Status of Neutrino Astronomy (Mini-review on neutrino telesopes) Alexander Kappes EPS 2011 21. July 2011, Grenoble, Frane
Outline Introdution Neutrino telesopes Current status - Sensitivities of neutrino telesopes - Galati and extragalati soures - Dark Matter - Beyond neutrino physis: osmi-ray anisotropies 2
Neutrino fluxes sr -1 ] s -1 m -2-1 flux [MeV 24 20 15 5 1-5 - -15-20 -25-30 osmi ν bakground observed expeted solar ν s geo anti-ν s reprodued from Xing, Nusky 2011 supernova ν burst (SN 1987A) ν s from AGNs reator anti-ν s supernova reli ν bakground atmospheri ν s GZK ν s -7-5 -3-1 3 5 E! 7 [ev] 9 11 13 15 17 19 3
Neutrino fluxes sr -1 ] s -1 m -2-1 flux [MeV 24 20 15 5 1-5 - -15-20 -25-30 ULE ν s osmi ν bakground observed expeted solar ν s geo anti-ν s reprodued from Xing, Nusky 2011 supernova ν burst (SN 1987A) ν s from AGNs HE ν s reator anti-ν s supernova reli ν bakground atmospheri ν s GZK ν s -7-5 -3-1 3 5 E! 7 [ev] 9 11 13 15 17 19 3
Why neutrino astronomy? Neutrinos point bak to the soure Neutrinos travel osmologial distanes Neutrinos esape also optial dense soures Neutrinos are a smoking-gun evidene for hadron aeleration p + p(γ) π ± + X µ + νµ e + νµ + νe Neutrinos provide omplementary information to gamma-ray photons and protons 4
Detetion priniple muon µ 43 asade ν µ shower Time & position of hits PMT amplitudes νµ nulear reation µ (~ ν) diretion Energy 5
Neutrino signatures: Trak-like: Soure: νµ CC interation Good angular resolution (< 1 ) Sensitive instrumented volume Casade-like: Soure: νe, νμ, ντ NC + νe CC interation Good energy resolution (few %) Bad angular resolution ( > O( ) ) Sensitive instrumented volume muon (IeCube) Composites: Soure: ντ CC + νµ CC inside instrumented volume Challenging to reonstrut asade (IeCube) 6
Bakgrounds Muons deteted per year atmospheri* µ 7 atmospheri** ν µ 8 4 p osmi rays osmi ν µ ~ * 2000 per seond ** 1 every 6 minutes µ νµ bakground osmi νµ νµ µ atmosphere p 7
Sky overage Visibility South Pole (IeCube) 0% 0% Visibility Mediterranean (Antares) > 75% 25% 75% < 25% TeV gamma-ray soures Galati extragalati 8
Neutrino Telesope Projets ANTARES NEMO NESTOR Baikal IeCube 9
Sensitivities to point soures 90% CL sensitivity for E -2 spetrum SuperK ANTARES talk D. Dorni Disovery region AMANDA IeCube 40 IeCube 80 (predited IC40) IeCube 40+59 KM3NeT (predited) talk A. Tsirigotis fator 00 in 15 years plenary talk T. Montaruli
Arbitrary Saling (E 2 dϕ/de) Sensitivities to point soures 90% CL sensitivity for Differential E -2 spetrum Sensitivity IeCube δ = - 8 δ = - 30 δ = +60 δ = - 60 δ = +30 SuperK ANTARES talk D. Dorni Upgoing (Northern sky) TeV PeV Disovery region δ = +6 AMANDA IeCube 40 Downgoing (Southern sky) PeV EeV IeCube 80 (predited IC40) IeCube 40+59 KM3NeT (predited) IC40 talk A. Tsirigotis fator 00 in 15 years plenary talk T. Montaruli
Sensitivities to diffuse neutrino flux atm. neutrinos WB bound AMANDA-II ANTARES (2007-09) IeCube 40 WB GRBs 11
Galati soures Energy Galati CRs: ~ -12 erg/m 3 injetion power: ~ -26 erg/(m 3 s) (esape time CRs ~3 6 yr) Cosmi ray spetrum SNe provide energy and environment - % of 51 erg/sn every 30 yr (Baade and Zwiky 1934) - shok aeleration (Fermi 1949) 12
Galati soures Cosmi rays must produe pioni γ-rays in interations with hydrogen in Galati plane Cygnus region seen by Milagro p + p π 0 + π + + π - γ γ νμ μ + μ - νμ μ + νμ νe e +... translation of γ into ν fluxes Best environments: star forming regions Staking of 6 Milagro SNRs (Abbasi et al. 2011): model sensitivity p-value upper limit 3 events 2.9 model 2% (posteriori) 7.2 model model Halzen, AK, O Murhadha (2008) 13
