7 Li in a WbLS Detector Gabriel D. Orebi Gann JinPing Solar Workshop, LBNL June 10th, 2014 U. C. Berkeley & LBNL
Probing the Transition Region: why we need 8 B Largest affect on shape of survival probability R. Bonventre Best fit Pee for scalar long-range forces Δχ 2 = 2.9 C.L. = 0.58 R / R 8B produced closest into the core of the Sun Phys. Rev. D 88 (2013) 053010
Concept Load WbLS detector with 7 Li CC interaction (E )= G2 F cos2 c k e E e F(Z +1,E e )d cos de e 2 [1.0(1 + cos ) (E 0.35 E e ) +1.7471(1 1 3 cos ) (E 0.35 E e ) +1.6303(1 1 3 cos ) (E 0.35 0.4291 E e ) +0.01135(1 1 3 cos ) (E 0.35 6.73 E e ) +0.07317(1 1 3 cos ) (E 0.35 7.21 E e )] Cross section from W. C. Haxton W.C. Haxton PRL 76 (1996) 10
Concept Load WbLS detector with 7 Li CC interaction ES (E )= G2 F cos2 c k e E e F(Z +1,E e )d cos de e 2 [1.0(1 + cos ) (E 0.35 E e ) +1.7471(1 1 3 cos ) (E 0.35 E e ) +1.6303(1 1 3 cos ) (E 0.35 0.4291 E e ) +0.01135(1 1 3 cos ) (E 0.35 6.73 E e ) +0.07317(1 1 3 cos ) (E 0.35 7.21 E e )] Cross section from W. C. Haxton W.C. Haxton PRL 76 (1996) 10
Concept Load WbLS detector with 7 Li CC interaction ES (E )= G2 F cos2 c k e E e F(Z +1,E e )d cos de e 2 [1.0(1 + cos ) (E 0.35 E e ) 1 CC 8B +1.7471(1 3 cos ) (E 0.35 E e ) +1.6303(1 1 3 cos ) (E 0.35 0.4291 E e ) +0.01135(1 1 3 cos ) (E 0.35 6.73 E e ) +0.07317(1 1 3 cos ) (E 0.35 7.21 E e )] Cross section from W. C. Haxton W.C. Haxton PRL 76 (1996) 10
Concept Load WbLS detector with 7 Li CC interaction ES CC CNO (E )= G2 F cos2 c k e E e F(Z +1,E e )d cos de e 2 [1.0(1 + cos ) (E 0.35 E e ) 1 CC 8B +1.7471(1 3 cos ) (E 0.35 E e ) +1.6303(1 1 3 cos ) (E 0.35 0.4291 E e ) +0.01135(1 1 3 cos ) (E 0.35 6.73 E e ) +0.07317(1 1 3 cos ) (E 0.35 7.21 E e )] Cross section from W. C. Haxton W.C. Haxton PRL 76 (1996) 10
Detector Parameters Target composition (# targets) - - % Li loading (5%) WbLS cocktail composition Detector mass & livetime (1kT, 10 yrs) 210 Bi background (for CNO study) (Bx) Energy threshold (varies) Lightyield: p.e. / MeV (100) detector response fn R = " 1 p 2 (Te ) exp # (T eff T e ) 2 2 2
Directionality SK III angular resolution Cut on cosθ (of course one would fit!) Select CC (reject ES) - weak +ve slope Select ES, reject bkg e.g. 210Bi
Solar Neutrino Energy Spectra pp 7 Be 13 N 7 Be pep 15 O 8 B 17 F hep
Detected Spectrum cosθ < 0.4
Detected Spectrum cosθ < 0.4
8 B Study Neutrino spectrum * Pee for model n Convolve with x-sec, detector response Predicted detected electron spectrum Create fake data set (i.e. poisson fluctuate) Fit to predicted spectrum for MSW Float norm ± 4% (SNO uncert) Take residuals, find χ 2 NB currently background-free model
Pee Models (1) Flat survival probability Pee = 0.35 (2) - (37) NSI models from A. Friedland
Detected Spectra Flat survival probability Pee = 0.35 (1) No cosθ cut (2) cosθ < 0.8
Residuals CC: 98.8% ES: 62.0% 1kT Ethresh = 1.5MeV
1kT: 5% loading, 10 yrs 10kT+: 1% loading, 5 yrs Rejecting Null Hypothesis Detector Size 1kT
Rejecting Null Hypothesis Detector Size 35 30 10kT 1kT CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 Significance of rejection of null hypothesis 1kT: 5% loading, 10 yrs 10kT+: 1% loading, 5 yrs
