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A New Method to Determine the Energy Scale for High-Energy Cosmic - - PowerPoint PPT Presentation

Jul 29, 2023 99 likes •324 views

A New Method to Determine the Energy Scale for High-Energy Cosmic Rays Using Radio Measurements at the Pierre Auger Observatory Raphael Krause for the Pierre Auger Collaboration ICRC 2017 Busan, South Korea Pierre Auger Observatory located

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Raphael Krause for the Pierre Auger Collaboration ICRC 2017 Busan, South Korea

A New Method to Determine the Energy Scale for High-Energy Cosmic Rays Using Radio Measurements at the Pierre Auger Observatory

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Raphael Krause | RWTH Aachen University

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3000km2

Pierre Auger Observatory

3000km 2 17km 2

  • located near Malargüe, Argentina
  • largest cosmic-ray experiment worldwide
  • energy range: E > 1017eV
  • baseline detector:

1660 surface detectors (SD) 27 fluorescence detectors (FD) 153 radio stations (AERA)

  • Auger Engineering Radio Array

largest cosmic-ray radio detector in coincidence with

  • ther Auger detectors

sensitive on energy and Xmax duty cyle ~100%

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Raphael Krause | RWTH Aachen University

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AERA Radio Stations

solar powered GPS for timing wifi communication 1.47 m 4.25 m 1.8 m 2.28 m electronics

  • NS and EW polarized antenna
  • antenna alignment:

to magnetic north with precision < 1°

  • bandwidth: 30 – 80 MHz
  • autonomous radio station

Log-Periodic Dipole Antenna (LPDA) Butterfly Antenna

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Raphael Krause | RWTH Aachen University

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Radio Energy Calibration

  • zenith angle < 55°

energy resolution: 17%

15.8 MeV

  • LPDA stations
  • coincidence with surface detector

126 events

Aab et al., PRL 116 241101 (2016) Aab et al., PRD 93 122005 (2016)

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Raphael Krause | RWTH Aachen University

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E-field 2-dim LDF model radiation energy per unit area atmosphere transparent to radio waves first principles classical electrodynamics

Theoretical calculation Measurement

EM shower energy

Independent Determination of Cosmic-Ray Energy Scale

coincident measurement with other detectors

  • A. Aab. et al.

PRL 116 241101 (2016) PRD 93, 122005 (2016)

Glaser et al., JCAP 09(2016)024

  • A. Aab et al.

JINST in press arXiv:1702.01392

detector response

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Raphael Krause | RWTH Aachen University

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E-field 2-dim LDF model radiation energy per unit area atmosphere transparent to radio waves

Theoretical calculation Measurement

EM shower energy

Independent Determination of Cosmic-Ray Energy Scale

coincident measurement with other detectors

  • A. Aab. et al.

PRL 116 241101 (2016) PRD 93, 122005 (2016)

Glaser et al., JCAP 09(2016)024

detector response

  • uncertainties of the energy scale?

first principles classical electrodynamics

  • A. Aab et al.

JINST in press arXiv:1702.01392

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Raphael Krause | RWTH Aachen University

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E-field 2-dim LDF model radiation energy per unit area atmosphere transparent to radio waves

Theoretical calculation Measurement

detector response EM shower energy

Independent Determination of Cosmic-Ray Energy Scale

coincident measurement with other detectors

  • A. Aab. et al.

PRL 116 241101 (2016) PRD 93, 122005 (2016)

Glaser et al., JCAP 09(2016)024

  • uncertainties of the energy scale?

first principles classical electrodynamics

  • A. Aab et al.

JINST in press arXiv:1702.01392

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SLIDE 8

Raphael Krause | RWTH Aachen University

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Detector Response Calibration

  • R: distance between both antennas
  • Pr : receiving power
  • Pt : injected power to trans. antenna
  • Gt: directional pattern of trans. antenna

Gt Pt Pr

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Raphael Krause | RWTH Aachen University

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LPDA Response Pattern

  • overall uncertainty in median:

|HΦ|: 7.4% |Hθ|: 10.3%

  • flight-dependent uncertainties:

 trans. antenna position: 1.5%  signal generator stability: 2.9%  receving power: 5.8%

  • global uncertainties:

 injected power: 2.5%  transmitting antenna gain: 5.8%

combination of multiple flights: example of one single flight:

  • A. Aab et al.

