Cosmic ray and Neutrino Physics Ultra-High Energy Cosmic ray and Neutrino Physics using the Moon Olaf Scholten KVI, Groningen June 25-27, 2008 ARENA 2008

Large Area ?? Use the Moon!! Area = 2 107 km2 June 25-27, 2008 ARENA 2008

Principle of the measurement Cosmic ray Detection: Westerbork antennas 107 km2 100MHz Radio waves Proefje door Tjalling Nijboer en Martin Stokroos: Statische electriciteit van wrijfstok is hoorbaar via radio ontvanger op de middengolf. June 25-27, 2008 ARENA 2008

Detection off the Moon Goldstone Lunar UHE Neutrino Search (GLUE) P. Gorham et al., PRL 93, 041101 (2004) First experiment: 12 hrs using single Parkes 64m dish in Australia: T. Hankins et al., MNRAS 283, 1027 (1996) Two antennas at JPL’s Goldstone, Calif. Tracking Station @ 2.2 GHz, 123 hours June 25-27, 2008 ARENA 2008

Askaryan effect: Coherent Cherenkov emission ~10 cm ~2 m Cosmic ray shower Wave front Leading cloud of electrons, v  c Typical size of order 10cm Coherent Čerenkov for ν  2-5 GHz cos θc =1/n , θc=56o for ∞ shower length Length of shower, L  few m Important for angular spreading June 25-27, 2008 ARENA 2008

Askaryan effect: confirmation in sand Experiment at SLAC with beams of photons And 1010 e-/bunch: effective shower energies 0.06-1.10 1019 eV Angular spread Z0 ~ Δc~λ/L=1/Lν D. Saltzberg et al PRL 86 (2001) 2802 1 Jy = 10-26 W/m2/Hz June 25-27, 2008 ARENA 2008

Spreading around Cherenkov-cone Based on physics principles GHz Old parametrization Sine profile L=1.7 m , E=1020 O.S. etal., Astropart.Phys. 2006 June 25-27, 2008 ARENA 2008

Reflection Spreading is diminishing internal reflection 3 GHz 100 MHz June 25-27, 2008 ARENA 2008

Cosmic rays, Position on Moon Calculations for Ecr=4 1021 eV 100 MHz 3 GHz Partial Detection probability With decreasing ν : - increasing area - increasing probability ∫ over surface Moon D  ν-3 Normalized distance from center June 25-27, 2008 ARENA 2008

Detection Limits, Cosmic rays Minimum Flux for detecting 1 count/100h Detection threshold = 500Jy Decreasing ν : Increasing threshold like ν-1 Increase sensitivity like ν-3 June 25-27, 2008 ARENA 2008

NuMoon Experiment @ WSRT Use Westerbork radio observatory Advantages: 117-175 MHz band 25 m diameter dishes 5 degree field of view 12-14 coincident receivers 500 hour observation time 40 M samples/sec (PuMa2) Polarization information June 25-27, 2008 ARENA 2008

NuMoon Experiment @ WSRT Use Westerbork radio observatory 4 frequencies June 25-27, 2008 ARENA 2008

Processing Pipeline 18 TB raw data per 6 hr slot Excision of narrow-band interference De-Dispersion of ionosphere with GPS TEC values Indentification of peaks in time spectrum Data reduction 100:1 to 180 GB June 25-27, 2008 ARENA 2008

Trigger: 4σ pulse in all four frequency bands + dedispersion June 25-27, 2008 ARENA 2008 Trigger: 4σ pulse in all four frequency bands

June 25-27, 2008 ARENA 2008

Trigger Power Spectrum Effect successive steps in analysis Gaussian noise June 25-27, 2008 ARENA 2008

Prelimenary Results Analysis of 10 h 40 min data Additional observation time: 7 June +10h June 25-27, 2008 ARENA 2008

NuMoon Experiment @ LOFAR Total collecting area 0.5 km2 Cover whole moon, Sensitivity 25 times better than WSRT. Bands: 30-80 MHz (600 Jy) 115-240 MHz (20 Jy) June 25-27, 2008 ARENA 2008

Neutrinos WSRT, 100 hours 0 counts LOFAR, 30 days ~60 counts Theoretical predictions: Waxman-Bahcall limit GZK induced flux Phys.Rev.D64(04)93010 June 25-27, 2008 ARENA 2008

Future: SKA,LORD 1 year observation, LFB: 100-300 MHz MFB: 300-500 MHz From: O.S., SKA Design Study report June 25-27, 2008 ARENA 2008

SKA-Hadrons June 25-27, 2008 ARENA 2008

Resonant neutrino absorption Neutrinos are absorbed on relic neutrino background by forming Z-boson A. Ringwald, L. Schrempp, JCAP 0610 (2006) 012 30 day z=5 z=20 z=50 Measured pulse-height spectrum can distinguish sources at various distances OS& A. van Vliet,JCAP06(2008)015 June 25-27, 2008 ARENA 2008

Conclusions NuMoon Future: NuMoon @ WSRT NuMoon @ LOFAR NuMoon @ SKA Competitive Sensitivity for cosmic rays and neutrinos NuMoon NuMoon collaboration: O.S., Stijn Buitink, Heino Falcke, Ben Stappers, Kalpana Singh, Richard Strom June 25-27, 2008 ARENA 2008

LORD efficiency for neutrinos June 25-27, 2008 ARENA 2008

The observed Universe June 25-27, 2008 ARENA 2008

Some distance scales Nearest star, Proxima Centauri – 4 LY Diameter of our galaxy – 100,000 LY Distance to nearest galaxy – the Sagittarius dwarf galaxy, which is being “eaten” by the Milky Way – 80,000 LY Size of our “Local Group” – a collection of at least 30 galaxies, including Andromeda – 3 Million LY Size of our “Local Supercluster” which contains our Local Group, the Virgo Cluster, and others – 100 Million LY 1pc = 3.26 LY June 25-27, 2008 ARENA 2008

Influence of frequency Case: Shower @ 2.50 with surface Calculations for Ecr=4 1021 eV Influence of frequency Simulations for Moon Minimal signal = 3000Jy 0.1 GHz 85% of area 2.2 GHz 0.8% of area June 25-27, 2008 ARENA 2008 Intensity v.s. cos θ, φ

Shock wave acceleration Colliding galaxies “Fermi shock acceleration” proton passes several times through shock front due to magnetic field. Spectrum  E -2 Active galactic nucleus Need large scale magnetic fields June 25-27, 2008 ARENA 2008

Short-range particle astronomy Larmor radius for a charged particle (charge Z) and energy E (1020 eV) in a magnetic field with strength B(nG): ρ(Mpc)=108·(E/1020eV)·(1/BnG)·(1/Z). Galaxy about 1000 nG; proton escapes; iron wanders around From: M. Teshima 2006 June 25-27, 2008 ARENA 2008

June 25-27, 2008 ARENA 2008

Greisen – Zatsepin - K’uzmin (GZK) Transport Greisen – Zatsepin - K’uzmin (GZK) Energetic protons loose energy through Interactions with the cosmic microwave background June 25-27, 2008 ARENA 2008

Possible Sources within 1.5 Mpc Local Group June 25-27, 2008 ARENA 2008