Atmospheric Neutrinos High Energy Neutrino Astronomy Supernova Burst SN1987A

Neutrino Physics (Rapporteur talk)

M.Nakahata Kamioka observatory ICRR, Univ. of Tokyo

1 Physics of wide energy range

Solar neutrinos Atmospheric neutrinos High energy neutrino astronomy Supernova burst SN1987A

6 9 12 15 18 21 10 10 10 10 10 10 Energy (eV)

2 Many physics topics Origin of cosmic ray Neutrino oscillations Acceleration mechanism

ne Supernova mechanism

n m nt

T.K.Gaisser(2006)

Solar SN Atmospheric High energy neutrinos

6 9 12 15 18 21 10 10 10 10 10 10 Energy (eV)

3 Contribution papers to ICRC2013 (to NU-EX, NU-IN and NU-TH) topics papers Solar neutrinos 1 Supernova neutrinos 5 Atmospheric neutrinos 13 High energy astrophysical neutrinos 64 Others 5 Total 88 papers

4 Contribution papers to ICRC2013 (to NU-EX, NU-IN and NU-TH) topics papers Solar neutrinos 1 Supernova neutrinos 5 Atmospheric neutrinos 13 High energy astrophysical neutrinos 64 Others 5 Total 88 papers

In which 20 are results from IceCube 10 are results from ANTARES

5 Current knowledge of neutrino masses and mixings

6 Neutrino oscillations n e Ue1 Ue2 Ue3 n1 Weak Mass eigenstates nm = Um1 Um2 Um3 n2 eigenstates( n ) ( U U U ) ( n ) t t1 t2 t3 3

Pontecorvo-Maki-Nakagawa-Sakata (PMNS) matrix

-id 1 0 0 +c13 0 +s13e +c12 +s12 0

0 +c23 +s23 0 1 0 -s12 +c12 0

-id 0 -s23 +c23 -s13e 0 +c13 0 0 1

sij=sinqij、cij=cosqij

d : Dirac CP phase7 2 q23 – Dm32 : SK atm. and accelerators

SK atm. 3n

T2K 2011

MINOS T2K

SK atm. L/E

2 2 2 8 Future: T2K will reach accuracy of d(sin 2q23)=0.01 and d(Dm 32)=0.0001eV . 2 q12 – Dm21 : solar and KamLAND-reactor H.Sekiya (ID:48) NU-EX03

2 +0.20 -5 2 Δm 12=7.45- 0.19 x10 eV Green: Solar global 2 sin θ12=0.304±0.013 dashed only SK+SNO 5σ Blue: KamLAND reactor 4σ Red: Solar global+KamLAND 3σ

Combined KamLAND Solar Data f8B=(5.25±0.20) x 106/(cm2∙sec)

9 Summary of q13 measurements

±1s range

2 sin 2θ13 All results are consistent. 2 Reactor combine: sin 2θ13 =0.093 ± 0.009 10 Current summary of neutrino properties

Normal hierarchy? Inverted hierarchy? Degenerate?

2 m 2 m3 2 Dm 2=~7.4x10-5 eV2 2 21 m1

2 -3 2 Dm32 =~2.4x10 eV ne n m 2 -3 2 Dm32 =~ー2.4x10 eV nt

2 m2 Dm 2=~7.4x10-5 eV2 2 21 2 m1 m3

Unknown properties  Which mass hierarchy ?  What is the value of CP phase d ?

 (q23 – 45°） = 0?, >0?, or <0 ?  Absolute value of mass ?  Majorana or Dirac mass ? 11 Solar neutrinos

Solar neutrinos

6 9 12 15 18 21 10 10 10 10 10 10 Energy (eV) 12 Measured solar neutrino survival probability H.Sekiya (ID:48) NU-EX03

+ Pee p+p➝d+e +ν e (99.77%) - all solar p+e +p➝d+ν e BORE- BOREXINO (0.23%) XINO

d+p➝3He+γ MSW (solar&KL) MSW (solar) SK & SNO

3 7 Ηe+α➝ Be+γ 15.08% 3 3 Ηe+ Ηe➝α+2p 84.92% 3He+p➝α+e++ν e Cl BORE- 7Be+e-➝7Li+ν e 99.9% 7 8 XINO Be+p➝ B+γ 0.1%

8B+➝8Be*+e++ν e

7Li+p➝α+α; 8Be*➝α+α 13 Indication of terrestrial matter effect(Super-K) NU-EX03 H.Sekiya (ID:48) During night, n e day probability increases Day flux – Night flux ADN= due to the earth 0.5 (Day flux + Night flux) matter effect.

