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OUTLINE

OUTLINE. Overview Instruments Scientific Objectives. AGILE MISSION. Prepared by ASI with the participants INFN&IASF. Sensitive in the range 30 Mev-50 Gev & 15-45keV. Having a large FOV covering 1/5 of the entire sky at energies above 30Mev.(3 sr)

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OUTLINE

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  1. OUTLINE • Overview • Instruments • Scientific Objectives

  2. AGILE MISSION • Prepared by ASI with the participants INFN&IASF. • Sensitive in the range 30 Mev-50 Gev & 15-45keV. • Having a large FOV covering 1/5 of the entire sky at energies above 30Mev.(3 sr) • Based on the state-of-the-art technology of solid state Silicon detectors and associated electronics developed in Italian Lab. • 120kg (the total satellite mass is 350kg) • Primary scientific goals include the study of ; -AGN -GRBs -Galactic sources -Unidentified Gamma-ray sources -Diffuse Gamma-ray emission -High-precision timing studies -Quantum Gravity testing

  3. AGILE was succesfully launched on April 23, 2007 at 10:00 GMT in an equatorial orbit with an altitude of 550 km and inclination of  0-6 deg.by the Indian PSLV rocket from the Shriarikota ISRO base (Chennai-Madras), India. AGILE Launch PSLV-C6

  4. Fig7:The AGILE operations and Ground Segment.

  5. AGILE MISSION

  6. INSTRUMENTS Fig1:LEFT:The AGILE integrated satellite in its final configuration. RIGHT:Hard X-ray imager,the gamma-ray Tracker, and the Calorimeter.

  7. TheAGILEpayload is made of three detectors combined into one integrated instrument with broad-band detection and imaging capabilities.The Anticoincidenceand Data Handling systemscomplete instrument. 1.The Gama-Ray Imaging Detector (GRID) 2.The Hard X-ray Imager (Super-AGILE) 3.The Mini-Calorimeter (MC)

  8. The Gamma-Ray Imagıng DetectorGRID • Sensitive in the range30Mev-50Gev • Consisting of ; - A Silicon-Tungsten Tracker - A Cesium Iodide Calorimeter - The Anticoincidence System • Characterised by the smallest ever obtaineddeadtime≲200μs • Source location accuracy15´ • FOV2.5 sr Fig2:Engineering model of the AGILE instrument. The GRID is made of 12 silicon-tungsten planes and the Mini Calorimeter positioned at the bottom of the instrument.

  9. THE SILICON-TRACKERST Fig4:The Silicon-Tracker

  10. Providing the γ-ray imager is based on photon conversion into electron-positron pairs. • Consisting of a total of 12 trays… • The fundamental Silicon detector unit is a tile of area 9.5x9.5 cm2,microstrip pitch equal to 121 μm,and thickness 410 μm(Fig5). • The adopted ‘floating readout strip ’ system has a total of 384 readout channels and three readout TAA1 chips per Si-tile.

  11. Fig5:Schematic layout of the fundamental 9.5x9.5 cm2 unit(tile) of the AGILE Sİ-Tracker.

  12. Fig6:Left and right panels;an example of two environmental γ-ray events produced by cosmic-rays and detected by the AGILE-GRID during the integrated satellite scientific acquisiiton runs with the whole ST trigger logic implemented.(May 2006)

  13. Fig6: (Tracking perf.)Schematic rep.and typical results of beamtests carried out at CERN. The right panel shows the results of the AGILE beamtest carried out in August,2000 at the CERN T11 beamline.(East Hall,CERN PS)

  14. MINI CALORIMETERMC • Operating in the ‘burst’ mode is the 3rd AGILE detector. • The energy range for this non-imaging detector is 25keV-200MeV. • Made of 30 Thallium activated Cesium Iodide (CsI(Tl)) bars arranged in two planes,for a total radiation length 1.5 X 0. The signal from each CsI bar is collected by two photodiodes placed at both ends. • deadtime 5 μs • The main goals are ; • obtaining additional information on the energy deposited in the CsI bars…. • detecting GRBs and other impulsive events with spectral and intensity information in the range ~0.3-100MeV

  15. THE ANTICOINCIDENCE SYSTEM AC • Aimed at both charged particle background rejection and preliminary direction reconstruction for triggered photons. • Completely surrounding with AGILE detectors. • Each lateral face segmented in three plastic scintillator layers connected with photomultipliers placed at the bottom.

