DOCSLIB.ORG

Study for the Wide-Angle Air Cherenkov Detector Hiscore and Time Gradient Event Reconstruction for the H.E.S.S

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Study for the Wide-Angle Air Cherenkov Detector Hiscore and Time Gradient Event Reconstruction for the H.E.S.S Study for the wide-angle air Cherenkov detector HiSCORE and time gradient event reconstruction for the H.E.S.S. experiment Dissertation zur Erlangung des Doktorgrades des Department Physik der Universitat¨ Hamburg vorgelegt von Daniel Hampf aus Recife (Brasilien) Hamburg 2012 Gutachter der Dissertation: Prof. Dr. Dieter Horns Prof. Dr. Bruce Dawson Gutachter der Disputation: Prof. Dr. Erika Garutti Dr. Axel Lindner Datum der Disputation: 22.05.2012 Vorsitzender des Prufungsausschusses:¨ Dr. Georg Steinbruck¨ Vorsitzender des Promotionsausschusses: Prof. Dr. Peter Hauschildt Dekan der MIN Fakultat:¨ Prof. Dr. Heinrich Graener If I can see any further, it is only because I am standing on the shoulders of giants. after Bernard of Chartres Dedicated to the memory of the countless men and women who throughout the centuries have devoted their lives to the quest for truth, the advancement of reason and the fight against ignorance. Only the pursuit of enlightenment has enabled humankind to rise above the received conventions of existence, into the boundless space of intellect. Abstract This thesis presents efforts to extend the range of astronomical gamma-ray observations to the ultra high en- ergy regime, i.e. to energies above 3×1013 eV. Current gamma-ray instruments like the H.E.S.S. Cherenkov telescope array have limited sensitivity towards those energies, since the flux of gamma-ray sources is ex- tremely small in this regime and not enough events can be detected with the available effective areas. It is shown that the potential of H.E.S.S. for the observation at ultra high energies can be improved by utilising the data on the time evolution of the recorded Cherenkov light images. Essentially this becomes possible since the timing data offers an additional, rather robust method for the core position and direction reconstruction of events with large core distances. The potential of this method is quantified using air shower and detector simulations along with a newly developed event reconstruction algorithm. Additionally, the use of time information is tested on real H.E.S.S. data. While the timing data analysis can improve the performance of current gamma-ray instruments towards the high energy end of their sensitivity range to a certain extent, opening up the window to ultra high energy gamma-ray observations will only be possible with dedicated instruments. To that end, a new gamma-ray observatory with a very large effective area is proposed. A study of this new detector, called HiSCORE, is presented. The HiSCORE design is based on an array of wide-angle, non-imaging Cherenkov light detectors, spaced more than hundred metres apart from each other. The Cherenkov light front is sampled by photomultipliers and a fast readout system. Due to a cost-effective design of the detector stations and the large inter-station spacing it becomes feasible to equip an area of 10km2 to 100km2 at a reasonable effort. It is shown in this thesis that despite the large inter-station spacing and thus the low number of data channels a decent event reconstruction is possible using a specifically developed algorithm. The resolution of the direction and energy reconstruction is comparable to current gamma-ray observatories. The energy range between 5 × 1013 eV and 1016 eV is ideally suited to complement the currently possible gamma-ray observations. The expected sensitivity is sufficient to study in detail the ultra high energy continuation of the energy spectra of currently known sources, and to search for the – yet undiscovered – Galactic objects that 15 accelerate cosmic rays to energies above 10 eV (pevatrons). Additionally, the HiSCORE detector offers possibilities for cosmic ray and, indirectly, particle physics measurements. Additionally, the question of a suitable deployment site for the detector is discussed. Several possible locations are examined using a pre-defined set of criteria. Special focus is given to the visible sky region and to the night sky brightness at the site. One candidate site, the Fowler’s Gap research station in New South Wales, Australia, has been visited for closer examination, and the night sky brightness on site has been characterised using dedicated measurements. 