future directions radio a skaryan u nder ice r adio a rray hagar landsman science advisory committee...
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![Page 1: Future Directions Radio A skaryan U nder ice R adio A rray Hagar Landsman Science Advisory Committee meeting March 1 st, Madison](https://reader035.vdocuments.site/reader035/viewer/2022062806/56649ee85503460f94bf998a/html5/thumbnails/1.jpg)
Future DirectionsRadio
Askaryan
Under ice
Radio
Array
Hagar Landsman
Science Advisory Committee meetingMarch 1st, Madison
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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
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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
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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
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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
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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)
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March 1st 2007, Hagar Landsman
TRACR
DOM-MB
Metal Plate
Antennas
DRM electronics
ROBUST
Metal can /w electronics
Sealing the DRM
Going down
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March 1st 2007, Hagar Landsman
Antennas
17 cm
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March 1st 2007, Hagar Landsman
Front end electronics testing
Tests and calibration
Anechoic antenna chamber tests
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March 1st 2007, Hagar Landsman
Integrated cluster Testing• Testing clusters down to -45o
• On ice pre-deployment testing
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March 1st 2007, Hagar Landsman
Antennas
Pressure
vessels
DRM
Antenna cables
Waiting to be deployed
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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.
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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
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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
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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
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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.
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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.
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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
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March 1st 2007, Hagar Landsman
End
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March 1st 2007, Hagar Landsman
Front end electronic
−Signal amplification and filtering.
− Electronics inside a metal pressure vessel
− Each unit weight 20kg
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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
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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