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)

Geminga

Vela pulsar

Galactic Center ?

Orion Cloud

3EG J1835+5918 (Isolated Neutron Star?)

3EG J0010+7309 (CTA 1 SNR?)

2CG 135+1 (LSI +61o303 ?)

-Cygni SNR ?

3EG J1837-0423 (unidentified transient)

Crab (pulsar & SNR)

AGNs detected above 30 MeV by EGRET

Strongest AGN γ-ray flare, but…

PKS 1622-287

GRBs and a subclass of Type Ic SNe (hypernovae: very broad spectral lines)

SN 1998bw - GRB 980425SN 2003dh - GRB 030329

GRBs from stellar explosions…

The mystery of the unidentified gamma-ray sources

• 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

EGRET AGILE

• 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

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)

AGILE: Attività in area romana

Contributi dell’AGILE Team dell’area romana

• 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

Super-Agile: X-ray imaging (15-40 keV)

AGILE Engineering Model

Super-AGILE Team

• 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

5

EM Super-Agile

Super-Agile: GRB detection capability

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

Super-Agile detection capability forGalactic sources Extragalactic sources

(1) 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:

GRID angular response vs. EGRET

AGILE Data Handling System

D A T A H A N D L IN G H A R D W A R E S O F T W A R E

G P S

S S A C

S T

M C A L

S A

G R ID : T R IG G E R 1 & 1 .5

R E A D O U T P R E -P R O C E S S IN G

B U R S T : M C A L B U R S T D A Q

S A B U R S T IM A G IN G

S A : P H O T O N -B Y -P H O T O N

G R ID : C L U S T E R ID

M C A L Z E R O -S U P P R E S S IO N

T R IG G E R 2

B U R S T : R IC E R C A D I B U R S T D E C O N V O L U Z IO N E

IM M A G IN I S A

T E L E M E T R I A

B U S

F A S T L IN K

O B T (r isp e tto a ll`U T C ): t < 2 µ s M a r c a tu r a te m p o r a le – G R ID : t < 2 µ s M a r c a tu r a te m p o r a le – S A , M C A L : t < 5 s R ic o str u z io n e d `a sse tto : ~ 1 a r c m in .

S ilic o n T r a c k e r : 3 6 8 4 4 c a n a li S u p e r -A G IL E : 6 1 4 4 c a n a li M in i-C a lo r im e tr o : 6 0 c a n a li A n tic o in c id e n za : 1 6 c a n a li

Data Handling and Analysis group

• 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”

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

Gamma-ray exposure (~1 year)

EGRET AGILE

~ 3·108 cm² s sr

(~4 yrs)

~ 3·109 cm² s sr

(~1 yrs)

Main science topics

• AGNs• Gamma-Ray Bursts• Pulsars• Unidentified gamma-ray sources• SNRs • X-ray transients, Galactic compact obj.• Millisecond transients and fundamental

physics

ANALISI DATITEORIA

ASTROFISICAAAE

PI-shipGESTIONE

TECNICA DI PAYLOADE SCIENTIFICA DI MISSIONI

R & D

REALIZZAZIONEPAYLOAD

1. HW realizzatoin casa

2. Supervisione contratti industriali

ATTIVITA’ DI AGILE

ASDC

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

Super-AGILE effective area

Super-Agile sensitivity

Super-Agile sensitivity (10-40 keV)

GRID Effective Area

20-100 MeV

AGILE-GRID angular resolution

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

On-board GRID background rejection (Simulations by Cocco, Longo, Giuliani, Pellizzoni, Lipari,

Pittori, Tavani, 2000-2002)

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

EGRET Cycle-1 pointings

AGILE gamma-ray spectral deconvolution (preliminary, A. Giuliani et al.)

F = 1/5 Crab

F= k (E/100) –

Assumed values:k= 2.4 10 –14

= 2

Fit values:k= 2.49 +0.38 –0.34

2.016+0.234 -0.196