4 Zusammenfassung In dieser Arbeit werden Moglichkeiten¨ untersucht, die Beobachtungen von kosmischer Gammastrahlung auf den Energiebereich jenseits von 3 × 1013 eV (ultrahohe Energien) auszudehnen. Zur Zeit existierende Experimente, wie das H.E.S.S. Cherenkov Teleskop System, haben bei diesen Energien nur eine begrenz- te Sensitivitat,¨ da der Gammastrahlungsfluss in diesem Bereich sehr gering ist und mit den verfugbaren¨ effektiven Flachen¨ nicht genugend¨ Ereignisse detektiert werden konnen.¨ Es wird gezeigt, dass das Potenzial des H.E.S.S. Experiments fur¨ die Beobachtung bei ultrahohen Energi- en verbessert werden kann, wenn die Informationen aus der Zeitentwicklung des Cherenkovlichts ebenfalls ausgwertet werden. Im Wesentlichen ist dies moglich,¨ da die Zeitinformation eine zusatzliche,¨ robuste Me- thode zur Bestimmung des Kernorts und der Herkunftsrichtung, insbesondere fur¨ Ereignisse, die weit ent- fernt von den Teleskopen auftreffen, bietet. Das Potenzial dieser Methode wird mit Hilfe einer Luftschauer- und Detektorsimulation und einem neuen Algorithmus zur Ereignisrekonstruktion untersucht. Zusatzlich¨ wird die Zeitanalyse an echten H.E.S.S. Daten getestet. Fur¨ sensitive Beobachtungen bei ultrahohen Energien sind jedoch neue, dedizierte Instrumente mit viel großeren¨ effektiven Flachen¨ notwendig. Eine Studie fur¨ ein solches Experiment, den HiSCORE Detektor, wird vorgestellt. Das HiSCORE Design beruht auf einem Feld aus nichtabbildenden Weitwinkel-Cherenkovdetektoren mit einem Stationsabstand von mehr als hundert Metern. Die Cherenkovlichtfront wird durch Photomultiplier und eine schnelle Ausleseelektronik aufgenommen. Durch die kostengunstige¨ Bauweise der Detektorstatio- nen und den großen Abstand zwischen den Stationen ist die Instrumentierung einer Flache¨ von 10km2 bis 100km2 realisierbar. In dieser Arbeit wird gezeigt, dass trotz des großen Stationsabstandes und der daraus resultierenden gerin- gen Anzahl an Datenkanalen¨ eine gute Ereignisrekonstruktion moglich¨ ist. Mit einem speziell entwickelten Rekonstruktionsalgorithmus wird eine Winkel- und Energieauflosung¨ erreicht, die vergleichbar mit jener heutiger Systeme fur¨ geringere Energien ist. Durch den Energiebereich von 5 × 1013 eV bis 1016 eV ist der Detektor ideal geeignet, um die heutzutage moglichen¨ Messungen zu ultrahohen Energien zu erweitern. Die erwartete Sensitivitat¨ ist ausreichend, um die Fortsetzung der bisher bekannten Energiespektren von Gammaquellen zu ultrahohen Energien zu untersuchen, und um nach den bisher unentdeckten galaktischen Objekten zu suchen, die die Teilchen der geladenen kosmischen Strahlung auf Energien von uber¨ 1015 eV beschleunigen (Pevatrons). Zusatzlich¨ ermoglicht¨ der HiSCORE Detektor die Messung der geladenen kos- mischen Strahlung und, indirekt, Untersuchungen aus dem Bereich der Teilchenphysik. Schließlich wird die Suche nach einem passenden Standort fur¨ den Detektor thematisiert. Verschiedene mogliche¨ Standorte werden nach bestimmten Kriterien betrachtet. Ein besonderes Augenmerk liegt auf der beobachtbaren Himmelsregion und auf der Resthelligkeit des Nachthimmels. Ein moglicher¨ Standort, die Forschungsstation Fowler’s Gap in New South Wales (Australien), wurde fur¨ genauere Untersuchungen besucht, und die Nachthimmelshelligkeit vor Ort wurde mit Hilfe von Messungen charakterisiert. 