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Heat – a Low Energy Enhancement of the Pierre Auger Observatory : Volume 7, Issue 2 (19/05/2011)

By C. Meurer1 and N. Scharf1 on Behalf of the Pierre Auger Collaboration2,*

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Book Id: WPLBN0003993056
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Reproduction Date: 2015

Title: Heat – a Low Energy Enhancement of the Pierre Auger Observatory : Volume 7, Issue 2 (19/05/2011)  
Author: C. Meurer1 and N. Scharf1 on Behalf of the Pierre Auger Collaboration2,*
Volume: Vol. 7, Issue 2
Language: English
Subject: Science, Astrophysics, Space
Collections: Periodicals: Journal and Magazine Collection (Contemporary), Copernicus GmbH
Historic
Publication Date:
2011
Publisher: Copernicus Gmbh, Göttingen, Germany
Member Page: Copernicus Publications

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Meurer&Lt, C., Sup&Gt,, 1&Lt,, /Sup&Gt,, Scharf&Lt, A. N., Sup&Gt,,.../Sup&Gt,. (2011). Heat – a Low Energy Enhancement of the Pierre Auger Observatory : Volume 7, Issue 2 (19/05/2011). Retrieved from http://new.worldlibrary.net/


Description
Description: RWTH Aachen University, III. Physikalisches Institut A, Aachen, Germany. The High Elevation Auger Telescopes (HEAT) are three tiltable fluorescence telescopes which represent a low energy enhancement of the fluorescence telescope system of the southern site of the Pierre Auger Observatory in Argentina.

The Pierre Auger Observatory is a hybrid cosmic ray detector consisting of 24 fluorescence telescopes to measure the fluorescence light of extensive air showers complemented by 1600 water Cherenkov detectors to determine the particle densities at ground. In this configuration air showers with a primary energy of 1018 eV and above are investigated.

By lowering the energy threshold by approximately one order of magnitude down to a primary energy of 1017 eV, HEAT provides the possibility to study the cosmic ray energy spectrum and mass composition in a very interesting energy range, where the transition from galactic to extragalactic cosmic rays is expected to happen.

The installation of HEAT was finished in 2009 and data have been taken continuously since September 2009. Within these proceedings the HEAT concept is presented. First data already demonstrate the excellent complement of the standard Auger fluorescence telescopes by HEAT.


Summary
HEAT – a low energy enhancement of the Pierre Auger Observatory

Excerpt
Abbasi, R. U., Abu-Zayyad,T., Allen, M. et al. [HiRes]: First Observation of the Greisen-Zatsepin-Kuzmin Suppression, Phys. Rev. Lett., 100, 101101-1 - 101101-5, 2008.; Abraham, J., Abreu, P., Aglietta, M. et al. [The Pierre Auger Collaboration]: Measurement of the energy spectrum of cosmic rays above 1018 eV using the Pierre Auger Observatory, Phys. Lett. B, 685, 239-246, 2010a.; Antoni, T., Apel, W. D., Badea, F. et al. [KASCADE]: The Cosmic-Ray Experiment KASCADE, Nucl. Instrum. Meth. A, 513, 490-510, 2003.; Abraham, J., Abreu, P., Aglietta, M. et al. [The Pierre Auger Collaboration]: Measurement of the Depth of Maximum of Extensive Air Showers above 1018{eV}, Phys. Rev. Lett. 104, 091101-1 - 091101-7, 2010b.; Abraham, J., Abreu, P., Aglietta, M. et al. [The Pierre Auger Collaboration]: The Fluorescence Detector of the Pierre Auger Observatory, Nucl. Instrum. Meth. A 620, 227-251, 2010c.; Antoni, T., Apel, W. D., Badea, A. F. et al. [KASCADE]: KASCADE measurements of energy spectra for elemental groups of cosmic rays: Results and open problems, Astropart. Phys. 24, 1-25, 2005.; Bertaina, M. for the KASCADE Grande Coll.: The all particle energy spectrum of KASCADE-Grande in the energy region $10^{16} - 1018}$}{eV} by means of the $N_{\textrm{ch - N_\mu$ technique, Proc. 31th Int. Cosmic Ray Conf., 2009. %15-18; Blümer, J., Engel, R. and Hörandel J.: Cosmic rays from the knee to the highest energies, Prog. in Part. and Nucl. Phys. 63, 293-338, 2009.; Heitler, W.: The Quantum Theory of Radiation, Oxford University Press, 3rd edition, 1954.; Kleifges, M. for the Pierre Auger Coll.: Extension of the Pierre Auger Observatory using high-elevation fluorescence telescopes (HEAT), Proc. 31th Int. Cosmic Ray Conf., 2009.; Matthews, J.: A Heitler model of extensive air showers, Astropart. Phys. 22, 387-397, 2005.

 

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