Author:
Abe S.,Adams J.H.,Allard D.,Alldredge P.,Aloisio R.,Anchordoqui L.,Anzalone A.,Arnone E.,Baret B.,Barghini D.,Battisti M.,Bellotti R.,Belov A.A.,Bertaina M.,Bertone P.F.,Bianciotto M.,Bisconti F.,Blaksley C.,Blin-Bondil S.,Bolmgren K.,Briz S.,Burton J.,Cafagna F.,Cambié G.,Campana D.,Capel F.,Caruso R.,Casolino M.,Cassardo C.,Castellina A.,Černý K.,Christl M.J.,Colalillo R.,Conti L.,Cotto G.,Crawford H.J.,Cremonini R.,Creusot A.,Cummings A.,de Castro Gónzalez A.,de la Taille C.,Diesing R.,Dinaucourt P.,Di Nola A.,Ebisuzaki T.,Eser J.,Falk S.,Fenu F.,Ferrarese S.,Filippatos G.,Finch W.W.,Flaminio F.,Fornaro C.,Fouka M.,Fuehne D.,Fuglesang C.,Fukushima M.,Gardiol D.,Garipov G.K.,Golzio A.,Gorodetzky P.,Guarino F.,Guépin C.,Haungs A.,Heibges T.,Isgrò F.,Judd E.G.,Kajino F.,Kaneko I.,Kim S.-W.,Klimov P.A.,Krizmanic J.F.,Kungel V.,Kuznetsov E.,López Martínez F.,Mandát D.,Manfrin M.,Marcelli A.,Marcelli L.,Marszał W.,Matthews J.N.,Mese M.,Meyer S.S.,Mimouni J.,Miyamoto H.,Mizumoto Y.,Monaco A.,Nagataki S.,Nachtman J.M.,Naumov D.,Neronov A.,Nonaka T.,Ogawa T.,Ogio S.,Ohmori H.,Olinto A.V.,Onel Y.,Osteria G.,Pagliaro A.,Panico B.,Parizot E.,Park I.H.,Paul T.,Pech M.,Perfetto F.,Picozza P.,Piotrowski L.W.,Plebaniak Z.,Posligua J.,Prevete R.,Prévôt G.,Przybylak M.,Reali E.,Reardon P.,Reno M.H.,Ricci M.,Romoli G.,Sagawa H.,Sahnoune Z.,Sakaki N.,Saprykin O.A.,Sarazin F.,Sato M.,Schovánek P.,Scotti V.,Selman S.,Sharakin S.A.,Shinozaki K.,Soriano J.F.,Szabelski J.,Tajima N.,Tajima T.,Takahashi Y.,Takeda M.,Takizawa Y.,Thomas S.B.,Tkachev L.G.,Tomida T.,Toscano S.,Traïche M.,Trofimov D.,Tsuno K.,Unger M.,Vallania P.,Valore L.,Venters T.M.,Vigorito C.,Vrabel M.,Wada S.,Watts J.,Wiencke L.,Winn D.,Wistrand H.,Yashin I.V.,Young R.,Zotov M.Yu.,
Abstract
Abstract
The complexity of modern cosmic ray observatories and the
rich data sets they capture often require a sophisticated software
framework to support the simulation of physical processes, detector
response, as well as reconstruction and analysis of real and
simulated data. Here we present the EUSO-Offline framework. The
code base was originally developed by the Pierre Auger
Collaboration, and portions of it have been adopted by other
collaborations to suit their needs. We have extended this software
to fulfill the requirements of Ultra-High Energy Cosmic Ray
detectors and very high energy neutrino detectors developed for the
Joint Exploratory Missions for an Extreme Universe Observatory
(JEM-EUSO). These path-finder instruments constitute a program to
chart the path to a future space-based mission like POEMMA. For
completeness, we describe the overall structure of the framework
developed by the Auger collaboration and continue with a description
of the JEM-EUSO simulation and reconstruction capabilities. The
framework is written predominantly in modern C++ (compliled against
C++17) and incorporates third-party libraries chosen based on
functionality and our best judgment regarding support and
longevity. Modularity is a central notion in the framework design, a
requirement for large collaborations in which many individuals
contribute to a common code base and often want to compare different
approaches to a given problem. For the same reason, the framework is
designed to be highly configurable, which allows us to contend with
a variety of JEM-EUSO missions and observation scenarios. We also
discuss how we incorporate broad, industry-standard testing coverage
which is necessary to ensure quality and maintainability of a
relatively large code base, and the tools we employ to support a
multitude of computing platforms and enable fast, reliable
installation of external packages. Finally, we provide a few
examples of simulation and reconstruction applications using
EUSO-Offline.