AGILE1 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 1
Agile 5 invited talks Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 2 2
AGILE Pubblicazioni Risultati 2009-2010 Multiwavelength Observations of a TeV-Flare from W Comae ApJ, 690, 2009, 1018-1030 Discovery of extreme particle acceleration in the microquasar CygnusX-3 Nature 462, 620-623 published online 22 November 2009 [arxiv:0910.5344] Detection of Gamma-Ray emission from the Eta-Carinae Region ApJ Letters 698 No 2 (2009) L142-L146, [arxiv:0904.2736] Discovery of new gamma-ray pulsars with AGILE ApJ 695 No 1 (2009 April 10) L115-L119, [arxiv:0903.0087] First AGILE Catalog of High Confidence Gamma-Ray Sources A&A 506, 1563-1574 (2009) [arxiv:0902.2959] The June 2008 flare of Markarian 421 from optical to TeV energies ApJ 691 No 1 (2009 January 20) L13-L19 [arxiv:0812.1500] Multiwavelength observations of 3C 454.3 II. The AGILE 2007 December campaign Astrophys. J. 707 (2009) 1115-1123 The extraordinary gamma-ray flare of the blazar 3C 454.3 Astrophysical Journal 718 (2010) 455 [arxiv:1005.4891] Direct evidence for hadronic cosmic-ray acceleration in the supernova remnant IC 443 ApJ (2010) 710 L151 [arxiv:1001.5150] Agile Detection of Delayed Gamma-Ray Emission from the Short Gamma-Ray Burst GRB 090510 ApJ 708 (2010) L84 [arxiv:0908.1908] Episodic Transient Gamma-Ray Emission From The Microquasar Cygnus X-1 3 ApJ 712 (2010) L10-L15 [arxiv:1002.4967] 3
AGILE Pubblicazioni Risultati 2009-2010 AGILE detection of GeV gamma-ray emission from the SNR W28 A&A 516 (2010) L11 Detection of Gamma-Ray Emission from the Vela Pulsar Wind Nebula with AGILE Science 327 (2010) 663-665 AGILE detection of a rapid gamma-ray flare from the blazar PKS1510-089 during the GASP-WEBT monitoring A&A. 508 1 (2009) 181-189 Monitoring the hard X-ray sky with SuperAGILE A&A 510 (2010) A9 Detection of Terrestrial Gamma-Ray Flashes up to 40 MeV by the AGILE satellite J. Geophys. Res., 115 (2010) Multiwavelength observations of 3C 454.3. III. Eighteen months of AGILE monitoring of the "Crazy Diamond" Astrophys.J. 712 (2010) 405-420 [arxiv:1002.1020] Temporal properties of GX 301-2 over a year-long observation with SuperAGILE Astrophys. J. 708 (2010) 1663-1673 A year-long AGILE observation of Cygnus X-1 in hard spectral state A&A Accepted Gamma-Ray Localization of Terrestrial Gamma-Ray Flashes Accepted by Phys. Rev. Lett. (2010) AGILE detection of intense gamma-ray activity from the blaza PKS 0537-441 in October 2008 A&A Accepted +... 4 lista completa su http://people.roma2.infn.it/~agile/agile_pub.html 4
The AGILE gamma-ray sky (E > 100 MeV) 2 year exposure: July 2007 June 2009 5 5
Some of the highlights Black hole astrophysics -Discovery of gamma-ray emission from Cyg X-3 and Cyg X-1: microquasar patterns, extreme particle acceleration (not Comptonized!) -massive black hole jet ejections, particle acceleration Origin of cosmic rays, SNR surprises New Galactic gamma-ray transients Pulsars and Pulsar Wind Nebulae GRB surprises Terrestrial gamma-ray Flashes 6 6
The brightest Gamma-ray blazars detected by AGILE PKS 0716+714 3C 454.3 7 7
The brightest gamma-ray blazars detected by AGILE 3C 454.3 HB 1510-089 TXS 0716+714 3C 279 3C 273 Mrk 421 PKS 0537-441 spectral properties radio/optical/x-ray vs. gamma BL Lacs and BZ limit why always the same blazars? 8 8
The AGILE gamma-ray sky, 3-4 December, 2009. Detection of the strongest gamma-ray flaring source ever observed: the black hole ( Crazy Diamond ) in the active galaxy 3C 454.3 (z=0.859, F γ > 2000 10-8 ph. cm -2 s -1,L iso = 6x10 49 erg s -1, for d =10, L jet 1 Earth/sec) the Vela pulsar the black hole Crazy Diamond in the galaxy 3C 454.3 9 9
Flux ( DRY ) INTERMEDIATE BL LACs (AGILE Coll. 2009) 0716+714 Kinetic power L T =3 x 10 45 erg / s L r =2 x 10 45 erg / s Blandford-Znajek limit 10 10
Galactic Sources Carina-Vela Regions Cygnus Region Galactic Center 11 11
12 Galactic Black Holes 12
Microquasar studies at gamma-ray energies Mechanisms of extreme particle acceleration and strongly non-thermal (or Comptonized) emission above 100 MeV Jet geometry can play a crucial role in detection (see the case of Cyg X-3) transient acceleration & gamma-ray emission on hourday timescales Gamma-ray emission in special states (Cyg X-3) Bright future for understanding BHs 13 13
Cyg X-3 appears to be special A very variable microquasar Very strong (up to 10-20 Jy) radio flares Jets pointing towards the Earth Correlated radio/soft X-ray/hard X- ray states 14 14
AGILE and Cygnus X-3 (Nature, Nov. 22, 2009) see also FERMI detection of Cyg X-3, Abdo et al. Science Nov. 26, 2009) AGILE detects several gamma-ray flares from Cygnus X-3, and also weak persistent emission above 100 MeV very interesting correlations with radio and X-ray spectral state changes gamma-ray flares usually before radio flares 15 15
