Next Generation neutrino detector in the South Pole Hagar Landsman, University of Wisconsin, Madison Askaryan Under-Ice Radio Array.

Slides:



Advertisements
Similar presentations
RICE bounds on UHE Neutrino fluxes in the GZK Regime plus bounds on new physics Data from 2000 through 2004 confront models of the world (PRELIMINARY)
Advertisements

J. Alvarez-Muñiz, ARENA 2005 Simulations of radio emission from EM showers in different dense media E. Marqués R.A. Vázquez E. Zas Jaime Alvarez-Muñiz.
Detection of Gamma-Rays and Energetic Particles
AMANDA Lessons Antarctic Muon And Neutrino Detector Array.
July 29, 2003; M.Chiba1 Study of salt neutrino detector for GZK neutrinos.
The NuMoon experiment: first results Stijn Buitink for the NuMoon collaboration Radboud University Nijmegen 20 th Rencontres de Blois, 2008 May 19.
Kay Graf University of Erlangen for the ANTARES Collaboration 13th Lomonosov Conference on Elementary Particle Physics Moscow, August 23 – 29, 2007 Acoustic.
The Pierre Auger Observatory Nicolás G. Busca Fermilab-University of Chicago FNAL User’s Meeting, May 2006.
Radio detection of UHE neutrinos E. Zas, USC Leeds July 23 rd 2004.
By Devin Gay Radio Ice Cerenkov Experiment. RICE got off the ground and into the ice in 1995 They got started when AMANDA collaborations agreed to co-
Shower & RF theory David Seckel, ANITA Collab. Mtg. Nov , /2002 Theory Notes on Shower and Radio Pulse.
SUSY06, June 14th, The IceCube Neutrino Telescope and its capability to search for EHE neutrinos Shigeru Yoshida The Chiba University (for the IceCube.
P. Gorham, SLAC SalSA workshop1 Saltdome Shower Array: Simulations Peter Gorham University of Hawaii at Manoa.
ANtarctic Impulsive Transient Antenna NASA funding started 2003 for first launch in 2006 Phase A approval for SMEX ToO mission 600 km radius, 1.1 million.
Tuning in to UHE Neutrinos in Antarctica – The ANITA Experiment J. T. Link P. Miočinović Univ. of Hawaii – Manoa Neutrino 2004, Paris, France ANITA-LITE.
Acoustic simulations in salt Justin Vandenbroucke UC Berkeley Salt Shower Array workshop SLAC, February 3, 2004.
Askaryan effect in salt: SLAC T460, June T460 rock-salt target 4lb high-purity synthetic rock-salt bricks (density=2.07) – 6 tons of it. + some.
Future prospects for large area ground & space-based neutrino detectors Peter Gorham JPL Tracking & Applications Section 335 RADHEP 2000.
The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
Transmission Media / Channels. Introduction Provides the connection between the transmitter and receiver. 1.Pair of wires – carry electric signal. 2.Optical.
Hagar Landsman, University of Wisconsin, Madison.
Sebastian Böser Acoustic test setup at south pole IceCube Collaboration Meeting, Berkeley, March 2005.
July 10, 2007 Detection of Askaryan radio pulses produced by cores of air showers. Suruj Seunarine, Amir Javaid, David Seckel, Philip Wahrlich, John Clem.
Summary of the Acoustic R&D Parallel Session R. Nahnhauer DESY September 23rd, 2011 IceCube Meeting Uppsala1 x AAL Quo vadis?
Radovan Milinčić and Predrag Miočinović SLAC International SalSA Workshop, February 3-4, T(CR) 3 IC Testbed for Coherent Radio Cherenkov Radiation.
Studies of the Energy Resolution of the ANITA Experiment Amy Connolly University of California, Los Angeles CALOR06 June 6 th, 2006.
Simulation Issues for Radio Detection in Ice and Salt Amy Connolly UCLA May 18 th, 2005.
Lecture 1.3: Interaction of Radiation with Matter
ARIANNA: Searching for Extremely Energetic Neutrinos Lisa Gerhardt Lawrence Berkeley National Laboratory & University of California, Berkeley NSD Monday.
IRA April 2006 D.F. Cowen/IceCube Collab. Beyond IceCube Beijing UHE  Workshop 1 Beyond the South Pole Outline  Introduction: Optical vs. Radio.
AMANDA and IceCube neutrino telescopes at the South Pole Per Olof Hulth Stockholm University.
Future Directions Radio A skaryan U nder ice R adio A rray Hagar Landsman Science Advisory Committee meeting March 1 st, Madison.
RICE = “Radio Ice Cherenkov Experiment”
Why Neutrino ? High energy photons are absorbed beyond ~ 150Mpc   HE  LE  e - e + HE s are unique to probe HE processes in the vicinity of cosmic.
Medical Imaging Radiation I. Naked to the Bone: Medical Imaging in the Twentieth Century (Paperback)by Bettyann Kevles Bettyann Kevles E=mc2: A Biography.