5 6 Acknowledgements Frequently used software tools and websites This chapter acknowledges the most important software tools used during the work on this thesis. As most of these tools are freeware / open source, I would like to thank all the authors who devote their time and money to the development and distribution of these programmes. • Linux in all its variations • kile for writing LATEX • Gnuplot for plots and figures • xfig for schematics and illustrations • gimp for image file type conversions and image manipulation • python, including the modules given in appendix A.8 • LabView for the hardware control during the NSB measurements • CORSIKA for air shower simulations • sim_telarray for the H.E.S.S. simulations The same is true for the many websites and forums that helped me so often with technical problems. An exhaustive collection is obviously impossible, so let me mention only the most frequently used: • www.dict.cc and dict.leo.org for help with my English • www.wikipedia.org for knowing an answer to (almost) everything • www.google.de for finding answers to everything else • adsabs.harvard.edu for its fantastic paper database • arxiv.org for bringing us a long way towards Open Access of scientific information Financial support I would like to acknowledge the financial support the German Federal Ministry of Education and Research, BMBF (contract number 05A08GU1), as well as the German Academic Exchange Service (DAAD) for its support of the field studies in Australia under the “Kurzstipendium fur¨ Doktoranden” scheme. 7 Personal acknowledgements I would like to thank my supervisor Dieter Horns for giving me the opportunity to work on this magnificent project, for the freedom to pursue the project my way and for giving me all support a PhD student could possibly dream of to develop my own scientific standing. A special thanks goes to my unshakable project coordinator and office mate Martin Tluczykont, who was an inspiring teacher and fantastic partner in our joint
Load more

Recommended publications
  • Cherenkov Light Imaging in Astroparticle Physics
    Cherenkov light imaging in astroparticle physics U. F. Katz Erlangen Centre for Astroparticle Physics, Friedrich-Alexander University Erlangen-N¨urnberg, Erwin-Rommel-Str. 1, 91058 Erlangen, Germany Abstract Cherenkov light induced by fast charged particles in transparent dielectric media such as air or water is exploited by a variety of experimental techniques to detect and measure extraterrestrial particles impinging on Earth. A selection of detection principles is discussed and corresponding experiments are presented together with breakthrough-results they achieved. Some future develop- ments are highlighted. Keywords: Astroparticle physics, Cherenkov detectors, neutrino telescopes, gamma-ray telescopes, cosmic-ray detectors 1. Introduction Photomultiplier tubes (PMTs) and, more recently, silicon pho- tomultipliers (SiPMs) [3,4] are the standard sensor types. They In 2018, we commemorate the 60th anniversary of the award are provided by specialised companies who cooperate with the of the Nobel Prize to Pavel Alexeyewich Cherenkov, Ilya experiments in developing and optimising sensors according to Mikhailovich Frank and Igor Yevgenyevich Tamm for the dis- the respective specific needs (see e.g. [5,6]). covery and the interpretation of the Cherenkov effect [1,2]. In the following, the detection principles of different types of The impact of this discovery on astroparticle physics is enor- Cherenkov experiments in astroparticle physics are presented mous and persistent. Cherenkov detection techniques were ins- together with selected technical details and outstanding results. tumental for the dicovery of neutrino oscillations; the detection of high-energy cosmic neutrinos; the establishment of ground- based gamma-ray astronomy; and important for the progress in 2. Ground-based gamma-ray detectors cosmic-ray physics.
