Neutrinos from the Sun and other sources: Results from the Borexino experiment

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1 Neutrinos from the Sun and other sources: Results from the Borexino experiment Marianne Göger-Neff

2 Neutrinos from the Sun and other sources: Results from the Borexino experiment Motivation: solar neutrinos Borexino: detector, signal and background Solar neutrino results: 7Be 8B pep and CNO Geoneutrinos SOX: Short distance neutrino Oscillations with BoreXino

3 Nuclear reactions in the solar core pp chain ~ 99% of energy CNO cycle <1% of energy poorly known not directly measured yet 5 ν species 3 ν species

4 Expected solar neutrino spectrum on Earth solar neutrino fluxes on Earth are predicted using the Standard Solar Model Borexino SuperK, SNO Realtime water Cerenkov-experiments (SNO, SuperK) measure < 10-4 of the total solar neutrino flux Borexino measures > 10% of the total solar neutrino flux 99% of solar neutrino flux is < 1 MeV Serenelli et al. 2011

5 Source The solar metallicity problem Recent improvements in SSM (>2004) suggest lower metallicity Z But: low Z models are in conflict with helioseismology (R CZ, Y surf ) Can solar neutrino measurements decide? Neutrino Flux [cm -2 s -1 ] SSM-GS98 high Z model Neutrino Flux [cm -2 s -1 ] SSM-AGS09 low Z model Difference [%] pp 5.98(1±0.006) (1±0.006) pep 1.44(1±0.012) (1±0.012) Be 5.00(1±0.07) (1±0.07) B 5.58(1±0.13) (1±0.13) N 2.96(1±0.15) (1±0.15) O 2.23(1±0.16) (1±0.16) F 5.52(1±0.18) (1±0.16) CNO total 5.24 x x

6 Main goals of Borexino real-time spectroscopy of low energy solar neutrinos: 7 Be, pep, CNO, pp (99% of solar neutrino flux is < 1 MeV) neutrino physics: test transition region MSW to vacuum oscillations (1 4 MeV) precision measurement θ 12, Δm 2 21 search for Non-Standard Interactions astrophysics: determination of CNO: important for heavy stars high/ low Z SSM test luminosity constraint L ν = L other: geoneutrinos reactor neutrinos sterile neutrinos Matter-enhanced region

7 Borexino: detection principle elastic scattering of neutrinos on electrons in organic liquid scintillator detection via scintillation light: + low energy threshold (< 0.2 MeV) + good energy & position resolution + pulse shape discrimination but: no directionality no distinction of ν induced events from other β events extreme radiopurity of the scintillator required shielding, material selection, purification

8 Milano Napoli Heidelberg Hamburg Mainz Gran Sasso München Genova TU Dresden Perugia Borexino Collaboration Virginia Tech Houston UMass Amherst Paris St. Petersburg JINR Dubna Los Angeles Princeton Jagiellonian Kraków Moscow Kurchatov Moscow

9 Borexino: Detector Location INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ), Italy overburden: ~3500 m.w.e Borexino Detector and Plants

10 The Borexino Detector Target: 280 t PC + PPO (1.5 g/l) in 0.1 mm nylon vessel (8.5m Ø) Fiducial volume: 100 t (6 m Ø) Buffer: 900 t PC + DMP (5g/l) in stainless steel sphere (13.7m Ø) Target: 280t PC+PPO Rn diffusion barrier (11m Ø) PMTs (1800 with concentrators) Muon veto: PMTs 2200 t H 2 O in steel tank (18m Ø)

11 taking data since May 2007 A. Ianni LNGS, March 5th 2008

12 Borexino Expected Solar ν Spectrum Be-7 pep pp CNO Spectrum with irreducible backgrounds ( 10 C, 11 C..)

13 Data reduction raw data muons subtracted + fiducial volume cut 210 Po 11 C α s subtracted detection threshold is 25 pe (~ 50 kev) total rate above threshold ~ 30 Hz

14 Precision measurement of 7 Be neutrino rate 740 live days Phys. Rev. Lett. 107, (2011) MC Fit Analytical Fit spectral fit including the following signal + intrinsic background components 7 Be, 85 Kr, 14 C, 11 C 210 Bi (very similar to CNO in this limited energy region) pp, pep, 8 B, and CNO neutrinos fixed at SSM-LMA value fit with and without statistical subtraction of 210 Po events, based on a/b pulse shape discrimination. two independent ways (MC based and analytical fit) were applied

