RCNP A Super-Kamiokande KamLAND, LVD, AMANDA/IceCube
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1 RCNP A Super-Kamiokande KamLAND, LVD, AMANDA/IceCube
2 SN1987A
3
4 M.Koshiba Kamiokande-II detector neutrino Inner counter: 2140 tons inch PMTs Anti-counter inch PMTs e
5 Vander Velde IMB-3
6 Kamiokande IMB Kamiokande-II IMB-3
7 Detection efficiency
8 Raffelt eorg Raffelt, Max-Planck-Institut für Physik, München, Germany Interpreting SN 1987A Neutrinos Twenty Years After SN 1987A, February 2007, Hilton Waikola, Hawaii Jegerlehner, Neubig & Raffelt, PRD 54 (1996) 1194 Total Binding Energy 95 % CL Contours _ Spectral ν Temperature e Theory Assume thermal spectra and equipartition of energy between the six degrees of freedom ν e, ν µ, ν τ and their antiparticles
9 Angular distribution to SN1987a
10 aavedra Liquid Scintillator Detector (LSD) H=5200 m.w.e. 72 counters 90 tons of n H 2n (n~9), 200 tons of Fe Fe (2 cm) 6 m 4.5 m # of event Time, UT 2ms Energy, MeV :52:36,79 40,65 41,01 8m 42,70 43,80 6,2 7 5,8 8 7,8 11 7,0 7 6,8 9 Fe (10 cm) 1 2 7:36:00,54 7:36:18,88 8 9
11 .Suntzeff SN1987A in 2003
12 N.Suntzeff
13 N.Suntzeff Evolution of the Ring Spot 1 V band evolution P. Challis CfA
14 Y,Tanaka
15 Y,Tanaka
16 Y,Tanaka ( Park et al., 2005) (Haberl et al., 2006) (Hasinger et al., 1996)
17 Y,Tanaka 17 Jan Dec Apr Dec May Dec Jul Jan 04 22Jul Jan 05 Park & Burrows
18 Super-Kamiokande 32,000 ton MeV energy threshold KamLAND 1000 ton Sub-MeV LVD 1000 ton segmented 4MeV threshold AMANDA/IceCube 1 dark noise rate coherent
19 1996 Start History of Super-Kamiokande Detector SK-I Accident Partial Reconstruction SK-II Full reconstruction SK-III Number of ID PMTs (photocoverage) 11,146 (40%) 5,182 (19%) 11,129 (40%) (Number of OD PMT: 1885) SK-I SK-II 50kton water Cherenkov detector with 32kton photosensitive volume 1000m underground SK-III
20 Expected number of events from a supernova at SK Neutrino flux and energy spectrum from Livermore simulation (T.Totani, K.Sato, H.E.Dalhed and J.R.Wilson, ApJ.496,216(1998)) 5MeV threshold ~7,300 ν e +p events ~300 ν+e events (-) ~100 ν e + 16 O events for 10 kpc supernova
21 Neutrino flux and spectrum from Livermore simulation Neutrino oscillations are not taken into account here. Expected time profile and spectrum Expected number of events in parentheses Time profile SN at 10kpc Visible energy spectrum
22 Time profile Effect of neutrino oscillations SN at 10kpc Neutrino flux and spectrum from Livermore simulation Dot: Inverted hierarchy (P H =0) Dash: Nomal, Inv.(P H =1) Solid: No oscillation P H : crossing probability at H resonance (P H =0: adiabatic) Neutrino oscillation increase number of events by 10~30 %.
23 Neutronization burst Number of events from 20msec to 0.1 sec (e - +p n+ n+ν e ) SN at 10kpc Neutrino flux and spectrum from Livermore simulation Event rate of ν e +p events Event rate of neutronization burst (forward peaked ν+e scattering events) No oscillation Normal P H =1 or Inverted hierarchy Normal hierarchy P H =0 P H : crossing probability at H resonance (P H =0: adiabatic) Number of events from neutronization burst is 0.7~5 event for SN@10kpc. ν e p events during this 10msec is about 5-20 events
24 νe energy spectrum and time variation of energy Visible energy spectrum in each time range range Time variation of average energy Events/MeV Events/MeV Neutrino flux and spectrum from Livermore simulation ν e Time= sec 161 events < 0.1sec Energy (MeV) ν e Time= sec 3140 events Energy (MeV) Events/MeV ν e Time= 1-18 sec 3979 events 0.1-1sec 1-18sec Energy (MeV) Average energy (MeV) Error of energy (MeV) SN at 10kpc 20 time bins ν e Time (sec)
25 Model dependence of luminosity and energy Burst models Livermore simulation Totani, Sato, Dalhed and Wilson, ApJ.496,216(1998) Thompson, Burrows and Pinto, ApJ.592, 434(2003) Buras, Janka, Rampp and Kifonidis, A&A 457, 281(2006) (s112_128_f). Sumiyoshi, Yamada, Suzuki, Shen, Chiba and Toki, ApJ.629, 922(2005) Shen EOS Liebendorfer, Rampp, Janka, and Mezzacappa, ApJ. 620, 840(2005) AGILE-BOLTZTRAN Liebendorfer, Rampp, Janka, and Mezzacappa, ApJ. 620, 840(2005) VERTEX Thanks to H.Suzuki for compiling the model.
