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Marco Feroci (INAF/IASF Roma)

Astrofisica X e Gamma dopo due anni di AGILE (ed uno di GLAST). Marco Feroci (INAF/IASF Roma). Outline. Gamma Ray Astronomy today The AGILE Mission Highlights of Scientific Results from AGILE: AGNs Gamma-ray Pulsars Galactic compact sources Galactic Transients Gamma Ray Bursts.

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Marco Feroci (INAF/IASF Roma)

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  1. Astrofisica X e Gamma dopo due anni di AGILE (ed uno di GLAST) Marco Feroci (INAF/IASF Roma)

  2. Outline Gamma Ray Astronomy today The AGILE Mission Highlights of Scientific Results from AGILE: AGNs Gamma-ray Pulsars Galactic compact sources Galactic Transients Gamma Ray Bursts

  3. Gamma-ray Astrophysics Missions (above 30 MeV)

  4. A new era in Gamma-ray Astronomy After ~10 years, two Gamma-ray observatories in orbit Major advances in: - A *  * t -> many photons from many sources - angular resolution - time resolution and dead-time - real-time analysis and multi- availability and flexibility (e.g., Swift, optical, …) Gamma-ray Astronomy passes from pioneeristic to systematic studies of sources

  5. From EGRET From EGRET to AGILE From EGRET to AGILE to GLAST

  6. The AGILE Mission

  7. The AGILE Payload: the most compact instrument for high-energy astrophysics It combines for the first time agamma-ray imager (30 MeV- 30 GeV) with a hard X-ray imager (18-60 keV) with large FOVs (1-2.5 sr) and excellent angular resolution

  8. only ~100 kg of Payload only ~100 W of PL absorbed power only 350 kg of satellite… Small Mission budget and resources The AGILE challenge…

  9. AGILE: inside the cube… HARD X-RAY IMAGER (SUPERAGILE) INAF/IASF Roma GAMMA-RAY IMAGER SILICON TRACKER INFN-Trieste INAF/IASF Milano, Roma ANTICOINCIDENCE (INAF/IASF Milano) (MINI) CALORIMETER INAF/IASF Bologna

  10. AGILE in context…

  11. AGILE in context… GLAST Dr Evil Mini-Me AGILE from “Austin Powers” (1999)

  12. AGILE in orbit: • launched April 2007 • > 10.000 orbits • > 94% in nominal scientific observation • no sign of instrument degradation • approved through April 2011

  13. 2-year -ray exposure

  14. 2-year -ray sky by AGILE

  15. AGILE First Catalogof X- and -raysources AGILE First Catalog of -ray sources Average flux above 100 MeV Pittori et al. 2009 Pittori et al., 2009

  16. AGILE Fast Reactions 39 Astronomers’ Telegrams (ATel): 27 on Gamma-ray Transients 12 on X-ray Transients 37 GRB Coordinate Network (GCN) Telegrams: 21 on Gamma Ray Bursts 4 on Magnetars 12 with InterPlanetary Network (IPN) One fast communication every ~10 days

  17. Papers on Refereed Journals Del Monte et al. GRB 070724B A&A 478 (2008) L5 Vercellone et al. 3c 454.3 ApJ 676 (2008) L13 Giommi et al. S 0716+714 A&A 487 (2008) L49 Bulgarelli et al. 3EG J1835+5918 A&A 489 (2008) L17 Chen et al. S 0716+714 A&A 489 (2008) L37 Marisaldi et al. MCAL GRBs A&A 490 (2008) 1151 Pucella et al. PKS 1510-089 A&A 491 (2008) L21 Giuliani et al. GRB 080514B A&A 491 (2008) L25 Halpern et al. PSR J2021+3651 ApJ 688 (2008) L36 Vercellone et al. 3c 454.3 ApJ 690 (2009) 1018 Donnarumma et al. Mkn 421 (w/TeV) ApJ 691 (2009) L13 Pellizzoni et al. Known Pulsars ApJ 691 (2009) 1618 Pacciani et al. 3c 273 A&A 494 (2009) 49 Giuliani et al. 3c 279 A&A 494 (2009) 509 Pellizzoni et al. New Pulsars ApJ 695 (2009) L115 Tavani et al. Eta Carinae ApJL 2009 in press Pittori et al. First GRID Catalog A&A submitted Donnarumma et al. 3c 454.3 ApJ, to be submitted Vercellone et al. 3c 454.3 ApJ, to be submitted Feroci et al. SA results A&A, to be submitted Tavani et al. IC 443 ApJ, in preparation Evangelista et al. GX 301-2 (X-rays) A&A, in preparation Del Monte et al. Cyg X-1 (X-rays) A&A, in preparation

  18. AGILE Results on Active Galactic Nuclei

  19. A Multi- Approach MOJAVE Radio imaging Spitzer IR REM IR-Optical WEBT-GASP Optical, radio, mm, IR Swift UV & Soft X-ray & Hard X-ray Suzaku Soft X-ray & Hard X-ray INTEGRAL Hard X-ray Super-AGILE Hard X-ray AGILE/GRID Gamma-rays MAGIC TeV VERITAS TeV ARGO TeV HESS TeV