15 Precision measurement of 7 Be neutrino rate 740 live days Phys. Rev. Lett. 107, (2011) MC Fit Analytical Fit Systematics Result on 7 Be neutrino rate: stat 1.5 c / d100 t combined error: 4.6% no oscillation excluded at 5 σ

16 Implications of the 7 Be measurement electron equivalent flux (862 kev line): Φ Be =(2.78 ± 0.13) x 10 9 cm -2 s -1 assuming MSW-LMA: f 7Be = φ/φ SSM = 0.97± 0.09 including all solar experiments + luminosity constraint: f pp = ± 0.01 f CNO < 1.7% (95 % C.L.) P ee = 0.51 ± 862 kev no power to resolve low/high metallicity problem

17 Absence of day-night asymmetry for 7 Be ν MSW: a possible regeneration of electron neutrinos in the Earth matter during night effect depends on the oscillation parameters and on energy solar neutrino data WITHOUT Borexino LMA Phys. Lett. B 707, 22-26, 2012 solar neutrino data WITH Borexino LMA LOW A DN = ± 0.012(stat) ± 0.007(syst) in agreement with MSW-LMA LOW region excluded at > 8.5 s with solar neutrinos only for the first time without the use of antineutrinos (KamLAND)

18 Annual modulation of the 7 Be-ν signal Enlarged, dynamic FV: mean ton ( 7 Be flux measur ton) ( t) cos T t max T = 1 year min 6.8% Spectral fit in sub-periods not possible: too large stat. errors! Rate analysis: Select a proper energy region (optimize signal/bgr), group data in time bins and search for a periodical component Reconstructed vessel shape = f (time), 1 week bins Based on 210 Bi on the vessel

19 Gatti(pulse shape) Annual modulation of the 7 Be-ν signal Detector response is very stable (energy, position reco, pulse shape id.) Problem: background rate ( 210 Bi) is not stable in time! 210 Po(a) b - like Energy (p.e.) R 210 Bi R 0 e Bi t Hard Gatti (pulse shape cut): removal of the events above the red line Counts in an energy region dominated by 210 Bi as a function of time 19

20 Annual modulation of the 7 Be-ν signal different analysis methods (consistent results) Fit of the rate (+ bckgr) vs time Data counts in 60 days bins Charge p.e. R R 0 e Bi t 2 R 1 2 cos T arxiv: Phase I Lomb Scargle analysis SPD (1 year) = 7.96

21 Low threshold measurement of the 8 B solar ν Phys. Rev. D82 (2010) Borexino energy spectrum above 2.8 MeV: 488 live days threshold of 2.8 MeV due to 208 Tl ( 2.6 MeV) raw data µ subtracted FV cut cosmogenic isotopes rejected 208 Tl Expected count rate due to 8 B neutrinos above 2.8 MeV 0.26±0.03 c/d/100 tons Signal/Backgr.(>2.8 MeV): ~ 1/6000

22 Low threshold measurement of the 8 B solar ν Phys. Rev. D82 (2010) Rate [c/d/100 t] Φ ES exp [10 6 cm 2 s 1 ] MeV MeV 0.22±0.04± ±0.02± ±0.4 ± ±0.4 ±0.2 Φ ES exp/φ ES th 0.88± ± Be and 8 B flux measured with the same detector Borexino 8 B flux above 5 MeV agrees with existing data (SNO, SuperK) Neutrino oscillation is confirmed at 4.2 σ

23 The first pep ν measurement Phys. Rev. Lett. 108 (2012) Motivation: test MSW-LMA solution pep ν flux more precisely known than 7 Be flux (1.2%) also monoenergetic line flux 10 x lower than 7 Be 11 C Expected pep interaction rate: 2-3 cpd/100t 210 Bi pep Main background: 11 C, 210 Bi, external γ CNO 210 Bi and CNO: very similar spectral shape Multivariate analysis: combined fit of energy spectra radial distribution of the events pulse shape parameter

