Aldo Morselli INFN Roma Tor Vergata On behalf of Marco Tavani and the AGILE Team
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1 the AGILE space mission Aldo Morselli INFN Roma Tor Vergata On behalf of Marco Tavani and the AGILE Team Annapolis Sept th INTEGRAL Workshop A Synergistic View of the High Energy Sky Aldo Morselli, INFN Roma Tor Vergata! 1!
2 the AGILE space mission AGILE Aldo Morselli INFN Roma Tor Vergata On behalf of Marco Tavani and the AGILE Team Annapolis Sept th INTEGRAL Workshop A Synergistic View of the High Energy Sky Aldo Morselli, INFN Roma Tor Vergata! 2!
3 the AGILE space mission AGILE Aldo Morselli INFN Roma Tor Vergata On behalf of Marco Tavani and the AGILE Team Annapolis Sept th INTEGRAL Workshop A Synergistic View of the High Energy Sky Aldo Morselli, INFN Roma Tor Vergata! 3!
4 The beginning Aldo Morselli, INFN Roma Tor Vergata! 4!
5 Compton Observatory figure Aldo Morselli, INFN Roma Tor Vergata! 5!
6 Compton Observatory Scheme Aldo Morselli, INFN Roma Tor Vergata! 6!
7 High Energy Gamma Experiments Experiments ~1993 Aldo Morselli, INFN Roma Tor Vergata! 7!
8 The CAPRICE 94 flight 8 Aldo Morselli, INFN Roma Tor Vergata! 8!
9 The TS93 and CAPRICE silicon-tungsten imaging calorimeter. 48 cm 48 cm 9 Aldo Morselli, INFN Roma Tor Vergata! 9!
10 Aldo Morselli, INFN Roma Tor Vergata! 10!
11 GILDA Aldo Morselli, INFN Roma Tor Vergata! 11!
12 So we were ready to respond to the Call for Ideas for Small Missions ASI (Sciences of the Universe) 26 June 1997 and responded with two proposals:: GILDA 40 and AGILE Aldo Morselli, INFN Roma Tor Vergata! 12!
13 Aldo Morselli, INFN Roma Tor Vergata! 13!
14 Aldo Morselli, INFN Roma Tor Vergata! 14!
15 Aldo Morselli, INFN Roma Tor Vergata! 15!
16 THE AGILE MISSION Aldo Morselli, INFN Roma Tor Vergata! 16!
17 AGILE Silicon Tracker prototype 121 µm Aldo Morselli, INFN Roma Tor Vergata! 17!
18 The Silicon Tracker Aldo Morselli, INFN Roma Tor Vergata! 18!
19 The Silicon Tracker Aldo Morselli, INFN Roma Tor Vergata! 19!
20 AGILE: inside the cube HARD X-RAY IMAGER (SUPER-AGILE) Energy Range: kev SILICON TRACKER ANTICOINCIDENCE GAMMA-RAY IMAGER (GRID) Energy Range: 30 MeV - 30 GeV (MINI) CALORIMETER Energy Range: MeV Aldo Morselli, INFN Roma Tor Vergata! 20!
21 SAS-2! 11/1972-7/1973!! Anti-Coincidence Dome! Spark Chamber! Trigger Telescope! Cerenkov Counter! Energy Calorimeter! EGRET! 4/ ! Cos-B! 8/1975-4/1982! AGILE! 2007-! Aldo Morselli, INFN Roma Tor Vergata! 21!
22 AGILE on PSLV-C8 Sriharikota, India April 2007 The AGILE Payload: the most compact instrument for high-energy astrophysics: only ~100 kg ~ cm Payload ASI Mission with INFN, INAF e CIFS participation γ-ray astrophysics: 30 MeV - 30 GeV energy range and simultaneous X-ray capability between kev Aldo Morselli, INFN Roma Tor Vergata! 22!
23 April 23, 2007: Launch! SHAR base (Chennai), India Equatorial orbit: 550 Km, < 3º inclination angle Aldo Morselli, INFN Roma Tor Vergata! 23!
24 AGILE orbital parameters Baseline equatorial orbit: 550 Km, 3º inclination Semi-major axis: km (± 0.1 km) Requirement: ± 10 km Inclination angle: 2.48 (±0.04 ) Requirement: < 3 Eccentricity: (±0.0015) Requirement: < 0.1 TPZ orbital decay estimate: Height < 400Km on 20/04/2017 (A/M=0.009 sqm/kg) Worst case (A/M=0.012 sqm/kg): 02/11/2015 Best case (A/M=0.006 sqm/kg): 29/04/2023 (March 2013 updated estimate, using recent solar flux Schatten forecasts + 2σ) You can follow AGILE with AGILE Science App.!! Aldo Morselli, INFN Roma Tor Vergata! 24!