Extragalati soures Soure requirements: - aeleration up to 20 ev - produe energy in osmi rays (~3-19 erg/m 3 ~8 44 erg Mp -3 yr -1 ) Cosmi ray spetrum Best (only?) andidates: AGNs and GRBs Ative Galati Nulei (AGNs): - Auger: soures revealed? weak AGN orrelation dereased sine 2008 in onflit with omposition measurements - neutrino-flux preditions diffiult Auger orrelation with VCV atalogue Auger, ApJ 34, 314 (20) 14
Extragalati soures: GRBs Gamma-Ray Bursts (GRBs): - provide energy and environment to explain extragalati osmi rays (~ 52 erg 0/Gp 3 ) osmi rays Halzen, Nusky 2011 Soure model (Ahlers et al. 2011): - aeleration in internal shoks (fireball model) - ollide aelerated protons with photons: p + γ n + π + and p + π 0 osmi rays from n deay photons and neutrinos Halzen, Nusky 2011 - observed osmi rays from n deay - Neutrino and photon flux from pion deay IeCube hallenges GRBs as major soures of extragalati osmi rays from π 0 after asading in CMB π + neutrinos 15
Dark Matter (WIMPs) Gravitational apture of WIMPs in the Sun followed by self annihilation Neutrino rate only depends on sattering ross setion (equilibrium between apture and annihilation) Sensitive to spin-dependent ross setion Expeted ν energies < 1 TeV ν,ν WIMP 16
WIMP sensitivities Spin-independent σsat well onstrained by diret searhes Solar dark matter searhes probe spin-dependent σsat DeepCore will probe large region of allowed phase spae talks F. Lee (low energy), H. Melbeus (Kaluza-Klein), G. Lambard (Antares) Neutralino WIMP D. Cowen, Nusky 2011 17
WIMP sensitivities Spin-independent σsat well onstrained by diret searhes Kaluza-Klein Neutralino WIMP (IC 22) D. Cowen, Abbasi Nusky et al., 20 2011 Solar dark matter searhes probe spin-dependent σsat DeepCore will probe large region of allowed phase spae talks F. Lee (low energy), H. Melbeus (Kaluza-Klein), G. Lambard (Antares) 17
Neutrino telesope physis flaring/periodi soures follow-up programs supernovae (MeV ν s) neutrino osillation osmi ray anisotropy Lorentz violation ~20σ without osillations with osillations 18
Cosmi-ray anisotropy Desiati, Nusky 2011 equatorial oordinates TeV IeCube-59 relative intensity Abbasi et al., APJL 718, L194 (20) Gyroradius < 1 p in µg Galati B-field Closest soures ~0 p osmi rays should not point! 19
Cosmi-ray anisotropy Desiati, Nusky 2011 equatorial oordinates Tibet-III 5 TeV TeV IeCube-59 relative intensity Abbasi et al., APJL 718, L194 (20) Gyroradius < 1 p in µg Galati B-field Closest soures ~0 p osmi rays should not point! 19
Cosmi-ray anisotropy relative intensity equatorial oordinates preliminary Desiati, Nusky 2011 360 0 no energy seletion -90 energy 360 0 20 TeV -90 360 0 400 TeV -90 20
Summary Full-sky overage with ompleted neutrino telesopes - IeCube sans northern sky with unsurpassed sensitivity - Antares observes interesting Galati enter region...... but KM3NeT in Northern hemisphere badly needed Analysis results so far: - Searhes for osmi neutrinos with negative results - IeCube limits hallenge GRBs as major soures of extragalati osmi rays - Exiting physis beyond neutrino astronomy Outlook: - IeCube enters disovery region for Galati soures - Upoming years will be ritial for neutrino astronomy 21