Hagar Landsman

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Askaryan Under Ice Radio Array

• Hagar Landsman
• University of Wisconsin, Madison
• APS 2007

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A few Good reasons for UHE neutrino astronomy
GZK Neutrinos Multi Messenger astronomy UHE and
far universe Hidden sources The unknown
IceCube sensitivity 1011 ev-1018 ev AURA
sensitivity gt 1016 ev-
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The next step

• The predicted flux of GZK neutrinos is no more
  than 1 per km2 per day.

.but only 1/500 will interact in ice.
IceCube will measure 1 event per year.
We need a 1000km3 sr to allow Statistics,
Event reconstruction ability, flavor id

• A larger detector requires a more efficient and
  less costly technology.
• Alternative options include radio and acoustic
  detection.

.but only 1/500 will interact in ice.
IceCube will measure 1 event per year.
We need a 1000km3 sr to allow Statistics,
Event reconstruction ability, flavor id
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Why Radio?

• Askaryan effect
• Coherent Cherenkov RF emission of from cascades.
  
• Radio emission exceeds optical radiation at 10
  PeV
• Completely dominant at EeV energies.
• Process is coherent ? Quadratic rise of power
  with cascade energy
• A Less costly alternative
• Larger spacing between modules
• (Large Absorption length)
• Shallower holes
• Narrower holes
• Good experience
• Experimental measurement of RF enhanced signal
  from showers
• Technology used for RICE, ANITA, and other

Astro-ph/9510119 P.B.Price 1995
Radio
Effective Volume per Module (Km3)
Ice, no bubbles (1.5-2.5 km)
optical
Water (Baikal 1km)
Ice, bubbles (0.9 km)
1015
1014
1016
1012
1013
Energy (eV)
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• IceCube
• Pressure vessel
• Connectors
• Main board
• DAQ
• Cables
• Holes

• ANITA
• LABRADOR chip
• low power consumption
• low dead time
• large bandwidth
• cold rated

AURA
RICE Antennas Data analysis Electronics and
control
KU
University of Maryland
University of Delaware
University of Hawaii
Kansas University
University of Wisconsin - Madison
Penn State University
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The Radio Cluster
Counting house
surface junction box

• Each cluster is composed of
• 1 Digital Radio Module (DRM) Electronics
• 4 Antennas
• 1 Antenna Calibration Unit (ACU)
• Signal conditioning and amplification happen at
  the front end, signal is digitized and triggers
  formed in DRM
• A cluster uses standard IceCube sphere, DOM main
  board and surface cable lines.
• Use a DOM-MB as communication and power platform.
  
• Advantage get a free design for power, comms
  and time stamping.

Not to scale!
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Waiting to be deployed
Antenna cables
Pressure vessels
Antennas
DRM
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Digital Radio Module (DRM)
Digital Optical Module (DOM)
6 Penetrators 4 Antennas 1 Surface cable
1 Calibration unit
TRACR Board Trigger Reduction and Comm for
Radio Data processing, reduction, interface to MB
MB (Mainboard) Communication, timing, connection
to IC DAQ infrastructure,
Shielding separates noisy components
ROBUST Board ReadOut Board UHF Sampling and
Triggering Digitizer card
SHORT Boards Surf High Occupancy RF Trigger
Trigger banding
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Integrated cluster Testing

• Testing clusters down to -45o
• On ice pre-deployment testing

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RF Versus optical
450 MHz Filters
Anechoic antenna chamber tests
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78 rock , 1st ,Deployment, Deep, 4
Receivers, 1Transmitters 57 scissors, 2nd
deployment, Shallow, 4 Receivers,
1Transmitters 47 paper 3rd Deployment, Deep,
1 Transmitter
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AURA in ice Preliminary data Verification and
detector studies
RICE InIce Transmitter AURA receiving
AURA transmitting AURA receiving
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SPATSSouth Pole Acoustic Test Setup
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The next step

• 10km scale hybrid GZK detector
  Acoustic/optical/RF
• Challenges
• Independent detector
• Power distribution and DAQ over large distances.
• New radio DAQ. Keep using mb utilities?
• Smaller holes
• Packaging, cabling, deployment
• RD for antennas design, RF electronics,
  triggering.
• Simulation studies
• Interface with optical and acoustic modules.

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Summary

• Neutrino are an excellent astrophysical probe.
• High energy neutrino are out there. It is a
  matter of time (or volume) until we will catch
  them.
• 3 Radio clusters were co-deployed with the
  IceCube detector this season.
• The Clusters are taking verification and
  calibration data
• First step toward a hybrid 10km scale detector.

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The End
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Multiple bandwidth trigger

• 16 combinations of triggers
• 4 antennas
• 4 bandwidth on each antenna
• Trigger condition will be tuned to maximize data
  rates within the cable bandwidth.
• Remove a noisy frequency