1. AGILE M. Tavani INAF, Roma, 15 dic. 2003

2. EGRET

3. EGRET • 30 MeV-30 GeV • (1.8 tons) • Spark chamber • TOF • Calorimeter (NaI)

4. EGRET gamma-ray sky (>100 MeV)

5. EGRET Galactic Sources (>100 MeV) 3EG J1835+5918 (Isolated Neutron Star?) Vela pulsar 3EG J0010+7309 (CTA 1 SNR?) Geminga 2CG 135+1 (LSI +61o303 ?) Crab (pulsar & SNR) -Cygni SNR ? Orion Cloud 3EG J1837-0423 (unidentified transient) Galactic Center ?

7. AGNs detected above 30 MeV by EGRET

8. Strongest AGN γ-ray flare, but… PKS 1622-287

10. GRBs and a subclass of Type Ic SNe (hypernovae: very broad spectral lines)SN 1998bw - GRB 980425SN 2003dh - GRB 030329

11. GRBs from stellar explosions…

12. The mystery of the unidentified gamma-ray sources

13. Excellent gamma-ray imaging with a large Field-of-View (2.5 sr) Simultaneous broad-band spectral information (15-40 keV, 30 MeV – 30 GeV) Microsecond timing Efficient transient detection and alerts AGILE: Italian Small Mission

14. EGRET AGILE

15. AGILE, is an ASI Small Scientific Mission with crucial participation by IASF/INAF, INFN, CIFS Total satellite mass ~ 330 kg Scientific Instrument mass 120 kg

16. Scientific Institutes involved in the development of the AGILE Payload and Mission (PI: M. Tavani, IASF-Roma, co-PI: G. Barbiellini, INFN, Ts) • IASF - CNR, sez. Milano • IASF - CNR, sez. Bologna • IASF - CNR, sez. Roma • INFN- Sez. Trieste • INFN- Sez. Roma I • INFN- Sez. Roma II • Università di Trieste • Università di Roma “Tor Vergata” • Università “La Sapienza” • CIFS - Consorzio Interuniversitario per la Fisica Spaziale (Torino)

17. AGILE: Attività in area romana

18. Gestione scientifica dell’intera Missione Realizzazione dell’imager-X (Super-Agile) Sviluppo e test Data Handling Sviluppo SW analisi dati X e gamma Calibrazioni scientifiche Supporto all’ASDC Astrofisica X e gamma Contributi dell’AGILE Team dell’area romana

19. Super-Agile: X-ray imaging (15-40 keV) AGILE Engineering Model

20. E. Costa IASF sez. Roma M. Feroci IASF sez. Roma I. Lapshov IKI, Moscow, and IASF sez. Roma F. Lazzarotto CIFS Torino, and IASF-CNR sez.Roma M. Mastropietro IASF sez. Roma E. Morelli IASF sez. Bologna L. Pacciani IASF sez. Roma G. Porrovecchio IASF sez. Roma B. Preger IASF sez. Roma M. Rapisarda ENEA, sez. Roma A. Rubini IASF sez. Roma P. Soffitta IASF sez. Roma M. Del Monte IASF sez. Roma M. Frutti IASF sez. Roma L. Barbanera IASF sez. Roma Super-AGILE Team

21. 5

22. EM Super-Agile

23. Super-Agile: GRB detection capability

24. Alerts for GRB and other transients:AGILE Fast Link (ORBCOMM)

25. Super-Agile detection capability forGalactic sources Extragalactic sources

28. optimal imaging capabilities and large FOV in the energy bands: * 15 keV - 40 keV (Super-Agile) * 30 MeV - 50 GeV(GRID: Tracker+MCAL) (2) Excellent X-ray/γ-ray timing (GPS) (3) Burst search with large dynamic range (sub-milliseconds-60 seconds) and independent triggering of the Mini-Calorimeter (300 keV-100 MeV). 3 innovative features of AGILE:

29. GRID angular response vs. EGRET

30. AGILE Data Handling System

31. M. Tavani IASF sez. Roma, and Univ. “Tor Vergata” T. Froysland CIFS Torino, and INFN sez. Roma-2 P. Lipari Università “La Sapienza”,and INFN sez. Roma-1 A. Morselli Università “Tor Vergata”, and INFN sez. Roma-2 P. Picozza Università “Tor Vergata”, and INFN sez. Roma-2 C. Pittori Università “Tor Vergata”, and INFN, sez. Roma-2 D. Zanello INFN sez. Roma-1, and Università “La Sapienza” Data Handling and Analysis group

32. AGILE pointing strategy optimized with ground based observations (radio, optical, TeV)

33. Gamma-ray exposure (~1 year) EGRET AGILE ~ 3·108 cm² s sr (~4 yrs) ~ 3·109 cm² s sr (~1 yrs)

34. AGNs Gamma-Ray Bursts Pulsars Unidentified gamma-ray sources SNRs X-ray transients, Galactic compact obj. Millisecond transients and fundamental physics Main science topics

35. ATTIVITA’ DI AGILE ANALISI DATI TEORIA ASTROFISICA AAE PI-ship GESTIONE TECNICA DI PAYLOAD E SCIENTIFICA DI MISSIONI R & D • REALIZZAZIONE • PAYLOAD • HW realizzato • in casa • 2. Supervisione • contratti • industriali ASDC

39. Super-Agile Field of View (~1 sr)(on-axis sensitivity: ~5 mCrab @15 keV)

40. Super-AGILE effective area

41. Super-Agile sensitivity

42. Super-Agile sensitivity (10-40 keV)

43. GRID Effective Area 20-100 MeV

44. AGILE-GRID angular resolution

45. (Aeff * T)1/2 vs. Time (orbital phase) 20 < θ < 40, GLAST Upper-Tracker vs. AGILE

46. On-board GRID background rejection(Simulations by Cocco, Longo, Giuliani, Pellizzoni, Lipari, Pittori, Tavani, 2000-2002)

47. Super-Agile mapping(Lapshov, Preger, Feroci, Soffitta, 2001-2002)

48. EGRET Cycle-1 pointings

50. AGILE gamma-ray spectral deconvolution (preliminary, A. Giuliani et al.) F = 1/5 Crab F= k (E/100)–a Assumed values: k= 2.4 10 –14 a= 2 Fit values: k= 2.49 +0.38 –0.34 a= 2.016+0.234 -0.196