Gisela Anton LAUNCH 09 Heidelberg, November 10 th, 2009 High Energy Neutrino Astronomy

Alexander Kappes, DPG-Frühjahrstagung, München, Content Introduction to high energy neutrino astronomy Neutrino-Telescopes: IceCube and ANTARES Selected results Future perspectives of IceCube und KM3NeT Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Messengers of the high energy universe Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009    p p e Cosmic ray spectrum

Alexander Kappes, DPG-Frühjahrstagung, München, The high energy universe Gamma-ray Burst (GRB B, X-Ray, SWIFT) Active Galactic Nuclei (artists view) Supernova Remnant (SN1006, optiical, radio, X-ray) Microquasar (artists view) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Acceleration of particles Shock front (Fermi-acceleration) Objects with strong magnetic fields (pulsars, magnetars) Beam dump (secondary particles) Interaction of high energy particles with photons or matter -Protons: pion production and decay -Electrons: inverse Compton-Scattering of Photons e + γ(low energy) → e + γ (TeV) Production mechanisms p + p(γ) → π ± + X μ + ν μ e + ν μ + ν e p + p(γ) → π 0 + X γ + γ (TeV) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Photon ↔ neutrino connection: Observed from RX J1713.7–3946: -γ-rays up to several 10 TeV → particle acceleration up to 100 TeV and above Calculated neutrino fluxes: Estimated neutrino fluxes (SNR) RX J1713.7–3946 p + p → π ± + X μ + ν μ e + ν μ + ν e p + p → π 0 + X γ + γ For strong sources: – TeV -1 cm -2 s 1 TeV AK, Hinton, Stegmann, Aharonian, ApJ (2006) Halzen, AK, O’Murchadha, PRD (2008) Kistler, Beacom, PRD (2006)... AK, Hinton, Stegmann, Aharonian, ApJ (2006) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Neutrinos as cosmic messengers Neutrinos point back to sources Neutrinos travel cosmological distances Neutrinos escape dense sources Neutrinos are related to hadron acceleration Neutrinos complement high energy proton and gamma observation Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Detection of Neutrinos muon νμνμ nuclear reaction cascade Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Background: atmospheric muons and neutrinos p atmosphere cosmic rays μ νμνμ νμνμ cosmic background p μ νμνμ Flux from above dominated by atmospheric muons Neutrino telescopes mainly sensitive to neutrinos from below Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Sky visibility in neutrinos Horizon above below Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Neutrino Telescopes: Baikal, IceCube and ANTARES Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, NT200 8 strings (192 optical modules) Instrumented volume 1×10 -4 km 3 Running since 1998 NT200+ NT outer strings (36 optical modules) Instrumented volume km 3 Running since 2005 Baikal NT200+ Single storey Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Sky coverage Visibility ANTARES (Mediterranean Sea) > 75% 2 25% – 75% < 25% TeV γ-Sources galactic extragalactic Visibility IceCube (Southpole) 100% 0% Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, IceCube at the Southpole Southpole IceCube Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, I Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Optical properties of Ice Photon-Propagation in ice dominated by scattering λ abs ~100 m λ scat ~20 m Event reconstruction sensitive to ice properties Detailed measurement of ice properties (dust layer) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, ANTARES in the Mediterranean Main cable (45km) Shore station Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Lines (885 PMTs) Completion May 2008 Instrumented volume: ~0.01 km 3 ANTARES 2100 m 2475 m Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Lines moving in the sea current Acoutic positioning system + tiltmeter and compasses:  x < 10 cm Monitoring of the positioning with laser pulses  Precision ~0.5 ns = 10 cm Position determination for PMTs Laser 0.5 ns Time measured – calculated (ns) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Optical Background Optical background due to 40K-decay and bioluminescense Typical rate per PMT kHz Additional short bursts and periods with higher rates Mar.’06Sept.’06Mar.’07Sep.’07Mar.’08 Median rate (kHz) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Selected Results Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, ANTARES: Atmospheric Myons & Neutrinos up going: ν-induced myons ANTARES (173 days) down going: atm. myons Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Need of calibration source for proof of detector pointing capability and resolution Nature offers deficit of muons from direction of the Moon -Diameter of the Moon 0.5° Angular resolution -IceCube 80-String < 1° -ANTARES < 0.5° First observation of the Moon shadow with IceCube 40-String data IceCube: the shadow of the moon Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009 A. ICRC 2009 RA relative to moon position Dec rel. moon

