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Low Energy n Astronomy in Super-Kamiokande

Low Energy n Astronomy in Super-Kamiokande. APS – DPF Meeting at Brown University Tuesday August 9 th 2011 Michael Smy, UC Irvine. Birth of Neutrino Astronomy. in 1987 the star Sanduleak -69 0 202a (distance: 50kpc) exploded and coincident within 13 sec

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Low Energy n Astronomy in Super-Kamiokande

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  1. Low Energy n Astronomy in Super-Kamiokande APS – DPF Meeting at Brown University Tuesday August 9th 2011 Michael Smy, UC Irvine

  2. Birth of Neutrino Astronomy • in 1987 the star Sanduleak -690 202a (distance: 50kpc) exploded and coincident within 13 sec • 11 neutrino interactions were seen by Kamiokande II • 8 neutrino interactions were seen by IMB • 5 neutrino interactions were seen by Baksan • in the same year, Kamiokande observed an excess of events in the solar direction due to solar neutrino-electron elastic scattering • since then, no extra-terrestrial neutrino sources have been observed K. S. Hirata et al. PRL 63,16-19 (1989) Michael Smy, UC Irvine

  3. Search for Other n Sources (just SK) • no neutrinos from “Astrophysical Point Sources” E. Thrane et al., APJ 704: 503-512 (2009) • no neutrinos from “GRB 080319B” E. Thrane et al., APJ 697: 730-734 (2009) • no “Supernova Neutrino Bursts” M. Ikeda et al., APJ 669: 519-524 (2007) • no “High Energy Neutrino Astronomy” K. Abe et al., APJ 652:198-205 (2006) • no “Diffuse Astrophysical Neutrino Flux” M. Swanson et al., APJ 652: 206-215 (2006) • no neutrinos from “Dark Matter WIMPs” S. Desai et al., PRD70: 083523 (2004) • no “Supernova Relic Neutrinos” M. Malek, PRL 90: 061101 (2003) • no neutrinos from “Gamma Ray Bursts” S. Fukuda et al., APJ 578: 317-324 (2002) Michael Smy, UC Irvine

  4. Neutrino Flavour Mixing: MNS Matrix Known Parameters Two Mass2 Diff. scales atmospheric: Dm223 solar /KamLAND: Dm212 Two Mixing Angles atmospheric : q23 solar/KamLAND: q12 Mass2 ordering solar: Dm212 n3 Dm223 n2 Dm212 n1 ne nm nt • Unknown Parameters • Third Mixing Angle q13 (only limit) • CP-Violating Phases • accessible via n oscillation: d • accessible only via 0nbb: a1,a2 • Mass2 ordering • atmospheric: Dm223 • Other • Mass? • Majorana or Dirac? Courtesy T. Maruyama, KEK

  5. pp 7Be 8B Solar Neutrinos ne survival probability (at best fit parameter) P(ne ne) transition from vacuum to matter osc. “upturn” in 8B relative spectrum. • conclusive proof that the sun shines because of nuclear reactions • monitors directly solar core • MSW-resonant flavor conversion happens in the sun for high energy solar neutrinos (>~3 MeV) • flavor conversion modified if neutrinos pass through the earth Vacuum osc. dominant matter dominant Michael Smy, UC Irvine

  6. Solar n Physics Began with Ray Davis… SK-III result for 8B Flux: 2.32+/-0.04(stat.)+/-0.05(syst.) (x106/cm2/s) (somewhat larger since oscillated solar neutrinos contribute) Michael Smy, UC Irvine

  7. Water Cherenkov Technique n + e- n + e- Outer Detector • Timing information vertex position • Ring pattern direction • Number of hit PMTs energy Inner Detector (color: time) Ee = 9.1MeV cosqsun = 0.95 ~6hit / MeV (SK-I, III, IV) (software improvement) • Resolutions (for 10MeV electrons) • Energy: 14%Vertex: 87cmDirection: 26o SK-I • Energy: 14%Vertex: 55cmDirection: 23o SK-III 7 Courtesy Y. Takeuchi, ICRR

  8. Solar Neutrino Oscillation Data neutrino oscillations started from “solar problem” sensitive to Dm212q12 and q13 SK Data SK-I 1496 days, spectrum 5.0-20MeV + D/N (E ≥ 5.0MeV) SK-II 791 days, spectrum 7.0-20MeV + D/N (E ≥ 7.5MeV) SK-III 548 days, spectrum 5.0-20.0MeV + D/N (E ≥ 5.0MeV) SNO Data CC flux (Phase-I & II & III) NC flux (Phase-III & LETA combined): (5.14±0.21)x106/cm2s Day/Night asymmetry (Phase-I, II & III) Radiochemical: Cl (Homestake), Ga (GALLEX/GNO/SAGE) Ga rate: 66.1±3.1 SNU (All Ga global): PRC80, 015807(2009) Cl rate: 2.56±0.23: Astrophys. J. 496 (1998) 505 Borexino 7Be rate: 46±2.2 cpd/100tons: arXiv: 1104.1816v1 (2011) KamLAND: Data 2008 8B spectrum: Winter(2006) updates since our previous oscillation analysis (PRD78,032002(2008)) Courtesy Y. Takeuchi, ICRR

