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