Towards real-time cosmic-ray identification with the LOw Frequency ARay

The radio signals emitted by Extensive Air Showers have been successfully used for the last decade by LOFAR to reconstruct the properties of the primary cosmic rays. Since an effective real-time recognition system for the very short radio pulses is lacking, cosmic-ray acquisition is currently triggered by an external array of particle detector, called LORA, limiting the LOFAR collecting area to the area covered by LORA. A new algorithm for the real-time cosmic-ray detection has been developed for the LOFAR Low Band Antenna, which are sensitive between 10 and 90 MHz, and is here presented together with the latest results.

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ADVANCED DETECTION METHODS OF RADIO SIGNALS FROM COSMIC RAYS FOR KASCADE GRANDE AND AUGER

International Journal of Modern Physics A ◽

10.1142/s0217751x06033702 ◽

2006 ◽

Vol 21 (supp01) ◽

pp. 242-246 ◽

Cited By ~ 10

Author(s):

H. GEMMEKE ◽

W. D. APEL ◽

F. A. BADEA ◽

L. BÄHREN ◽

K. BEKK ◽

...

Keyword(s):

Cosmic Rays ◽

Low Frequency ◽

Extensive Air Showers ◽

Detection Methods ◽

Next Generation ◽

Air Showers ◽

Array Technology ◽

Radio Signals ◽

Radio Measurements ◽

Positive Results

The LOPES experiment (LOfar Prototype Station) has been built at the KASCADE-Grande experiment in order to test the LOFAR (LOw Frequency ARray) technology and demonstrate its capability for radio measurements in Extensive Air Showers (EAS). After the first positive results in the framework of the KASCADE-Grande experiment we developed the next generation of antennas, electronics, and trigger. The main new features are easy calibration of antennas with precise detection of polarization, and good capability of self-triggering. The results from this new design are under test in Karlsruhe. Furthermore the background situation was measured and analyzed.

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Atmospheric Monitoring at a Cosmic Ray Observatory - a long-lasting endeavour

EPJ Web of Conferences ◽

10.1051/epjconf/201919702001 ◽

2019 ◽

Vol 197 ◽

pp. 02001

Author(s):

Bianca Keilhauer

Keyword(s):

Cosmic Rays ◽

Cosmic Ray ◽

Extensive Air Showers ◽

Pierre Auger Observatory ◽

Ultrahigh Energy ◽

Atmospheric Conditions ◽

Air Showers ◽

Atmospheric Monitoring ◽

Surface Detector ◽

Planning And Construction

The Pierre Auger Observatory for detecting ultrahigh energy cosmic rays has been founded in 1999. After a main planning and construction phase of about five years, the regular data taking started in 2004, but it took another four years until the full surface detector array was deployed. In parallel to the main detectors of the Observatory, a comprehensive set of instruments for monitoring the atmospheric conditions above the array was developed and installed as varying atmospheric conditions influence the development and detection of extensive air showers. The multitude of atmospheric monitoring installations at the Pierre Auger Observatory will be presented as well as the challenges and efforts to run such instruments for several decades.

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ARIANNA: Measurement of cosmic rays with a radio neutrino detector in Antarctica

EPJ Web of Conferences ◽

10.1051/epjconf/201921602008 ◽

2019 ◽

Vol 216 ◽

pp. 02008 ◽

Cited By ~ 1

Author(s):

Christian Glaser

Keyword(s):

Cosmic Rays ◽

Cosmic Ray ◽

Cost Effective ◽

Neutrino Detector ◽

Air Showers ◽

Ice Shelf ◽

Ross Ice Shelf ◽

Radio Signals ◽

Single Detector ◽

The Antarctic

The ARIANNA detector aims to detect neutrinos with energies above 1016 eV by instrumenting 0.5 Teratons of ice with a surface array of a thousand independent radio detector stations in Antarctica. The Antarctic ice is transparent to the radio signals caused by the Askaryan effect which allows for a cost-effective instrumentation of large volumes. Several pilot stations are currently operating successfully at the Moore’s Bay site (Ross Ice Shelf) and at the South Pole. As the ARIANNA detector stations are positioned at the surface, the more abundant cosmic-ray air showers are also measured and serve as a direct way to prove the capabilities of the detector. We will present measured cosmic rays and will show how the incoming direction, polarization and electric field of the cosmicray pulse can be reconstructed from single detector stations comprising 4 upward and 4 downward facing LPDA antennas.

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