Pos(Nufact08)003 Oscillation Ν ∗ Niki@Fnal.Gov Speaker

Home , ICARUS experiment, OPERA experiment, Soudan 2

PoS(Nufact08)003 http://pos.sissa.it/ Oscillation ν ∗ [email protected] Speaker. We will start with a brief overview ofunanswered neutrino questions. oscillation physics Next with emphasis we on will thetrino discuss remaining oscillation results experiments and that status are in ofto a long start mature baseline data data accelerator taking. taking neu- mode, Then, have wea just will primary started present goal or the to are next search about generation forintroduce of the the long yet plans baseline to for experiments future be with long measured baselinethe third accelerator primary neutrino neutrino mixing goals oscillation angle. experiments are of Finally the which of we search the will for neutrino mass CP hierarchy. violation Weneutrino in will beams, focus the either on neutrino existing experiments or sector, utilizing in and powerful the (0.7 design the phase. - determination 4.0 MW) ∗ Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

10th International Workshop on Neutrino Factories,June Super 30 beams - and July Beta 5 beams 2008 Valencia, Spain Fermi National Accelerator Laboratory E-mail: Niki Saoulidou Status and Prospects of Long Baseline Experiments PoS(Nufact08)003 µ ν , of 735 dis- s f µ = ν L ] MINOS Niki Saoulidou 12 . Fitting the NC-like ) µ ) . In addition, fitting the ν s | ν → ], the existence of sterile 2 32 → µ µ ν m ( 11 ν ( ∆ P | oscillations. The first P ],[ − 1 ) ’s in the beam whose CC inter- e 10 e ν = ν s f we show the recent [ → , for which only a limit exists from the 1 µ ν 13 ( θ 2%, of P ∼ respectively. oscillation parameters, the comparison between σ 2 7 ) . τ ν beam produced by the Fermilab Main Injector (NUMI → µ and 5 ν µ σ ν 7 ( under the pure neutrino decay and pure neutrino decoherence . ] in 2006. In Figure 3. MINOS near and far detectors are magnetized segmented 6 P 1 CC and NC using the different characteristics of hadronic and ∼ would result in a depletion of the far detector NC-like data with Oscillation Experiments µ s > ν ν ν E to ]). However, there are still many open questions: < 8 µ ν ]-[ 1 is a two detector long baseline neutrino oscillation experiment (baseline , as well as the study of the subdominant s ] experiment ? ν 9 ]. Oscillations of MINOS 13 MINOS has recently completed the first analysis of NC interactions in the near and far detec- The first three of the five questions we can address with experiments using reactor and/or • Non-zero neutrino masses are perhaps the only experimental evidence we have so far, for the actions are distinguished from electromagnetic showers. MINOS primarycise physics goals measurement using of accelerator the neutrinosneutrino dominant are oscillations the and pre- alternative disappearance hypotheses [ active neutrinos that oscillate to sterile neutrino species with hypotheses and comparing it to thedisfavor fit them under with the a significance neutrino of oscillation 3 hypothesis, MINOS is able to respect to expectation. The magnitude of such a depletion would depend on the fraction, tors [ km) with its near detector locatedoratory. at It utilizes Fermilab an and almost its pure farbeam) (98%) detector with at a SOUDAN mean Underground energy Lab- (steel/scintillator) tracking calorimeters. Muon neutrinomarily charged current identified (CC) by interactions the are pri- the presence absence of of a it. muon-like track There and is neutral a current small (NC) contamination, interactions by neutrinos appearance results were published [ accelerator neutrinos, and the remaining two with natural neutrinos. 2. MINOS-OPERA-ICARUS 2) Do neutrinos violate CP symmetry3) and What if is so the by hierarchy how of much? 4) neutrino What masses? are the absoluteformation values only of on neutrino the masses? mass differences Neutrino5) between oscillation Are the experiments neutrinos different provide Majorana eigenstates. or in- Dirac6) particles? Are there stillinvolving more neutrinos "surprises" that to will come resultfor in in some entirely neutrino of "unexpected" us, physics this experimental ? is observations? the Namely, Perhaps, most exciting is scenario there new physics disappearance results, obtained with a factorin of the three first higher analysis, statistics compared which to presentenergy the the distribution sample shown most in used precise Figure measurement of 1) What is the value of the third neutrino mixing angle, existence of physics beyond the Standardprogress Model. has been In made the towards pastferences precisely ten and measuring years mixings and tremendous ([ (experimental) better understanding neutrino mass dif- Status-Prospects of Long Baseline 1. Introduction CHOOZ [ PoS(Nufact08)003 . τ . to to ν L we . µ µ 3 C ν ν ] with 14 (black dotted contours from . Niki Saoulidou . oscillate to L 68 at 90% . L ) disappearance . . µ τ 0 C beam. OPERA is C ν ν contours (gray line). < µ . s ν L (to f . beam from the CERN C µ µ ν is at the current CHOOZ ν 13 730 km) located at the Gran θ limit of ’s would have energies above = τ s f L ν (right plot). If 2 3 17 GeV, such that ∼ > (left plot), under the assumption that appearance. OPERA will also study subdominant decays through the so called "kink decay topology". (blue line) analyses and the K2K 90% 2 τ E CC