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ALICE is one of four large experiments at the CERN Large Hadron Collider near Geneva, specially designed to study particle production in ultra-relativistic heavy-ion colli- sions. Located 52 meters underground with 28 meters of overburden rock, it has also been used to detect muons produced by cosmic ray interactions in the upper atmosphere. In this paper, we present the multiplicity distribution of these atmospheric muons and its compari- son with Monte Carlo simulations. This analysis exploits the large size and excellent tracking capability of the ALICE Time Projection Chamber. A special emphasis is given to the study of high multiplicity events containing more than 100 reconstructed muons and corresponding to a muon areal density ρμ > 5.9 m−2. Similar events have been studied in previous under- ground experiments such as ALEPH and DELPHI at LEP. While these experiments were able to reproduce the measured muon multiplicity distribution with Monte Carlo simulations at low and intermediate multiplicities, their simulations failed to describe the frequency of the highest multiplicity events. In this work we show that the high multiplicity events observed in ALICE stem from primary cosmic rays with energies above 1016 eV and that the frequency of these events can be successfully described by assuming a heavy mass composition of primary cosmic rays in this energy range. The development of the resulting air showers was simulated using the latest version of QGSJET to model hadronic interactions. This observation places significant constraints on alternative, more exotic, production mechanisms for these events.
Study of cosmic ray events with high muon multiplicity using the ALICE detector at the CERN Large Hadron Collider
Adam, J.;Adamov, D.;Aggarwal, M. M.;Aglieri Rinella, G.;Agnello, M.;Agrawal, N.;Ahammed, Z.;Ahn, S. U.;Aiola, S.;Akindinov, A.;Alam, S. N.;Aleksandrov, D.;Alessandro, B.;Alexandre, D.;Alfaro Molina, R.;Alici, A.;Alkin, A.;Almaraz, J. R. M.;Alme, J.;Alt, T.;Altinpinar, S.;Altsybeev, I.;Garcia Prado, C. A.;Andrei, C.;Andronic, A.;Anguelov, V.;Anielski, J.;Antičić, T.;Antinori, F.;Antonioli, P.;Aphecetche, L.;Appelshäuser, H.;Arcelli, S.;Armesto, N.;Arnaldi, R.;Arsene, I. C.;Arslandok, M.;Audurier, B.;Augustinus, A.;Averbeck, R.;Azmi, M. D.;Bach, M.;Badalà, A.;Baek, Y. W.;Bagnasco, S.;Bailhache, R.;Bala, R.;Baldisseri, A.;Baltasar Dos Santos Pedrosa, F.;Baral, R. C.;Barbano, A. M.;Barbera, R.;Barile, F.;Barnaföldi, G. G.;Barnby, L. S.;Barret, V.;Bartalini, P.;Barth, K.;Bartke, J.;Bartsch, E.;Basile, M.;Bastid, N.;Basu, S.;Bathen, B.;Batigne, G.;Batista Camejo, A.;Batyunya, B.;Batzing, P. C.;Bearden, I. G.;Beck, H.;Bedda, C.;Belikov, I.;Bellini, F.;Bello Martinez, H.;Bellwied, R.;Belmont, R.;Belmont Moreno, E.;Belyaev, V.;Bencedi, G.;BEOLE', Stefania;Berceanu, I.;Bercuci, A.;Berdnikov, Y.;Berenyi, D.;Bertens, R. A.;Berzano, D.;Betev, L.;Bhasin, A.;Bhat, I. R.;Bhati, A. K.;Bhattacharjee, B.;Bhom, J.;Bianchi, L.;Bianchi, N.;Bianchin, C.;Bielčík, J.;Bielčíková, J.;Bilandzic, A.;Biswas, R.;Biswas, S.;Bjelogrlic, S.;Blair, J. T.;Blanco, F.;Blau, D.;Blume, C.;Bock, F.;Bogdanov, A.;Bøggild, H.;Boldizsár, L.;Bombara, M.;Book, J.;Borel, H.;Borissov, A.;Borri, M.;Bossú, F.;BOTTA, Elena;Böttger, S.;Braun Munzinger, P.;Bregant, M.;Breitner, T.;Broker, T. A.;Browning, T. A.;Broz, M.;Brucken, E. J.;Bruna, E.;Bruno, G. E.;Budnikov, D.;Buesching, H.;Bufalino, S.;Buncic, P.;Busch, O.;Buthelezi, Z.;Butt, J. B.;Buxton, J. T.;Caffarri, D.;Cai, X.;Caines, H.;Calero Diaz, L.;Caliva, A.;Calvo Villar, E.;Camerini, P.;Carena, F.;Carena, W.;Carnesecchi, F.;Castillo Castellanos, J.;Castro, A. J.;Casula, E. A. R.;Cavicchioli, C.;Ceballos Sanchez, C.;Cepila, J.;Cerello, P.;Cerkala, J.;Chang, B.;Chapeland, S.;Chartier, M.;Charvet, J. L.;Chattopadhyay, S.;Chattopadhyay, S.;Chelnokov, V.;Cherney, M.;Cheshkov, C.;Cheynis, B.;Chibante Barroso, V.;Chinellato, D. D.;Cho, S.;Chochula, P.;Choi, K.;Chojnacki, M.;Choudhury, S.;Christakoglou, P.;Christensen, C. H.;Christiansen, P.;Chujo, T.;Chung, S. U.;Chunhui, Z.;Cicalo, C.;Cifarelli, L.;Cindolo, F.;Cleymans, J.;Colamaria, F.;Colella, D.;Collu, A.;Colocci, M.;Conesa Balbastre, G.;Conesa Del