Rejecting Null Hypothesis Detector Size 35 30 10kT 20kT 1kT CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 1kT: 5% loading, 10 yrs 10kT+: 1% loading, 5 yrs Significance of rejection of null hypothesis
Rejecting Null Hypothesis Detector Size 35 30 10kT 20kT 50kT 1kT CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 1kT: 5% loading, 10 yrs 10kT+: 1% loading, 5 yrs Significance of rejection of null hypothesis
Rejecting Null Hypothesis Detector Size 35 30 10kT 20kT 50kT 70kT 1kT CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 1kT: 5% loading, 10 yrs 10kT+: 1% loading, 5 yrs Significance of rejection of null hypothesis
Rejecting Null Hypothesis Detector Size 35 30 100kT 10kT 20kT 50kT 70kT 1kT CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 1kT: 5% loading, 10 yrs 10kT+: 1% loading, 5 yrs Significance of rejection of null hypothesis
Rejecting Null Hypothesis Light collection 35 20kT, 50 pe/mev 30 CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 Significance of rejection of null hypothesis
Rejecting Null Hypothesis Light collection 35 20kT, 100 50 pe/mev 30 CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 Significance of rejection of null hypothesis
Rejecting Null Hypothesis Light collection 35 20kT, 100 150 pe/mev 30 CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 Significance of rejection of null hypothesis
Rejecting Null Hypothesis Energy threshold 35 30 20kT, 100 pe/mev, Eth = 1.0MeV CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 Significance of rejection of null hypothesis
Rejecting Null Hypothesis Energy threshold 35 30 20kT, 100 pe/mev, Eth = 1.0MeV 1.5MeV CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 Significance of rejection of null hypothesis
Rejecting Null Hypothesis Energy threshold 35 30 20kT, 100 pe/mev, Eth = 1.0MeV 2.0MeV 1.5MeV CC 25 ES 20 15 10 5 0 0 1 2 3 4 5 Significance of rejection of null hypothesis
CNO study Full 1D extended Likelihood fit (Teff) Include major backgrounds: 210 Bi pep 7 Be Fix F to 0.01 * (N+O) Constrain (N - O) / (N + O) to 0.15 ± 30%
CNO PDFs 1kT 5% 7 Li 100 pe/mev Ethresh = 0.4 MeV 210 Bi at Bx level No cut on cosθ
CNO PDFs 1kT 5% 7 Li 100 pe/mev Ethresh = 0.4 MeV 210 Bi at Bx level cosθ < 0.4
CNO Sample Fit 1kT 5% 7 Li 100 pe/mev Ethresh = 0.4 MeV 210 Bi at Bx level No cut on cosθ
CNO Sample Fit 1kT 5% 7 Li 100 pe/mev Ethresh = 0.4 MeV 210 Bi at Bx level cosθ < 0.4
1kT 5% 7 Li 100 pe/mev Ethresh = 0.4 MeV 210 Bi at Bx level No cut on cosθ CNO Sample Fit Single CNO Individual F/N/O Nev % uncert Nev % uncert 13N 15O 17F / CNO 7Be pep 210Bi 28677 9.3% 55734 4.0% 85801 3.9% 1389 6.1% 6.50E+05 0.3% 6.50E+05 0.3% 7.30E+04 1.9% 7.30E+04 1.9% 1.10E+05 3.4% 1.10E+05 3.9%
1kT 5% 7 Li 100 pe/mev Ethresh = 0.4 MeV 210 Bi at Bx level cosθ < 0.4 CNO Sample Fit Single CNO Individual F/N/O Nev % uncert Nev % uncert 13N 15O 17F / CNO 7Be pep 210Bi 656 11.8% 2594 7.8% 3315 7.7% 65 9.3% 2461 21.5% 2461 21.8% 4388 3.7% 4388 3.7% 76221 1.2% 76221 1.2%
CNO Comments The fit is surprisingly good! (Tests ongoing) Not very sensitive to resolution, size etc (beyond obvious scaling) Stats beat shape i.e. addition of CC does not improve fit uncertainty (2D fit clearly beats both!) But: cut on cosθ reduces correlations Safer when introducing systematics!