interactions originating in a pure ν τ τ E < / ν to L µ in a hybrid emulsion spectrometer via the detection of the pro- Oscillation Experiments ν τ ν ν appearance is on-going and results are expected soon (end of 2008, e ν CC interactions has been successfully demonstrated by the DONUT ex- τ ν (black continuous line) contours along with Super-Kamiokande 90% . is a long baseline neutrino oscillation experiment ( L . ]. OPERA, during the October 2007 GNGS run, has accumulated 369 neutrino in- C 15 Left Figure: MINOS Far detector reconstructed energy (GeV) spectrum for charged current-like lepton in the with the same mass-squared difference, MINOS obtains an τ OPERA production threshold. The OPERA detector is a hybrid lead-emulsion spectrometer [ s , in order to observe and identify MINOS analysis on • The primary goal of the OPERA experiment is the direct, unambiguous, verification of The direct observation of ν µ τ oscillations by the observation of oscillations, the existence of sterile neutrinos, and alternative hypothesis to neutrino oscillations 1 ] limit MINOS has the potential of being the first experiment to observe it. If not, MINOS will τ e 9 and beginning of 2009). The potentialstatistics at of the this end analysis, of for data the taking, is current shown statistics n as Figure well as for the full [ teractions, 38 of which were recorded and reconstructed in the emulsion target. In Figure both the zenith angle (red line) and the far detector spectrum, shown in Figure Sasso Underground Laboratory (LNGS). It utilizes an almost pure (98%) ν complementary to the MINOS experiment : MINOS has studied in detail further improve the current CHOOZ limit. line) and 90% SPS accelerator with a mean energy target mass of 1.25KTons. The< emulsion target provides the very high spatial resolution needed, and OPERA will study inν detail like neutrino decay and decoherence. duced Figure 1: events. Black points are theunder data, the black neutrino solid line oscillation the hypothesis. unoscillated expectation Right and Figure: red solid MINOS line two the dimensional best 68% fit periment [ Status-Prospects of Long Baseline the PoS(Nufact08)003 e 3 0 20 ν − π 10 10 at the Right × × 13 oscillate from θ 5 2). µ 25 . . / e ν 2 π 3 = Niki Saoulidou | = 2 32 δ as a function of the m ) ∆ | 13 θ 2 ( 2 6 GeV. The far detector is the Super- . . 0 4 ∼ > E exclusion limit on sin 0). Blue solid line is the expectation under the . < L . ) = 4 C e ν → µ ν ( P with the latter allowed to have its maximal possible value ( e ν Oscillation Experiments CC events assuming maximal mixing with a 0 and ν τ and ν τ ) = ν s 76 . ν we show cosmic ray and neutrino events in the detector which clearly 0 for the current and total foreseen integrated statistics (Protons on Target). → 5 ± 4 ] with a sensitivity as shown in Figure µ . ] is a 600 Ton Liquid Argon (LAr) Time Projection Chamber (TPC) now lo- ν CC from NC interactions. These capabilities enable OPERA to perform a ( : MINOS Far detector reconstructed visible energy (GeV) spectrum for neutral current- 16 e delta 17 P oscillate to [ ( ν µ ] is a next generation long baseline accelerator neutrino oscillation experiment with τ CC interactions, and with the the full statistics sample, corresponding to 2 295 km and a mean neutrino energy ν ν τ 19 = [ ν 2 L . 1 ICARUS T2K ∼ Due to the excellent spatial resolution of the emulsion target one can distinguish Perhaps one of the most important goals of the ICARUS experiment is to prove that this de- • • : MINOS projections (Monte Carlo) of the 90% . 2 eV and also reconstruct kinematic variableshelp (momentum to imbalance separate in theappearance transverse study plane) [ that can CP violating phase show an event with a "kink"showers topology originating classified from as the a neutrino charmto interaction see candidate vertex. having In two the electromagnetic 2008protons GNGS on run target, 10 OPERA expects hypothesis that current CHOOZ limit, normal neutrinoPlot mass hierarchy and maximal CP violation with a baseline tector technology can function asof expected, time, in performing an a underground variety laboratory,and of and solar physics for neutrinos. measurements sizable using periods atmospheric, accelerator, supernova 3. T2K-NOvA cated in the LNGS.calendar The year installation (2008). is This detector well hastial under excellent resolution way three similar dimensional and imaging to start capabilitiessensitivity. those with of spa- of operation In bubble is Figure chambers, anticipatedillustrate this how but powerful with this detector electronic technology readout is. and continuous Status-Prospects of Long Baseline exclusively to Figure 2: Left Plot like events. Black points are the data. Red solid line is the expectation under the hypothesis that PoS(Nufact08)003 ) narrow o 5 oscillations . 13 sensitivity to θ e Niki Saoulidou 2 ν . with a similar 2 L . sin to 13 .With the full sensitivity on C µ θ . 2 23 ν L -1 m OPERA . 10 ∆ C CC signal, especially the ) CNGS : ICARUS Cosmic Ray at 90% C.L. in a three family mixing scenario, % e 13 ν 11 θ : Neutrino interactions in a -2 . The sensitivity with the higher intensity CNGS beam is ◦ 10 (left plot). In addition, due to its = 45 7 OPERA 90% we show the 90% 23 Nominal intensity High intensity (+50 θ 6 as a function of with Right Plots ) τ ν -3 13 ↔ θ µ 10 ν -2 -3 -4 2 (