Valle, Z.;Connors, M. E.;Contreras, J. G.;Cormier, T. M.;Corrales Morales, Y.;Cortés Maldonado, I.;Cortese, P.;Cosentino, M. R.;Costa, F.;Crochet, P.;Cruz Albino, R.;Cuautle, E.;Cunqueiro, L.;Dahms, T.;Dainese, A.;Danu, A.;Das, D.;Das, I.;Das, S.;Dash, A.;Dash, S.;De, S.;De Caro, A.;De Cataldo, G.;De Cuveland, J.;De Falco, A.;De Gruttola, D.;De Marco, N.;De Pasquale, S.;Deisting, A.;Deloff, A.;Dénes, E.;D'Erasmo, G.;Dhankher, P.;Di Bari, D.;Di Mauro, A.;Di Nezza, P.;Diaz, M. A.;Corchero, Null;Dietel, T.;Dillenseger, P.;Divià, R.;Djuvsland, Ø.;Dobrin, A.;Dobrowolski, T.;Domenicis Gimenez, D.;Dönigus, B.;Dordic, O.;Drozhzhova, T.;Dubey, A. K.;Dubla, A.;Ducroux, L.;Dupieux, P.;Ehlers, R. J.;Elia, D.;Engel, H.;Epple, E.;Erazmus, B.;Erdemir, I.;Erhardt, F.;Espagnon, B.;Estienne, M.;Esumi, S.;Eum, J.;Evans, D.;Evdokimov, S.;Eyyubova, G.;Fabbietti, L.;Fabris, D.;Faivre, J.;Fantoni, A.;Fasel, M.;Feldkamp, L.;Felea, D.;Feliciello, A.;Feofilov, G.;Ferencei, J.;Fernández Téllez, A.;Ferreiro, E. G.;FERRETTI, Alessandro;Festanti, A.;Feuillard, V. J. G.;Figiel, J.;Figueredo, M. A. S.;Filchagin, S.;Finogeev, D.;Fionda, F. 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2016-01-01
Abstract
ALICE is one of four large experiments at the CERN Large Hadron Collider near Geneva, specially designed to study particle production in ultra-relativistic heavy-ion colli- sions. Located 52 meters underground with 28 meters of overburden rock, it has also been used to detect muons produced by cosmic ray interactions in the upper atmosphere. In this paper, we present the multiplicity distribution of these atmospheric muons and its compari- son with Monte Carlo simulations. This analysis exploits the large size and excellent tracking capability of the ALICE Time Projection Chamber. A special emphasis is given to the study of high multiplicity events containing more than 100 reconstructed muons and corresponding to a muon areal density ρμ > 5.9 m−2. Similar events have been studied in previous under- ground experiments such as ALEPH and DELPHI at LEP. While these experiments were able to reproduce the measured muon multiplicity distribution with Monte Carlo simulations at low and intermediate multiplicities, their simulations failed to describe the frequency of the highest multiplicity events. In this work we show that the high multiplicity events observed in ALICE stem from primary cosmic rays with energies above 1016 eV and that the frequency of these events can be successfully described by assuming a heavy mass composition of primary cosmic rays in this energy range. The development of the resulting air showers was simulated using the latest version of QGSJET to model hadronic interactions. This observation places significant constraints on alternative, more exotic, production mechanisms for these events.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2318/1559391
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simulazione ASN
Il report seguente simula gli indicatori relativi alla produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione.
La simulazione si basa sui dati IRIS e presenta gli indicatori calcolati alla data indicata sul report. Si ricorda che in sede di domanda ASN presso il MIUR gli indicatori saranno invece calcolati a partire dal 1° gennaio rispettivamente del quinto/decimo/quindicesimo anno precedente la scadenza del quadrimestre di presentazione della domanda (art 2 del DM 598/2018).
In questa simulazione pertanto il valore degli indicatori potrà differire da quello conteggiato all’atto della domanda ASN effettuata presso il MIUR a seguito di:
Correzioni imputabili a eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori.
Presenza di eventuali errori di catalogazione e/o dati mancanti in IRIS
Variabilità nel tempo dei valori citazionali (per i settori bibliometrici)
Variabilità della finestra temporale considerata in funzione della sessione di domanda ASN a cui si partecipa.
La presente simulazione è stata realizzata sulla base delle regole riportate nel DM 598/2018 e dell'allegata Tabella A e delle specifiche definite all'interno del Focus Group Cineca relativo al modulo IRIS ER. Il Cineca non si assume alcuna responsabilità in merito all'uso che il diretto interessato o terzi faranno della simulazione.