  16. The operating principle of GRID is based on; the conversion of γ-ray photons in electron-positron pairs by thin tungsten sheets and tracking the pairs, in energy and directions, by microstrip silicon detectors,thus reconstructing the kinematic of the impinging photon(Feroci,M. et al.2007)

  17. 2. The Hard X-Ray ImagerSuper-AGILE Fig7:Super-AGILE

  18. 2. The Hard X-Ray ImagerSuper-AGILE • Sensitive in the 15-45keV • Made of properly arranged four square detectors(19x19cm2) • # of readout channels is 6.144 • Scientific goals ; i)photon-by-photon detection and imaging -in10-40keV, -with a FOV of≳1 sr, -good angular resolution2arcmin, ii)simultaneous X-ray and γ-ray spectral studies of high energy sources iii)excellent timing≲4 μs iv)burst trigger for the GRID and MC v)burst alert and quick on-board positioning capability for transient and GRBs first detected GRB...

  19. AGILE’s SCIENTIFIC OBJECTIVES • AGN -wide FOV survey. -quick reaction to transients. -SA monitoring in the hard X-ray band. -correlative obs. in the radio,optical,X-ray,TeV • GRB -expected detection rate above 50 MeV:5-10 event/year -broad-band spectral information -SA imaging(~1’-2’ for intense GRBs) -search for sub-milisecond GRB pulses

  20. PULSARS -high-resolution timing of known γ-ray pulsars, -period searches for Galactic unidentified sources, -milisecond pulsars. • UNIDENTIFIED SOURCES -deep exposure,variability studies, -refined positions,search for counterparts, -serach for new transients and quicklook alert • SUPERNOVA REMNANTS -search and precise imaging with deep exposures -monitoring of plerions in SNRs -γ-ray /TeV studies

  21. BINARY SYSTEMS -neutron star binaries, -black-hole systems;microquasars -interacting binaries, -SA monitoring and simultaneous detection. • DIFFUSE EMISSION -deep exposure and precise mapping mapping of Galactic emission, -study of cosmic-ray origin and propagation • GALAXIES -deep pointings at the SMC and LMC -testing dark matter model(by deep exposures of Andromeda) -deep exposures of cluster of galaxies

  22. SOLAR FLARES -Si-tracker ratemeter transient detection(≳100keV), -MC detection in the range 25keV-200MeV, • FUNDAMENTAL PHYSICS -quantum gravity tests for sub-ms GRB pulses, -high-precision pulsar timing and QG effects, -MACHO emission from our and nearby galaxies.

  23. Fig8:Density map (in counts s-1 sr-1) of gamma-rays above 30 MeV (in polar coordinates where the radial distance provides the zenithal angle θ ,  and the polar angle corresponds to the azimuthal angle) detected by the AGILE instrument in the IABG facility. Despite the strong angular dependence of the gamma-ray background - intensity proportional to  a function between cos3 (θ)  and cos4 (θ) - AGILE is capable of detecting gamma-rays with large incidence angles up to 50-60 degrees. This is the largest field of view (FOV) ever achieved by a space gamma-ray instrument

  24. REFERENCES 1.Science with AGILE,2004 http://agile.asdc.asi.it/a-science-27.pdf 2. The AGILE mission and its scientific instruments ,Tavani,M. Et al, 2006SPIE.6266E.2T 3. Gamma-ray Astrophysics with the Space AGILE Detector,Pittori,C.;Tavani,M.;the AGILE Team,2006ChJAS.6a.373P 4.ASI Data Center http://agile.rm.iasf.cnr.it/

  25. FINE

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