Searching for Physics Beyond the Standard Model. IceCube Neutrino Observatory. with the. John Kelley for the IceCube Collaboration

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Searching for Physics Beyond the Standard Model with the IceCube Neutrino Observatory John Kelley for the IceCube Collaboration Wisconsin IceCube

1 Searching for Physics Beyond the Standard Model with the IceCube Neutrino Observatory John Kelley for the IceCube Collaboration Wisconsin IceCube Particle Astrophysics Center University of Wisconsin Madison, U.S.A. Beyond the Standard Model of Particle Physics July 16, 2012, Quy Nhon, Vietnam

2 IceCube from the Air IceCube South Pole Station control room skiway 16/07/2012 J. Kelley, BSM

3 The IceCube Detector AMANDA-II Array! (precursor to IceCube)! digital optical module (DOM) 16/07/2012 J. Kelley, BSM

4 Event Signatures Positions, times, and amplitudes of Cherenkov light deposition: neutrino direction + energy e CC + all flavor NC CC (+CR muons!) 16/07/2012 J. Kelley, BSM CC ( double-bang )

5 16/07/2012 J. Kelley, BSM

6 g E! / GeV Detector Performance y normalization E 2 flux of neutrinos as a ction. The black contours indicate the 90% n. Simulated tracks Simulated cascades Median Angular Resolution [ ] Southern Sky (" < 0 ) Northern Sky (" % 0 ) log E! / GeV angular resolution: ~1º le between neutrino and reconstructedmuon (verified with CR Moon shadow) at the final cut level in the up-going region ation. The median of the PSF versus energy hern skies (right). The improvement in the quality cuts. Fig. 3. Left: Offset between the reconstructed and the deposited logarithmi the reconstructed and the deposited logarithmic energy. The deviation from t saturation effects on the energy reconstruction. from the improved light-propagation model. In this case, the search for the minimum is reduced to a numerical root finding problem: ( ) 172 Continual time synchronization to 173 ~2 ns; ice calibration with in-situ flashers 174 IC40 E -2 spectrum energy resolution: ~35% μ energy estimation via de/dx angular resolution: ~30º 16/07/2012 J. Kelley, BSM ligh ene sim

7 Searches for New Physics with IceCube Need a neutrino source! Atmospheric neutrinos (CR+Earth s atmosphere) violation of Lorentz invariance? ev-scale sterile neutrinos? Neutrinos from dark matter annihilation WIMP signal from the Sun, Earth, or Galactic Center? Neutrinos from cosmic ray accelerators or CR+CMB may eventually be useful for new physics searches, but... first step is detection! 16/07/2012 J. Kelley, BSM

8 Atmospheric Neutrino Spectra s -1 sr -1 ] -2 [GeV cm 2! "! E conventional! µ conventional Frejus! µ Frejus! e SuperK! µ AMANDA! µ unfolding forward folding IceCube! µ unfolding forward folding ~200 atm. neutrinos / day in IceCube -6-7!e prompt! µ,! e neutrino point sources? diffuse HE flux? cosmogenic neutrinos? [GeV]) 16/07/2012 J. Kelley, BSM 2012! 8 log (E

9 Violation of Lorentz Invariance (VLI) Different limiting velocity eigenstates: VLI oscilations* VLI atmospheric ν µ survival probability maximal mixing, δc/c = -27 *see González-García, Halzen, and Maltoni, hep-ph/ /07/2012 J. Kelley, BSM

10 AMANDA VLI limits Abbasi et al., PRD 79, 2005 (2009) zenith angle number of OMs hit Data consistent with SM atmospheric neutrinos + O(1%) background δc/c < (90%CL) IceCube will improve by an order of magnitude 16/07/2012 J. Kelley, BSM 2012

Direction-dependent VLI Oscillations Standard Model Extension includes interaction coefficients that violate rotational invariance Vector Model : energy-independent directional VLI, a L +

11 Direction-dependent VLI Oscillations Standard Model Extension includes interaction coefficients that violate rotational invariance Vector Model : energy-independent directional VLI, a L + energy-dependent directional VLI, c L ( ( s) ( φ0) ( c) ( φ0) ) 2 Pν 1 sin L A sin RA A cos RA µ ν µ µτ µτ = µτ ˆ Y X TX X Y TY A = N a Ec N a Ec ( 2 ) ˆ ( 2 ) X X TX ( 2 ) ˆ Y Y TY ( 2 ) s L L L L µτ A = Nˆ a Ec N a Ec c L L L L ˆ XY, are unit vectors N for the neutrino's direction, and depend on RA Kostelecky and Mewes, PRD 70, Survival probability a c a c X L TX L X L TX L Y = a = L TY = c = 0 L Y = a = 0 L TY = c = L /07/2012 J. Kelley, BSM

