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Presented by A.A . Leonov on behalf of GAMMA-400 collaboration

Presented by A.A . Leonov on behalf of GAMMA-400 collaboration Perspectives of the GAMMA-400 space observatory for high-energy gamma rays and cosmic rays measurements. ICCPA, Moscow, October 9, 2015. GAMMA-400 collaboration

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Presented by A.A . Leonov on behalf of GAMMA-400 collaboration

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  1. Presented by A.A. Leonov on behalf of GAMMA-400 collaboration Perspectives of the GAMMA-400 space observatory for high-energy gamma rays and cosmic rays measurements ICCPA, Moscow, October 9, 2015

  2. GAMMA-400 collaboration A.M. Galpera,b, V. Bonvicinic, N.P. Topchieva, O. Adrianid, R.L. Aptekare, I.V. Arkhangelskayab, A.I. Arkhangelskiyb, A.V. Bakaldinb, L. Bergstromf, E. Bertid, G. Bigongiarig, S.G. Bobkovh, M. Boezioc, E.A. Bogomolove, S. Bonechig, M. Bongid, S. Bottaid, G. Castellinii, P.W. Cattaneoj, P. Cumanic, O.D. Dalkarova, G.L. Dedenkob, C. De Donatok, V.A. Dogiela, N. Finettid, M.S. Gorbunovh, Yu.V. Gusakova, B.I. Hnatykl, V.V. Kadilinb, V.A. Kaplinb, A.A. Kaplunb, M.D. Kheymitsb, V.E. Korepanovm, J. Larssonn, A.A. Leonova,b, V.A. Loginovb, F. Longoc, P. Maestrog, P.S. Marrocchesig, A.L. Men’shenino, V.V. Mikhailovb, E. Mocchiuttic, A.A. Moiseevp, N. Morid, I.V. Moskalenkoq, P.Yu. Naumovb, P. Papinid, M. Pearcen, P. Picozzak, A. Rappoldij, S. Ricciarinii, M.F. Runtsob, F. Ryden, O.V. Serdinh, R. Sparvolik, P. Spillantinid, Yu.I. Stozhkova, S.I. Suchkova, A.A. Taraskinb, M. Tavanir, A. Tiberiod, E.M. Tyurinb, M.V. Ulanove, A. Vacchic, E. Vannuccinid, G.I. Vasilyeve, Yu.T. Yurkinb, N. Zampac, V.N. Zirakashvilis and V.G. Zverevb aLebedev Physical Institute, Russian Academy of Sciences, Moscow, Russia bNational Research Nuclear University MEPhI, Moscow, Russia cIstituto Nazionale di Fisica Nucleare, Sezione di Trieste and Physics Department of University of Trieste, Trieste, Italy dIstituto Nazionale di Fisica Nucleare, Sezione di Firenze and Physics Department of University of Florence, Firenze, Italy eIoffe Institute, Russian Academy of Sciences, St. Petersburg, Russia fStockholm University, Department of Physics; and the Oskar Klein Centre, AlbaNova University Center, Stockholm, Sweden gDepartment of Physical Sciences, Earth and Environment, University of Siena and Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, Italy hScientific Research Institute for System Analysis, Russian Academy of Sciences, Moscow, Russia iIstituto di Fisica Applicata Nello Carrara - CNR and Istituto Nazionale di Fisica Nucleare, Sezione di Firenze, Firenze, Italy jIstituto Nazionale di Fisica Nucleare, Sezione di Pavia, Pavia, Italy kIstituto Nazionale di Fisica Nucleare, Sezione di Roma 2 and Physics Department of University of Rome Tor Vergata, Rome, Italy lTaras Shevchenko National University of Kyiv, Kyiv, Ukraine oResearch Institute for Electromechanics, Istra, Moscow region, Russia mLviv Center of Institute of Space Research, Lviv, Ukraine nKTH Royal Institute of Technology, Department of Physics; and the Oskar Klein Centre, AlbaNova University Center, Stockholm, Sweden pCRESST/GSFC and University of Maryland, College Park, Maryland, USA qHansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, USA rIstituto Nazionale di Astrofisica IASF and Physics Department of University of Rome Tor Vergata, Rome, Italy sPushkov Institute of Terrestrial Magnetism, Ionosphere, and Radiowave Propagation, Troitsk, Moscow region, Russia ICCPA, Moscow, October 9, 2015