JINST in press arXiv:1702.01392

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Raphael Krause | RWTH Aachen University

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Uncertainty of Energy Fluence

  • uncertainty of energy fluence due to LPDA calibration
  • systematic uncertainty: ~10%
  • A. Aab et al.

JINST in press arXiv:1702.01392

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Raphael Krause | RWTH Aachen University

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E-field 2-dim LDF model radiation energy per unit area atmosphere transparent to radio waves

Theoretical calculation Measurement

detector response EM shower energy

Independent Determination of Cosmic-Ray Energy Scale

coincident measurement with other detectors

  • A. Aab. et al.

PRL 116 241101 (2016) PRD 93, 122005 (2016)

Glaser et al., JCAP 09(2016)024

first principles classical electrodynamics

  • A. Aab et al.

JINST in press arXiv:1702.01392

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Raphael Krause | RWTH Aachen University

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Theoretical Calculation of Radiation Energy

  • air shower simulations using CoREAS (CORSIKA 7.4)
  • radio energy estimator:
  • quadratic relation:
  • scatter less than 3%

→ more details: Glaser et al., JCAP 09(2016)024

air-density correction

geometry of radio emission correction

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SLIDE 13

Raphael Krause | RWTH Aachen University

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Uncertainties of Energy Scale using AERA

systematic uncertainty: comparable to fluorescence technique

experimental:

detector response: ~10% signal chain: < 1% LDF model: 2.5%

theoretical calculation:

classical electrodynamics → no free parameters approximations made in simulation → small compared to exp.uncertainty

environment:

changing atmospheric conditions: 1% changing ground conditions: 1%

invisible energy:

radio emission only from EM shower correct for neutrinos and high-energy muons → uncertainty: 3% at 1018 eV

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Raphael Krause | RWTH Aachen University

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Summary

  • Pierre Auger Observatory

 well calibrated environment for development of future detector technologies

  • Auger Engineering Radio Array (AERA)

 largest experiment to measure radio emission of extensive air showers

  • AERA calibration:

 measurement of the LPDA response (|HΦ| and |Hθ|) using an octocopter  systematic uncertainty: ~10%

  • independent determination of energy scale from first principles

 detector response identified as dominant uncertainty  systematic uncertainty: comparable to fluorescence technique

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Raphael Krause | RWTH Aachen University

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Backup

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Raphael Krause | RWTH Aachen University

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Scientific Objective of AERA

  • proof of principle:

explore optimal setup for cosmic-ray measurements using a radio detector (R&D, antenna type, grid spacing) trigger (self-trigger, external trigger, hybrid detector)

  • investigation of EM shower development

first principles of classical electrodynamics

  • determine cosmic-ray properties

arrival direction energy Xmax → composition

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Raphael Krause | RWTH Aachen University

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From Voltage To Cosmic-Ray Energy

voltage [V] electric field [V/m] radiation energy fluence [eV/m²] radiation energy

  • f air shower [eV]

cosmic-ray energy estimator

detector response time integral of Poynting vector Fit 2D-LDF + spatial integral geometry correction 1/sin(α)² with α (v,B) radiation energy per unit area

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Raphael Krause | RWTH Aachen University

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Emission Processes and Radiation Energy Fluence

polarized into direction of Lorentz force radially polarized towards shower axis

energy fluence

geomagnetic charge excess

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Raphael Krause | RWTH Aachen University

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  • H: relation of voltage to incoming e-field
  • horizontal antenna most sensitive to zenith direction

Vector Effective Length

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Raphael Krause | RWTH Aachen University

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Measurement of |Hφ| and |Hθ| |Hφ|: |Hy|: |Hz|: |Hθ| = cos(θ)|Hy| + sin(θ)|Hz|

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Raphael Krause | RWTH Aachen University

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|Hφ| - Reproducibility

  • multiple measurements performed at different days
  • measurements agree on a 6% level