ADN (±stat.±sys.) SK-I -2.0±1.7±1.0 % SK-I,II,III,IV Combine Day/Nightnight Asymmetry SK-II -4.3±3.8±1.0 %

) 1

(

2 2 y sin θ =0.314 sin θ =0.025 SK-III -4.3±2.7±0.7 %

r 12 13

t e

m 0 m

y SK-IV -3.4±1.8±0.6 %

h g

i -1 SK

N /

y -3.2±1.1±0.5 % a

D combined -2 Best Fit 1σ Stat. -3 2.7 σ away 1σ Stat. + from zero.

-4 Sys. Day/night asymmetry Day/night (%) asymmetry -5 2 4 6 8 10 12 14 16 18 20 22 2 -5 2 Dm21 (10 eV ) ±1σ Solar ±1σ Kamland 14 Supernova Neutrinos

SN1987A

Supernova neutrinos

6 9 12 15 18 21 10 10 10 10 10 10 Energy (eV) 15 History of supernova detectors 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 2 2 2 2 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 0 0 0 0 0 0 0 0 0 0 0 0 0 0 8 8 8 8 8 8 8 8 8 8 9 9 9 9 9 9 9 9 9 9 0 0 0 0 0 0 0 0 0 0 1 1 1 1 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 BAKSAN (330t liq.sci.) IMB (7000t water) Kamiokande (2140t water) LSD(90t liq. sci.) LVD (3301000t liq. sci.) SN1987a Super-Kamiokande (32000t water) Amanda/IceCube

SNO (1000t D2O) KamLAND(1000t liq.sci.)

Borexino(300t liq.sci.)

HALO (76t Pb, 3He counter) 16 Summary of current supernova n detectors # of events expected for 10kpc. Directionality Baksan 330 ton liquid scintillator No + (1980-) ~100 nep e n events. LVD 1000 ton liquid scintillator. 840 counters 1.5m3 each. 4 MeV No (1992-) thres., ~50% eff. for tagging decayed signal. + ~300 nep e n events. Super-K 32,000 tons of water target. Yes + (1996-) ~7300 nep e n, ~300 nene scattering events. KamLAND 1000 ton liquid scintillator, single volume. No 12 (2002-) ~300 nep , several 10 CC on C, ~60 NC g, ~300 np  np ICECUBE Gigaton ice target. No (2005-) By coherent increase of PMT single rates. High precision time structure measurement. BOREXINO 300 ton liquid scintillator, single volume. No 12 (2007-) ~100 nep , ~10 CC on C, ~20 NC g, ~100 np  np HALO SNO 3He neutron detectors with 76 ton lead target. No (2010-) ~40 events expected. 17 Supernova burst searches Baksan A. Gaponenko(ID:621) LVD C. Vigorito (ID:453) Poster(NU-EX) Poster(NU-EX) 330 ton liquid 1000 ton liquid scintillator in 3180 scintillator in 840 tanks. tanks at Gran 850 m.w.e. at Sasso. Baksan lab.

Criteria: ≥9 events with E>8MeV in 20 sec Criteria: ≥N events with E>7MeV or in the lower horizontal layers (130 ton) E>10MeV events within 20sec. Detection efficiency

E>10MeV No candidate for 28 years from 1980 to E>7MeV 2013. Upper limit of SN rate: < 0.082 /yr

No candidate for 19.3 years from 1992 to 2013. Upper limit of SN rate: < 0.12 /yr 18 Supernova neutrino at IceCube Improvement of Data Acquisition Off-line burst search G. Kroll(ID:446) system Poster(NU-EX) D. Heereman(ID:444) Significance plot of data vs. expectations Poster(NU-IN)

The newly installed HitSpool Interface enables

• Record all hit information in [-30s, +60s] data around the burst with Data with muon subtraction is blinded above 6 full data stream (instead of current 887 days’ data from April 2008 to May 2011 2 ms time binning). • Use correlation of hits of DOMs to High efficiency for galactic supernova. estimate mean energy (~30% error for 10kpc supernova).