    [Show full text]
  • From Cosmic Ray to Gamma-Ray Astronomy
    The Tunka experiment: from cosmic ray to gamma-ray astronomy. N.Budnev, Irkutsk State University For Tunka&TAIGA - collaboration High energy charged particles and gamma – ray detections - Charged particles - Cherenkov light P, N, For electrons with - Fluorescence light γ -Radio emission Ee >25 MeV Ve > C/ n Atmosphere as a huge calorimeter EAS Energy EAS Cherenkov light g wide-angle detection E = A · [Nph (200m)] Density of Cherenkov light at distance 200 m from technique θ, φ core g = 0.94±0.01 (for 10 16 – 10 18 eV) Xmax Average CR Xmax = C –D· lg τ (400) mass A (τ(400) - width of a Cherenkov pulse LnA ~ Xmax at distance 400 m EAS core from) Xmax = F( P) X0 P -Steepness of a Lateral Distribution Function (LDF ) Tunka-133 array: 175 optical detectors distributed on 3 km2 area 1 км 50 km from Lake Baikal Tunka Collaboration S.F.Beregnev, S.N.Epimakhov, N.N. Kalmykov, N.I.KarpovE.E. Korosteleva, V.A. Kozhin, L.A. Kuzmichev , M.I. Panasyuk, E.G.Popova, V.V. Prosin, A.A. Silaev, A.A. Silaev(ju), A.V. Skurikhin, L.G.Sveshnikova I.V. Yashin, Skobeltsyn Institute of Nucl. Phys. of Moscow State University, Moscow, Russia ; N.M. Budnev, O.A. Chvalaev, O.A. Gress, A.V.Dyachok, E.N.Konstantinov, A.V.Korobchebko, R.R. Mirgazov, L.V. Pan’kov, A.L.Pahorukov, Yu.A. Semeney, A.V. Zagorodnikov Institute of Applied Phys. of Irkutsk State University, Irkutsk, Russia ; B.K. Lubsandorzhiev, B.A. Shaibonov(ju) , N.B. Lubsandorzhiev Institute for Nucl.
    [Show full text]
  • Radio Measurements of the Energy and the Depth of the Shower Maximum of Cosmic-Ray Air Showers by Tunka-Rex
    Home Search Collections Journals About Contact us My IOPscience Radio measurements of the energy and the depth of the shower maximum of cosmic-ray air showers by Tunka-Rex This content has been downloaded from IOPscience. Please scroll down to see the full text. JCAP01(2016)052 (http://iopscience.iop.org/1475-7516/2016/01/052) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 131.169.95.182 This content was downloaded on 09/01/2017 at 10:16 Please note that terms and conditions apply. You may also be interested in: The wavefront of the radio signal emitted by cosmic ray air showers W.D. Apel, J.C. Arteaga-Velázquez, L. Bähren et al. Tunka-Rex: a Radio Extension of the Tunka Experiment F G Schröder, D Besson, N M Budnev et al. Radio Measurements of Air Showers with LOPES F G Schröder, W D Apel, J C Arteaga-Velazquez et al. High-energy cosmic rays and the Greisen–Zatsepin–Kuz'min effect A A Watson Reconstruction of inclined air showers detected with thePierre Auger Observatory The Pierre Auger collaboration Polarized radio emission from extensive air showers measured with LOFAR P. Schellart, S. Buitink, A. Corstanje et al. Search for the end of the energy spectrum of primary cosmic rays M Nagano Cosmic-Ray Energy Spectrum1017-1018.3 eV T. Abu-Zayyad, K. Belov, D. J. Bird et al. ournal of Cosmology and Astroparticle Physics JAn IOP and SISSA journal Radio measurements of the energy and the depth of the shower maximum of cosmic-ray air showers by JCAP01(2016)052 Tunka-Rex The Tunka-Rex collaboration P.A.
