on behalf of the GAMMA Collaboration

Slides:



Advertisements
Similar presentations
JNM Dec Annecy, France The High Resolution Fly’s Eye John Matthews University of Utah Department of Physics and High Energy Astrophysics Institute.
Advertisements

EAS EXPERIMENT ON BOARD OF THE AIRBUS A380 J. N. Capdevielle, F. Cohen, PCC, College de France K. Jedrzejczak, B. Szabelska, J. Szabelski, T. Wibig The.
A.U. Kudzhaev, D.D. Dzhappuev, V.V. Alekseenko, A.B. Chernyev, N.F. Klimenko, A.S. Lidvansky, A.B. Chernyev, N.F. Klimenko, A.S. Lidvansky, V.B. Petkov.
TeVPA, July , SLAC 1 Cosmic rays at the knee and above with IceTop and IceCube Serap Tilav for The IceCube Collaboration South Pole 4 Feb 2009.
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:
Chiba, July 29, 2003Tom Gaisser Comments on atmospheric muon and neutrino backgrounds in neutrino telescopes Use semi-analytic estimates to display some.
Fine structure of all-particle energy spectrum in the knee region A Garyaka 1, R Martirosov 1, S Ter-Antonyan 3, H Babayan 2, A Erlykin 4, Y Gallant 5,
Variations of the high energy muon flux and space-time structure of the temperature profile in the atmosphere M.G. Kostyuk 1, V.B. Petkov 1, R.V. Novoseltseva.
Status of Cosmic Rays Physics at the Knee Andrea Chiavassa Università and INFN Torino NOW 2006 Otranto 9-16 September 2006.
Yu. Stenkin, UHECR'20081 On PRISMA project (proposal) Yuri V. Stenkin INR RAS.
Size and Energy Spectra of incident cosmic radiation obtained by the MAKET - ANI surface array on mountain Aragats. (Final results from MAKET-ANI detector)‏
A new approach to EAS investigations in energy region eV R.P.Kokoulin for DECOR Collaboration Moscow Engineering Physics Institute, Russia.
TAUP Conference, Sendai September The primary spectrum in the transition region between direct and indirect measurements (10 TeV – 10 PeV)
Contributions of the University of Bucharest to the study of high energy cosmic rays in the framework of the KASCADE-Grande experiment Octavian Sima Faculty.
Ground level enhancement of the solar cosmic rays on January 20, A.V. Belov (a), E.A. Eroshenko (a), H. Mavromichalaki (b), C. Plainaki(b), V.G.
The short particle bursts during thunderstorms: EAS or lightning seeds? G. Hovsepyan, A. Chilingarian, A. Alikhanian National Laboratory, Armenia.
Spectra of the Thunderstorm Correlated Electron and Gamma-Ray Measured at Aragats Bagrat Mailyan and Ashot Chilingarian.
Page 1 HEND science after 9 years in space. page 2 HEND/2001 Mars Odyssey HEND ( High Energy Neutron Detector ) was developed in Space Research Institute.
Properties of giant air showers and the problem of energy estimation of initial particles M.I. Pravdin for Yukutsk Collaboration Yu.G. Shafer Institute.
Multi-TeV  -ray Astronomy with GRAPES-3 Pravata K Mohanty On behalf of the GRAPE-3 collaboration Tata Institute of Fundamental Research, Mumbai Workshop.
SN 1987A as a Possible Source of Cosmic Rays with E 0 < eV by Yakutsk EAS Array Data A.V. Glushkov, L.T. Ksenofontov, M.I. Pravdin Yu.G. Shafer Institute.
12/22/ Y.Gallant, 1 A.Garyaka, 2 A.D.Erlykin 5 L.Jones, 1 R.Martirosov, 2 N.Nikolskaya, 3 J.Procureur, 1 S.Ter-Antonyan 1 Yerevan Physics Institute.
Air-showers, bursts and high-energy families detected by hybrid experiment at Mt.Chacaltaya M.Tamada Kinki University M.Tamada ICRC2011, Beijing, 15 Aug.
Tunka Experiment: Towards 1км 2 EAS Cherenkov Array B.K.Lubsandorzhiev for TUNKA Collaboration.
“The Cosmic Ray composition in the knee region and the hadronic interaction models” G. Navarra INFN and University, Torino, Italy For the EAS-TOP Collaboration.
Study of high energy cosmic rays by different components of back scattered radiation generated in the lunar regolith N. N. Kalmykov 1, A. A. Konstantinov.
The primary energy spectrum measured by using the time structure of extensive air showers with compact EAS arrays (ID441) H. Matsumoto 1, A. Iyono 1, I.
High-energy Electron Spectrum From PPB-BETS Experiment In Antarctica Kenji Yoshida 1, Shoji Torii 2 on behalf of the PPB-BETS collaboration 1 Shibaura.