19 Supernova Relic Neutrinos at Super-K

ne spectrum n L. Marti(ID:719) n NU-IN01 e p Gd + e γ SRN predictions (ne fluxes) 8 MeV ΔT~20μs Vertices within 50cm GADZOOKS!: Dissolve ~100ton (0.2%) of

Gd2(SO4)3 to the Super-K tank.

Expected SRN events 1.3 -6.7 events/year/22.5kt (10-30MeV) SK fiducial volume R&D work is on-going with a 200ton tank (EGADS project). Good water transparency has been achieved. 20 Atmospheric Neutrinos

Atmospheric neutrinos

6 9 12 15 18 21 10 10 10 10 10 10 Energy (eV) 21 2 2 sin q23 – Dm32 : From latest Super-K atmospheric n NH IH

Fixed reactor q13 Fixed reactor q13

0.14 3 2 0.36 3 2 2.82 0.47 10 eV (1s ) 2.66 0.33 10 eV (1s ) 0.39  0.64(90%C.L.) 0.41 0.64(90%C.L.)

Fixed reactor q Fixed reactor q NH 13 IH 13

99% C.L. 99% C.L.

90% C.L. 90% C.L. 68% C.L. 68% C.L.

22 CP d and mass hierarchy: from Super-K atmospheric n

Fixed reactor q13 90% C.L. NH

68% C.L. IH

Fixed reactor q13 2 NH  min = 557.7 / 477 dof 90% C.L. 2 IH  min = 556.2 / 477 dof

2 2 68% C.L. min (NH )  min (IH )  1.5

23 Atmospheric neutrino oscillations M. Medeiros(ID:958) IceCube/DeepCore C.Wiebusch (ID:848) MINOS Poster(NU-EX) May 2010 – May 2011 (312d) NU-EX03 Analysis of beam+atmospheric L/E vs. Ratio (Nobs/Nno_osc.)

 Log10(L/E)

eV 3

- This work

/ / 10

32 32

m D J.P.Yanez (ID:450) poster

2 sin (2q23) Sensitivity study for sterile neutrinos at 24 IceCube (M. Wallraff (ID:455)) Poster(NU-EX) Neutrino mass hierarchy study with PINGU Determine mass hierarchy using earth matter effect. A. Gross(ID:555) High energy and angular resolutions are necessary. NU-IN01 Oscillation prob. at 10 GeV Potential design 20 strings case 40 strings case

Expected sensitivity for mass hierarchy

25 Calculation of Atmospheric Neutrino Flux with NRLMSISE-00 NRLMSISE-00 atmospheric model gives density variation M. Honda (ID:990) as a function of position on the earth and the time in a year. Poster(NU-TH) Flux averaged over Monthly Fluxes at 10 TeV at South Pole direction and time nm+nm ne+ne

Solid: NRLMSISE-00 Dotted: previous model (US-standard76)

Difference is small when averaged over a year.

Seasonal variation of the fluxes is expected in the NRLMSISE-00 atmospheric model even at 10 TeV at South Pole. 26 Seasonal variation of atmospheric n at IceCube P. Desiati (ID:492) zenith angle range 90 < q < 120 deg. Poster(NU-EX) Data between April 2008 and July 2011 (data points).

Black curve: effective temperature change

downward muon event rate

Seasonal variation is observed with about 5% amplitude with 3.4 sigma level.

27 Flux calculation of atmospheric neutrinos Include prompt neutrinos using charm in new version of SIBYLL Gaisser (ID:1144) NU-TH01 ne nm

Charm Charm crossover crossover ~10 TeV ~100 TeV

nm spectrum 1PeV

Conventional + prompt calculated with Models of primary various nucleon spectra ERS = PR D78 (2008) 043005 nucleon spectrum TIG = Astropart. Phys. 5 (1996) 309 FBD = PRD86 (2012)

Another calculation of prompt flux by S.I.Sinegovsky(ID:40) Poster(NU -TH) 28 High Energy Neutrinos SNR RX J1713.7-3946 Chandra Cassiopeia A H.E.S.S.

