Future Directions Radio A skaryan U nder ice R adio A rray Hagar Landsman Science Advisory Committee...
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Transcript of Future Directions Radio A skaryan U nder ice R adio A rray Hagar Landsman Science Advisory Committee...
Future DirectionsRadio
Askaryan
Under ice
Radio
Array
Hagar Landsman
Science Advisory Committee meetingMarch 1st, Madison
March 1st 2007, Hagar Landsman
Why EeV neutrinos ?– GZK cutoff
• No Cosmic rays above ~1020 eV • High energy neutrinos
– Study of energetic and distant objects (Photons attenuation length decrease with energy)
– Study highest energy neutrino interaction– Point source– Exotic sources– The unknown
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
March 1st 2007, Hagar Landsman
Why Radio?
• Askaryan effectCoherent 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
optical
Radio
Ice, n
o bubbles (1.5-2
.5 km)
Ice, bubbles
(0.9 km)
Water (
Baikal 1
km)
Eff
ect
ive
Vo
lum
e p
er
Mo
du
le (
Km
3 )
Energy (eV) 1012 1013 1014 1015 1016
Astro-ph/9510119 P
.B.P
rice 1995
March 1st 2007, Hagar Landsman
IceCube• Pressure vessel• Connectors • Main board• DAQ• Cables• Holes
ANITA LABRADOR chip:• low power consumption• low dead time• large bandwidth• cold rated
RICE Antennas
Data analysisElectronics and control
KU
University of Maryland
University of Delaware
University of Hawaii
KansasUniversity
University of Wisconsin - Madison
Penn State University
March 1st 2007, Hagar Landsman
surface junction
box
Counting house
Each unit 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!
The Radio Cluster
March 1st 2007, Hagar Landsman
Toantenna
Toantenna
To
antenna
To
surface
ToCalibrationunitTo
antenna
Modified glass sphere 6 Penetrators: 4 Antennas 1 Surface cable 1 Calibration unit
Radio BoardsUHF Sampling, Triggering, Digitizing, data processing, trigger banding, interface to the mb
MB (Main board)Communication, timing, connection to IC DAQ infrastructure,
Digital Radio Module (DRM)
March 1st 2007, Hagar Landsman
TRACR
DOM-MB
Metal Plate
Antennas
DRM electronics
ROBUST
Metal can /w electronics
Sealing the DRM
Going down
March 1st 2007, Hagar Landsman
Antennas
17 cm
March 1st 2007, Hagar Landsman
Front end electronics testing
Tests and calibration
Anechoic antenna chamber tests
March 1st 2007, Hagar Landsman
Integrated cluster Testing• Testing clusters down to -45o
• On ice pre-deployment testing
March 1st 2007, Hagar Landsman
Antennas
Pressure
vessels
DRM
Antenna cables
Waiting to be deployed
March 1st 2007, Hagar Landsman
AURA GOALS for 06/07 season
The five point goals were defined in July 06 PDR• Assess the suitability of the IceCube environment• Receive, amplify, and digitize over 0.2 to 1 GHz• Antenna trigger and timing• Multiple cluster trigger• Measure RF noise beyond RICE frequency (600 MHz)
Deploy a minimum of two clusters at two different depths
We have successfully deployed 3 clusters.All 3 clusters are collecting data.
Installation and operation did not conflict with IceCube’s string installations or data acquisition.
We have the in ice hardware needed to achieve those goals.
March 1st 2007, Hagar Landsman
Deployment this season
57: “scissors”, 2nd deployment, Shallow4 Receivers, 1Transmitters
47: “paper” 3rd Deployment, Deep1 Transmitter
78: “rock” , 1st ,Deployment,Deep4 Receivers, 1Transmitters
March 1st 2007, Hagar Landsman
Short term planIn Ice units
– Calibration using ACU– Calibration using RICE
transmitters– Tests of mb-TRACR
operation-• Triggering• Timing• Data rates • Durability
– Wave forms characterization
– Ice Suitability – RF noise
March 1st 2007, Hagar Landsman
Building and deploying ~10 additional units • Intermediate scale GZK detector• Coincidence with IceCube.• Ice RF survey• On the way of a GZK detector: New designs, Independency from
IceCube.
– Keep using IceCube infrastructure.
– Based on lessons learned this season improve:• Design of the cluster, Antennas and front-end.• Data acquisition and testing tools.• Deployment and on Ice handling• Power distribution and control
– Simulation studies• Geometry, antenna design, wave propagation• detector simulation
Short term plansNext year deployment
March 1st 2007, Hagar Landsman
The next step10km scale hybrid GZK detector –
Acoustic/optical/RFChallenges:• Independent detector
– Power distribution and DAQ over large distances.
– New radio DAQ. Keep using mb utilities?
– Smaller holes– Packaging, cabling, deployment
• R&D for antennas design, RF electronics, triggering.
• Simulation studies• Interface with optical and
acoustic modules.
March 1st 2007, Hagar Landsman
PROPOSAL
• Proposal was submitted: 2 years R&D, simulation, detectors.
• Document posted under “additional materials” in docushare.
• Additional funding sources have been used for recent design and production of first radio clusters.
March 1st 2007, Hagar Landsman
Summary
•Last Season 3 Radio clusters successfully deployed
• In the next yearsFurther DRM development and deployment
• Far Future Towards >100 km2 scale detector
March 1st 2007, Hagar Landsman
End
March 1st 2007, Hagar Landsman
Front end electronic
−Signal amplification and filtering.
− Electronics inside a metal pressure vessel
− Each unit weight 20kg
March 1st 2007, Hagar Landsman
Neutrino interact in ice showers
ννdCRdP ∝
Charge asymmetry: 20%-30% more electrons than positrons.
Moliere Radius in Ice ~ 10 cm:This is a characteristic transverse dimension of EM showers. <<RMoliere (optical), random phases P N >>RMoliere (RF), coherent P N2
Hadronic (initiated by all ν flavors)EM (initiated by an electron, from νe)
Askaryan effect
Vast majority of shower particles are in the low E regime dominates by EM interaction with matter
Less Positrons:Positron in shower annihilate with electrons in matter e+ +e- Positron in shower Bhabha scattered on electrons in matter e+e- e+e-
More electrons:Gammas in shower Compton scattered on electron in matter e- + e- +
Many e-,e+, Interact with matter Excess of electrons Cherenkov radiation Coherent for wavelength larger than shower dimensions
March 1st 2007, Hagar Landsman
• Antennas KU• Front end electronics UMD, KU, Hawaii• DRM Electronic component:
– Digitizer Hawaii– data control KU– main board UW– Power converter bartol
• Electronic integration KU• Connectors, cables, sphere, pressure vessel,
installationUW• Detector integration, testing, packaging UW• Firmware/software KU, UW, PSU