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Potential Neutrino Point Sources for KM3NeT Rezo Shanidze University of Erlangen

Potential Neutrino Point Sources for KM3NeT Rezo Shanidze University of Erlangen. WP2 (. ) Meeting. CPPM, Marseille, 24-25/10/2006. Introduction. Potential neutrino point sources studied in Erlangen: Galactic sources (H.E.S.S. g -sources): A. Kappes and Ch. Stegmann

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Potential Neutrino Point Sources for KM3NeT Rezo Shanidze University of Erlangen

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  1. Potential Neutrino Point Sources forKM3NeTRezo ShanidzeUniversity of Erlangen WP2 ( ) Meeting CPPM, Marseille, 24-25/10/2006

  2. Introduction Potential neutrino point sources studied in Erlangen: • Galactic sources (H.E.S.S. g -sources): A. Kappes and Ch. Stegmann A. Kappes, J.Hilton, C.Stegmann, F.Aharonian, astro-ph/0607286 • Extragalactic transient sources: Gamma Ray Burst (GRB): M. Naumann-Godó, ANTARES-PHYS-2005-005 • Calculation of high energy n -fluxes from HESS sources (FGal(En,Wn)) andGRBs(FExt.Gal(En,Wn,tn) )andevent rates for KM3NeT CPPM, Marseille, 25/10/2006

  3. Sources of High Energy n and g CR interactions with protons(photons): pp(pg)gp , po , … • pgmnmgenmnmne poggg hadron decays are producing fluxes of high energy n and g: ∫ En F(En) dEn eT ∫EgF(Eg) dEg e T– source transparency ( eT1 ) • (For VHE g from ICSgeT=0 ) neutrinos Identification of CR acceleration sites g detection high energy n flux (or po reconstruction )

  4. Is it Possible to Reconstruct po ? Not on Earth ! VHE photons from poggg: minimal angle: Qgg > Qmin ~ mp/Ep for Ep ~ 1 PeV, Qmin ~ 10-7, Source at L=10 kpc: g detected in ACT (H.E.S.S.,MAGIC) Second g from po: • ~ outside of solar system neutrinos from p decay: no minimal angle CPPM, Marseille, 25/10/2006

  5. H.E.S.S. Sources of VHE g Catalog of H.E.S.S. sources: www.mpi-hd.mpg.de/hfm/HESS/ > 30 sources of VHE g Selection of Galactic sources, calculation of corresponding nflux: A.Kappes et al., astro-ph/0607286 27 Galactic sources: - 12 PWN - 6 SNRs - 3 XRB - 6 Unidentified All sources are considered as potential CR accelerators (example for PWN: W.Bednarek, astro-ph/0610307) Aharonian et al., (HESS Collaboration), Astoph. J. 636(2006), asto-ph/0510397

  6.  Point Sources for KM3NeT Point sources: DQp  DQR RX J1713 signal ANTARES Neutrino telescope: Source size (degrees) 0.2° forE > 10TeV H.E.S.S. : DQR0.1 o

  7. From H.E.S.S. Data to Fn(En) If g VHE g are produced from po gggin pp interactions ( pp gpo+X ) No significant contribution: 1. of non hadronic processes 2. g-ray absorption within the source 3. pg interaction No interaction and energy loss 4. of p+ and p - before decay 5. of m decay Other processes: 6. NN considered in same way as pp 7. Full mixing due to oscillations: ne:nm:nt = 1:1:1 H.E.S.S sources : ~ kgE-G x (cutoff) H.E.S.Ssources <G> ~ 2.1 Power index (G)

  8. Expected Fn(En) from H.E.S.S Relation between: CR (p)  hadron (p)  photon and lepton (g,n) energy spectrum first approximation: CR(p), p, n/g ~ similar E-a Galactic CR(p): Ep < ~ 106÷7 GeV, g cut-off in n/g spectra S.R.Kelner, F.Aharonian, V.Bugayov, et al., PRD 47(2006),034018  new parameterization • CR protons: Fp(Ep)= kp E-a exp(-Ep/ep) dN/dEg/n = Fn/g(En/g) = k E-G exp(-(E/e)½ ) kn (0.71-0.16 a) kg GnGga-0.1 en 0.59 egep/40

  9. Neutrino Energy Spectrum Example: neutrino spectra for 2 sources: RX J1713.7-3946 and Vela X A.Kappes et al., astro-ph/0607286 1serror bands include systematic errors (20% norm., 10% index & cut-of )

  10. Expected Event Rates Event rates in neutrino telescope(KM3NeT ) Nn= T ∫F(En,W) Aeff(En,W,) dEn dWn Integration: Emin(1 TeV) ÷Emax(100 TeV) T - time source is below horizon, T = eV (d) Ty eV (d) - Observation efficiency, d – source declination , Aeff– effective area of KM3NeT ( talk by Sebastian Kuch) Event rates from atm. neutrino flux: Volkova parameterization (Volkova, Sov.J.Nucl.Phys., 1980, 31(6), 784