    [Show full text]
  • From Cosmic Ray to Gamma-Ray Astronomy in the Tunka Valley
    Home Search Collections Journals About Contact us My IOPscience The TAIGA experiment: from cosmic ray to gamma-ray astronomy in the Tunka valley This content has been downloaded from IOPscience. Please scroll down to see the full text. 2016 J. Phys.: Conf. Ser. 718 052006 (http://iopscience.iop.org/1742-6596/718/5/052006) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 129.13.72.197 This content was downloaded on 09/08/2017 at 07:34 Please note that terms and conditions apply. You may also be interested in: The Tunka Radio Extension: Latest Analysis Results D Kostunin, P A Bezyazeekov, N M Budnev et al. The Tunka detector complex: from cosmic-ray to gamma-ray astronomy N Budnev, I Astapov, N Barbashina et al. The Tunka-Grande experiment R.D. Monkhoev, N.M. Budnev, A. Chiavassa et al. TAIGA the Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy — present status and perspectives. N M Budnev, I I Astapov, A G Bogdanov et al. The HiSCORE experiment and its potential for gamma-ray astronomy M Tluczykont, D Hampf, U Einhaus et al. Tunka-Rex: a Radio Extension of the Tunka Experiment F G Schröder, D Besson, N M Budnev et al. THE RESULTS OF PHOTOMETRIC RECORDING OF THE OCCULTATION OF THE STAR HIP 97157 BY ASTEROIDDAPHNE WITH (41) THE TELESCOPE OF THE GLOBAL MASTER ROBOTIC NET E. M. Trunkovsky, E. S. Gorbovskoy, D. V. Denisenko et al. First deployment and prototype data of HiSCORE R Nachtigall, M Kunnas, S N Epimakhov et al.
    [Show full text]
  • Exploring Cosmic Ray Origins with Ground-Based EAS Arrays Tunka and Hiscore
    Exploring cosmic ray origins with ground-based EAS arrays Tunka and HiSCORE Sergey Epimakhov Exploring cosmic ray origins with ground-based EAS arrays Tunka and HiSCORE Dissertation with the aim of achieving a doctoral degree at the Faculty of Mathematics, Informatics and Natural Sciences Department of Physics University of Hamburg Submitted by Sergey Epimakhov Hamburg 2015 Gutachter der Dissertation: Prof. Dr. Dieter Horns Dr. Vasily Prosin Gutachter der Disputation: Prof. Dr. G¨unter Sigl Prof. Dr. Caren Hagner Dr. Martin Tluczykont Datum der Disputation: 24.09.15 Dekan der MIN Fakult¨at: Prof. Dr. Heinrich Graener Dedicated to my family Per aspera ad astra Abstract The main properties of cosmic radiation over the last hundred years have been studied with good accuracy and are not in doubt: cosmic rays are nuclei of almost all elements of the periodic table with a small fraction of other particles coming from the outer space at Earth with the non-thermal energy spectrum from 106 to 1020 eV. However, the source of cosmic rays still remains unknown. To examine the question of the origin of cosmic rays neutral particles are perfectly suited as messengers. Thereby the gamma ray sky in the range above 10 { 100 TeV is of great interest. Hypothetical galactic accelerators, pevatrons, must have gamma ray spectra up to these energies. A new non-imaging wide-angle Cherenkov experiment HiSCORE is aimed at search- ing the ultra-high energy gamma rays above 30 TeV and measuring the primary spectrum and mass composition of cosmic rays above 100 TeV with a unprece- dented accuracy.
    [Show full text]
  • Status and Perspectives of Astroparticle Physics in Europe
    SStatustatus aandnd PPerspectiveerspective ooff AAstroparticlestroparticle PPhysicshysics inin EEuropeurope Astroparticle Physics Roadmap Phase I ASPERA Roadmap • Phase I • Astroparticle physics for Europe 2 ASPERA Roadmap • Phase I • On this document The Steering Committee of ApPEC (Astroparticle Physics European Coordination) has charged the ApPEC Peer Review Committee (PRC) in 2005 to prepare a roadmap for astroparticle physics in Europe* which covers the next decade. The need for such a roadmap arises since projects in astroparticle physics move to ever larger sensitivity and scale, with costs of individual projects on the 100 M€ scale or beyond. The roadmap document presented here was prepared by the PRC between October 2005 and January 2007. As a first step towards the roadmap, the state of the experiments in the field was evaluated using a questionnaire filled out by the spokespersons of all astroparticle experiments in Europe, or with European participation (see Appendix 2). Based on this information, on input from the proponents and on presentations given to ApPEC in the last years, the most promising research areas and instrumental approaches were identified. A town meeting in Munich in 2005 served to discuss and iterate these initial concepts with the community at large. The recommendations given in the roadmap were in several stages iterated in particular with the spokespersons of the experiments as well as with the ApPEC Steering Committee. After a large meeting in Valencia (Nov.7/8, 2006), further significant modifications have been prepared by smaller working groups, submitted by individuals and included in the present version. The resulting ApPEC roadmap marks the first stage (ASPERA Roadmap/Stage I) of a strategy process which foresees a “final” roadmap (ASPERA Roadmap/Stage 3) in July 2008.