radio lobe sound disk  t p ~ km  optical light cone The Vision *) see e.g. A. Ringwald,ARENA 2005 Build ~100 km 3 hybrid detector to: Confirm GZK cutoff.
Mar 9, 2005 GZK Neutrinos Theory and Observation D. Seckel, Univ. of Delaware.
March 02, Shahid Hussain for the ICECUBE collaboration University of Delaware, USA.
Humberto Salazar (FCFM-BUAP) for the Pierre Auger Collaboration, CTEQ- Fermilab School Lima, Peru, August 2012 Ultrahigh Cosmic Rays: The highest energy.
for the ARA collaboration,
“Radio detection”, Hagar Landsman; IceCube Science Advisory Committee May 5, 08; Future methods::Radio Hagar Landsman University of Wisconsin, Madison.
Detection of UHE Shower Cores by ANITA By Amir Javaid University Of Delaware.
Hagar Landsman, Mike Richman, and Kara Hoffman On behalf of the IceCube Collaboration Ice index of refraction n(z) Ice Attenuation Length (point to point)
Laboratory Particle- Astrophysics P. Sokolsky High Energy Astrophysics Institute, Univ. of Utah.
M.Chiba_ARENA20061 Measurement of Attenuation Length for Radio Wave in Natural Rock Salt and Performance of Detecting Ultra High- Energy Neutrinos M.Chiba,
RICE David Seckel, NeSS02, Washington DC, Sept ,/2002 R adio I ce C herenkov E xperiment PI presenter.
Sept. 2010CRIS, Catania Olaf Scholten KVI, Groningen Physics Radio pulse results plans.
ANtarctic Impulsive Transient Antenna University of Hawaii at Manoa Peter Gorham, PI John Learned and Gary S. Varner Ohio-State University Jim Beatty and.
Simulation of a hybrid optical, radio, and acoustic neutrino detector Justin Vandenbroucke with D. Besson, S. Boeser, R. Nahnhauer, P. B. Price IceCube.
Feasibility of acoustic neutrino detection in ice: First results from the South Pole Acoustic Test Setup (SPATS) Justin Vandenbroucke (UC Berkeley) for.
Neutrinos and Z-bursts Dmitry Semikoz UCLA (Los Angeles) & INR (Moscow)
Neutrino Detection at the South Pole: Instrumentation Issues Dr. Steve Churchwell University of Canterbury, Christchurch, New Zealand The RICE detector.
RICE: ICRC 2001, Aug 13, Recent Results from RICE Analysis of August 2000 Data See also: HE228: Ice Properties (contribution) HE241: Shower Simulation.
Studies of Askaryan Effect, 1 of 18 Status and Outlook of Experimental Studies of Askaryan RF Radiation Predrag Miocinovic (U. Hawaii) David Saltzberg.
IceRay-0 Testbed: A Radio Surface Listening Station John Kelley IceCube Collaboration Meeting April 30, 2008 UH Radio Detection Group: P. Gorham, G. Varner,
31/03/2008Lancaster University1 Ultra-High-Energy Neutrino Astronomy From Simon Bevan University College London.
“Radio detection”, Hagar Landsman; IceCube Science Advisory Committee May 5, 08; Future methods::Radio Hagar Landsman University of Wisconsin, Madison.
Jeong, Yu Seon Yonsei University Neutrino and Cosmic Ray Signals from the Moon Jeong, Reno and Sarcevic, Astroparticle Physics 35 (2012) 383.
June 18-20, 2009 Detection of Askaryan radio pulses produced by cores of air showers. Suruj Seunarine, David Seckel, Pat Stengel, Amir Javaid, Shahid Hussain.
IceRay: an IceCube-Centered Radio GZK Array John Kelley University of Wisconsin, Madison for the IceRay working group ARENA08, Rome.
1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.
Shih-Hao Wang 王士豪 Graduate Institute of Astrophysics & Leung Center for Cosmology and Particle Astrophysics (LeCosPA), National Taiwan University 1 This.
Bergische Universität Wuppertal Jan Auffenberg et al. Rome, Arena ARENA 2008 A radio air shower detector to extend IceCube ● Three component air.
Simulation of a hybrid optical-radio-acoustic neutrino detector at South Pole D. Besson [1], R. Nahnhauer [2], P. B. Price [3], D. Tosi [2], J. Vandenbroucke.
Future high energy extensions of IceCube with new technologies: Radio and/or acoustical detectors Karle.
Discussion session: other (crazy
ARA The Askaryan Radio Array A new instrument for the detection of highest energy neutrinos. Hagar Landsman, UW Madison.
Relativistic Magnetic Monopole Flux Constraints from RICE
IceCube radio extension Status and results
Acoustic vs radio vs optical detection of neutrino-induced cascades in ice and water Relevant papers by PBP: 1. Mechanisms of attenuation of acoustic.
Presentation transcript:

Next Generation neutrino detector in the South Pole Hagar Landsman, University of Wisconsin, Madison Askaryan Under-Ice Radio Array

Outline Askaryan Effect and neutrino detection Why Ice? Why Radio? Radio detection Experiment Design and prospective A skaryan U nder ice R adio A rray

Tribute to 45 m 25 m Ice Cube ~ 1km The Future: Hybrid Detector ~10 km

Quest for UHE neutrinos GZK Cut-off p+  CMB –No cosmic rays from proton above eV –As a by-product – neutrino flux –A non detection will be even more exciting Point Sources of neutrinos Dark matter

Why so big? To detect 10 GZK events/year, a detection volume of 100 km 3 ice is needed. A larger detector requires a more efficient and less costly technology. Alternative options include radio and acoustic detection.

Neutrino interact in ice  showers Charge asymmetry: 20%-30% more electrons than positrons. Moliere Radius in Ice ~ 10 cm: This is a characteristic transverse dimension of EM showers. <<R Moliere (optical), random phases  P  N >>R Moliere (RF), coherent  P  N 2 Hadronic (initiated by all flavors) EM (initiated by an electron, from e ) 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

As the energy increases, the multiplicity of the shower increases and the charge asymmetry increases.  As the energy increases, mean free path of electrons is larger then atomic spacing (~1 PeV) (LPM effect).  Cross section for pair production and bremsstrahlung decreases  longer, lower multiplicity showers The Neutrino Energy threshold for LPM is different for Hadronic and for EM showers  Large multiplicity of hadronic showers. Showers from EeV hadrons have high multiplicity ~ particles.  Photons from short lived hadrons  Very few E>100 EeV neutrinos that initiate Hadronic showers will have LPM LPM effect Landau- Pomeranchuk- Migdal  In high energy, Hadronic showers dominate  Some flavor identification ability

Measurements of the Askaryan effect Typical pulse profile Strong <1ns pulse 200 V/m Simulated curve normalized to experimental results Expected shower profiled verified Expected polarization verified (100% linear) Coherence verified. New Results, for ANITA calibration – in Ice Salt Ice D.Salzberg, P. Gorham et al. Were preformed at SLAC (Saltzberg, Gorham et al ) on variety of mediums (sand, salt, ice) 3 Gev photons are dumped into target and produce EM showers. Array of antennas surrounding the target Measures the RF output Results: RF pulses were correlated with presence of shower