High energy neutrinos

6 9 12 15 18 21 10 10 10 10 10 10 Energy (eV) 29 Physics of high energy neutrinos We know cosmic rays(p, He, ..) exist. So, there much be cosmic high energy neutrinos. Possible sources: AGN, supernova remnants, ….

nm nm ne + e+ m gsync + p

g sync e-

n e :n m :nt 1:1:1 when we observe (due to n osc.)

30 IceCube ANTARES

885 optical modules in 12 strings Detector volume:0.2 km x 0.2 km x 0.45 km 5160 optical modules in 86 strings Detector construction completed in 2008. Detector volume: (1 km)3 Data phases: IceCube 40 (2008-9) IceCube 59 (2009-10) IceCube 79 (2010-11) IceCube 86 (2011-) 31 Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector C. Kopper (ID:650) Data set: May 2010 – May 2012 (662 days) NU-EX03 Period: 79 and 86 strings Event selection: Vertex contained in fiducial volume. (no early timing hits in veto region)

28 events in 30-1200 TeV ~4s excess Background: 10.6 +5.0 (uncertainty of the prompt component is based on the upper -3.6 32 limit of IC59 nm data) Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector C. Kopper (ID:650) Data set: May 2010 – May 2012 (662 days) NU-EX03 Period: 79 and 86 strings Event selection: Vertex contained in fiducial volume. (no early timing hits in veto region)

Congratulations! 28 events in 30-1200 TeV ~4s excess Background: 10.6 +5.0 (uncertainty of the prompt component is based on the upper -3.6 33 limit of IC59 nm data) Evidence for High-Energy Extraterrestrial Neutrinos at the IceCube Detector C. Kopper (ID:650) NU-EX03 Energy spectrum Skymap

No significant clustering observed? Potential cutoff at about 2-5 PeV 2 -8 -2 -1 -1 Best fit: E fn= (1.2±0.4)x10 GeVcm sr s (per n flavor)

34 Cascade event search at IceCube-59 Data between May 2009 and April 2010 (335 days live time) A. Schönwald(ID:662) Event selection: Vertex is contained in the detector. NU-EX03 Some further criteria to select cascade events. 8 events found in data (from 39 TeV to 67 TeV) 4 expected background

Likelihood fit says best fir prompt atmospheric neutrino is

Upper limit on astrophysical neutrino flux was obtained to be 2 -8 -2 -1 -1 E f < 1.7x10 GeVcm sr s (per all n flavors, w/o cutoff)

This result is consistent with the IC79, IC86 data.

35 GRB correlation at IceCube IceCube 40, 59, 79, 86(1st year) was used, i.e. 4 yrs data. M. Richman (ID:1180)

Upgoing nm channel was used, i.e. sq is 1°(3TeV), 0.5 °(1PeV). Poster(NU-EX) The neutrino time window is at the same time as the observed gamma rays. 543 GRBs were observed during the analyzed time. Only one candidate remained. Flux upper limit

p-value is 0.11 (or 1.2s). So, it is not significant. Excluded models in which the entire cosmic ray New model and limit flux at the highest energies results from GRBs.

(Fireball and photospheric models)

Prediction is below the obtained limit, but they are very close.

36 GRB correlation at ANTARES C. W. James (ID:760) NU-EX01 Total 6.6 hours duration

Event selection • Within observed GRB duration (~1 minute/GRB) • Reconstructed direction: within 10° of GRB direction • Quality cuts (exclude down-going muons from cosmic rays) • Extended maximum likelihood (signal vs background) on remaining data

No coincident events observed and set upper limit. Dotted curves: 90% CL limits Solid curves: predictions Blue: Guetta et al. Red: NeuCosmA et al. 37 Point and extended source search at IceCube All-sky scan using 4 years data J. A. Aguilar (ID:550) 394,000 total events in 1371 days NU-EX01 (178k neutrino candidates in North, 216k atmospheric muons in South)