  11. H.E.S.S. sources from ANTARES NEMO and NESTOR ANTARES NEMO/NESTOR Source Dec. (o)

  12. Event Rates from H.E.S.S. Sources Muon neutrino events as a function of neutrino energy detected in KM3NeT (5 y) for 2 sources: RX J1713.7-3946 and Vela X A.Kappes et al., astro-ph/0607286

  13. Expected Neutrino Events from H.E.S.S. Sources Sources with observed cut-off KM3NeT (1 km3, 5 years) E > 1 TeV E > 5 TeV Type Ø [o] Src Bkg Src Bkg • Vela X PWN 0.8 9 – 23 23 5 – 15 4.6 • RX J1713.7–3946 SNR 1.3 7 – 14 41 2.6 – 6.7 8.2 • RX J0852.0–4622 SNR 2.0 7 – 15 104 1.9 – 6.5 21 • HESS J1825–137 PWN 0.3 5 – 10 9.3 2.2 – 5.2 1.8 • Crab Nebula PWN <0.1 4.0 – 7.6 5.2 1.1 – 2.7 1.1 • HESS J1303–631 NCP 0.3 0.8 – 2.3 11 0.1 – 0.5 2.1 • LS 5039* (INFC) Binary <0.1 0.3 – 0.7 2.5 0.1 – 0.3 0.5 NCP: No counterpart at other wavelengths *no -ray absorption 20 further H.E.S.S. sources investigated: • All -ray spectra show no cut-offs (but limited statistics) • Source event numbers mostly comparable to background CPPM, Marseille, 25/10/2006

  14. Summary (Galactic Sources) • Likely all strongest Galactic TeV -ray sources are discovered by H.E.S.S collaboration. • Measured -ray spectra allow robust prediction of neutrino fluxes • Event rates for 5 year calculated for the KM3NeT detector model : - ~ 1-10 event (En>1 TeV) for brightest sources - about equal number of background and signal events

  15. Gamma Ray Burst Neutrino Fluxes and Expected Rates in KM3NeT A study of individual GRBs from the BATSE catalogue Bursting sources: GRB • Power of GRB: Lg ~ 1052 erg/s • 10% radiated in neutrinos ? • Expected neutrino flux ( E-2): F(En)= ∑ ∫Fi(En,Wi,ti)d(W-DWi)d(t-Dti) dWdt • ti and Wi – provided by GRB-network satellites (GCN). • GCN: TheGammaray burstsCoordinates Network • http://gcn.gsfc.nasa.gov/ Expected GRB rate (year): ~ 1000 / 4p GRB studies in Erlangen: Melitta Naumann-Godó

  16. Calculation of GRB -Flux • neutrino production via photomeson-interactions • normalisation of -spectrum • Model 1 (generic): 10% of -flux • Model 2 (individual): w.r.t. GRB-luminosity • Parameters of individual GRB are different • - luminosity Lg • - spectrum parameters • - Lorentz factor  • - burst duration t, • -redshift z • BATSE catalogue: • 2704 GRB parameters CPPM, Marseille, 25/10/2006

  17. Short duration bursts T90: 0.01 s – 2 s Assumed progenitor: Old binary neutron star systems or neutron-star and black hole binary systems, which merge GRB parameters (example) Long duration bursts • T90: 2 s – 1000 s • Assumed progenitor: • Young, very massive stars which might explode in hypernova # burst short duration long duration short long # burst Log10(T[s]) Log10(F[GeV/m²]) CPPM, Marseille, 25/10/2006

  18. Short burst average flux Muon-neutrino fluxes Long burst average flux Waxman&Bahcall Model 1 Model 2 Waxman&Bahcall Model 1 Model 2 CPPM, Marseille, 25/10/2006

  19. Electron-neutrinos Muon-neutrinos atmos.  Model 1 Model 2 atmos. e Model 1 Model 2 GRB and atm-n Rates • Signal/background flux ratio (atm. -flux suppressed by 1010 !) • Time window per burst: ca. 100 s ( ~ 10-5 Ty) • Angular window per burst: ½° (muons), 10° (electrons) (for m: 10-5 )  0.025 nmevents/GRB above 10 TeV: ( ~ 10 nm events year ) CPPM, Marseille, 25/10/2006

  20. High-Energy Observatories 2004-2020 SRG/ROSITA/Lobster HMXT (SIMBOL-X) (XEUS) (NeXT) GLAST Agile Suzaku Con-X Swift XMM-Newton Integral Chandra 2004 2004 2006 2006 2014 2014 2016 2016 2010 2010 2012 2012 2018 2018 2008 2008 2020 2020 G. Hasinger, Astroparticle physics school, Erlangen, 2006 China Europe JAXA ESA NASA

  21. Summary (GRB) • Neutrino Fluxes from GRB calculated based on parameters of individual bursts from BATSE catalogue • GRB-neutrino flux depends of the type of burst: long bursts yield higher fluxes on average than short bursts • KM3NeT has good chances to detect neutrinos from GRBs • GRB-detection below the horizon is essentially background-free, especially with additional energy cut Few GRB-neutrino would already be significant! CPPM, Marseille, 25/10/2006

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