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 D. Seckel, Univ. of Delaware

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Topics Concept: –A source to test radio techniques –CR composition ? (not today) 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 (not today) Detection –IceCube: shallow array, AURA –ANITA (not today)

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Theorist’s view of the UHE neutrino sky

Askaryan pulses from air shower cores, UMD Radio Mtg., June (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, UMD Radio Mtg., June (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, UMD Radio Mtg., June (Seckel) Askaryan pulses from air shower core

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Critical dimensions

Askaryan pulses from air shower cores, UMD Radio Mtg., June (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, UMD Radio Mtg., June (Seckel) Ground level particles (above 10 GeV)  e-e-   n,p Radiation fraction increases with primary energy

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Radial distributions by particle ID radiating mesons baryons muons

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) E vs r (AIRES)

Askaryan pulses from air shower cores, UMD Radio Mtg., June (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, UMD Radio Mtg., June (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, UMD Radio Mtg., June (Seckel) RF: (E p = 1 EeV, E cut = 1 TeV )

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) RF Cerenkov Rings

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) RF vs Core Size – (old)

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Characterization of Air Showers 40 10PeV Vertical CORSIKA showers. Hadrons cut. Looked at RF pattern on vertical string of 10 detectors every 10m starting at 200m deep, 150m from shower. A look at waveforms from single 1PeV and 10PeV events. Peaks taken from 10PeV waveforms to determine Cherenkov radiation pattern. Justification for raising the energy cuts.

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) 10PeV Waveforms on string

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Depth Profiles and Energy Cuts Waveform peaks at depth for 40 10PeV showers. Peak vmax values at different energy cuts.

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) RF vs core energy

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Parameterize Air Showers Use shower radius (R), shower length (L) and shower size (S) to fit shower radiation patterns. Peaks match up with some variation at the tails. Five event RF detection patterns (solid) with their parameterizations (dashed).

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Event Rate Calculation

Askaryan pulses from air shower cores, UMD Radio Mtg., June (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, UMD Radio Mtg., June (Seckel) AURA geometry

Askaryan pulses from air shower cores, UMD Radio Mtg., June (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, UMD Radio Mtg., June (Seckel) END

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Radial distributions by energy

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Sample the Cerenkov Ring

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Subshowers & Coherence of RF pulses

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) Comparison of Fe/p

Askaryan pulses from air shower cores, UMD Radio Mtg., June (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, UMD Radio Mtg., June (Seckel) Time Domain Waveforms

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) EeV/TeV again

Askaryan pulses from air shower cores, UMD Radio Mtg., June (Seckel) 1PeV Waveforms on String