  9. Solar n Flavor Physics is done? • Super-Kamiokande-I and SNO established solar neutrino flavor conversion, oscillation parameters are measured agree with reactor neutrino data… • …but transition from solar resonance to averaged vacuum oscillation has not been probed; resulting distortion to the observed spectrum so far not confirmed • … but modification of conversion by Earth matter effect is unobserved • … but a better measurement of solar mass splitting Dm212 is needed for a more meaningful comparison to reactor neutrino measurements Michael Smy, UC Irvine

  10. SK-III solar neutrino results • Total live time: 548 days, Etotal ≥ 6.5 MeV 289 days, Etotal < 6.5 MeV • Energy region: Etotal=4.5/5.0-20.0MeV • 8B Flux: 2.32±0.04(stat.) ±0.05(syst.)(x106/cm2s) • SK-I: 2.38±0.02(stat.) ±0.08(syst.) • SK-II: 2.41±0.05(stat.)+0.16/-0.15(syst.) (recalc. SK-I,II with the Winter06 8B spectrum) • Day / Night ratio: • SK-I: -0.021±0.020(stat) ±0.013(syst.) • SK-II: -0.063±0.042(stat) ±0.037(syst.) Courtesy Y. Takeuchi, ICRR

  11. Fit Day/Night Amplitude to SK Data • used for SK-I: ADN(I)=-0.018±0.016(stat) ±0.013(syst) • ADN(II)=-0.036±0.035(stat), ADN(III)=-0.040±0.025(stat) • depends on Dm2 • Combine SK-I/II/III -0.026±0.013(stat) at KamLAND Dm2 • consistent with expected amplitude • consistent with zero within 2s • systematic uncertainty under study % expected amplitude KamLAND best fit Michael Smy, UC Irvine

  12. Vertex distributions in SK-III Rate/bin 4.5-5.0MeV (12.3kt) 5.0-5.5MeV (13.3kt) 5.5-20MeV (22.5kt) Final data sample before tight fiducial volume cut SK-III fid. volume Z R reduce dissolved Radon gas bkg by water flow control detector (very precise injection water temp control) convection cell at the detector bottom transports Rn tight fiducial volume cut is applied in Etotal<5.5MeV to remove the background events. (probably Rn, g-rays from detector wall). SK detector Courtesy Y. Takeuchi, ICRR

  13. SK-IV • no hardware trigger threshold; all triggers applied by software • see solar n elastic scattering peak >4 MeV

  14. Probe Lower Energies:How to Reduce Radon Background? • work I did with my student Andrew Renshaw; not yet part of the official SK analysis • Radon decays to 214Bi which b decays: real electrons <3.1MeV fluctuating in light yield up to 6.5 MeV equivalent • multiple Coulomb scattering (mCs) is still that of ~2 to 3 MeV electrons: events more isotropic than 4-5 MeV solar neutrinos • reconstruct mCs from Cherenkov hit pattern: “goodness” of direction fit to simple cone • select large “goodness”: sharper angular resolution Michael Smy, UC Irvine

  15. goodness<0.33 0.33<goodness<0.45 goodness>0.45 cos qsun Resolution for LINAC qsun defined as the angle between –z (beam direction) and reconstructed direction 4.8 MeV Linac Data taken at (-3.9,-0.1,0)m the “ES peak” sharpens in regions of higher goodness (true for all LINAC momenta at all positions) SK-I Data >12 MeV, “goodness”>0.45 SK-I Data >12 MeV, “goodness”<0.45 size of sun: ~0.50, so cos qsunmax~0.99996 largest possible ES angle for 5 MeV electrons

  16. large “goodness” medium “goodness” small “goodness” SK IV 4-4.5 MeV SK IV 4.5-5 MeV SK IV 5-5.5 MeV SK IV 5.5-6 MeV

  17. Supernova Neutrinos Chandra/Hubble View of E0102-72

  18. νe+ 16O  16N + e+ 10 Supernova Neutrinos in SK νe+ p  e+ + n 0.1 • ~10k event burst at 10kpc distance • or search for diffuse, distant supernova n’s (DSN) • mostly inverse b’s • elastics will point • mCs reconstruction can help determine SN direction quickly and accurately • from MC simulations pointing accuracy is three to four degrees • work in progress 10-3 νe+ 16O  16F + e- 10-5 ν+ e  ν + e- 10-7 0 10 20 30 40 Electron energy [MeV]

  19. Simulated SN n Burst (10kpc): 6-20 MeV 0.21<good <0.275 good>0.4 0.275<good <0.33 0.33<good <0.4 <0.21 ES only all

  20. Diffuse Supernova Neutrinos (DSN) =signal from all past supernovae 0.8 -5.0 events/year/22.5kton (10-30MeV) 0.5 -2.5 events/year/22.5kton (16-30MeV) 0.3 -1.9 events/year/22.5kton (18-30MeV) Predicted SRN flux Motivation DSN studies n emission of typical supernova folded with the supernova rate and thereby the cosmic star formation history no signal has been detector thus far: M. Malek, et al, Phys. Rev. Lett. 90, 061101 (2003) for SK SNO, KamLAND and Borexino have searched as well Ando et al (2005) (LMA) R. A. Malaney (1997) Kaplinghat et al (2000) Hartmann, Woosley (1997) Totani et all (1996) (constant SN rate)