24 11 C reduction: Threefold coincidence (TFC) m + 12 C m + 11 C + n 11 C t ~ 30 min + p d + g in Borexino: ~ 4300 muons/day > 250 neutrons /day ~ C /day Interaction point and 11C production point muon position of the n capture 11 B + e + + n e cylindrical cut around muon + spherical cut around γ removes 90% of 11 C residual exposure 48.5%

25 pep and CNO neutrinos: results Phys. Rev. Lett. 108 (2012) pep neutrinos: Rate: 3.1 ± 0.6(stat) ± 0.3(sys) cpd/100 t Φpep = (1.6 ± 0.3) x 10 8 cm -2 s -1 No oscillations excluded at 97% C.L. Absence of pep solar ν excluded at 98% CNO neutrinos: only limits, strong correlation with 210 Bi CNO limit obtained assuming SSM CNO rate < 7.1 cpd/100 t (95% C.L.) ΦCNO < cm -2 s -1 (95% C.L.) ΦBx < 1.5 ΦSSM the strongest limit to date not sufficient to resolve metallicity problem

26 Physics implication of the Borexino results MSW-LMA confirmed ( 7 Be,pep and 8 B measurement) Combined analysis Borexino&solar Before the Borexino results LOW excluded (solar only) by day-night-asymmetry

27 Borexino Phase 1 and Phase 2 Solar n Phase 1 Data taking and calibration Scintillator purification Solar n Phase 2 May 2007 May 2010 Aug Oct Phase 1 Results First solar 7 Be-n measurement Absence of 7 Be-n day-night asymmetry Low-threshold 8 B-n First pep-n detection Best upper limit on CNO-n First geo-n observation at > 4s Limits on rare processes Neutrons and other cosmogenics Evidence of 7 Be-n seasonal modulation Program for Phase 2 > 3 years of undisturbed data taking extensive calibration at the end improvement of 7 Be (3%) measurement of CNO n precision measurement of pep and low energy 8 B direct measurement of pp (15%) search for sterile n with an artificial n source ( 51 Cr, 144 Ce)

28 Work in progress: pp neutrino flux first direct detection of pp neutrinos need to evaluate 14 C background and pile-up, energy resolution at low energies 14 C+pileup 210 Po pp 7 Be 210 Bi pep+ 8 B CNO 85 Kr expected statistical precision ~ 15%

29 Geoneutrinos in Borexino Geoneutrinos = antineutrinos from the decay of 238 U, 232 Th, 40 K in the Earth Main goal: determine the contribution of the radiogenic heat to the total surface heat flux input and test for many geophysical/geochemical models of the Earth Further goals: tests and discrimination among geological models, study of the mantle homogeneity (several expts), Detection via inverse beta decay (IBD) p n e E n >1.8 MeV prompt signal e+: energy loss + annihilation delayed signal n capture after thermalization 2.2 g

30 Geoneutrinos in Borexino New result: G. Bellini et al. Phys. Lett. B 722 (2013) 295 Exposure: ( ) ton-year after cuts Event selection E prompt > 480 p.e., E delayed [860,1300]p.e., R < 4 m (25 cm distance from vessel) R (prompt-delayed) < 1m, Dt (prompt-delayed): ms, Gatti < ( b-like ) Geo 46 golden coincidences Reactor MC defined efficiency: 0.84 ± 0.01 Background not due to reactors is < 1ev

31 Geoneutrinos in Borexino: result Phys. Lett. B 722 (2013) 295 Unbinned maximal likelihood fit with unconstrained geo and reactor component; N reactor = in agreement with expectation of 33.3 ± 2.4 events (with osc.) Fixed Th/U mass ratio to chondritic value of 3.9: N geo = 14.3 ± 4.4 events S geo = 38.8 ± 12.0 TNU Th/U ratio free in the fit: S( 238 U) = 26.5 ± 19.5 TNU S( 232 T) = 10.6 ± 12.7 TNU compatible with chondritic value * 1 TNU = 1 event / target protons / year

32 SOX: Short distance Oscillations with BoreXino calibration with an artificial neutrino source was planned in Borexino from the beginning of the project ( source pit below the detector) 51 Cr source successfully implemented by Gallex and SAGE Several experimental anomalies (Gallium, Reactor, LSND) difficult to accomodate in a simple 3-flavor scenario existence of a fourth (= sterile) neutrino?