    [Show full text]
  • Cherenkov Experiments in the Tunka Valley
    The Tunka Experiment: Cosmic Ray and Multi-TeV Gamma-Ray Astronomy Arrays in the Tunka Valley Bayarto Lubsandorzhiev Institute for Nuclear Research of RAS, Moscow Russia for TUNKA and TAIGA Collaborations Outline Introduction Tunka-25 Tunka-133 TAIGA (Tunka Advanced Internatinal Gamma and cosmic ray Array) Victor Hess 1912 г. – the discovery of cosmic rays On a balloon at an altitude of 5000 meters Victor Hess discovered “penetrating radiation” coming from space. Nobel prize 1936 The origin of cosmic rays? – XX-XXI century mystery! Where from? - Energy? Where? - Sources? How? - Acceleration mechanisms? Detection of Cherenkov light from EAS Cherenkov experiments in the Tunka Valley Tunka Valley “…..till Baikal it is the Siberia’s dull prose, just from Baikal the Siberian delightful poetry starts….” A.P.Chekhov (Letters from Siberia) Cherenkov experiments in the Tunka Valley 1993 - ………. 1991-1992: first experiments at the Lake Baikal ice with QUASAR-370 photodetectors (Bezrukov, Kuzmichev, Lubsandorzhiev et al.) 1993г. - Move to the Tunka Valley. (Bezrukov, Budnev, Kuzmichev, Lubsandorzhiev, Pokhil et al.) SMECA: Surface Mobile Eas Cherenkov Array Kuzmichev, Lubsandorzhiev, Pokhil et al Eth~400 TeV, <>~0.5 Tunka Valley, Buryatia Republic Tunka-4 4 QUASAR-370 phototubes Bezrukov, Kuzmichev, Lubsandorzhiev, Pokhil et al. 24th ICRC 1995 Rome. “Knee” in the energy spectrum at 31015 эВ. TUNKA-25 COLLABORATION E.Korosteleva, L.Kuzmichev, V.Prosin, I.Yashin Scobeltsyn Institute of Nuclear Physics of MSU (Moscow, Russia) N.Budnev, O.Gress, L.Pankov,
    [Show full text]
  • Jopcs632(2015)012034.Pdf
    Home Search Collections Journals About Contact us My IOPscience The Tunka detector complex: from cosmic-ray to gamma-ray astronomy This content has been downloaded from IOPscience. Please scroll down to see the full text. 2015 J. Phys.: Conf. Ser. 632 012034 (http://iopscience.iop.org/1742-6596/632/1/012034) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 141.34.3.98 This content was downloaded on 26/01/2016 at 10:01 Please note that terms and conditions apply. 24th European Cosmic Ray Symposium (ECRS2014) IOP Publishing Journal of Physics: Conference Series 632 (2015) 012034 doi:10.1088/1742-6596/632/1/012034 The Tunka detector complex: from cosmic-ray to gamma-ray astronomy N Budnevb, I Astapovi, N Barbashinai, A Bogdanovi , D Bogorodskiib, V Boreykoj, M Bükerf, M Brücknerk, A Chiavassad, O Chvalaevb, O Gressb, T Gressb, A Dyachokb, S Epimakhovf, A Gafatovb , N Gorbunovj , V Grebenyukj , A Grinukj , A Haungsl, R Hillerl, D Hornsf, T Huegel, A Ivanovab, A Kalininj , N Karpova, N Kalmykova, Y Kazarinab, V Kindini, N Kirichkovb, S Kiryuhinb, M Kleifgesm, R Kokoulini , K Komponiesti, A Konstantinova, E Konstantinovb, A Korobchenkob, E Korostelevaa, D Kostuninl, V Kozhina, O Krömerm, M Kunnasf, L Kuzmicheva, V Lenokb, B Lubsandorzhievc, N Lubsandorzhieva, R Mirgazovb, R Mirzoyane,b, R Monkhoevb, R Nachtigallf, A Pakhorukovb, M Panasyuka, L Pankovb, A Petrukhini, V Platonovb, V Poleschukb, E Popovaa, A Porellih, V Prosina, V Ptusking, G Rubtsovc, C Rühlem, V Samoligab, P Satuning, V Savinovb, A Saunkinb,F Schröderl, Yu Semeneyb, B Shaibonov (junior)c, A Silaeva, A Silaev (junior) a, A Skurikhina, V Sluckaj , C Spieringh, L Sveshnikovaa, V Tabolenkob,A Tkachenkoj , L Tkachevj , M Tluczykontf, D Voroninb, R Wischnewskih, A Zagorodnikovb, V Zurbanovb , I Yashini.