25 Aldo Morselli, INFN Roma Tor Vergata! 25!
26 AGILE Total Intensity Map (E> 100 MeV) Pointing + Spinning (up to july 30, 2011) The First AGILE-GRID Catalog of High Confidence Gamma-Ray Sources C. Pittori et al., A&A 506, 2009 Aldo Morselli, INFN Roma Tor Vergata! 26!
27 AGILE: 7th year in orbit AGILE demonstrates for the first time the covering of ~ 1/5 of the entire gamma-ray sky (FoV ~ 2.5 sr) with excellent angular resolution and competitive sensitivity. AGILE shows for the first time an optimal performance of its gamma-ray and hard X-ray imagers. Pointing observation mode up to October 18, 2009 and spinning observation mode since October Very good scientific performance, especially at ~ 100 MeV Guest Observer Program open to the scientific community: Cycle-1: completed, Dec. 1, 2007 Nov 30, 2008 Cycle-2: completed, Dec. 1, 2008 Nov 30, 2009 Cycle-3: completed, Dec. 1, 2009 Nov 30, 2010 Cycle-4: completed, Dec. 1, 2000 Nov 30, 2011 Cycle-5 and Cycle-6: on-going data taking Aldo Morselli, INFN Roma Tor Vergata! 27!
28 AGILE: very fast Ground Segment (with contained costs) Satellite Malindi Ground Station ~1 hr Fucino TZP MOC ASDC AGILE Team Automatic data processing ~0.5 hr ~0.5-1 hr Guest Observers ~(2-2.5) hr Public data access Record for a gamma-ray mission! Aldo Morselli, INFN Roma Tor Vergata! 28!
29 The variable Crab Nebula! FIRST&PUBLIC&ANNOUNCEMENT&& Sept.&22,&2010:&AGILE&issues&the& Astronomer s&telegram&n.&2855& announcing&a&gammajray&flare&from& the&crab&nebula& &Science&Express&(6&January&2011)&&&&&&& Aldo Morselli, INFN Roma Tor Vergata! 29!
30 Sect. 6.1 Notes on individual sources: AGILE&first&detecUon&of&a&strong&& gammajray&flare&in&oct.&2007& reported&in&the&first&agile&source& catalog&as&possible&short& unexpected&flux&increase&& Flare date Duration Peak γ-ray flux Instruments October 2007 ~ 15 days ~ ph cm -2 s -1 AGILE February 2009 ~ 15 days ~ ph cm -2 s -1 Fermi September 2010 ~ 4 days ~ ph cm -2 s -1 AGILE, Fermi April 2011 ~ 2 days ~ ph cm -2 s -1 Fermi, AGILE March 2013: new γ-ray flaring state detected by Fermi and AGILE a big theoretical challenge: the Crab Nebula is not a standard candle in gamma-rays! Aldo Morselli, INFN Roma Tor Vergata! 30!
31 AGILE&gammaJray&monitoring&of&the&Crab&& 31 Aldo Morselli, INFN Roma Tor Vergata! 31!
32 AGILE MAIN GALACTIC DISCOVERIES above 100 MeV Aldo Morselli, INFN Roma Tor Vergata! 32!
33 Carina region: γ-ray detection of the colliding wind massive binary system η-car with AGILE Tavani et al.[agile Coll.], ApJ, 698, L142, 2009 (arxiv: ) Cygnus region microquasars: AGILE observations of Cygnus X-1 gamma-ray flares Sabatini et al.[agile Coll.], ApJ 2010, Del Monte et al., A&A 2010 AGILE detects several gamma-ray flares from Cygnus X-3, and also weak persistent emission above 100 MeV Tavani et al.[agile Coll.], Nature 462, 620, 2009 (arxiv: ) Detection of Gamma-Ray Emission from the Vela Pulsar Wind Nebula with AGILE Pellizzoni et al.[agile Coll.], Science 327, 2010 Neutral pion emission from accelerated protons in the SNR W44 Giuliani et al.[agile Coll.], ApJ, 742, 2011 Aldo Morselli, INFN Roma Tor Vergata! 33!
34 Microquasars Open questions (pre-agile): Can jet formation accelerate relativistic particles? Can the jet emit γ-rays above 100 MeV? The discovery of the γ-ray activity from Cygnus X-3 is the proof of extreme particle acceleration in microquasars. Aldo Morselli, INFN Roma Tor Vergata! 34!
35 The Cygnus region in γ-rays: AGILE Intensity Map (100 MeV-10 GeV) Pointing Mode: Nov Oct. 2009, ~13 Ms net exposure time SNR G (Gamma Cygni) AGILE GO pulsar (Halpern) 3 pulsars 3 TeV sources 2 microquasars Aldo Morselli, INFN Roma Tor Vergata! 35!
