July 10, 2007 Detection of Askaryan radio pulses produced by cores of air showers. Suruj Seunarine, Amir Javaid, David Seckel, Philip Wahrlich, John Clem.

Slides:

Advertisements

Similar presentations

TIERRAS: an AIRES package to simulate high energy cosmic ray showers underground and underwater Matías Tueros Instituto de Física La Plata – Universidad.

Advertisements

Ultrahigh Energy Cosmic Ray Nuclei and Neutrinos

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.

Radio detection of UHE neutrinos E. Zas, USC Leeds July 23 rd 2004.

TeVPA, July , SLAC 1 Cosmic rays at the knee and above with IceTop and IceCube Serap Tilav for The IceCube Collaboration South Pole 4 Feb 2009.

The presence of the South Pole Air Shower Experiment (SPASE) on the surface provides a set of externally tagged muon bundles that can be measured by AMANDA.

Sean Grullon For the IceCube Collaboration Searching for High Energy Diffuse Astrophysical Neutrinos with IceCube TeV Particle Astrophysics 2009 Stanford.

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.

Search for Extremely-high Energy Cosmic Neutrino with IceCube Chiba Univ. Mio Ono.

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.

Apr 9, 2005 Scaling of Askaryan Pulses D. Seckel, Univ. of Delaware.

IAU Sydney Per Olof Hulth Particle Astronomy from Antarctica Per Olof Hulth Stockholm University.

MP BACH MultiPixel Balloon-borne Air CHerenkov Detection of Iron Cosmic Rays Using Direct Cherenkov Radiation Imaged with a High Resolution Camera University.

David Seckel, Radio Detection of Astrophysical Neutrinos, Karlsruhe, Oct. 14, 2003 Radio Detection of Astrophysical Neutrinos David Seckel University of.

EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara for the IceCube collaboration Chiba University.

10 18 eV Neutrinos associated with UHECR (>10 19 eV) sources Zhuo Li ( 黎卓 ) Peking University, Beijing Collaborators: Eli Waxman & Liming Song Li & Waxman,

Simulation Issues for Radio Detection in Ice and Salt Amy Connolly UCLA May 18 th, 2005.

Exploring the Cosmos with Neutrinos Aart Heijboer …all of them. nm

Steps towards a cosmogenic neutrino detector at the South Pole Summary of meeting on Sep 14 Opportunities - outer ring extension Acoustic & Radio technique,

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

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.

Contributions of the University of Bucharest to the study of high energy cosmic rays in the framework of the KASCADE-Grande experiment Octavian Sima Faculty.

Low frequency radio- emission associated with UHE cosmic rays KALYANEE BORUAH Physics Department, Gauhati University.

SEARCHING FOR A DIFFUSE FLUX OF ULTRA HIGH-ENERGY EXTRATERRESTRIAL NEUTRINOS WITH ICECUBE Henrik Johansson, for the IceCube collaboration LLWI H.

UCL Xmas 2006 : Dec 18 1 From the Tevatron to the Zevatron Mark Lancaster Simon Bevan, Amy Connolly, Ryan Nichol, Dave Waters.

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.

1 Cosmic Rays in IceCube: Composition-Sensitive Observables Chihwa Song a, Peter Niessen b, Katherine Rawlins c for the IceCube collaboration a University.

Detection of UHE Shower Cores by ANITA By Amir Javaid University Of Delaware.

Laboratory Particle- Astrophysics P. Sokolsky High Energy Astrophysics Institute, Univ. of Utah.

APRIM Chiang Mai July 28, 2011 Heliospheric Physics with IceTop Paul Evenson University of Delaware Department of Physics and Astronomy.

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.

“The Cosmic Ray composition in the knee region and the hadronic interaction models” G. Navarra INFN and University, Torino, Italy For the EAS-TOP Collaboration.

ANtarctic Impulsive Transient Antenna University of Hawaii at Manoa Peter Gorham, PI John Learned and Gary S. Varner Ohio-State University Jim Beatty and.

School of Cosmic-ray Astrophysics, Erice, July 4, 2004 Thomas K. Gaisser Role of particle interactions in high-energy astrophysics Uncorrelated fluxes.

Detection of UHE Shower Cores by ANITA By Amir Javaid University Of Delaware.

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.

Steps towards a cosmogenic neutrino detector at the South Pole Summary of meeting on Sep 14 Opportunities - outer ring extension Acoustic & Radio technique,

Physical Description of IceTop 3 Nov IceTop Internal Review Madison, November 3-4, 2010 Physical Description of IceTop Paul Evenson, University.

RICE: ICRC 2001, Aug 13, Recent Results from RICE Analysis of August 2000 Data See also: HE228: Ice Properties (contribution) HE241: Shower Simulation.

Study of VHE Cosmic Ray Spectrum by means of Muon Density Measurements at Ground Level I.I. Yashin Moscow Engineering Physics Institute,

What we do know about cosmic rays at energies above eV? A.A.Petrukhin Contents 4 th Round Table, December , Introduction. 2. How these.

Studies of Askaryan Effect, 1 of 18 Status and Outlook of Experimental Studies of Askaryan RF Radiation Predrag Miocinovic (U. Hawaii) David Saltzberg.