12 IceCube Direction-dependent VLI limits Right ascension distribution consistent with atmospheric neutrino expectation Set upper limits on VLI coefficients based on power in Fourier modes IC40 atmospheric muon neutrino RA Phys. Rev. D 82, (20) a c X Y 23 L, al < 1.8 GeV ( ) TX TY 27 L, cl < syst. For energy-dependent effects: results 3-4 orders of magnitude improved over MINOS MINOS: a< 3 and c< Adamson, et. al, Phys. Rev. Lett.1, (2008) 32 bins in RA (using zenith 97 to 120 degrees) 16/07/2012 J. Kelley, BSM

Sterile Neutrinos No direct weak interactions Can mix with 3 active states Recent hints of an ev-scale sterile neutrino LSND and MiniBooNE antineutrino disappearance LSND MiniBooNE 0.6 0.7 0.8 0.

13 Sterile Neutrinos No direct weak interactions Can mix with 3 active states Recent hints of an ev-scale sterile neutrino LSND and MiniBooNE antineutrino disappearance LSND MiniBooNE ROVNO88_3S 18.2 m ROVNO88_2S 25.2 m ROVNO88_1S 18.2 m ROVNO88_2I 18.0 m ROVNO88_1I 18.0 m SRP-II 23.8 m SRP-I 18.2 m Krasnoyarsk-III 57.3 m Krasnoyarsk-II 92.3 m Krasnoyarsk-I 33.0 m ILL 8.76 m Goesgen-III 65.0 m Goesgen-II 46.0 m Goesgen-I 38.0 m Bugey m Bugey m Bugey-3/ m ROVNO m review: Abazajian et al., arxiv Reactor antineutrino anomaly 0.92X±0.01X± X±0.01X± X±0.01X± X±0.01X± X±0.01X± X±0.01X± X±0.01X± X±0.01X± X±0.18X± X±0.03X± X±0.06X± X±0.04X± X±0.02X± X±0.02X± X±0.11X± X±0.01X± X±0.00X± X±0.02X±0.03 Bugey-3/ m 0.93X±0.00X±0.03 " =881.5s n PDG20 Average 0.927X ± /07/2012 J. Kelley, BSM ! Measured /! Expected, NEW

Sterile MSW Resonance calculated muon antineutrino survival probability PRELIMINARY!#8/.

$') Events/bin/year 4500 4000 3500 3000 2500 2000 1500 00 predicted DeepCore rates thick:

5 $ %3 ev 2 15-30 GeV 30-60 GeV 60-120 GeV 500 2 2 #m 43= 1 ev 2 2 #m 43= 1 ev sin 2 " = 0.

z Effects on oscillations observable in both TeV and sub-tev range With control of

14 Sterile MSW Resonance calculated muon antineutrino survival probability PRELIMINARY!#8/.1) %./(#(.$') Events/bin/year predicted DeepCore rates thick: with sterile; thin; without 2 %3 2 #m 32 = $ ev #m 32 2 = % 2.5 $ %3 ev GeV GeV GeV #m 43= 1 ev 2 2 #m 43= 1 ev sin 2 " = 0.04 sin 2 " = cos! z cos! z Effects on oscillations observable in both TeV and sub-tev range With control of systematics: IceCube will conclusively test this explanation of LSND/MiniBooNE! Choubey, arxiv: /07/2012 J. Kelley, BSM 2012 Razzaque and Smirnov, arxiv: Esmaili, Halzen, and Peres, arxiv:

Indirect Detection of Dark Matter χ velocity

accumulation near Galactic Center, Earth core,

15 Indirect Detection of Dark Matter χ velocity distribupon ρ χ ν interacpons σ scaq Γ capture Γ annihilapon Sun ν µ annihilapon channels c c, b b, t t, τ ±,W ±,Z,H ±,H 0 µ Similar accumulation near Galactic Center, Earth core, and dwarf spheroidal galaxies 16/07/2012 J. Kelley, BSM

16 Limits on Scattering Cross Section Phys. Rev. D 85, (2012) no excess of high-energy neutrinos from Sun (AMANDA data) MSSM branching ratios WIMP annihilation limit DM density; capture rates; equilibrium SD cross section limit 16/07/2012 J. Kelley, BSM

Galactic Center and halo limits 17 Probes velocity-averaged self annihilation crosssection Galactic halo analysis: IC22 up-going tracks Phys.Rev.