The KASCADE-Grande Experiment: an Overview Andrea Chiavassa Universita’ di Torino for the KASCADE-Grande Collaboration.
Cosmic Rays from to eV. Open Problem and Experimental Results. (KASCADE-Grande view) Very High Energy Phenomena in the Universe XLIV th Rencontres.
Study of VHE Cosmic Ray Spectrum by means of Muon Density Measurements at Ground Level I.I. Yashin Moscow Engineering Physics Institute,
What we do know about cosmic rays at energies above eV? A.A.Petrukhin Contents 4 th Round Table, December , Introduction. 2. How these.
Workshop on AstroParticle Physics, WAPP 2009 Bose Institute, Darjeeling, December 2009 Extensive Air Showers and Astroparticle Physics Observations and.
Juan Carlos Arteaga-Velázquez for the KASCADE-Grande Collaboration Institute of Physics and Mathematics Universidad Michoacana, Mexico 132nd ICRCJ.C.Arteaga.
NEVOD-DECOR experiment: results and future A.A.Petrukhin for Russian-Italian Collaboration Contents MSU, May 16, New method of EAS investigations.
Tunka-133: Primary Cosmic Ray Energy Spectrum in the energy range 6·10 15 – eV L.A.Kuzmichev (SINP MSU) On behalf on the Tunka Collaboration 32th.
1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.
32 nd ICRC –Beijing – August 11-18, 2011 Silvia Vernetto IFSI-INAF Torino, ITALY On behalf of the ARGO-YBJ collaboration Observation of MGRO J with.
Michael Prouza Center for Particle Physics Institute of Physics Academy of Sciences of the Czech Republic Prague Studies of the ultra-high energy cosmic.
Yu.V. Stenkin, 32 ICRC. Beijing'20111 The PRISMA project and the cosmic ray knee problem Yuri V. Stenkin Institute for Nuclear Res. of RAS, Moscow, Russia.
Measurement of the CR light component primary spectrum B. Panico on behalf of ARGO-YBJ collaboration University Rome Tor Vergata INFN, Rome Tor Vergata.
Cosmic Ray Composition Primary cosmic particles collide with atoms in the Earth's atmosphere and produce a cascade of short lived particles, which can.
A Method of Shower Reconstruction from the Fluorescence Detector M.Giller, G.Wieczorek and the Lodz Auger group GZK-40 Moscow Workshop, May 2006.
on behalf of the NUCLEON collaboration
Measurement of high energy cosmic rays by the new Tibet hybrid experiment J. Huang for the Tibet ASγCollaboration a a Institute of high energy physics,
Scaling behavior of lateral distribution of electrons in EAS
On behalf of the ARGO-YBJ collaboration
Solar gamma-ray and neutron registration capabilities of the GRIS instrument onboard the International Space Station Yu. A. Trofimov, Yu. D. Kotov, V.
Muons in IceCube PRELIMINARY
L.L.Ma for LHAASO collaboration Beijing China
Recent Results from the new Tibet hybrid experiment
completed in austral season South Pole completed in austral season.
Direct Measurement of the Atmospheric Muon Spectrum with IceCube
Andrea Chiavassa Universita` degli Studi di Torino
A.S. Lidvansky, M.N. Khaerdinov, N.S. Khaerdinov
Remarks on astrophysical origin of the knee in cosmic ray spectrum
Electron Observations from ATIC and HESS
Pierre Auger Observatory Present and Future
Results on the Spectrum and Composition of Cosmic Rays
John Kelley for the IceCube Collaboration
Traditional image of the CR energy spectrum ( knee ) ( ankle )
A New Component of Cosmic Rays?
Litao Zhao Liaoning University&IHEP
Latest Results from the KASCADE-Grande experiment
Unfolding performance Data - Monte Carlo comparison
The energy spectrum from the KASCADE-Grande muon data
Bagrat Mailyan, Alikhanian National Laboratory (Former YerPhI)
National Research Nuclear University MEPhI
The Aperture and Precision of the Auger Observatory
Andrea CHIAVASSA and Elena CANTONI Universita` degli Studi di Torino
Presentation transcript:

on behalf of the GAMMA Collaboration Energy spectrum and mass composition of primary cosmic radiation in the region above the knee from the GAMMA experiment Romen Martirosov on behalf of the GAMMA Collaboration A.A. Alikhanyan National Laboratory, Armenia (Former Yerevan Physics Institute) Martirosov, 32nd ICRC, August 11 -18, 2011

