PPT-Optical Energy Recovery for a High Duty Cycle Gamma Ray Source

Challenge Laser accelerators can achieve very high accelerating gradients but as a rule require very high peak power High peak power lasers are not easily scalable to high average power Many HEP applications ie ILC positron source or . ASTROPHYSICAL SCENARIOS. Félix Mirabel. CEA-Saclay-France . *. Neutron stars & Black . holes. in . stellar. . binary. . systems. . that. . radiate. in gamma-rays.. (Will not . refer. Manel. Martinez. 4. 3. rd. . Winter Meeting. March 2015-Benasque. Outline. 1) Introduction. 2) Basics on VHE Gamma Astronomy physics. 3) VHE gamma observatories. 4) CTA. 5. ) Conclusions. 1) INTRODUCTION. High Energy & Cosmic Ray Research Ctr.. North Bengal University. TeV Neutrinos and Gamma rays from Pulsars/Magnetars. Introduction. The energy spectrum of cosmic rays extends to extremely high energies, values exceeding 10. H. . Herrmann (LANL. ). e. -. Next . Steps. Cherenkov detectors . Energy . thresholded. Gas limited to >2.5 . MeV. Solid limited to <~0.2 . MeV. Aerogel. might span the gap. Real . g. -ray spectroscopy (Energy resolved) . ACD and Calorimeter Stability ContinuousMonitoring of ACDrq MIP eakPparticle peak Pedestals Veto threshold ContinuousMonitoring of CAL Zero suppressionthresholdsCALgly tal1zi Overall trigger rate -few -. What Fermi Adds to the Picture. Brian R. Dennis. GSFC, Solar Physics Lab., Code 671. High Energy Solar . Flares. Eruptive Events. Tutorial on Solar Eruptive Events. Analysis of GBM spectral data. North Bengal University. TeV Neutrinos and Gamma rays from Pulsars/Magnetars. Introduction. The energy spectrum of cosmic rays extends to extremely high energies, values exceeding 10. 20. . eV. .. The origin of the cosmic rays and the mechanism responsible for acceleration of cosmic rays to such high energies . G. amma . R. ays from the Large-scale Disk of the Large . Magellanic. . Cloud. Qing-Wen Tang. 1,2. with Xiang-Yu Wang, . Ruo. -Yu Liu, Fang-Kun Peng and P.H.T. Tam. [1] CCAPP , Ohio State University, USA (with John . Shielding Materials Daniel R. McAlister , Ph.D. PG Research Foundation, Inc. 1955 University Lane Lisle, IL 60532, USA Revision 6 . 1 June 18 , 201 8 Introduction Attenuation or s hielding of gamma r Flashes. Gamma Ray . Astronomy. . Beginning. started . as a small budget research program in 1959. monitor. ing. compliance with the 1963 Partial Test Ban Treaty by the Soviet Union, and other nuclear-capable states. Observing Galactic Center & . Dark Matter . Search. MAGIC Team. . Ryoma. Murata (UT B3). Hiroki . Sukeno. (UT B3). Tomohiro Inada (Kobe Univ. B3. ). Fermi . Team. . Yuta. Sato (TUS B4). Taketo Mimura (. T. elescope. Liz Hays. NASA GSFC. Lecture Plan. The Fermi Observatory. Science Motivation. Instruments. Detecting gamma rays with the Large . A. rea Telescope. Instrument Subsystems. Angular resolution. 1. W.Blotz. Motivation. Southern Wide field-of-view Gamma-ray Observatory (SWGO). Planned to be built to monitor the Southern sky. Look for transient phenomena and extended sources. What should be the energy range of the observatory?. 1. Author:. Name. Affiliation. Address. Email. Menzo Wentink. Qualcomm. Utrecht,. The Netherlands. mwentink. qti qualcomm. Introduction. These slides show some simulation results in a scenario with 3 Wi-Fi networks and 6 narrowband (NB) links in...