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April 28, 2006 Tokai-to-Kamioka (T2K) Long Baseline Neutrino Oscillation Experiment Proposal Executive Summary In this document, we propose to construct a neutrino beam facility, using the fast extracted proton beam from J-PARC proton synchrotron in Tokai and to perform a long baseline neutrino oscillation experiment, using existing Super-Kamiokande detector (T2K experiment). This experiment is an international collaboration of Japan, Canada, France, Italy, Korea, Poland, Russia, Spain, UK and USA. Budget request of each country has been submitted to each financial agency. This proposal is the first stage of the physics program. The feasibility of the future neutrino program depends on the results of this first stage, especially on the result of νμ → νe search. The goal of the T2K experiment We request total integrated beam power larger than 0.75 MW x 15000h at any proton energies between 30 and 50 GeV. Since one year run with full beam power will probe physics by unprecedented sensitivities, it is possible that new finding occur any time. Even if we do not see new phenomena, every yearly run will produce meaningful upper limit. Thus it is critical to increase the beam power as soon as possible after commissioning of accelerator complex. The experiment has three main well defined goals. 1. The discovery of νμ → νe A factor of 20 improvement in sensitivity over the present upper limit is possible. The goal is 2 2 to extend the search down to sin 2θ13 2sin 2θμe > 0.008. The νe appearance measurement is important for two reasons. • The mixing angle θ13 is the last of the mixing angles in three neutrino scheme. We already know that other two mixing are large. One of the most interesting question is whether the third mixing angle is at same order of magnitude or small by many order of magnitudes. The observation of νμ → νe in the first stage of the experiment prove that θ13 is not extremely small, so that a future CP violation search become practical. 2 • This is an appearance channel and has a sub-leading oscillation of νμ involving Δm13. The new developments in solar and reactor neutrino experiments indicate that νμ will 2 oscillate to νe with a rather large mixing angle and Δm12. This oscillation can compete 2 with the one with a mass squared difference of Δm13. The former oscillation is suppressed 2 by a small Δm and the latter is suppressed by the small mixing angle, θ13. Hence, the two processes can compete. This is one of the necessary conditions for a CP violation effect to be observable. 2. The precision measurements of oscillation parameters in νμ disappearance Observation of the oscillation minimum, a 1% measurement (about the same precision as Cab- 2 2 bibo angle in quark sector) of the mixing angle and a 3% measurement of Δm (δ(Δm23)= −4 2 2 10 eV and δ(sin 2θ23)=0.01), may show the mixing of second and third generation neu- trinos to be consistent with maximal at 1% accuracy. This may impose a constraint on the quark-lepton unification in the future. 3. Search for sterile components in νμ disappearance by detecting the neutral-current events If a non-zero sterile component is found, the physics of fermions will need modification to accommodate extra member(s) of leptons. Feature of the T2K experiment Needless to say, it is important to look for unexpected phenomena as well with new sensitivity. The neutrino beam has been designed with emphasis on the neutrino energy determination and on the flavor identification, taking into account the characteristics of Super-Kamiokande detector. 