June 25 27 2008 Olaf Scholten KVI Groningen

June 25 -27, 2008 Olaf Scholten KVI, Groningen ARENA 2008

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

Principle of the measurement Cosmic ray Detection: Westerbork antennas 107 km 2 100 MHz Radio waves June 25 -27, 2008 ARENA 2008

Goldstone Lunar UHE Neutrino Search (GLUE) Detection off the Moon P. Gorham et al. , PRL 93, 041101 (2004) First experiment: 12 hrs usingle Parkes 64 m dish in Australia: T. Hankins et al. , MNRAS 283, 1027 (1996) Two Calif. Tracking Juneantennas 25 -27, 2008 at JPL’s Goldstone, ARENA 2008 Station @ 2. 2 GHz, 123 hours

Askaryan effect: Coherent Cherenkov emission ~2 m Cosmic ray ~10 cm shower Wave front • Leading cloud of electrons, v c Typical size of order 10 cm Coherent Čerenkov for ν 2 -5 GHz cos θc =1/n , θc=56 o 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 e. V Angular spread D. Saltzberg et al PRL 86 (2001) 2802 Z 0 ~ Δc~λ/L=1/Lν 1 Jy = 10 -26 W/m 2/Hz June 25 -27, 2008 ARENA 2008

Spreading around Cherenkov-cone n=1. 8 GHz Based on physics principles 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 3100 GHz MHz June 25 -27, 2008 ARENA 2008

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

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

Nu. Moon Experiment @ WSRT Use Westerbork radio observatory June 25 -27, 2008 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 (Pu. Ma 2) • Polarization information ARENA 2008

Nu. Moon 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

+ 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 +10 h June 25 -27, 2008 ARENA 2008

Nu. Moon Experiment @ LOFAR • Total collecting area 0. 5 km 2 • 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. D 64(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, JCAP 06(2008)015 June 25 -27, 2008 ARENA 2008

Conclusions Nu. Moon @ WSRT Future: Nu. Moon @ LOFAR Nu. Moon @ SKA Nu. Moon collaboration: O. S. , Stijn Buitink, Heino Falcke, Ben Stappers, Kalpana Singh, June 25 -27, 2008 ARENA 2008 Richard Strom

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 1 pc = 3. 26 LY June 25 -27, 2008 ARENA 2008

Calculations for Ecr=4 1021 e. V 0. 1 GHz Influence of frequency Simulations for Moon 85% of area June 25 -27, 2008 Intensity v. s. cos θ, φ Minimal signal = 3000 Jy ARENA 2008 Case: Shower @ 2. 50 with surface 2. 2 GHz 0. 8% of area

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

June 25 -27, 2008 ARENA 2008

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