2. Topics The case for remote radio detection of neutrinos
Overview (increasing remoteness)
Balloon
Satellite
Telescope
Not remote enough
ANITA

3. Cosmic rays since 1912 Flux Sources Neutrinos
Above GeV, steeply falling flux
UHE large signals, starved for events
Sources
Acceleration: charged particles
Propagation: still charged!
dE/dx: interactions with CMBR: GZK threshold
Magnetic deflection
Neutrinos
produced in source/propagation
point back to source
detect at EeV and above?

4. Go Remote: aperture v threshold

5. Overview of remote techniques
Telescope
Satellite
Balloon
Remotish-ground operations

6. Radio telescope observations of moon
Parkes
GLUE (Goldstone)
Kalyazin
LUNASKA (Parkes/ACTA)
nuMoon (WSRT)
RESUN (EVLA)
LOFAR
SKA

7. Prize for best drawing (Jeager, Mutel, Gayley)

8. Overview of lunar cherenkov (JMG)

9. Frequency, TIR, and Dq
Scholten, etal

10. frequency: aperture v threshold

11. Fine … until compare to CR events: Jeong, Reno, Sarkevic

12. Events

13. CR 100x n – what to do
separate n from CR? (spatially, by features (e.g. g-ray astronomy))
proximity of surface suppresses CR signal
up rate dominates?
return to high-f?
true for orbiter, too. (LORD)
(JRS) fluxes already nu-optimistic
some science still OK?
point sources
cross-sections

14. Lunar technique promising for CR
techniques going forward – see other talks
ATCA: coherent addition of signals from several ants
LOFAR: triggering(?)
difficult for nu’s
a lot of detail still to be done
see ANITA list of details

15. Satellites: Lunar sats …
Stal, etal

16. LORD
From “ARENA”

17. FORTE (Lehtinen, etal.)

18. PRIDE (Miller, etal.: Europa)

19. BB radio detection of cosmic particles
Overview
Neutrino detection
event generation
event simulation
ANITA detector
analysis
results
Cos-Ray detection
Monopoles
EVA

21. Overview

22. Neutrino detection Simulation Detector Operations Analysis
event generator
event simulation
Detector
Operations
Analysis
calibration
backgrounds
reconstruction

23. Neutrino interactions

24. Cherenkov and Total Internal Reflection

25. Aperture

26. ANITA flight(s)

27. Event Simulation Askaryan mechanism Determine list of sources
Signal Characteristics
Determine list of sources
For each source
Determine launch angle via ray tracing
Propagation effects
Emission spectrum
Spectrum at detector
Sum spectra from sources

28. Event ® source list CC events Better modeling of fluctuations
ne em + hadronic shower
nt, nm brem/photonuclear ® secondary showers
nt decay
Better modeling of fluctuations
multiple sub-showers
Multiple paths
reflection from bottom
internal refraction (not for ANITA)
Exotica
Monopoles: quasi-continuous photonuclear

29. Askaryan Frequency domain – linear response
ice attenuation
velocity of propagation
antenna, amps, filters (time domain for discriminators)
Spectrum from Alvarez-Muniz, Zas, & Friends
Could be improved.

30. Scaling of Askaryan signals
R: Moliere radius
L: Width of shower max
Hadronic
EM: LPM effect

31. Askaryan

32. Find launch angle (ray tracing)

33. Propagation: Attenuation

34. Propagation: Attenuation

35. Propagation: focusing

36. Propagation: birefringence
We don’t simulate this, but …
dn/n ~ 10-3 is possible
dt = 5 ns per km.
Predict Hpol arrives first

37. Cerenkov Beam

38. ANITA detector Efficient data handling
Airframe and payload infrastructure
Analog front end
Antennas
Low Noise Amps, filter, splitter
Cables/connectors/boxes
Trigger
multistage, narrow dt: reduce accidentals
Digitizer
Low power switched capacitor array
Efficient data handling

39. ANITA Payload
Weight
Rigidity
Form-factor
Power
Thermal
Remote

40. Front end: antennas

41. RF subsystems (ANITA-I)

42. Triggers

43. Digitizing electronics (Anita-I)
Key component: Switched Capacitor Array (SCA) by G. Varner.

44. Operations Campaign operations C3 NH preparations McMurdo Flight
Recovery
Taylor Dome C3

45. ANITA-View display

46. Analysis Timing Calibration Interferometry Backgrounds
Thermal (reconstruction amplitude)
Anthropogenic (clustering)
I: 0 neutrino candidates
II: 1 neutrino candidate
Limits

47. Calibration

48. Interferometry

49. Backgrounds

50. Clustering

51. Candidate events

52. ANITA GZK flux limit
Also – no news from GRBs

53. Cosmic Ray Detection

54. ANITA-I analysis Event selection Strong interference amplitude
14 below horizon
2 above
Consistent waveforms w/reflection
Correlated with B

55. Air shower highlites 16 events in ANITA I
WaveForms: 2 direct, 14 reflected
Tan(V/H) vs. B

56. MC and Energy Scale exposure reflection w/roughness freq-spectrum
E-spectrum
angular offset
see Konstantin’s talk

57. Magnetic Monopoles

58. Worlds best limit for (relativistic) monopoles

59. ANITA-III ANITA-III Fly 2013/14
Low resolution phased trigger (improve S/N)
Dual triggers UHECR/UHEN
More antennas

60. ExaVolt Antenna (Gorham, etal - 1102.3883v2)

61. Summary Remote techniques sacrifice threshold for aperture
Lunar observations hold promise for CR, but confirming a neutrino flux will be difficult
Satellites ?
Balloon borne radio detection provides large aperture at modest cost.
Sensitive to GZK neutrinos. Constrain optimistic models, approaching baseline models.
Detect UHE cosmic ray induced air showers at inclined angles. Energy scale still somewhat uncertain.

62. extra slides

63. Constant index of refraction

64. Comparison – for discussion only (Dec 2009)