2 • The far detector T2K will use the world largest water Cherenkov detector, Super-Kamiokande (SK), as the far detector. Super-Kamiokande has excellent energy resolution and e/μ identification capability in low energy neutrino reactions, backed by about twenty years of experience of water Cherenkov detector. • The neutrino beam energy The maximum sensitivity of the oscillation parameters can be achieved by tuning the neutrino beam energy to the oscillation maximum. The oscillation maximum will occur at a neutrino 2 −3 2 energy, Eν, less than 1 GeV for the 295 km baseline with Δm ∼ 3 × 10 eV . This neutrino energy is well matched to the detector capability. • Eν reconstruction The charged current interaction is dominated by the quasi-elastic interaction (CCQE) below 1 GeV. This enable us to make a precision determination of the neutrino energy of both νμ and νe. The energy can be calculated by a formula: m E − m2/ N l l 2 Eν = , (1) mN − El + plcosθl where mN and ml are the masses of the neutron and lepton (=e or μ), El, pl and θl are the energy, momentum, and angle of the lepton relative to the neutrino beam, respectively. • Off-axis beam The precision of the measurements are limited mainly due to the background events from high-energy components. The inelastic reactions of high-energy neutrinos constitute the back- grounds to neutrino energy measurements with the CCQE. In addition, the inelastic reactions 0 produce π s that are the main background for νe appearance search. The experiment will use an off-axis beam to accomplish the highest possible intensity of low energy neutrinos with only a small high-energy tail in the spectrum. • Start up of the experiment SK has been in operation for many years and the relevant software already exists. The intensity of the low energy neutrino beam is proportional to the proton beam power and does not require a specific proton energy in the initial operation of the accelerator. The experiment will be able to accommodate any reasonable start-up scenario of the accelerator, and can produce physics results in a short time after initial operation. 3 Japan KEK Y. Ajima, O. Araoka, Y. Fujii, K. Hayashi, N. Higashi, A. K. Ichikawa, T. Ishida, T. Ishii, K. Kasami, N. Kimura, T. Kobayashi, S. Koike, Y. Makida, T. Nakadaira, T. Nakamoto, K. Nakamura, K. Nishikawa∗, T. Ogitsu, H. Ohhata, T. Okamura, Y. Oyama, K. Sasaki, K. Sakashita, T. Sekiguchi, S. Suzuki, M. Tada, K. Tanaka, M. Tanaka, A. Terashima, T. Tomaru, T. Tsukamoto, Y. Yamada, H. Yamaoka ICRR, University of Tokyo T. Abe, Y. Hayato, Y. Itow, J. Kameda, Y. Koshio, M. Miura, S. Moriyama, M. Nakahata, Y. Obayashi, H. Sekiya, M. Shiozawa, Y. Suzuki, A .Takeda, Y. Takeuchi RCCN, University of Tokyo I. Higuchi, T. Kajita, K. Kaneyuki, S. Nakayama, K. Okumura, C. Saji Hiroshima University T. Takahashi Kobe University S. Aoki, T. Hara, A. Suzuki Kyoto University T. Nakaya, H. Tanaka, M. Yokoyama Tohoku University T. Hasegawa University of Tokyo T. Abe, H. Aihara, M. Iwasaki, H. Kakuno, N. Hastings Canada TRIUMF P. Amaudruz, M. Barnes, E. Blackmore, S. Chen, H. Coombes, J. Doornbos, W. Faszer, P. Gumplinger, R. Helmer, R. Henderson, I. Kato, P. Kitching, A. Konaka, L. Kurchaninov, G. Marshall, J. Macdonald, A. Miller, K. Olchanski, R. Openshaw, J.M. Poutissou, R. Poutissou, F. Retiere, P. Vincent, G. Wait, S. Yen, University of Alberta J.P. Archambault, J. McDonald, M.G Vincter University of British Columbia M. Bryant, J. Coulombe, C. Hearty, S. Oser, J. Wendland University of Regina T. Mathie, R. Tacik University of Toronto J. Martin University of Victoria P. Birney, A. Dowling, K. Fransham, C. Hansen, D. Karlen, R. Langstaff, M. Lenckowski, P. Poffenberger, M. Roney York University S. Bhadra ∗ T2K Contact person: Koichiro Nishikawa, Email address : [email protected] 4 France CEA SACLAY - DSM/DAPNIA - Service de Physique des particules J. Argyriades, P. Baron, J. Bouchez, D. Calvet, Ch. Cavata, P. Colas, E. Delagnes, A. Delbart, F. Druillole, M. Fechner, A. Giganon, Y. Giomataris, J. Mallet, J.