26 Sensitivity of SK for time variation measurement Assuming a supernova at 10kpc, expected statistical error is plotted. Time variation of event rate Time variation of mean energy Enough statistics to test those models
27 events/bin Identification of νe scattering events by direction to supernova Energy = 5-10 MeV ν+e events/bin Energy = MeV ν+e SN at 10kpc events/bin cos(θ SN ) 60 Energy = MeV νe+p ν+e νe+p events/bin cos(θ SN ) νe+p cos(θ SN ) 25 Energy = MeV ν+e νe+p cos(θ SN ) Direction of supernova can be determined with an accuracy of 2-3 degrees. νe scattering events can be statistically extracted using the direction to supernova. Neutrino flux and spectrum from Livermore simulation
28 ν e +ν x spectrum measurement by νe scattering SN at 10kpc SN at 2kpc events/2mev Spectrum of νe - (10kpc) 32kton volume events/2mev Spectrum of νe - SK 32 kton 2kpc 1 10 error/mean Electron energy (MeV) Spectrum measurement up to ~20MeV. error/mean Electron energy (MeV) Spectrum measurement up to ~50MeV. Neutrino flux and spectrum from Livermore simulation
29 On-line supernova alarm system Data Acquisition system Offline computer ALARM Notify to shift person and supernova experts Check vertex distribution and event pattern Online host computer A few minutes later Supernova watch computer can process within 5 min. If a candidate is found (for 10kpc supernova) Send signal to SNEWS SNEWS: (SuperNova Early Warning System) Selection criteria: 25 ev. in inner 22.5kton volume within 20 sec. Rmean > 7.5m Rmean: averaged distance between event vertices. This cut rejects spallation and flasher backgrounds. Alarm rate was about once per ~10 days. (specification of SNEWS).
30 LAND 1000
31 P. Vogel
32 Solid: sum of all ν µ ν µ ν τ ν τ P. Vogel ν e ν e
33 LVD detector LVD consists of an array of 840 counters, 1.5 m 3 each. Total target: 1000 t of C n H 2n 900 t of Fe 4MeV threshold With <1MeV threshold for delayed signal (neutron tagging efficiency of %) E resolution: 13%(1σ) at 15MeV At Gran Sasso Lab. Fulgione Twenty Years after SN1987A Fulgione@to.infn.it
34 L.Koepke The Giga-ton IceCube Detector Array IceTop Design Specifications Fully digital detector concept Number of strings 75 Number of surface tanks 160 Number of DOMs 4820 Instrumented volume 1 km 3 Angular resolution < 1.0 Collaboration AMANDA construction: IceCube construction: institutions, ~ 250 members Collecting physics data
35 L.Koepke AMANDA/IceCube as MeV ν detector first proposed by Halzen, Jacobsen & Zas, astro-ph/ ice uniformly illuminated detect correlated rate increase on top of PMT noise
36 L.Koepke IceCube as MeV ν detector accretion phase IceCube 10 kpc Helmholtz cooling phase Disadvantage: no pointing no energy intrinsic noise Advantage: high statistics (0.75% stat. 0.5s and 100ms bins) Good for fine time structures (noise low)! Simulation based on a numerical Livermore model at 10 kpc (normalization to SN1987A would give flux 1/3 lower) Totani, Sato, Dalhed & Wilson, ApJ 496 (1998) 216 See also Dighe, Keil & Raffelt, hep-ph/ for pointing out IceCube s capabilities
37 S. Ando
38 S. Ando
39 S. Ando
40 S. Ando
41 Neutrino Flux per sq-cm per second per MeV Supernova Relic Neutrinos) Reactor ν Solar 8 B Solar hep Population synthesis (Totani et al., 1996) Constant SN rate (Totani et al., 1996) Cosmic gas infall (Malaney, 1997) Cosmic chemical evolution (Hartmann et al., 1997) Heavy metal abundance (Kaplinghat et al., 2000) LMA ν oscillation (Ando et al., 2002) SRN predictions Atmospheric ν Neutrino Energy (MeV)
42 SRN flux S.Ando, NNN05
43 Neutrino spectrum from each Z range S.Ando, Astrophys.J. 607, 20(2004)
44 Energy spectrum of SK-I I and SK-II (>18MeV) SK-I (1496days) SK-II(791 days) 90% CL limit of SRN Total background Atmospheric ν µ invisible µ decay e Events/4MeV Atmospheric ν µ invisible µ decay e Atmospheric ν e Atmospheric ν e Remaining spallation Energy (MeV) Observed spectrum is consistent with estimated background.