    [Show full text]
  • Acoustic and Radio Eev Neutrino Detection Activities Book of Abstracts
    ARENA 2012 - Acoustic and Radio EeV Neutrino Detection Activities Tuesday 19 June 2012 - Friday 22 June 2012 Erlangen Castle (centre of town) Book of abstracts ARENA 2012 - Acoustic and Radio EeV Neutrino Detection Activities / Book of abstracts Monday 18 June 2012 Table of contents Introduction ............................................................................................................................... 1 Welcome Address ....................................................................................................................... 1 Radio Detection in Dense Matter: Balloon, telescope, satellite ............................................................... 1 LUNASKA neutrino search with the Parkes and ATCA telescopes ......................................................... 1 Searching for neutrino radio flashes from the Moon with LOFAR ......................................................... 2 Lunar Imaging and Ionospheric Calibration for the Lunar Cherenkov Technique ..................................... 2 Lunar Space Missions for Observation of Ultrahigh-Energy Cosmic Rays and Neutrinos ............................ 3 Overview of MHz air shower radio experiments and results ................................................................. 3 Recent developments at the Auger Engineering Radio Array ................................................................ 3 Energy Estimation for Cosmic Rays Measured with the Auger Engineering Radio Array ........................... 4 Spectral index analysis of the data
    [Show full text]
  • Very-High Energy Gamma-Ray Astronomy
    Very-high energy gamma-ray astronomy A 23-year success story in high-energy astroparticle physics Eckart Lorenz1;a and Robert Wagner1;2;b 1 Max-Planck-Institut fur¨ Physik, Fohringer¨ Ring 6, 80805 Munchen,¨ Germany 2 Excellence Cluster “Origin and Structure of the Universe”, Boltzmannstraße 2, 85748 Garching b. Munchen,¨ Ger- many Abstract. Very-high energy (VHE) gamma quanta contribute only a minuscule fraction – be- low one per million – to the flux of cosmic rays. Nevertheless, being neutral particles they are currently the best “messengers” of processes from the relativistic/ultra-relativistic Universe because they can be extrapolated back to their origin. The window of VHE gamma rays was opened only in 1989 by the Whipple collaboration, reporting the observation of TeV gamma rays from the Crab nebula. After a slow start, this new field of research is now rapidly expanding with the discovery of more than 150 VHE gamma-ray emitting sources. Progress is intimately related with the steady improvement of detectors and rapidly increasing computing power. We give an overview of the early attempts before and around 1989 and the progress after the pio- neering work of the Whipple collaboration. The main focus of this article is on the development of experimental techniques for Earth-bound gamma-ray detectors; consequently, more empha- sis is given to those experiments that made an initial breakthrough rather than to the successors which often had and have a similar (sometimes even higher) scientific output as the pioneering experiments. The considered energy threshold is about 30 GeV. At lower energies, observa- tions can presently only be performed with balloon or satellite-borne detectors.