-Ph. Mols, L. Mosca, F. Pierre, A. Sarrat, M. Zito LPNHE-IN2P3 Paris J. Dumarchez Italy INFN - Sezione di Bari M.G. Catanesi, E. Radicioni INFN - University of Napoli G. De Rosa, V. Palladino INFN - University of Padova M. Mezzetto, M. Laveder INFN - University of Roma U. Dore, C. Gargiulo, P.F. Loverre, L. Ludovici, C. Mariani University of Ljubljana T. Podobnik Unversity of Naples Federico II G. De Rosa Korea Chonnam Naitonal University J.Y. Kim, I.T. Lim Dongshin University M.Y. Pac Kyungpook National University W. Kim, V. Batourine Kangwon University S.K. Nam KyungSang National University I.G. Park Sejong University Y.D. Kim Seoul National University S. Choi, E.J. Jeon, K.K. Joo, S.B. Kim SungKyunKwan University Y.I. Choi, C.W. Park Yonsei University Y. Kwon Gyeongsang National University I.G. Park 5 Poland Warsaw University D. Kielczewska Russia Institute for Nuclear Research RAS A.V. Butkevich, M. Khabibullin, A. Khotjantsev, Yu.G. Kudenko, B. Lubsandorjiev, V.A. Matveev, S.P. Mikheyev, O. Mineev, Y. Mussienko, N. Yershov ITEP M. Danilov, V. Balagura Spain University of Barcelona J.L. Alcaraz, S. Andringa, X. Espinal, E. Fern´andez, F. S´anchez, T. Lux University of Valencia J. Burguet, J. Catala, A. Cervera-Villanueva, E. Couce, P.N Garijo, J.J. Gomez-Cadenas, P. Novella, M. Sorel, A. Tornero Switzerland ETH/Zurich A. Rubbia University of Geneva A. Blondel, P. Bene, A. Cervera, D. Ferrere, F. Masciocchi, E. Perrin, R. Schroeter UK Imperial College London S. Boyd, P. Dornan, G. Hall, M. Raymond, I. Taylor, Y. Uchida, A. Vacheret, F. van Schalkwyk, D.L. Wark Lancaster University I. Bertram, L. Kormos, P. Ratoff University of Liverpool C. Chavez, J. Fry, R. Gamet, D. Payne, P. Sutcliffe, C. Touramanis Queen Mary Westfield College London F.Di Lodovico, C.M. Cormack, R.A. Owen, A. Poll, C. Williams Rutherford Appleton laboratory A. Belias, J. Butterworth, S. Canfer, C. Densham, R.
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  • Icecube Searches for Neutrinos from Dark Matter Annihilations in the Sun and Cosmic Accelerators

    Icecube Searches for Neutrinos from Dark Matter Annihilations in the Sun and Cosmic Accelerators

    UNIVERSITE´ DE GENEVE` FACULTE´ DES SCIENCES Section de physique Professeur Teresa Montaruli D´epartement de physique nucl´eaireet corpusculaire IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators. THESE` pr´esent´ee`ala Facult´edes sciences de l'Universit´ede Gen`eve pour obtenir le grade de Docteur `essciences, mention physique par M. Rameez de Kozhikode, Kerala (India) Th`eseN◦ 4923 GENEVE` 2016 i Declaration of Authorship I, Mohamed Rameez, declare that this thesis titled, 'IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators.' and the work presented in it are my own. I confirm that: This work was done wholly or mainly while in candidature for a research degree at this University. Where any part of this thesis has previously been submitted for a degree or any other qualifica- tion at this University or any other institution, this has been clearly stated. Where I have consulted the published work of others, this is always clearly attributed. Where I have quoted from the work of others, the source is always given. With the exception of such quotations, this thesis is entirely my own work. I have acknowledged all main sources of help. Where the thesis is based on work done by myself jointly with others, I have made clear exactly what was done by others and what I have contributed myself. Signed: Date: 27 April 2016 ii UNIVERSITE´ DE GENEVE` Abstract Section de Physique D´epartement de physique nucl´eaireet corpusculaire Doctor of Philosophy IceCube searches for neutrinos from dark matter annihilations in the Sun and cosmic accelerators.