GAMMA Collaboration Yerevan Physics Institute, ARMENIA Romen Martirosov Alexandr Garyaka Moscow Lebedev Institute, RUSSIA Anatoly Erlykin Natalya Nikolskaya University of Michigan, USA Lawrence Jones Southern University, Baton Rouge, USA Samvel Ter-Antonyan University of Montpellier II, FRANCE Yves Gallant Warsaw University of Technology, POLAND Janusz Kempa 2

All-Particle energy spectra 1 – 100 PeV GAMMA

! It is necessary an individual analysis and Sources of these uncertainties may be found: in the big fluctuations of showers deeper in the atmosphere; in different assumption concerning the primary interaction and cascade development models used in data analysis; and/or in energy normalization uncertainty. ! It is necessary an individual analysis and comparison of spectra !

!Primary spectrum above the knee is not smooth! Common resume (in near past): - Global characteristics of the all-particle spectrum agree within of about 20-30% of the systematic errors. - Changing of slope of the all-particle energy spectrum from about -2.7 below the “knee” to about -3.1 after the “knee” may be considered as an experimentally established fact; ? !Primary spectrum above the knee is not smooth! It is necessary to pay special attention to the energy region of 10 - 100 PeV, where experimental results are still very limited.

GAMMA experiment created by Yerevan Physics Institute – Lebedev Physical Institute ARAGATS scientific station (late autumn) Hill sides of the Mt. Aragats, Armenia, 65 km from Yerevan Elevation: 3200 m a.s.l. (700 g/cm2 of atmospheric depth) Geographical coordinates: Latitude = 40.470 N, Longitude = 44.180 E

(after several modifications) GAMMA 2011 (after several modifications) S = 3x104 sq.m Surface part - 41 stations – 116 1 sq.m scintillation detectors Muon carpet – 150 scintillation detectors (Eµ > 5 GeV) 33 fast-timing channels for estimation of the EAS angular characteristics

All-Particle Energy Spectrum (2003-2006) GAMMA05: R < 25m; Q < 300 GAMMA07: R < 50m; Q < 450 J.Phys. G: Nucl. Part. Phys. 35 (2008) 115201 9 9

Energy estimator (SYBILL interaction model) where Nch, Nµ, s, cos θ – ! experimentally measured parameters ! The best energy estimations as a result of 2min(E0,E1) were achieved for the 7-parametric fit:  where x = LnNch, y = LnN (R<50m), c = cos() 10

Recent results (2003 – 2009)

Recent results (2003 – 2009) - 2.7 - 3.1

Recent results (2003 – 2009) - 2.7 from ~20 PeV index - 3.1 also KASCADE-Grande and Tunka-133 – deviation from index – 3.1

Recent results (2003 – 2009) > 4σ at ~ 70 PeV - 2.7 from ~20 PeV - 3.1 > 4σ at ~ 70 PeV

It was shown in our previous works that rigidity-dependent primary energy spectra cannot describe such behavior of the energy spectrum and the presence of additional component in the primary flux of nuclei is necessary. The hypothesis of two-component origin of cosmic ray flux was used to explain the fine structure of the spectrum.

Age parameter dependence on E0 Also the s dependence on E0 becomes roughly constant in the same region. The age is dependent on the distance from the depth of shower maximum to the observation level. Constancy of the age approximately means the constancy of the depth of maximum. This behaviour is possible if the flux became heavier with energy. !This consideration is rather qualitative.!

As a rule in the case of constant mass composition this dependence ε ~ 0.13 As a rule in the case of constant mass composition this dependence looks like Ne ~ E01+ε in the range after the shower maximum. Just such behavior is seen before the knee where ε is about 0.13. After the knee ε decreases and becomes about 0 at E0 > 10 PeV. Such behavior is provided with the approximate constancy of the depth of shower maximum.

Position of ‘bump’

Conclusion The all particle primary energy spectrum was derived on the basis of GAMMA data for 2003-2009 years. We confirm our previous result. In the energy range of 10-100 PeV the spectrum shows statistically significant feature of deviation (flattening) from the power law with index of -3.1. The observed bump can be described by a two-component model of the primary cosmic ray origin. The constancy of the EAS age parameter s and the proportionality of the EAS size Ne to the primary energy E0 indicates the growth of the mean logarithm of the mass <lnA> of primary cosmic rays above the knee. The data 2010-2011 are still analysing

GAMMA experiment http://gamma-armenia.org Thank you

2010 ~80 PeV