33 SOX: Short distance Oscillations with BoreXino calibration with an artificial neutrino source was planned in Borexino from the beginning of the project ( source pit below the detector) 51 Cr source successfully implemented by Gallex and SAGE Several experimental anomalies (Gallium, Reactor, LSND) difficult to accomodate in a simple 3-flavor scenario existence of a fourth (= sterile) neutrino? short baseline experiment with an artificial neutrino-/ antineutrino-source: search for sterile neutrinos or other short distance effects on Pee measurement of q W at low energy (~ 1 MeV) measurement of neutrino magnetic moment measurement of g V /g A at low energy

34 SOX: Short distance Oscillations with BoreXino 3 phases planned: 144 Ce SOX-C SOX-A: external 51 Cr- source SOX-B: external 144 Ce-source SOX-C: internal 144 Ce-source 1m 51 Cr SOX-A 144 Ce SOX-B source pit below Borexino detector

35 SOX-A: Cr-51 source Electron capture decay: monoenergetic electron neutrinos activity: 10 MCi source in external pit (8.25m distance from center) detection via ν-e-scattering T 1/2 = 27.7 d

36 SOX-A: Cr-51 source Expected sensitivity: activity: 10 MCi source in 8.25m distance from center detection via ν-e-scattering 3 months of data taking 1 % error on source activity 1 % error on FV T 1/2 = 27.7 d

37 Technology: 51 Cr source 36 kg of 50 Cr enriched at 38 % (old Gallex source) to be irradiated at Oak Ridge reactor with high neutron flux and delivered to Gran-Sasso 190 W/MCi from gammas => cooling ~ few msv/h on the surface => shielding precise determination of source activity: calorimetry gamma spectroscopy measurement of 51 V fraction 51 Cr W Gallex 1994

38 SOX-B: Ce144-Pr144 source (external) antineutrino source detection via inverse beta decay - practically background-free activity: 100 kci distance: 8.25 m from center 1.5 years data taking T 1/2 = 285 d

39 Technology: 144 Ce source 144 Ce fission product extraction from spent nuclear fuel at Mayak reprocessing facility 1 ton of SNF => 2.8 kg of Ce with 22 g of 144 Ce (= 80 kci) 800 W / 100 kci => cooling background due to 2.2 MeV γ reduction needed (W shielding) with 16 cm W: 5.2 µsv/h determine activity to 1.5% through calorimetry

40 Conclusions Phase 1 of the Borexino experiment successfully concluded First detection and 5% measurement of solar 7 Be neutrinos 8 B-ν at low energy (>3 MeV), 7 Be-ν day-night First detection of pep solar neutrinos, best limit on CNO Phase 2 is ongoing after successful scintillator purification rich program on solar neutrino physics: probe MSW through 8 B at low energy, pep and more precise 7 Be detect pp in real time constrain upper limit on CNO, probe solar metallicity SOX project (phase A/B): external 51 Cr/ 144 Ce source measurement planned for 2015/2016 prove/exclude reactor anomaly

41 Borexino References Solar neutrino results 7 Be evidence: PhysLett B (2008) 7 Be at 10% + f pp /f CNO : PhysRevLett 101, (2008) Measurement of the solar 8B neutrino rate with a liquid scintillator target and 3MeV energy threshold in the Borexino detector, PRD 82 (2010) Precision measurement of the 7Be solar neutrino interaction rate in Borexino, Phys. Rev. Lett. 107, , 2012 Absence of day-night asymmetry of 862 keb 7Be solar neutrinos in Borexino and MSW oscillation parameters, Phys. Lett. B 707, 22-26, 2012 First evidence of pep solar neutrinos by direct detection in Borexino, Phys. Rev. Lett. 108, , 2012 Other physics: Observation of Geo-Neutrinos, Phys. Lett. B687, , 2012 Cosmic muon flux and annual modulation in Borexino, JINST 1205,015, 2012 Measurement of CNGS muon neutrino speed with Borexino, Phys Lett B716, 401, 2012 Search of rare processes Anti-neutrinos from unknown sources, PLB 696 (2011) Limits on Pauli forbidden transitions on 12C, PRC 81 (2010) Search for solar axions from p(d,3he)a, PRD 85 (2012) more interesting results to come

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