  21. Spallation and Solar Cuts dE/dx Plot QPeak= sum of charge in window p.e.’s spallation expected here distance along muon track (50 cm bins) • SPALLATION is cut using correlation to cosmic ray muons • Original cut used 2-D spatial correlation, time and charge • New method allows 3-D spatial correlation from m dE/dx, and muon categorization • Stricter cut < 18 MeV • SOLAR events correlate with solar dir. • use new multiple scattering recon. • cut is tuned in 1 MeV bins using MC New threshold18 16 MeV! search < 16 MeV difficult due to “wall” of long-lived spallation products energy resolution half-life (s) 11Be 16N 16 MeV 15C 8Li 12C 8B 18 MeV 9Li 9C 8He 12B 14B 12Be 12N 11Li 13B 13O

  22. Total signal efficiency: Solar and Spallation cut inefficiency SPALLATION CUT SOLAR CUT 2003 cut new cut new cut Energy range 2003 cut 16-18 MeV N/A 23% N/A 18% 18-20 MeV 7%9% 36% 9% 20-24 MeV 7% 0% 36% 9% 24-34 MeV 7% 0% 36% 0% Michael Smy, UC Irvine

  23. Atmospheric n Background 2003: two channels: νμ CC spectrum modeled by decay electrons from cosmic ray m’s νe CC spectrum from MC Now: four channels: νμ CC νe CC NC elastic required by lower E threshold; spectrum from MC μ/πprod.: reduced by cuts; helps constrain NC in signal fit Michael Smy, UC Irvine

  24. Fit to Signal & Background Signal region Isotropic region Low angle events p ne N 42o n e+ 25-45o μ, π n reconstructed angle near 90o n (invisible) low region Isotro- pic region Michael Smy, UC Irvine

  25. 20-38 degrees Fit DSN Rate for “LMA” Model 38-50 degrees SK-I data νμ CC νe CC NC elastic μ/π > C. thr. all bkg relic SK-II data νμ CC νe CC NC elastic μ/π > C. thr. all bkg relic best fit 3.5ev/yr (shown) best fit negative show 0 DSN rate SK-II only 90%c.l. < 7.4/cm2s (>16 MeV) SK-I only 90%c.l. < 2.4/cm2s (>16 MeV) >90 degrees >90 degrees 20-38 degrees 38-50 degrees SK-III data νμ CC νe CC NC elastic μ/π > C. thr. all bkg relic E (MeV) best fit 6.5ev/yr (shown) logLikelihood comb 90%c.l. 5.1/22.5ktyr 2.7/cm2s (>16 MeV) SK-III only 90%c.l. < 8.1/cm2s (>16 MeV) SK-I (~1500d) SK-II (~790d) SK-III (~560d) combined E (MeV) Michael Smy, UC Irvine ev/yr interacting in 22.5 ktons

  26. Limits on SN n Emission Spectrum • effective emission spectrum with two parameters; anything more sophisticated couldn’t be resolved with relic neutrinos: do a little astrophysics even in the absence of observation: limit typical SN luminosity and temperature • assume FD spectrum & fix core-collapse SN rate as a function of red-shift: Astro-ph.HE 1004.3311v1, Astro-ph/0509297v2, New Journal of Physics 6 (2004) 170 • this example is based on the 2003 paper Yüksel/Ando/ Beacom based on SK-I data from Malek et al (PRL 2003) Michael Smy, UC Irvine; Courtesy J. Beacom

  27. LMA = Ando et al (LMA model) HMA = Kaplinghat, Steigman, Walker (heavy metal abundance) CGI = Malaney (cosmic gas infall) FS = Lunardini (failed SN model) CE = Hartmann/Woosley (chemical evolution) Limit of Diffuse Supernova Neutrinos dotted line represents 1-D limit, red area 2-D limit 1987a Kamiokande allowed 1987a IMB allowed Michael Smy, UC Irvine

  28. Future of DSN Search in SK-IV and beyond: Inverse b Neutron Tagging • search for 2.2 MeV g with e=19%, efake=1%: see 14 candidates between 14MeV amd 88 MeV • limit is in preparation Beacom/Vagins: Gadzooks! Dope SK with 0.1% Gd and see 8 MeV g cascade from n captures Michael Smy, UC Irvine

  29. Conclusions • SK-III data has already impacted solar n global fits: • lower background • solar neutrino flux estimate below 5 MeV • three flavor analysis • SK-IV can go lower in threshold: the goal is 4 MeV total recoil electron energy and it seems within reach • SK solar analysis begins to see oscillation signatures • SK diffuse supernova neutrino search sensitivity close to prediction • even w/o a signal, SK’s search already limits typical SN n emission spectrum • Neutron tagging techniques are likely to be required for further substantial progress Michael Smy, UC Irvine

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