17 Galactic Center and halo limits 17 Probes velocity-averaged self annihilation crosssection Galactic halo analysis: IC22 up-going tracks Phys.Rev. D84 (2011) Galactic Center analysis: IC40 downgoing tracks compare with offsource region <σ A v> [cm 3 s 1 ] <σ A v> [cm 3 s 1 ] unitarity bound natural scale unitarity bound natural scale m χ [GeV] IC40 m χ [GeV] bb, IC22 WW, IC22 µ µ, IC22 ν ν, IC22 µ µ, Fermi bb, Fermi WW, Fermi bb, this work WW, this work µ µ, this work ν ν, this work ν ν, IC22 µ µ, Fermi bb, Fermi WW, Fermi bb, IC22 WW, IC22 µ µ, IC22 ν ν, IC22 16/07/2012 J. Kelley, BSM

18 WIMP Searches with DeepCore Densely instrumented core of IceCube (30 MTon) Can use surrounding detector as a veto Allows efficient searches above the horizon (Galactic Center) Lower energy threshold (to ~ GeV): can probe lower WIMP masses Deep Core 16/07/2012 J. Kelley, BSM

19 GZK Effect Suppression ( cutoff ) of high-energy cosmic rays due to interaction with CMB photons (Greisen-Zatsepin- Kuzmin) ] 2 ev sr -1 yr Cosmic ray energy spectrum log (E/eV) ! sys (E)=22% J(E) [km -2 Threshold ~ 6 19 ev 3 E 37 HiRes Auger power laws power laws + smooth function Suppression observed in cosmic-ray flux consistent with GZK explanation Energy [ev] Auger Collaboration, Phys. Lett. B685 (20) /07/2012 J. Kelley, BSM

20 The Neutrino Connection GZK process also produces UHE neutrinos! GZK neutrino flux models Nuclei will tend to photodisintegrate first (reduced flux) range of iron best-fit proton New source for SM tests cosmological baselines probed energies ~ ev Anchordoqui et al., PRD (2007) 16/07/2012 J. Kelley, BSM

21 Possible New Physics with GZK neutrinos VLI-induced neutrino splitting modification of spectral shape see e.g. Mattingly, Liberati et al., arxiv: Neutrino / dark energy coupling leading to VLI / CPTV flavor ratio via angular dependence see e.g. Ando et al., arxiv: Cross section enhancement from large extra dimensions detection via angular dependence of event rate see e.g. Connolly, Thorne, and Waters, arxiv: /07/2012 J. Kelley, BSM

22 IceCube EHE Neutrino Search May 20 May 2012 (672.7 days livetime) Primary selection criterion: high NPE Track reconstruction quality removes corner-clippers, coincident CR events Background MC Experimental Data (%) Signal MC / '5$ 67899:*,&#(,;#$ <$ 876$=$>6:*,&#(,;#$.$ 16/07/2012 J. Kelley, BSM see also first IceCube upper limits: Phys. Rev. D 82, (20)

23 Neutrino Candidates Two events in unblinded data sample (background estimation: 0.14 events; 2.36 ) 3 Jan 2012: 96k PE, 312 DOMs 9 Aug. 2011: 70k PE, 354 DOMs 16/07/2012 J. Kelley, BSM

24 Event Brightness (atm. + conventional atm. No indication that they are cosmic-ray muons ~PeV energy deposit in detector (would imply 1- PeV neutrinos) Analysis of energy, directions ongoing 16/07/2012 J. Kelley, BSM

25 Conclusions and Outlook IceCube is completed and is operating well Atmospheric neutrinos: our high-statistics source limits on violation of Lorentz invariance searches for ev-scale sterile neutrino in progress WIMP searches MSSM-constraining limits on spin-dependent scattering cross section (via Sun) competitive limits on self-annihilation cross section (via GC, halo) extending to dwarf spheroidal galaxies EHE searches for the cosmogenic neutrinos no significant excess so far may eventually provide the next test beam 16/07/2012 J. Kelley, BSM

Measuring the neutrino mass hierarchy with atmospheric neutrinos in IceCube(-Gen2)

Measuring the neutrino mass hierarchy with atmospheric neutrinos in IceCube(-Gen2) Beyond the Standard Model with Neutrinos and Nuclear Physics Solvay Workshop November 30, 2017 Darren R Grant The atmospheric