10 10 10

) (eV

m 2 GeV. The NOvA detector is a fully active 15

∆ small ICARUS Prototype exposed in theneutrino beam. CERN The level of detail onacteristics, event observed char- even by naked eye,strate demon- how powerful such ais. detector technology Figure 5:events. Left Plots 2 2 for the full statistics: 5 year of operation at 750 Figure 4: sin statistics sample OPERA shouldplore be the able region to well below ex- the CHOOZ limit. ∼ 5 δ Figure 3: OPERA sensitivity to the parameter in presence of also given. > E 20 with respect to the current CHOOZ limit. The off < p ∼ + − Hadrons

µ + −

Oscillation Experiments µ → ν → n

X + + candidate. How- µ µ

τ ν ν ν produced in the ﬁnal state. In Figure o π ] is a next generation long baseline experiment with a much longer baseline than ] Water Cherenkov (WC) detector. The neutrino beam is an off axis (2 18 1 [ as a function of CP violating phase OPERA Charm candidate neutrino 810 km, and a mean energy of ) = 13 NOvA θ L 2 • The primary goal of the T2K experiment is to search for the subdominant The primary goal of the NOvA experiment is to search for a non-zero ( 2 Hadronic interaction EM shower Kamiokande [ KW of beam power. Thehave T2K ﬁrst results experiment possibly is by anticipated summer to of start 2010. taking data in April of 2009 and T2K, sin ever there are two electromagnetic showers originating from theseen interaction from vertex, the as reconstructedtion. clearly emulsion informa- band beam (NBB) which is currently under construction at JPARC. KTon liquid scintillator detector and the neutrinoNBB. beam is the NUMI off axis, at a angle of 14 mrad, sensitivity to that of the T2K experiment, as shown in Figure interaction. Thetopology" in presence one of ofclassify the a the emulsion interaction clear tracks as would a "kink- Figure 3: Status-Prospects of Long Baseline with a sensitivity greater byaxis a idea factor is of used inones order with to a highly single suppress NC backgrounds to the PoS(Nufact08)003 13 nd θ and ν and 2 st Niki Saoulidou discovery potential for . y L . C arch r ivity to the neutrino at 700 KW (continuous line), 1.2 discovery potential for normal (blue lines) and inverted mass hie ν . 13 L . θ C beams ν 95% C.L. Sensit as a function of the CP vio- 13 and for three different values of θ and 3 years of T2K 90% δ : NOvA plus T2K 95% ν (right plot) we show the neutrino mass hierarchy . This plots assumes full statistics: 5 - 6 ) 0 7 1 23 θ 2 ( 0 2 ≠ Right Plot ) 13 Figure 6: for a non-zero lating phase sin years of operation at 750 KW of beam power. -3 θ 10 0 (2