45 Flux limit and theoretical prediction E e >18 MeV (E ν >19.3 MeV) SK-II upper limit: < 3.7 /cm 2 /sec (preliminary) ν SK SK-I limit upper (90% limit: C.L.) < 1.2 /cm 2 /sec SK limit is close to the expectation! Flux revise in NNN05
46 ν e Possible improvement in future Neutron tagging p e + n Gd p Positron and gamma ray vertices are within ~50cm. Possibility 1 2.2MeV γ-ray T = ~ 200 µsec Possibility 2 n+gd ~8MeV γ T = ~30 µsec Add 0.2% GdCl 3 in water ( GAZOOKS! (M.Vagins and J.Beacom) ν e can be identified by delayed coincidence. γ γ n+p d + γ Number of hit PMT is about 6 in SK-III
47 possible π + production ν µ ν µ 16 O Post-activity Pre-activity Possible γ-ray emission Invisible µ Decay e T = ~ 2 µsec
48 Possibility of SRN detection Relic model: S.Ando, K.Sato, and T.Totani, Astropart.Phys.18, 307(2003) with flux revise in NNN05. If invisible muon background can be reduced by neutron tagging SK10 years (ε=80%) Assuming 90% of invisible muon B.G. can be reduced by neutron tagging. Assuming 80% detection efficiency. Signal: 22.7, B.G (E vis =15-30 MeV) Signal: 44.8, B.G (E vis =10-30 MeV)
49 Galactic supernova
50 Y.Suzuki S. Ando, J. F. Beacom and H.Yuksel, astro-ph/ ~1 SN /year if you have a sensitivity to 10 Mpc. ~0.3 SN /year to 4 Mpc. They pointed out that The true nearby supernova rates are probably about 3 times higher than in their calculation, which they regarded as quite conservative. Aim to have a sensitivity to 4 ~ 5 Mpc!! in order to observe 1 SN /yr
51 Y.Suzuki Expected # of neutrino 10kpc 1Mt 1Mpc 1Mt 5Mpc 1Mt 5Mpc 5Mt 10Mpc 5Mt Kamiokande 1987A 50kpc, ~2kt, 11 events (T=2.7 MeV) 140k IMB 1987A 50kpc, ~6kt, 8 events (T=4.0 MeV) 24 KM-II 310k Typical Simulation Ref: Totani et al., astroph/ J.F.Beacom hep-ph/ and others 260k For standard SN: ~ 5 for 5Mt detector
52 Y.Suzuki Deep-TITAND Tension Leg Platform (TLP) Laboratory, Office, Café, Power station, Water purification sys., Dormitory etc. Autonomous Underwater Vehicle (AOV) 85m 105m 85m Depth 1000 m Distance 600 m 85mx85mx105m=0.76Mt 76x76x96m 3 =0.554Mt (fiducial( fiducial) Inner surface: m 2 9 units 5 Mt (fid.) Placed at the depth of ~1000m
53 F. von Feilitzsch LENA N pe ~ 110 / MeV beta P - decay event PM ( 30% coverage) Scintillator: : PXE, non hazard, flashpoint 145 C, density 0.99, Light absorption L= 12m, ultrapure (as proven in Borexino design studies) 30kton
54 Event rates for a SN type IIa in the galactic center (10 kpc) F. von Feilitzsch Galactic Supernova neutrino detection with Lena (ca events for 30 kt) (1) (2) (3) (4) (5) (6) ν e ν e + ν + e x x x 12 ν + ν ν p C C + e + C p e e + e + x + n ν B N C * (Q = 1.8 (Q = 13.4 (Q = 17.3 MeV) with 12 MeV) C MeV) * 12 C + γ Electron Antineutrino spectroscopy Electron ν spectroscopy ~ 65 (Q = E = 15.1 MeV) ν x + e (elastic scattering off electrons) ~ 480 ν x + p (elastic scattering off protons). Neutral current interactions; info on all flavours ~ 4000 and ~ 2200,, det. of p recoil needs very low threshold (200 kev) γ ~7800
55 F. von Feilitzsch SNN-detection and neutrino oscillations Scintillator good resolution Water Cherenkov Modulations in the energy spectrum due to matter effects in the Earth Dighe, Keil, Raffelt (2003)
56 A.Rubbia
57 A.Rubbia
58 A.Rubbia
59 Conclusions Kamiokande-II IMB-3 SN1987A Super-Kamiokande galactic KamLAND, LVD, IceCube galactic supernova complementary Super-Kamiokande
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