Thank you for your attention
Back-up slides
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape P ee! JHEP 0311:004 (2003) E υ!
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape Low energy: Phase-averaged vacuum oscillations P ee! JHEP 0311:004 (2003) E υ!
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape Low energy: Phase-averaged vacuum oscillations P ee! High energy: Matter-dominated resonant conversion JHEP 0311:004 (2003) E υ!
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape In these regimes, Pee depends only on θ12, Low energy: Phase-averaged vacuum oscillations P ee! High energy: Matter-dominated resonant conversion JHEP 0311:004 (2003) E υ!
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape In these regimes, Pee depends only on θ12, Not the mass splitting or neutrino-matter interaction Low energy: Phase-averaged vacuum oscillations P ee! High energy: Matter-dominated resonant conversion JHEP 0311:004 (2003) E υ!
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape In these regimes, Pee depends only on θ12, Not the mass splitting or neutrino-matter interaction Low energy: Phase-averaged vacuum oscillations P ee! High energy: Matter-dominated resonant conversion Probe transition region to confirm MSW & search for new physics! JHEP 0311:004 (2003) E υ!
Non-Standard Model Testing Light sterile neutrino PRD 83:113011 (2011) Non-standard MSW Dynamics PRD 83:101701 (2011) Non-Standard Models, Solar Neutrinos and Large θ13 PRD 88: 053010 (2013) Non-standard forward scattering Mass-varying neutrinos Long-range leptonic forces Non-standard solar model Results limited by experimental precision Best fit Pee for fermiondensity dependent MaVaN model Δχ 2 = 3.4 C.L. = 0.81 Phys. Rev. D 88 (2013) 053010
Non-Standard Model Testing Light sterile neutrino PRD 83:113011 (2011) Non-standard MSW Dynamics PRD 83:101701 (2011) Non-Standard Models, Solar Neutrinos and Large θ13 PRD 88: 053010 (2013) Non-standard forward scattering Mass-varying neutrinos Long-range leptonic forces Non-standard solar model Results limited by experimental precision No significant effects (< 2σ) Best fit Pee for fermiondensity dependent MaVaN model Δχ 2 = 3.4 C.L. = 0.81 Phys. Rev. D 88 (2013) 053010
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape (2) Understanding stellar formation: The metallicity of the Sun s core
Questions Beyond the SNP (1) Searching for new physics: νe survival probability shape (2) Understanding stellar formation: The metallicity of the Sun s core
Low Energy Neutrino Astronomy 50kT (30kT FV solar), 30% coverage Unprecedented statistics 3σ discovery potential for 0.5%- amplitude temporal fluctuations in 7 Be CC on 13 C J. Winter et al, TAUP 2011 Proc. http://www.e15.ph.tum.de/research_and_projects/lena/
(C) Metallicity Status Largest effect on pp-chain flux: ~17% reduction of 8 B (± 14% theory) Hard to distinguish Not characteristic
(C) Metallicity Status Largest effect on pp-chain flux: ~17% reduction of 8 B (± 14% theory) Hard to distinguish Not characteristic SNO s 8 B obeys the ambiguity principle: Ambiguity Principle: For any given experimental test of a hypothesis, Nature will always strive to return the most ambiguous answer possible --- J. R. Klein
(C) Metallicity Status Largest effect on pp-chain flux: ~17% reduction of 8 B (± 14% theory) Hard to distinguish Not characteristic SNO s 8 B obeys the ambiguity principle: Ambiguity Principle: For any given experimental test of a hypothesis, Nature will always strive to return the most ambiguous answer possible --- J. R. Klein CNO flux depends linearly on core metallicity Predictions differ by >30%
(C) Metallicity Status Largest effect on pp-chain flux: ~17% reduction of 8 B (± 14% theory) Hard to distinguish Not characteristic SNO s 8 B obeys the ambiguity principle: Ambiguity Principle: For any given experimental test of a hypothesis, Nature will always strive to return the most ambiguous answer possible --- J. R. Klein CNO flux depends linearly on core metallicity Predictions differ by >30% Borexino have the only direct limit: 2-3 * SSM prediction PRL 108, 051302 (2012)