Presentation is loading. Please wait.

Presentation is loading. Please wait.

XXI èmes Rencontres de Blois Windows on the Universe Characteristics of high energy cosmic rays observed with CODALEMA : observed with CODALEMA : Evidence.

Published byErin Primrose Casey Modified over 8 years ago

Similar presentations

Presentation on theme: "XXI èmes Rencontres de Blois Windows on the Universe Characteristics of high energy cosmic rays observed with CODALEMA : observed with CODALEMA : Evidence."— Presentation transcript:

1 XXI èmes Rencontres de Blois Windows on the Universe Characteristics of high energy cosmic rays observed with CODALEMA : observed with CODALEMA : Evidence for a geomagnetic radio emission mechanism Evidence for a geomagnetic radio emission mechanism Olivier RAVEL SUBATECH, France CNRS/IN2P3, Université de Nantes, EMN Nantes XXIèmes Rencontres de Blois, Windows on the Universe

2 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 2 Radio detection & CODALEMA goals To measure the radio transient associated to the atmospheric shower produced by high energetic cosmic rays To understand the radio production mechanisms To determine key observables sensitive to the shower features and the primary cosmic particle To develop a detection technique competitive with conventional surface detectors in terms of : –Quality of data (sensitivity, resolution) –Efficiency and duty cycle –Simplicity, robustness and COST

3 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 3 EXPERIMENTAL SETUP (2008) 21 dipoles with EW polarization 3 dipoles with NS polarization 17 scintillators Trigger of the antenna array 2 detector arrays: Antenna array Scintillator array: Nancay Observatory

4 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 4 A dedicated LNA(ASIC) Aluminum dipole antenna CODALEMA active dipole Simple & cheap Low noise : sensitive to Galactic noise Wide bandwidth : 80 kHz à 230 MHz High dynamic Good linearity

5 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 5 Scintillator Detector Trigger rate: 1 evt/ 7 mins Energy threshold: 1.10 15 eV Informations on EAS: - Arrival direction - Shower core position - Energy estimate (CIC method) 2 different classes of trigger events (5 central stations in coincidence) : - Internal events: Station with the maximum signal is not on the edge of the array. Correct estimate of shower energy and core position. - External events: No estimation of shower energy and core position.

6 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 6 Voltage (v)Analysis: From raw signal to atmospheric shower… Raw signals : Full bandwidth Filtered signals Tagging Times, amplitudes triangulation Arrival directions Amplitudes Shower core position Lateral distribution Filtering Pulses determination CIC UHECR energy (30 %) Dipole Data Coincidences (SD and Antennas): angular difference < 20° time difference < 100 ns Well reconstructed cosmic ray shower Scintillator Data Data time x 10 -6 s Amplitude (V)

7 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 7 particle s radio Log 10 (E p ) Radio detection efficiency Number of events Log 10 (E p ) Energy distribution Efficiency 5. 10 16 eV Radiodetection threshold ~ 5.10 16 eV Particles threshold 10 15 eV Full efficiency reached above 10 18 eV Effective data taking time 659 days Trigger (SD events) 143795 Coincidences (SD and antennas) 1553 Coincidences (Internal) 450

8 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 8 Shower arrival direction Geomagnetic field axis - Large north/south asymmetry, relative deficit of events in the geomagnetic field axis area -For the scintillators, the azimutal acceptance is uniform North South EastWest North South EastWest Sky map Density map

9 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 9 A model to understand the asymmetry Hypothesis: - The electric field is proportional to the Lorentz force E  |v x B| -Charged particles in the shower are deflected by the geomagnetic field -Electric field polarization in the direction of the Lorentz force : a linear polarization is assumed E // to v x B -The number of count (ie the efficiency) depends on the electric field magnitude: a simple linear dependence is assumed  shower North South Geomagnetic field East

10 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 10 Projection on East-West axis (CODALEMA antenna polarization) Dipole pattern (EZNEC simulation) Trigger acceptance ( zenithal angle distribution ) vxB Model : Predicted density map Total Lorentz force (E  sin(α) ) X X

11 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 11 Carte de couverture prédite: Force de Lorentz totale (sin α) X X Lobe de l’antenne dipolaire (logiciel EZNEC) Acceptance du trigger particules (paramétrisation de la distribution en angle zénithal) X MODEL DATA North South EastWest North South East West MODEL vs DATA COMPARISON

12 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 12 MODEL – DATA COMPARISON Geomagnetic vxB model fits correctly experimental data: - in zenithal angle - in azimuthal angle (notably the local maximum in the South direction) data vxB model data vxB model Published in Astroparticle Physics 31 (2009) 192–200.