36 The γ-ray detection of Cygnus X-3: December 2, 2009: The AGILE-GRID detects 4 γ-ray flares from Cygnus X-3 ( Extreme particle acceleration in the microquasar Cygnus X-3, Tavani et al., Nature)! γ-ray flaring-fluxes greater than 1 order of magnitude with respect to the steady flux! coincident with prominent minima of the hard X-ray flux! a few days before major radio flares December 11, 2009: brief story of a discovery Fermi-LAT confirms AGILE detections ( Modulated High-Energy Gamma-Ray Emission from the Microquasar Cygnus X-3, Abdo et al., Science)! γ-ray detection of the orbital period (4.8 hours) temporal signature of the microquasar In 9 days a long-lasting mystery has been solved: Cygnus X-3 is able to accelerate particles up to relativistic energies and to emit γ-rays above 100 MeV! Aldo Morselli, INFN Roma Tor Vergata! 36!
37 Major gamma-ray flares in special transitional states in preparation of radio flares! Gamma-ray flares tend to occur in the rare lowflux/pre-flare radio states. For all gamma-ray flaring episodes, the radio and hard-x-ray fluxes are low or very low, while the soft X-ray flux is large figure adapted from Szostek Zdziarski & McCollough (2008) Aldo Morselli, INFN Roma Tor Vergata! 37!
38 Origin of Cosmic Rays Cosmic rays are particles (mostly protons) accelerated to relativistic speeds. Despite wide agreement that supernova remnants (SNRs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. When accelerated protons encounter interstellar material they produce neutral pions, which in turn decay into gamma rays. This offers a compelling way to detect the acceleration sites of protons. The identification of pion-decay gamma rays has been difficult because high-energy electrons also produce gamma rays via bremsstrahlung and inverse Compton scattering. Aldo Morselli, INFN Roma Tor Vergata! 38!
39 First evidence of proton acceleration in the Supernova Remnant W44 with AGILE A. Giuliani et al.[agile Coll.], ApJ 742, 2011 Aldo Morselli, INFN Roma Tor Vergata! 39!
40 Detection of the Characteristic Pion-decay Signature in Supernova Remnants Direct evidence that cosmic-ray protons are accelerated in SNR M.Ackermann et al.[fermi Coll.],Science 339 (2013) 80 [arxiv: ] Aldo Morselli, INFN Roma Tor Vergata! 40!
41 AGILE detected GRB A: the most energetic gamma-ray burst yet! Aldo Morselli, INFN Roma Tor Vergata! 41!
42 GeV emitting GRBs as high fluence events AGILE detected all the major characteristics of HE GRB (delayed emission, extended emission, power-law extracomponent) A cross calibration work with Fermi has started. Longo et al. [AGILE Coll.] 2012 A&A 547 Aldo Morselli, INFN Roma Tor Vergata! 42!
43 MCAL GRB catalog Contains the data of the 85 hard gammaray bursts observed by the MCAL (April October 2009) Timing data for 84 and spectral data for 21 bursts Galli et al.[agile Coll.] 2013, A&A, 553, A33 (2013) [arxiv: ] Aldo Morselli, INFN Roma Tor Vergata! 43!
44 AGILE: SURPRISES FROM THE EARTH ATHMOSPHERE Aldo Morselli, INFN Roma Tor Vergata! 44!
45 TGF Cumulative spectrum 110 TGFs 1806 photons 142 γ E> 10 MeV 26 γ E> 20 MeV RREA cutoff powerlaw model Broken powerlaw model β = -2.7 Significant detection of γ% >40 MeV!! Uneplained by standard RREA model: challenge for emission models Tavani et al.[agile Coll.], Phys. Rev. Lett. 106, (2011) AGILE-MCAL crucial spectral contribution up to 100 MeV!! Aldo Morselli, INFN Roma Tor Vergata! 45!
46 Normal lightnings involve a potential difference ~ 500 kvolts Terrestrial Gamma-Ray Flashes (TGF) involve DV > 100 MVolts! Models??: Relativistic Runaway Electron Avalanche (RREA) with relativistic feedback (Dwyer 2008). Bremsstrahlung + Compton scattering. Much theoretical work in progress RHESSI cumulative spectrum compatible with a production altitude of km (just above tropical thunderstorms) AGILE MCAL: an optimal detector for TGF MCAL energy range is extended up to 100 MeV Efficient trigger at ms and sub-ms time scale (the TGF time scale) AGILE equatorial orbit at 2.5 inclination is optimal for mapping the equatorial region, where most of the events take place A real-time monitoring and alert system can be implemented for correlation with other meteo resources (work in progress)" Aldo Morselli, INFN Roma Tor Vergata! 46!
47 a&future&axer&fermi&and&agile&?& Silicon(technology(very(well(tested(and(very( robust.( SubstanUal&PSF&improvement&expected&by&a& combinauon&of&noj&converter&+&analog&readout.& 47( Aldo Morselli, INFN Roma Tor Vergata! 47!
48 Conclusion : picture(of(the(day,(feb.(28,(2011,(nasacheasarc( 48 Aldo Morselli, INFN Roma Tor Vergata! 48! stay tuned! AGILE& Fermi&
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