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

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 near Malargüe, Argentina 3000km 2  largest cosmic-ray experiment worldwide  energy range: E > 10 17 eV  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 3000km 2 other Auger detectors  sensitive on energy and X max  duty cyle ~100% 17km 2 2 Raphael Krause | RWTH Aachen University

AERA Radio Stations Log-Periodic Dipole Antenna (LPDA) Butterfly Antenna 1.47 m wifi communication 1.8 m 2.28 m 4.25 m GPS for timing solar powered electronics  NS and EW polarized antenna  antenna alignment: to magnetic north with precision < 1 °  bandwidth: 30 – 80 MHz 3 Raphael Krause | RWTH Aachen University  autonomous radio station

Aab et al., PRL 116 241101 (2016) Radio Energy Calibration Aab et al., PRD 93 122005 (2016)  LPDA stations  zenith angle < 55 °  coincidence with surface detector energy resolution: 17% 15.8 MeV 126 events 4 Raphael Krause | RWTH Aachen University

Independent Determination of Cosmic-Ray Energy Scale Measurement Theoretical calculation EM shower energy first principles classical electrodynamics A. Aab et al. detector response Glaser et al., JINST in press JCAP 09(2016)024 arXiv:1702.01392 E-field A. Aab. et al. atmosphere transparent PRL 116 241101 (2016) PRD 93 , 122005 (2016) to radio waves radiation energy per unit area 2-dim LDF model coincident measurement with other detectors 5 Raphael Krause | RWTH Aachen University

Independent Determination of Cosmic-Ray Energy Scale Measurement Theoretical calculation EM shower energy first principles classical electrodynamics A. Aab et al. detector response Glaser et al., JINST in press JCAP 09(2016)024 arXiv:1702.01392 E-field A. Aab. et al. atmosphere transparent PRL 116 241101 (2016) PRD 93 , 122005 (2016) to radio waves radiation energy per unit area 2-dim LDF model coincident measurement with other detectors 6 Raphael Krause | RWTH Aachen University  uncertainties of the energy scale?

Independent Determination of Cosmic-Ray Energy Scale Measurement Theoretical calculation EM shower energy first principles classical electrodynamics A. Aab et al. detector response Glaser et al., JINST in press JCAP 09(2016)024 arXiv:1702.01392 E-field A. Aab. et al. atmosphere transparent PRL 116 241101 (2016) PRD 93 , 122005 (2016) to radio waves radiation energy per unit area 2-dim LDF model coincident measurement with other detectors 7 Raphael Krause | RWTH Aachen University  uncertainties of the energy scale?

Detector Response Calibration P t G t P r  R: distance between both antennas  P r : receiving power  P t : injected power to trans. antenna 8 Raphael Krause | RWTH Aachen University  G t : directional pattern of trans. antenna

LPDA Response Pattern example of one single flight: combination of multiple flights:  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%  A. Aab et al.  overall uncertainty in median : JINST in press arXiv:1702.01392  |H Φ |: 7.4% |H θ |: 10.3% 9 Raphael Krause | RWTH Aachen University

Uncertainty of Energy Fluence  uncertainty of energy fluence due to LPDA calibration   systematic uncertainty: ~10% A. Aab et al. 10 Raphael Krause | RWTH Aachen University JINST in press arXiv:1702.01392

Independent Determination of Cosmic-Ray Energy Scale Measurement Theoretical calculation EM shower energy first principles classical electrodynamics A. Aab et al. detector response Glaser et al., JINST in press JCAP 09(2016)024 arXiv:1702.01392 E-field A. Aab. et al. atmosphere transparent PRL 116 241101 (2016) PRD 93 , 122005 (2016) to radio waves radiation energy per unit area 2-dim LDF model coincident measurement with other detectors 11 Raphael Krause | RWTH Aachen University

Theoretical Calculation of Radiation Energy  air shower simulations using CoREAS (CORSIKA 7.4) → more details: Glaser et al., JCAP 09(2016)024  radio energy estimator: geometry of radio emission air-density correction correction  quadratic relation:  scatter less than 3% 12 Raphael Krause | RWTH Aachen University

Uncertainties of Energy Scale using AERA experimental: theoretical calculation: classical electrodynamics detector response: ~10% → no free parameters signal chain: < 1% LDF model: 2.5% approximations made in simulation → small compared to exp.uncertainty environment: invisible energy: changing atmospheric conditions: 1% radio emission only from EM shower changing ground conditions: 1% correct for neutrinos and high-energy muons → uncertainty: 3% at 10 18 eV systematic uncertainty: comparable to fluorescence technique 13 Raphael Krause | RWTH Aachen University

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 (|H Φ | and |H θ |) 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 14 Raphael Krause | RWTH Aachen University

Backup 15 Raphael Krause | RWTH Aachen University

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  X max → composition 16 Raphael Krause | RWTH Aachen University

From Voltage To Cosmic-Ray Energy voltage [V] detector response electric field [V/m] time integral of Poynting vector radiation energy fluence [eV/m²] Fit 2D-LDF + spatial integral radiation energy per unit area radiation energy geometry correction of air shower [eV] 1/sin( α )² with α (v,B) cosmic-ray energy estimator 17 Raphael Krause | RWTH Aachen University

Emission Processes and Radiation Energy Fluence geomagnetic charge excess energy fluence radially polarized polarized into towards shower direction of axis Lorentz force 18 Raphael Krause | RWTH Aachen University

Vector Effective Length  H: relation of voltage to incoming e-field  horizontal antenna most sensitive to zenith direction 19 Raphael Krause | RWTH Aachen University

Measurement of |H φ | and |H θ | |H φ |: |H y |: |H z |: |H θ | = cos( θ )|H y | + sin( θ )|H z | 20 Raphael Krause | RWTH Aachen University

|H φ | - Reproducibility  multiple measurements performed at different days  measurements agree on a 6% level 21 Raphael Krause | RWTH Aachen University