50 2

-50

150 100 (degrees) CP phase phase CP -100 -150 δ running at 750 KW, 1.5 MW and 3 MW of beam power for the JPARC Oscillation Experiments 1 ν ν 13 θ discovery potential for a non-zero 2 2 ivity to sin 2 2 σ sin eV eV -3 -5 = 1.0) = 0.9) = 0.9) 23 23 23 Sensit /4 θ θ θ π 2 2 2 -1 σ 2 2 2 = = 0.625 = 0.946 3 = 0.4 10 23 23 23 = 2.5x10 = 8.2x10 (sin θ (sin θ (sin θ 12 13 12 θ 2 2 2 m m : NOvA 3 ∆ ∆ tan -2 10 at 700 KW (continuous line), 1.2 MW (dashed line) and 2.3 MW (doted line) of beam power ν -3 The focus of future long baseline accelerator neutrino oscillation experiments is the discovery The measurement of the neutrino mass hierarchy requires a long baseline in order to enhance 10 0

-50

150 100 CP phase phase CP (degrees) -100 -150 δ (red lines) hierarchy. Running conditions:MW (dashed 3 line) years and of 2.3determining MW the (doted neutrino line). mass hierarchy3 assuming normal years hierarchy. of Running conditions: 3 years of beam. phase and is expected to start taking data in 2013. 4. Future Possibilities with JPARC and Fermilab (if present) of CPhierarchy. violation in the neutrino sector, and thematter determination effects. of The the measurement neutrino of CP mass violation requires information from both the 1 Figure 7: Left Plot for the NUMI beam and 6 years of discovery potential when NOvA and T2K are combined. NOvA is in the final design/construction Status-Prospects of Long Baseline is close to the current CHOOZ limit. In Figure long baseline, NOvA has the unique capability of determining the neutrino mass hierarchy if PoS(Nufact08)003 ∼ L where 2 MW 8 ≈ Niki Saoulidou ], which includes 21 oscillation maximum and one st oscillation maximum : Fermilab currently operates the NUMI beam st , and the neutrino mass hierarchy), are illustrated : JPARC will be soon (2009) operating the NBB 7 δ oscillation maximum. nd 5 KT LAr, placed either in the NUMI beam with an ∼ in order to break the inherent degeneracies between "genuine" Oscillation Experiments ) e ν ν , and the neutrino mass hierarchy), are illustrated in Figure δ → , CP Violating phase µ ν 13 ( θ P 1000 km, at the 2 ∼ L where one clearly sees the progressive increase in discovery potential. 9 Future Possibilities with Fermilab beams Future Possibilities with JPARC beams 800 km, or at the Deep Underground Science and Engineering Laboratory (DUSEL) with an The next step would be the construction, using most likely a modular approach,Finally, the of construction massive of "Project X" would increase the neutrino beam power from 700 KW The first step of the staged program is theAn NOvA intermediate liquid step, scintillator with experiment quite described interesting physics in capabilities, could be an upgraded (tech- • The physics capabilities of this program, in terms of discovery potentials for the parameters of There are two ways one can obtain information from both oscillation maxima: Both JPARC and Fermilab have developed plans for future experiments that• fulfill the above As far as detector masses and baselines are concerned there are two options examined: 1300 km. − = 700 L detectors, 300 KT of WCWBB and/or from 100KT Fermilab LAr, to at DUSEL. The DUSEL initial in beam parallel power with would the be 700to construction KW. 2MW. of The new physics capabilitiesparameters of of this interest, staged ( program, in terms of discovery potentials for the in Figure previous sections. nologically) detector consisting of an upgrade to the acceleratorof complex, beam power called for "Project proton X".neutrino energies beams. ranging "Project from X" 60-120 could GeV produce and resulting in very high intensity at 250 KW with an approvedof upgrade the plan previous to year 700 KW Fermilab for developed the a NOvA physics experiment. plan Over for the the course next decade [ one clearly sees advantage of theinvolving two longer detector baselines. configuration covering both oscillation maxima and interest, (CP Violating phase (1) Create a Wide Bandwith