1. 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

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

3. 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

4. Detection off the Moon Goldstone Lunar UHE Neutrino Search (GLUE)
P. Gorham et al., PRL 93, (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 2.2 GHz, 123 hours
June 25-27, 2008
ARENA 2008

5. 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

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

7. 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

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

9. Cosmic rays, Position on Moon
Calculations for
Ecr= 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

10. 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

11. NuMoon Experiment @ WSRT
Use Westerbork radio observatory
Advantages:
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

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

13. 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

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

15. June 25-27, 2008
ARENA 2008

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

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

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

19. 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

20. 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

21. SKA-Hadrons
June 25-27, 2008
ARENA 2008

22. 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

23. 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

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

25. The observed Universe
June 25-27, 2008
ARENA 2008

26. 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

27. Influence of frequency
Case:
with surface
Calculations for
Ecr= 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

28. 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

29. 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

30. June 25-27, 2008
ARENA 2008

31. 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

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