Pavalas G.E.; Pellegrino C.; Perrin-Terrin M.; Piattelli P.; Pieterse C.; Pikounis K.; Pisanti O.; Poire C.; Popa V.; Post M.; Pradier T.; Puhlhofer G.; Pulvirenti S.; Quinn L.; Rabyang O.; Raffaelli F.; Randazzo N.; Rapicavoli A.; Razzaque S.; Real D.; Reck S.; Reubelt J.; Riccobene G.; Richer M.; Rivoire S.; Rovelli A.; Greus F.S.; Samtleben D.F.E.; Losa A.S.; Sanguineti M.; Santangelo A.; Santonocito D.; Sapienza P.; Schnabel J.; Sciacca V.; Seneca J.; Sgura I.; Shanidze R.; Sharma A.; Simeone F.; Sinopoulou A.; Spisso B.; Spurio M.; Stavropoulos D.; Steijger J.; Stellacci S.M.; Taiuti M.; Tayalati Y.; Tenllado E.; Thakore T.; Tingay S.; Tzamariudaki E.; Tzanetatos D.; Van Elewyck V.; Vannoye G.; Vasileiadis G.; Versari F.; Viola S.; Vivolo D.; de Wasseige G.; Wilms J.; Wojaczynski R.; de Wolf E.; Zaborov D.; Zavatarelli S.; Zegarelli A.; Zornoza J.D.; Zuniga J.; Zywucka N.
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