Why Ice? Why Radio? -Long attenuation - Radio ~1km -Optical attenuation in ice 100m -No scattering for Radio In ice. -A lot of it. -Free to use. -South pole is isolated. RF quiet. -Antennas are cheaper and more robust than PMTs. -No need to drill wide holes lower drilling cost of deployment w.r.t optical detectors ~10 23 eV optical Radio Acoustic Ice, no bubbles ( km) Ice, bubbles (0.9 km) Water (Baikal 1km) Effective Volume per Module (Km 3 ) Energy (eV) Astro-ph/ P.B.Price Effective volume per detector element for e induced cascades

IceCube Pressure vessel Connectors Mainboard DAQ Cables Holes ANITA LABRADOR chip: low power consumption low deadtime large bandwidth cold rated 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

Deployment in the coming season surface junction box Counting house Each unit is composed of : − 1 Digital Radio Module (DRM) – Electronics − 4 Antennas − 1 calibration units Signal conditioning and amplification happen at the front end, signal is digitized and triggers formed in DRM Co-Deployment on spare breakouts on IceCube cables (top/bottom) or on a special breakout Depth possibilities: −Top (1450 m) : Colder Ice, less volume −Bottom (2450 m) : Warmer Ice, more volume −Dust layer : less efficient spot for ~400nm RF attenuation is longer at colder ice Not to scale!

Deployment in the coming season Planning to deploy 4 units. with IceCube. Start mid December rd hole (1400m) 8 th hole (1400m) 9 th hole (250m) 10 th hole(1400m) 11 th hole(250m) spare IceCube Holes Map for

To antenna To antenna To antenna To surface To Calibration unit To antenna Shielding separates noisy components 6 Penetrators : 4 Antennas 1 Surface cable 1 Calibration unit TRACR Board Trigger Reduction and Comm for Radio Data processing, reduction, interface to MB ROBUST Board ReadOut Board UHF Sampling and Triggering Digitizer card SHORT Boards Surf High Occupancy RF Trigger Trigger banding MB (Mainboard) Communication, timing, connection to IC DAQ infrastructure, Digital Radio Module (DRM) Digital Optical Module (DOM)

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

TRACR DOM-MB Metal Plate Antennas DRM electronics ROBUST Dipole Antennas IceCube DOM 17 cm

Time Calibration QA Monitoring Control Time order Event Trigger Analysis Sat. Data 3.5 Kbytes 25 Hz 3.5 Kbytes 25 Hz 3.5 Kbytes 25 Hz DRM HUB time Data Decrease rates to fit data storage/satellite volume L3 - Data quality on surface (HUB) L4 - Send over satellite? Save to tapes? Decrease rates to fit surface cable: L0 - Single frequency band trigger (SHORT, ROBUST) L1 – Multiple bands and multiple antennas (ROBUST) L2 – Higher level analysis filter-FFT (TRACR) DRM Offline processor DAQ layout

Our Mission: Build intermediate detector with improved effective volume over RICE, using IceCube infrastructure Experiment new Antenna and electronic design Further map the south pole ice radio properties Check interference between IceCube and AURA Adapt form factors for narrower holes drilled exclusively for radio. Correlate events with RICE On the way to a super-duper-hybrid GZK neutrino detector

Picture by Mark Krasberg

Backup Slides

Askaryan Signal Cherenkov angle=55.8 o Electric Field angular distributionElectric Field frequency spectrum Astro-ph/ Alvarez-Muniz, Vazquez, Zas 1999

Askaryan Signal Cherenkov angle=55.8 o Electric Field angular distributionElectric Field frequency spectrum Astro-ph/ Alvarez-Muniz, Vazquez, Zas 1999

Excpected Signal surface generated event as measured by RICE detectors at different depths

a larger, more technologically sophisticated array is needed for a neutrino observation… current hardware too expensive to scale up made surveys of rf properties of the ice at the South Pole set most stringent limits on the neutrino flux from 10^16 to 10^18 eV set limits on low scale gravity, magnetic monopoles and other exotica Note: RICE uses a 95% C.L. upper limit See latest results astro-ph/ channels in depths 100m - 300m

2 GHz Measurements of the Askaryan effect Typical pulse profile Strong <1ns pulse

Measurements of the Askaryan effect SLAC T444 (2000) in sand Sand Filed strength measure by…. E= prop to shower E 