neutrino one Beam detector (WBB) in order(2) to Use study Narrow both Band ofent them Beams baselines, at (NBB) and a at two fixed two detectors baseline afterwards. to different study off each axis one angles, of which them separately, involve combining two the differ- information requirements. i) One 540 KTon WC detector at Kamioka at the 1 Status-Prospects of Long Baseline oscillation maxima of CP violating and "fake" CP violation arising from matter effects. for the T2K experiment startingnominal value from 750 a KW. There beam are power upgradeMW of plans and that 100 ultimately could to KW increase 4 and the MW. JPARC gradually beam increasing power to to 1.7 the ii) Two 270 KTon WC detectorslocated in one Korea, located in Kamioka at the 1 PoS(Nufact08)003 Niki Saoulidou CP Violation discovery potential with , the neutrino mass hierarchy, and CP : 3(blue dashed line) and 2(gray dashed mass hierarchy discovery potential: 0.54 σ 13 θ σ Right Plot 8 running. ν oscillation maxima with NUMI NBB at 2MW, (5) 100 KTon nd Discovery potentials for σ Oscillation Experiments ν and 4 years of ν 500 KTon of WC) at DUSEL with new WBB at 2 MW. + 50 KTon LAr at 2 ∼ st mass hierarchy discovery potential with two 0.27 MTon WC detectors in Kamioka and : 3(blue dashed line) and 2(gray dashed line) σ Fermilab Staged Plan: 3 CP violation discovery potential with 0.54 MTon WC detector in Kamioka with the JPARC off axis σ Figure 9: violation. From lower to higher discoveryKTon LAr potentials: with (1) NUMI NOvA NBB+WBB with at NUMI(4) 700 NBB 50 KW, at KTon (3) 700 LAr NOvA+5 KW, at KTon (2) LAr 1 LAr NOvA+5 with (equivalent NUMI with NBB+WBB at 2 MW, Figure 8: Left Plot Status-Prospects of Long Baseline MTon WC detector in Kamioka2(black with thin the line) JPARC off axisKorea beam with upgraded the to JPARC off 4 axis MW. beamline) 3(black upgraded thick to line) 4 MW. and beam upgraded to 4 MW. 3(blacktwo thick 0.27 line) MTon and WC 2(black thin detectorsRunning line) conditions: in 4 Kamioka years and of Korea with the JPARC off axis beam upgraded to 4 MW. PoS(Nufact08)003 Niki Saoulidou 9 Oscillation Experiments ν 600pp. 29pp. Preprint: hep-ex/0106019 Dec 2007. 48pp. I would like to thank the Organizers of NUFACT 2008 for the kind invitation and the [1] J.Hosaka et al. (Super-Kamiokande),Phys.Rev.D73,112001 (2006) [2] B.Aharmim et al. (SNO),Phys.Rev.Lett. C72, 055502[3] (2005) T.Araki et al. (KamLAND),Phys.Rev.Lett. 94, 081801 (2005) [4] Y.Ashie et al. (Super-Kamiokande),Phys.Rev.D71,112005(2005) [5] M.H.Ahn et al. (K2K),Phys.Rev.D74, 072003 (2006) [6] D.G.Michael et al. (MINOS),Phys.Rev.Lett. 97,191801 (2006) [7] M.Ambrosio et al. (MACRO),Eur.Phys.J.C36,323(2004) [8] W.W.Allison et al. (Soudan-2),Phys.Rev.D72,052005 (2005) [9] M.Apollonio et al. (CHOOZ),Eur.Phys.J C27,331 (2003) [10] V. Barger et al., PRL82:2640(1999) [11] G.L. Fogli et al., PRD67:093006 (2003) [12] P. Adamson et al. (MINOS), Phys.Rev.Lett.101:131802 (2008) [13] P. Adamson et al. (MINOS), Preprint[14] arXiv:0807.2424 [hep-ex] M. Guler et al. (OPERA), CERN-SPSC-2000-028,[15] CERN-SPSC-P-318, LNGS-P25-00, K. Jul Kodama 2000 et al. (DONUT), Phys.Lett.B504:218-224[16] (2001) M. Komatsu, P. Migliozzi, F. Terranova, (OPERA),[17] J.Phys.G29:443 (2003) P. Cennini et al. (ICARUS), ICARUS-PROPOSAL, Sep.[18] (1993) D. Ayres et al. (NOvA Techinal Design Report), FERMILAB-DESIGN-2007-01, Oct 8, 2007. [19] Y. Itow et al. (T2K), KEK-REPORT-2001-4, ICRR-REPORT-477-2001-7, TRI-PP-01-05, Jun 2001. [20] T. Kajita, M. Ishitsuka, H. Minakata,[21] H. Nunokawa, J.Phys.Conf.Ser.39:332-334 E. (2006) Beier et al. (Fermilab Steering Group Report), FERMILAB-PUB-07-672-DO, FERMILAB-APC, hospitality to this very excitingvarious workshop. long I baseline would experiments also that likeinformation have to kindly in thank provided order all the to the necessary prepare Colleagues material an from and as the complete as possible review talk. References Status-Prospects of Long Baseline 5. Acknowledgements