13 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 13 Is the vxB model valid for the NS polarization ? 3 NS antenna in the array Most of the events are coming from East and West directions Data Model AzimuthZenith The statistic is lower but at the first look : YES

14 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 14 Pulse polarity The model assumes the electric field magnitude to be proportional to |(vxB) EW |. Is the signal polarity given by (vxB) EW ? Model Data tags are signed filtered dipole Signal : tags are signed given by the most numerous signed tags Event sign : given by the most numerous signed tags Positive Negative + - NS polarization Data Model EW polarization

15 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 15 -East/West asymmetry is well interpreted with the (v x B) model - Good agreement for North/ South polarization despite low statistic - Good agreement on the event pulse polarity Conclusion CODALEMA data demonstrate that the geomagnetic field is at the origin of the electric field radio detected by antennas

16 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 16 Perspectives : Physics objectives What is the geomagnetic mechanism involved in the emission process ? - geosynchrotron model (Huege and Falcke, 2000) ? - transversal current model (Lasty, Scholten and Werner, 2005) ? E field footprint Geosynchrotron Model - Field amplitude and primary energy correlation (partially done in the T.Saugrin Thesis, Univ Nantes 2008, publication under preparation) - Determination of the primary CR nature ? one way : study of the field polarization => Antenna with EW & NS polar

17 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 17 Perspectives GPS butterfly antennas, dual polar CODALEMA autonomous station ADC+trigger+power+OnboardPC Installation of autonomous station in the current array for testing and debugging Foreseen array of new stations at Nançay Extension of the current array –Higher antenna density at the center –Extension at larger scales (~1 Km 2 ) Installation for tests in Argentina. Participation at the AERA Project (AUGER)

18 XXI èmes Rencontres de Blois Windows on the Universe 24/06/2009Olivier RAVEL, SUBATECH Blois 09 18 Subatech Nantes ESEO Angers LPCE Orléans Observatory Paris-Meudon LAL Orsay LPSC Grenoble LAOB Besançon ObservatoryNançay COsmic ray Detection Detection Array with Array with Logarithmic Logarithmic Electro Electro Magnetic Magnetic Antennas Antennas CODALEMA The CODALEMA collaboration 8 French laboratories (IN2P3 and INSU) 1 experimental site

Download ppt "XXI èmes Rencontres de Blois Windows on the Universe Characteristics of high energy cosmic rays observed with CODALEMA : observed with CODALEMA : Evidence."

Similar presentations

Antonis Leisos KM3NeT Collaboration Meeting the calibration principle using atmospheric showers the calibration principle using atmospheric showers Monte.

Antonis Leisos KM3NeT Collaboration Meeting the calibration principle using atmospheric showers the calibration principle using atmospheric showers Monte.
The Tianshan Radio Experiment for Neutrino Detection Genesis & status of the TREND project Autonomous radio-detection of air showers.

The Tianshan Radio Experiment for Neutrino Detection Genesis & status of the TREND project Autonomous radio-detection of air showers.
Results from the Telescope Array experiment H. Tokuno Tokyo Tech The Telescope Array Collaboration 1.

Results from the Telescope Array experiment H. Tokuno Tokyo Tech The Telescope Array Collaboration 1.
Use of floating surface detector stations for the calibration of a deep-sea neutrino telescope G. Bourlis, N. A. B. Gizani, A. Leisos, A. G. Tsirigotis,

Use of floating surface detector stations for the calibration of a deep-sea neutrino telescope G. Bourlis, N. A. B. Gizani, A. Leisos, A. G. Tsirigotis,
Milky Way over 21CM array (Gu Junhua) The Tianshan Radio Experiment for Neutrino Detection Olivier Martineau-Huynh NAOC G&C lunch talk May 28, 2014.

Milky Way over 21CM array (Gu Junhua) The Tianshan Radio Experiment for Neutrino Detection Olivier Martineau-Huynh NAOC G&C lunch talk May 28, 2014.
The GRAND proto A prototype array to evaluate the potential of EAS identification of the radio technique.