Northern Sky

Southern Sky

Equatorial coordinates

Source based search • Among 44 candidate sources of supernova remnants, AGN and etc., no significant excess was found. • Searches using stacked source catalogs (Milagro SNRs, Starburst Galaxy, Galaxy cluster, Molecular Could SNR, Black hole) did not show significant excess, and upper limit was obtained. Analysis is not yet background dominated. More data is necessary. 38 Point and extended source search at IceCube All-sky scan using 4 years data J. A. Aguilar (ID:550) 394,000 total events in 1371 days NU-EX01 (178k neutrino candidates in North, 216k atmospheric muons in South) Most significant spots -log10(p) = 5.039 RA: 11.45° Dec: 31.35° Northern nSrcbest: 40.17 Sky Post trials p-values: γ best: 3.45 Northern Sky: 37.6% Southern Sky: 9.3%

-log10(p) = 5.958 Ra: 296.95° Dec: - 75.75° Southern Sky nSrcbest: 16.16 γ best: 2.34 Equatorial coordinates

Source based search • Among 44 candidate sources of supernova remnants, AGN and etc., no significant excess was found. • Searches using stacked source catalogs (Milagro SNRs, Starburst Galaxy, Galaxy cluster, Molecular Could SNR, Black hole) did not show significant excess, and upper limit was obtained. Analysis is not yet background dominated. More data is necessary. 39 Point and extended source search at ANTARES Data period 2007 – 2012  ~1340 days S. Schulte (ID:425) With 5516 neutrino candidates. NU-EX03 most signal like cluster found at α = -46.80º , δ = -64.90º (14 events within a 2 degree search cone) p-value = 2.1% sign = 2.3s

Extended source search Source list upper limits

40 More source related searches @ IceCube Cygnus region A. Bernhard(ID:471) Poster(NU-EX) Multi-flare AGNs A. Cruz (ID:539) Poster(NU-EX) Flaring and periodic sources J. Aguilar (ID:649) NU-EX01

@ ANTARES Coincidence with gravitational wave T. Pradier(ID:778) Poster(NU-EX) Gamma-ray flaring blazars D. Dormic(ID:296) Poster(NU-EX) Fermi Bubbles V.Kulikovskiy(ID:031) NU-EX01 2pt correlation analysis F. Schüssler (ID:420) NU-EX03 Gravitational lensing sources S. Mangano (ID:614) Poster(NU-EX)

No significant excess was found from them, but sensitivity will soon reach interesting flux level. 41 Possible interesting signals in future Tau neutrinos with double Glashow resonance at pulses at IceCube D. Xu(ID:643) IceCube J. Kiryluk(ID:494) Poster(NU-IN) Poster(NU-IN) A high energy n charged current (CC) interaction - - t Due to Glashow resonance(ne+e →W ), in the ice would produce two showers. event excess is expected at En=~6.3 PeV.

About 0.32±0.04 events/year nt CC events are expected assuming a flux of all neutrino 2 -8 -1 -1 -2 flavors E fn= 3.6x10 GeVsr s cm . Expect 0.9 (0.4) resonance events/year from

pp(pg) sources for 5PeV< Evis< 7PeV assuming 2 -8 - electron type flux of E f(ne+ne)= 1x10 GeVsr 1s-1cm-2.

42 Follow-Up program at ANTARES Project TAToO: For transient sources such as GRBs and SN D. Dornic (ID:299) neutrinos, send alert to optical telescopes. NU-EX01 Selection criteria ANTARES Shore Station: • Coincidence of 2 or more On-line reconstruction events in direction and time. Trigger decision • One single very high energy Alert message (GCN format) event. • One single event which its ANTARES direction in coincidence with Neutrino local galaxies. Telescope Requirements: ~2 alerts/month Alert sending delay ~20s ν with 0.3-0.5o TaToO alert system Optical telescopes Optical images operational since 2009.

43 Follow-Up program at IceCube For GRBs and choked jet supernovae, send alert from IceCube M. Voge (ID:852) to optical and X-ray telescopes. Poster(NU-EX) Selection criteria • Neutrino multiplets (Nν≥2): • Within 100 seconds in time • Within 3.5° in direction An interesting coincidence Doublet with 1.79 s, 1.32°separation. SN named PTF12csy discovered, very close (0.14°) from the neutrino direction.