25 June, 2006 UHE Neutrinos: II D. Seckel, Univ. of Delaware.

South Pole Astro April 4, 2011 Tom Gaisser1 125 m Cosmic-ray physics with IceCube IceTop is the surface component of IceCube as a three-dimensional cosmic-ray.

31/03/2008Lancaster University1 Ultra-High-Energy Neutrino Astronomy From Simon Bevan University College London.

NEVOD-DECOR experiment: results and future A.A.Petrukhin for Russian-Italian Collaboration Contents MSU, May 16, New method of EAS investigations.

June 19, 2009 Simulation of Askaryan Detectors and Events (SADE) David Seckel, Pat Stengel, Shahid Hussain D. Seckel, Univ. of Delaware.

IceTop Design: 1 David Seckel – 3/11/2002 Berkeley, CA IceTop Overview David Seckel IceTop Group University of Delaware.

The Large High Altitude Air Shower Observatory LHAASO.

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.

Lingling Ma IHEP China Measurement of Cosmic rays with LHAASO at 10PeV~100PeV 4th Workshop on Air Shower Detection at High Altitude Institute of High Energy.

Near-Field Effects of Cherenkov Radiation Induced by Ultra High Energy Cosmic Neutrinos Chih‐Ching Chen Collaboration with Chia-Yu Hu and Pisin Chen LeCosPA.

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.

EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara Chiba University.

Bergische Universität Wuppertal Jan Auffenberg et al. Rome, Arena ARENA 2008 A radio air shower detector to extend IceCube ● Three component air.

SADE ANITA Monte Carlo(SAM) Test Results Amir Javaid University of Delaware.

SADE ANITA Monte Carlo(SAM) Test Results Amir Javaid University of Delaware.

L.L.Ma for LHAASO collaboration Beijing China

Expectation of Cosmic Ray Energy Spectrum with LHAASO

D. Seckel, Univ. of Delaware

Karen Andeena, Katherine Rawlinsb, Chihwa Song*a

Presentation transcript:

July 10, 2007 Detection of Askaryan radio pulses produced by cores of air showers. Suruj Seunarine, Amir Javaid, David Seckel, Philip Wahrlich, John Clem D. Seckel, Univ. of Delaware

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Topics Concept: –A source to test radio techniques –CR composition ? Askaryan pulses & air shower dimensions Air shower properties (AIRES & CORSIKA) –Particle content –Radial and energy distributions Calculation of RF signal –Coherent addition of subshowers –Issues: near zone/far zone, ray tracing Composition studies Detection –IceCube: shallow array, AURA –ANITA

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Theorist’s view of the UHE neutrino sky

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Recall how radio works 5 m 10 cm JC, SY: “How do you know when you haven’t seen anything?”

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Radio Goals & Staging 100 events/yr above eV >1000 km 3 sr Validation of design for field work Prototype projects – more than upper limits Detect Air Showers: Signal/Background/Calib

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Askaryan pulses from air shower core

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Critical dimensions

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) High energy ground level particles at SP CORSIKA/AIRES –Primary energy: 1,10,100,1000 PeV –Cutoff: 1,10,100,1000 GeV –Compositionp & Fe Explore –Particle content rad - meson - baryon - mu –Radial profilesE sh vs r –Shower development dN/dE, ancestry

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Ground level particles  e-e-   n,p

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Radial distributions by particle ID radiating mesons baryons muons

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) E vs r (AIRES)

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) E vs r (CORSIKA) Fraction of available energy approaches 10% by 100 PeV Scaling allows use of high cutoff

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Synthesis of Askaryan pulses Many ground level particles –Superposition Individual RF pulses –Event: (id, t e, x e, n, E) –SubShower:(t s, x s, n, (r,l,s)) –Resolve geometry to antenna –Launch EM pulse(scaled AVZ) –Propagation effects (1/r, attenuation) –Adjust phase to common time basis Response –CoAdd spectra(t, n, pol, (complex spectrum)) –Antenna/DAQ

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Subshowers & Coherence of RF pulses

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Time Domain Waveforms

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) RF: (E p = 1 EeV, E cut = 1 TeV )

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) EeV/TeV again

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) RF Cerenkov Rings

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) RF vs Core Size

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Determining Cosmic Ray Composition AIRES showers (from S. Seunarine) E sh (r<20 cm) as proxy for radio High-lite: 10 PeV, True iron

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Comparison of Fe/p

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Scaling & Rates Rate independent of D Threshold increases with D True for E -3 –But not for E -2 Rate for 3PeV = 1/hour

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Shallow Array Concepts Drill 16 x 30m holes –1 dom per hole –4 antennas per dom 2 x 50m cables to each of four nearby strings & SJB 2 doms per cable

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) AURA geometry

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) ANITA (A. Javaid) Rate –A  km 2 sr – 1400/day E>10 19 – ? /dayE>10 20 High, Thin, Ice

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Summary Test beam for radio sure would be nice Air Shower Cores: E eff ~ 10% E p (at EeV) Synthetic RF looks usable CR Composition Measurement –Core energy anti-correlated with deep-  –p-Fe separation Three scenarios –Small subsurface array w/IceTop –AURA –ANITA

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) END

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Radial distributions by energy

Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) Sample the Cerenkov Ring