1 / 50

AGILE

AGILE. M. Tavani. INAF, Roma, 15 dic. 2003. EGRET. EGRET 30 MeV-30 GeV (1.8 tons) Spark chamber TOF Calorimeter (NaI). EGRET gamma-ray sky (>100 MeV). EGRET Galactic Sources (>100 MeV). 3EG J1835+5918 (Isolated Neutron Star?). Vela pulsar. 3EG J0010+7309 (CTA 1 SNR?). Geminga.

wilton
Télécharger la présentation

AGILE

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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 ?

  6. AGNs detected above 30 MeV by EGRET

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

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

  9. GRBs from stellar explosions…

  10. The mystery of the unidentified gamma-ray sources

  11. 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

  12. EGRET AGILE

  13. 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

  14. 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)

  15. AGILE: Attività in area romana

  16. 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

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

  18. 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

  19. 5

  20. EM Super-Agile

  21. Super-Agile: GRB detection capability

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

  23. Super-Agile detection capability forGalactic sources Extragalactic sources

  24. 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:

  25. GRID angular response vs. EGRET

  26. AGILE Data Handling System

  27. 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

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

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

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

  31. 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

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

  33. Super-AGILE effective area

  34. Super-Agile sensitivity

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

  36. GRID Effective Area 20-100 MeV

  37. AGILE-GRID angular resolution

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

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

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

  41. EGRET Cycle-1 pointings

  42. 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

More Related