Latency: ~1-4 minutes Earliest detection of PTF12csy was 169 days prior to the neutrino alert. P-value of the neutrino alert is 1.6%. Optical and X-ray follow-up programs run stably since Dec. 2008. No significant deviation from background.

Flow-up program to a Cherenkov telescope (e.g. MAGIC and VERITAS) is also running (D. Gora (ID:537)). Poster(NU-EX) 44 Future High energy neutrino detectors

45 Future High energy neutrino detectors (km)3 size in North KM3NeT (ID:891, 165, 1249, by water Cherenkov 1163, 1222, 164) BAIKAL-GVD (ID:510)

3 > 10 x (1km) by ARA (ID:704, 1230, 162, 1161) radio antenna array ARIANNA (ID:825, 834)

Other proposals presented in ICRC2013

• ExaVolt Antenna(EVA) super balloon radio detection (A. Connolly (ID:1152)) • Acoustic detector at ANTARES/KM3NeT (R. Lahmann (ID:745)) • Earth-skimming tau neutrino shower detection (Ashra) (M. Sasaki (ID: 977)) • Radio detection on the moon surface (A. Aminaei (ID:223), C.James (ID:1052)) • Radio detection in the salt mine (A. M. Badescu (ID:232))

• Neutrino-initiated EAS by JEM-EUSO (A. Guzman (ID: 533)) 46 NU-IN01 P. Coyle (891) KM3NeT NU-TH01 Multi-km3 neutrino telescope in the Mediterranean Sea A. Trovato(165) Optimal detector parameter Inter-string spacing: ~90m DOM Inter-DOM spacing: ~36m DOMs/string: 18 Building block: ~115 strings No of building blocks: 6

Discovery of RXJ1713.7-3946 (Vela X) after about 5 (3.3) observation years. Phase 1 funding secured. Decision taken for distributed infrastructure: - KM3NeT-France (Toulon) ~2500m - KM3NeT-Italy (Capo Passero) ~3400m Deploy method tested. - KMNeT-Greece (Pylos) ~4500m 47 BAIKAL-GVD neutrino project Poster (NU-EX) N. Budnev (ID:510) 4-5km to shore in Lake Baikal

For GVD4 Effective area: 0.25km2(1TeV), 1.8 km2(1PeV) Effective volume: 0.4km3(1TeV), 2.0 km3(1PeV)

In April 2013 the preproduction version of engineering array which comprised 72 OMs has been deployed.

Project timeline 2008-2011 2011-2014 2014-2020 R&D prototype Engineering arrays construction

48 ARA M. Richman (ID:704) Askaryan radio Array NU-IN01

Noise level

Attenuation length

Hardware prototyping is complete. 3 stations are operational 3 additional ARA stations planned for

2014-2015. 49 ARIANNA NU-EX02 S. Barwick (ID:825) Measure reflected Askaryan radio pulse Poster (NU-EX) C. Reed (ID:834) in the Ross Ice Shelf of Antarctica. Prototype detector HRA (Hexagonal Radio Array) has been installed. Bounce tests

Deployed 1 km Dec 2013

Determining pulse origin Angular resolution

Preliminary

Prototype detector is running well. ~0.17 °achieved Plan to enlarge the number of detectors, eventually >900 for ARIANNA. 50 Sensitivity of ARA and ARIANNA

Proto

IC08-09 ARIANNA IC10-12(prel.)

Should be able to detect large number of GKZ neutrino events.

51 Conclusions • In the solar neutrino observation, day/night difference due to matter effect was observed by SK. • Many detectors are waiting for a next galactic supernova, and fruitful measurements are expected. • Atmospheric neutrinos would determine mass hierarchy. • Evidence for high-energy extraterrestrial neutrinos at IceCube using cascade events. • More statistics are needed for high energy astrophysical neutrinos.

52 Conclusions • In the solar neutrino observation, day/night difference due to matter effect was observed by SK. • Many detectors are waiting for a next galactic supernova, and fruitful measurements are expected. • Atmospheric neutrinos would determine mass hierarchy. • Evidence for high-energy extraterrestrial neutrinos at IceCube using cascade events. • More statistics are needed for high energy astrophysical neutrinos.

Fruitful results from neutrino physics are coming soon!