  3. Physical scheme ICCPA, Moscow, October 9, 2015

  4. Scientific goals Physics goals for total telescope acceptance (~4200 cm2 sr) 1.1 The features in the energy spectra of high energy γ-ray emissions from discrete and extended sources associated with particles of dark matter 1.2 The variability of high energy γ-ray emissions from discrete sources in order to clarify the nature of particle acceleration in such sources 1.3 γ-ray bursts, including high-energy bursts 1.4 high-energy γ-ray emissions, fluxes of electrons and positrons, and nuclei in solar flares Physics goals for calorimeter onlyacceptance (~4 m2 sr) 2.1 HE e+, e- from Dark Mater annihilation 2.2 HE e+, e- acceleration mechanisms 2.3 HE protons and nuclei (>>GeV) PAMELA has revealed a break in proton and He spectrum (different slope) the knee of proton and helium the spectral hardening of nuclei (E>TeV) 2.4 CR propagtion in the Galaxy ICCPA, Moscow, October 9, 2015

  5. GAMMA-400 will be launched in highly elliptical orbit (500–300000 km) with an inclination angle of 51.8°. The initial orbit, after some months, evolves to a very high circular orbit (100.000 – 200.000 km) with an orbital period of about 7 days. GAMMA-400 is less as survey and more as “pointing telescope” (without occultation of the Earth). ICCPA, Moscow, October 9, 2015

  6. Interactions of gamma inside the instrument 100 MeV 10 GeV 1 GeV 1 TeV 100 GeV ICCPA, Moscow, October 9, 2015

  7. GAMMA-400 performance Effective area for vertical gamma. Effective area as a function of 100 GeV gamma incidence angle. ICCPA, Moscow, October 9, 2015

  8. Simulation plane 4600 mm AC 1200 mm S1 1000 mm S2 1000 mm Acceptance. ICCPA, Moscow, October 9, 2015

  9. Energy resolution ICCPA, Moscow, October 9, 2015

  10. Angular resolution ICCPA, Moscow, October 9, 2015

  11. Angular resolution > 1 GeV ICCPA, Moscow, October 9, 2015

  12. Initial circle distribution for supernova remnant IC 433 statistic ICCPA, Moscow, October 9, 2015

  13. 2 point sources (distance 0.050) to distinguish ICCPA, Moscow, October 9, 2015

  14. 2 point sources (distance 0.050) to distinguish ICCPA, Moscow, October 9, 2015

  15. Модели распределения темной материи в Галактике 15 ICCPA, Moscow, October 9, 2015

  16. Galactic center (-0.87<l<1; -0.285<b<0.3). 3FGL catalog ICCPA, Moscow, October 9, 2015

  17. ICCPA, Moscow, October 9, 2015

  18. ICCPA, Moscow, October 9, 2015

  19. ICCPA, Moscow, October 9, 2015

  20. GAMMA-400 only calorimeter CC2 (CsI(Tl)) performance Expected number of proton and helium events in 10 years data taking, according to the Polygonatomodel ICCPA, Moscow, October 9, 2015

  21. Calorimeter only proton energy resolution 10 TeV 100 TeV RMS=38% Aeff=4,9 m2 sr RMS=40% Aeff=5 m2 sr (E-Etrue)/Etrue (E-Etrue)/Etrue 1 PeV Resolutions and Aeff depend on cuts. Optimizeation for large acceptance. RMS=37% Aeff=4,8 m2 sr ICCPA, Moscow, October 9, 2015 (E-Etrue)/Etrue

  22. Nuclei energy resolution 100 TeV RMS % Aeff (m2sr) ICCPA, Moscow, October 9, 2015

  23. Calorimeter only angular resolution (gamma 100 GeV) 68% containment: 1.70±0.20 (Elena Vannuccini, INFN, Florence) For HE (>1 TeV) protons and nuclei with 68% containment ~30 (Sergio Bottai, INFN, Florence) ICCPA, Moscow, October 9, 2015

  24. Conclusion The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from 100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as well as protons and nuclei spectra up to the knee region. GAMMA-400 will allow to address a broad range of science topics, like search for signatures of dark matter, studies of Galactic and extragalactic gamma-ray sources, Galactic and extragalactic diffuse emission, gamma-ray bursts and charged cosmic rays acceleration and diffusion mechanism up to the knee. ICCPA, Moscow, October 9, 2015

  25. Thanks for your attention ICCPA, Moscow, October 9, 2015

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