The GRAND proto A prototype array to evaluate the potential of EAS identification of the radio technique.
10 th PISA meeting on Advanced Detectors, May 21-27 2006 The knowledge of the amplitude leads to the Energy of the primary cosmic ray The Knowledge of.

10 th PISA meeting on Advanced Detectors, May The knowledge of the amplitude leads to the Energy of the primary cosmic ray The Knowledge of.
The Pierre Auger Observatory Nicolás G. Busca Fermilab-University of Chicago FNAL User’s Meeting, May 2006.

The Pierre Auger Observatory Nicolás G. Busca Fermilab-University of Chicago FNAL User’s Meeting, May 2006.
March 2005E. Armengaud - Moriond Search methods for UHECR anisotropies within the Pierre Auger Observatory Eric Armengaud (APC/IAP - Paris) for the Auger.

March 2005E. Armengaud - Moriond Search methods for UHECR anisotropies within the Pierre Auger Observatory Eric Armengaud (APC/IAP - Paris) for the Auger.
George W.S. Hou & M.A. Huang Center for Cosmology and Particle Astrophysics Department of Physics, National Taiwan University, 1, Sec. 4, Roosevelt Rd.,Taipei,

George W.S. Hou & M.A. Huang Center for Cosmology and Particle Astrophysics Department of Physics, National Taiwan University, 1, Sec. 4, Roosevelt Rd.,Taipei,
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:

A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:
The Highest Energy Cosmic Rays Two Large Air Shower Detectors

The Highest Energy Cosmic Rays Two Large Air Shower Detectors
June 29-July 2, 2010, Nantes, France Didier Charrier, Subatech, Nantes, France “ Antenna development for astroparticles.

June 29-July 2, 2010, Nantes, France Didier Charrier, Subatech, Nantes, France “ Antenna development for astroparticles.
Radio Detection of High Energy Cosmic Ray Air Showers A short review XX th RENCONTRES DE BLOIS 18th - 23rd May 2008 “Challenges in Particle Astrophysics”

Radio Detection of High Energy Cosmic Ray Air Showers A short review XX th RENCONTRES DE BLOIS 18th - 23rd May 2008 “Challenges in Particle Astrophysics”
RADAR Detection of Extensive Air Showers Nils Scharf III. Physikalisches Institut A Bad Honnef31.08.2007 Nils Scharf III. Physikalisches Institut A Bad.

RADAR Detection of Extensive Air Showers Nils Scharf III. Physikalisches Institut A Bad Honnef Nils Scharf III. Physikalisches Institut A Bad.
Sky noise measurements with a dual polarization active dipole antenna WORKSHOP January 14 and 15 2008, subatech Nantes Didier CHARRIER Subatech,

Sky noise measurements with a dual polarization active dipole antenna WORKSHOP January 14 and , subatech Nantes Didier CHARRIER Subatech,
Andreas Horneffer for the LOPES Collaboration Detecting Radio Pulses from Air Showers with LOPES.

Andreas Horneffer for the LOPES Collaboration Detecting Radio Pulses from Air Showers with LOPES.
X.-X. Li, H.-H. He, F.-R. Zhu, S.-Z. Chen on behalf of the ARGO-YBJ collaboration Institute of High Energy Physics 2008.06.27 2008 Nanjing GRB Conference,Nanjing,

X.-X. Li, H.-H. He, F.-R. Zhu, S.-Z. Chen on behalf of the ARGO-YBJ collaboration Institute of High Energy Physics Nanjing GRB Conference,Nanjing,
Measurement of the UHECR energy spectrum from hybrid data of the Pierre Auger Observatory Presenter: Lorenzo Perrone Università del Salento and INFN Lecce.

Measurement of the UHECR energy spectrum from hybrid data of the Pierre Auger Observatory Presenter: Lorenzo Perrone Università del Salento and INFN Lecce.
Preliminary MC study on the GRAND prototype scintillator array Feng Zhaoyang Institute of High Energy Physics, CAS, China GRAND Workshop, Paris, Feb. 015.

Preliminary MC study on the GRAND prototype scintillator array Feng Zhaoyang Institute of High Energy Physics, CAS, China GRAND Workshop, Paris, Feb. 015.

Similar presentations

Ads by Google