    [Show full text]
  • TAIGA - an Advanced Hybrid Detector Complex for Astroparticle Physics and High Energy Gamma-Ray Astronomy in the Tunka Valley
    TAIGA - an advanced hybrid detector complex for astroparticle physics and high energy gamma-ray astronomy in the Tunka valley. N.Budnev, Irkutsk State University For TAIGA collaboration At present an Imaging Atmospheric Cherenkov Telescopes (IACT) are the main instruments for the ground based high energy gamma astronomy An Imaging Atmospheric camera Mirror with Cherenkov Telescope diameter 4-24 m (IACT) - narrow-angle telescope (3-5 FOV) with a mirror of 4 -24 m diameter which reflects EAS Cherenkov light into a camera with up to 1000 PMT where Cherenkov EAS image is formed. H.E.S.S. camera (D = 3 m!) EAScamera Imaging Atmospheric Cherenkov Arrays (2-5 IACT) Whipple HEGRA H.E.S.S. MAGIC VERITAS S ~ 0.1 km2 About 200 sources of gamma rays with energy more than 1 TeV were discovered with IACT arrays. But a few gamma quantum with energy more then 50 TeV were detected up to now. An area of an array should be a few square kilometers as minimum to detect high energy gamma rays. EAS Cherenkov light detection technique by wide angle arrays in the Tunka - Experiment EAS Energy Average CR mass A θ, φ g LnA ~ Xmax E = A · [Nph(200m)] Xmax g = 0.94±0.01 Xmax = C –D· lg τ (400) (τ(400) - width of a Cherenkov pulse at distance 400 m EAS core from) Xmax = F(P) X0 P -Steepness of a Lateral Distribution Function (LDF) Tunka-133 array: 175 Cherenkov detectors distributed on 3 km2 area, in operation since 2009y 1 км 50 km from Lake Baikal Advantage of the Tunka-133 array: 1.
    [Show full text]
  • Design of the LED Driver for the Precision Optical Calibration Module
    Design of the LED Driver for the Precision Optical CAlibration Module Master Thesis Antonio Becerra Esteban Technische Universit¨atM¨unchen Physics Department Chair for Experimental Physics with Cosmic Particles December 4, 2017 Supervisor: Prof. Dr. Elisa Resconi Abstract A study of the circuit designed by J.S.Kapustinsky et Al. in 1985 as a cheap fast flasher for the Precision Optical CAlibration Module (POCAM) is carried out. Its characteristics make it a perfect candidate as short light pulses generator in order to simulate neutrino double-bang-like events in the framework of the next IceCube upgrade, IceCube-Gen2. The response of diverse LEDs with different features was studied by varying the available charge, the bias voltage and the inductance of the Kapustinsky circuit. The pulses were measured with a PIN-Diode and a SiPM. The amplification of the signal was accomplished by a couple of charge sensitive preamplifiers and afterwards monitored and stored in the oscilloscope for further analysis. To produce an isotropic pulse, the LED flashed inside a PFTE sphere that spread the light in 4π. All the tests were carried out inside a dark metallic box with foam cladding to ensure the isolation from external photon sources. For a first test at the Gigaton Volume Detector (GVD) at Lake Baikal four different Kapustinky-like circuits were set up. This configuration allows the POCAM to produce four different light pulses: two long pulses (15 − 25 ns) and two short pulses (5 − 10 ns) in green (525 − 527 nm) and blue (455 − 470 nm). The final driver board includes the PIN-Diode and the SiPM as well as the preamplifiers that sends the information to an FPGA for its storage.
    [Show full text]