Major gamma-ray flares in special transitional states in preparation of radio flares! (AGILE Coll. Nature 2009) figure adapted from Szostek Zdziarski & McCollough (2008) 16 16
Origin of Cosmic rays GeV γ-ray emission from the SNR W28 AGILE counts map above 400 MeV AGILE radio location claud S CO emission Cloud N claud N CO emission Cloud S The combined AGILE and H.E.S.S. data strongly support an hadronic model 17 for the gamma-ray production in W28 Agile Coll. [arxiv:1005.0784] 17
Origin of Cosmic rays 2 GeV γ-ray emission from the SNR IC 443 AGILE counts map above 400 MeV Fermi EGRET AGILE hadronic models Bremsstrahlung models VERITAS MAGIC MAGIC The combined AGILE and H.E.S.S. data support an hadronic model for the gamma-ray 18 production in IC 443 Agile Coll. ApJ (2010) 710 L151 arxiv:1001.5150 18
IC 443 19 19
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EGRET source (Hartman et al. 1999) TeV source (MAGIC,VERITAS) 21 21
AGILE: gamma-ray imaging (E> 400 MeV) of IC 443 22 22
Facts on IC 443 ~100 MeV source and TeV source are non coincident absence of IC emission above 10-100 GeV at cloud E : electron/proton ratio ~10-2 (see also Gaisser et al. 1998) absence of prominent TeV emission along the SN shock front (and of non-thermal X-ray emission): electron contribution subdominant cloud E provides the target for proton-proton interaction and pion production/decay hadronic model of production at cloud E is the only viable 23 23
Terrestrial Gamma-ray Flashes (TGF) Gamma-ray flashes with incoming direction compatible with the Earth surface. Few millisecond typical duration; hard spectrum (up to tens MeV) Discovered by BATSE (Fishman et al., Science, 1994) and observed by RHESSI up to 20 MeV (Smith et al., Science, 2005) Clearly associated to lightning discharges during thunderstorms by means of correlation with VLF sferic waves detection on ground (Inan et al., GRL, 1996; Cummer et al., GRL, 2005)>2008: Observed by AGILE and Fermi-GBM2009 AGILE reports energy up to 40MeV (Marisaldi et al., JGR 2010) Geophysical phenomena observed from space by instruments designed for gamma-ray astrophysics Challenging detection: timing and energy range are key issues 24 24
TGFs and Lightnings 25 LIS-OTD High Resolution Full Climatology available at http://thunder.msfc.nasa.gov/data/ Good match between AGILE TGF pattern and lightning map 25
Cumulative spectrum of the 130 TGFs detected by AGILE-MCAL during the period mid-2007/january 2010 AGILE data pre-agile phenomenological model submitted to Nature 26
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Dal Rapporto ASI 2010 l satellite AGILE è stato sottoposto a un cambiamento di configurazione a novembre 2009. Il satellite, che prima operava con puntamenti fissi che coprivano circa1/4-1/5 del cielo con una stabilità di puntamento di circa 1 grado, si è trovato a operare nel cosiddetto modo di spinning che di fatto copre circa il 70-80% del cielo con lʼssetto del satellite variabile continuamente con velocità consolidata di 1 grado/sec. Le capacità dei sottosistemi dello strumento scientifico rimangono inalterate, e la performance strumentale è nominale. Dal punto di vista scientifico, AGILE-2 mantiene e rafforza le caratteristiche di uno strumento di primaria importanza per lʼastrofisica gamma anche e soprattutto in presenza del concomitante Fermi. Lʼottima sensibilità gamma intorno a 100 MeV, insieme con la capacità di rivelazione simultanea di transienti e GRB nella banda dellʼx-duro (Super-A) e con il timing e capacità di trigger di transienti al millisecondo mantengono e rafforzano la competitività di AGILE. il finanziamento ASI per le operazioni è attualmente previsto fino a estate 2011 con probabile estensione a estate 2012. il finanziamento per le attivita' scientifiche è previsto fino a estate 2013 con probabile estensione a estate 2014 28 28
last news: ATEL on flaring CRAB Nebula region 29 29
Pavia Composizione del Gruppo Roma 2 Roma 1 Trieste 30
Preventivi AGILE 2011 Pavia Preventivi AGILE 2011 Trieste incontri per collaborazioni internazionali contributi stampa articoli 31
Preventivi AGILE 2011 Roma Tor Vergata 32
altre slides 33
AGILE two lifes AGILE-1 AGILE-2 time period Jul.07 Oct.09 Nov. 2009 - attitude fixed variable (spinning, 1º/sec) sky coverage 1/5 ~ 70% source livetime fraction 1-day exposure (30 degree off-axis, 100 MeV) ~ 0.5 ~ 0.2 ~ 2 10 7 (cm 2 sec) (0.5-1) 10 7 (cm 2 sec) 34
Fermi exposure vs. time (astro-ph/ arxiv:1008.3235) 35
1. Cyg X-3 flare (3 Nov 2008) pointing mode 36
1. Cyg X-3 flare (3 Nov 2008) pointing mode 37
Example: Galactic Centre 2-days integration (13-14 Mar 2010) AGILE spinning mode vs. Fermi (Sabatini et al. 2010) Red data (AGILE) Blue data (Fermi) 38
Example: Fermi Galactic Centre 1-month integration (20 Feb-20 Mar 2010) off-axis angle vs. time and cumulative histogram Blue data (Fermi) 39