Alexander Kappes, DPG-Frühjahrstagung, München, Search for point sources – IceCube 40 strings (6 months) Preliminary Background: atm. neutrinos (6796 events) (10981 events) Background: atm. muons Most-significant spot: all-sky background probability: 61% Significance Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Point source sensitivities ANTARES: 12 lines 1 year (pred. sensitivity) Flux predictions Halzen, AK, O’Murchadha, PRD (2008) AK, Hinton, Stegmann, Aharonian, ApJ (2006) Kistler, Beacom, PRD (2006) Costantini & Vissani, App (2005)... MACRO (6 years) Super-K. (4.5 years) AMANDA (3.8 years) IceCube: IceCube 40 Strings 330 days (sensitivity) IceCube 80 Strings 1 yr (pred. sensitivity) 90% CL sensitivity for E -2 spectra (preliminary) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, triggered Search Sensitivity gain due to time and direction of burst measured by satellites Low number of events per GRB expected ➞ “Burst-Stacking” Un-triggered Search Possible large population of “choked“ GRBs; unvisible in γ-rays Search for excess of events in time and direction Gamma-Ray Bursts Fireball model Precursor ~-100 sT0T0 ~100 s> 1000 s TeV neutrinos PeV neutrinos EeV neutrinos Prompt Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Limits on neutrino fluxes from GRBs precursor prompt precursor: Meszaros & Waxman, PRL (2001) prompt: IceCube, AK et al., ICRC2009 Perspectives: 200 – 300 GRBs per year (Fermi, SWIFT) IceCube will be able to detect predicted fluxes within next years Baikal NT200+ (155 GRBs) (Avrorin et al., arXiv: ) IceCube 22-Strings (41 GRBs) (Abbasi et al, arXiv: ) AMANDA (417 GRBs) (Achterberg et al. (2008) ApJ 674, 357) predictions IceCube Baikal IceCube Amanda Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, First proposed by M. Kowalski (Kowalski and Mohr (2007), App 27, 533) IceCube: cooperation with ROTSE (4 telescopes) Antares: cooperation with TAROT (2 telescopes) Optical Follow-Up SN/GRB robotic optical telescopes neutrino telescope send alert Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Neutralino ( χ ) good WIMP candidate Gravitational capture in the Sun + self annihilation Neutrino rate only depends on scattering cross section (equilibrium between capture and annihilation) Dark Matter Searches (WIMPs) χ ν - ν Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, ` IceCube 86 with Deep Core Sensitivity 1 yr (prel., hard) WIMP searches Direct detection experiments (CDMS, COUPP, KIMS) Super-Kamiokande (2004) AMANDA 7 years soft hard IceCube 22-strings limits (PRL 102, (2009)) soft hard MSSM models } Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Expected Neutrino Events from Dark Matter Annihilation in ANTARES Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Diffuse neutrino flux Baikal Waxman-Bahcall IC22 ICRC2009 IceCube 22 strings (preliminary) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Further Physics Point Sources: Variable Sources -Extragalactic -source candidates are non persistent -Time search window given for instance by γ-ray signals  reduction of background Target of opportunity: 2 neutrinos within  t from same direction  send alert to optical telescope for follow up Other Topics: Supernovae (MeV neutrinos) Neutrino oszillation (atmospheric neutrinos GeV) Exotic physics (Lorentz symmetry violation, monopoles,...) Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Perspectives with IceCube und KM3NeT Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, IceCube: compared to AMANDA (7 years) factor 25 increased sensitivity -larger detector + data quality -accumulated data -improved analysis methods IceCube is in the region of realistic discovery potential, but - flux estimates indicate that IceCube is at the edge of the interesting region - IceCube covers only have of the sky Future of Neutrino-Astronomy Spiering, HGF review, 2009 Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, km 3 -scale neutrino telescope in the Mediterranean ( and infrastructure for marine and Earth science) Common effort of ANTARES, NEMO and NESTOR pilot projects + Institutes from marine science and oceanographic technologies On the Roadmap of the European Strategy Forum for Research Infrastructures (ESFRI) EU financed Design Study ( ) EU financed Preparatory Phase ( ) KM3NeT Artists view Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Semi-rigid system of horizontal elements (storeys): 20 storeys Each storey supports 6 OMs in groups of 2 Storeys interlinked by tensioning ropes, subsequent storeys orthogonal to each other Power and data cables separated from ropes Flexible tower with horizontal bars 6 m 40 m Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, OM with many small PMTs 31 3-inch PMTs in 17-inch glass sphere (cathode area ~3x10” PMTs) -19 in lower, 12 in upper hemisphere -Suspended by compressible foam core 31 PMT bases (D) (total ~140 mW) Front-end electronics (B,C) Al cooling shield and stem (A) Single penetrator 2mm optical gel (ANTARES-type) A B C C D PMT Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, KM3NeT Point Source Sensitivity (3 years) Aharens et al. Astr. Phys. (2004) – binned method Average value of sensitivity from R. Abbasi et al. Astro-ph (2009) R. Abbasi et al. Astro-ph (2009) scaled – unbinned method  Observed Galactic TeV-  sources (SNR, unidentified, microquasars) Aharonian et al. Rep. Prog. Phys. (2008), Abdo et al., ApJ 658 L33-L36 (2007) KM3NeT (binned/unb.) IceCube Typical fluxes Estimated costs: ~100 MEuro (+10% man power) Note: Double sensitivity for about double price... Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Next steps: Prototyping and design decisions organized in Preparatory Phase framework final decisions require site selection expected to be achieved in ~18 months Timeline: KM3NeT Timeline Feb 2006 Mar 2008 Oct 2009 Mar 2012 Construction phase Data taking phase TDRCDR Design Study Preparatory Phase 2011 Design decision Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Summary High energy neutrinos deliver complementary information to gamma photons and protons ANTARES completed, IceCube 70% installed, KM3NeT in design phase No cosmological high energy neutrinos observed yet IceCube will enter the region with discovery potential KM3NeT will exceed IceCube Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009

Alexander Kappes, DPG-Frühjahrstagung, München, Thank you for your attention muon νμνμ nuclear reaction cascade Gisela Anton, LAUNCH 09, Heidelberg, November 10th, 2009