  20. The Blazar Flavours • AGILE detected at least one object for each blazar category: • FSRQ 3C 454.3LBL PKS 0537-441 • IBL S5 0716+714 HBL MKN 421 • A few sources were detected more than once: • S5 0716+714; PKS 1510-089; 3C 454.3 • Variability level could be very different: • Extr. Low (3C 279); Extr. High (PKS 1510-089) • Gamma-ray activity could vary on different time scale: • A few days (W Comae); Months(3C 454.3)

  21. Mkn 421 Donnarumma et al., 2009, ApJL, 691, L13 <Fg> = (42  13)E-8 ph/cm2/s E>100MeV SA: 40mCrab (0.4 ph/cm2/s) 15—50 keV Swift/XRT: 2.6E-9 ph/cm2/s 2—10 keV (record!) Correlated variability (optical, X-rays, -rays, and TeV) The g-ray flare can be interpreted within the framework of the SSC model in terms of a rapid acceleration of leptons in the jet. June 2008

  22. AGILE & 3C 454.3 Vercellone et al. 2008, 2009, in prep.; Donnarumma et al. in prep. The longest monitoring so far of a g-ray blazar. A factor of about 10 in dynamic range in about 2 years (if considering also the Fermi data). A possible spectral trend (harder when brighter). Flux Photon Index 3c 454.3 is rebrightening again!

  23. The Multi- View of 3C 454.3 Multi—l: MOJAVE, MITSuME, Spitzer, GASP—WEBT, REM, Swift/UVOT, Swif/XRT, Suzaku, Swift/BAT, AGILE/GRID One year and half of AGILE monitoring:comparison of simultaneous SEDs, LCs, time—lags, spectra, etc…

  24. PKS 1510-089 Pucella et al., in preparation • D’Ammando et al., ATel #1957, 2009-03-08 14:00 UT and 2009-03-10 4:00 UT flux in excess of 200 x 10^-8 ph cm^-2 s^-1. • Pucella et al., ATel #1968, 2009-03-12 07:00 UT and 2009-03-13 05:00 UT flux in excess of 400 x 10^-8 ph cm^-2 s^-1. • Vercellone et al., ATel #1976, 2009-03-18 05:45 UT and 2009-03-19 05:33 UT flux of about 400 x 10^-8 ph cm^-2 s^-1. This value represents an increase of more than a factor of 3 within 24 hours compared with the gamma-ray flux level detected during the previous three days. 1 – 30 March 2009

  25. AGILE Observation of Sources in our Galaxy

  26. Gamma-ray Pulsars

  27. AGILE Pulsars… two years after… AGILE doubled the EGRET pulsar sample in only two years! J1524-5625 GEMINGA J2229+6114 J2021+3651 B1509-58 J1016-5857 B1706-44 J0737-3039 J1357-6429 VELA B1821-24 CRAB J2043+2740

  28. Rotation-powered pulsars Crab Vela Geminga Pellizzoni et al. 2009

  29. Gamma-ray emission from pulsar glitches? • Vela has shown 10 major glitches since 1969. • The chance occurrence of a strong Vela glitch in the wide AGILE field of view over three years of mission is 20%. • Starquake waves can “shake” magnetic fields generating strong electric fields which accelerate particles to relativistic energies, possibly emitting a burst of high-energy radiation (Ruderman, 1976, 1991; Alpar et al., 1994). • Cgglitch=1011hDn/n counts, • where h is the unknown conversion efficiency of the glitch energy to gamma-ray emission (Pellizzoni et al., 2009)

  30. Gamma-ray emission from pulsar glitches? Vela glitch=54,312.5+/-3 MJD Cgglitch=1011hDn/n counts Dn/n=10-9 h=0.1 15 photons in 4 minutes E>50 MeV Small Vela glitch in August 2007: burst emission possibly detected by AGILE

  31. AGILE Discovery of –ray pulsations from PSR J2021+3651 Phase-resolved images resolve a region including confused EGRET sources. -ray-pulse separation vs -ray-radio lag: data vs outer gap model (Romani & Yadigaroghu 1995). Relation holds for many Fermi new pulsars. Viewing Angle Halpern et al. 2008

  32. Discovery of New -Ray Pulsars J2229+6114, J2021+3651, …: Vela-like J1513-5908: High B pulsar J1824-2452: “variable” ms PSR in Globular Cluster ---------------------------------- J1016-5857: possibly 3EG source J1357-6429 J2043+2740: oldest gamma-ray pulsar (106 yrs) J1524-5625 Several other gamma-ray pulsars have been recently discovered by Fermi, including a second ms pulsar and the radio-quiet gamma-ray pulsar in CTA-1. Pellizzoni et al., 2009

  33. Double neutron star system 0737-3039 Orbital period: 2.4 h eccentricity=0.09 (Burgay et al., 2003; Lyne et al., 2004) PRELIMINARY Pellizzoni et al. 2009

  34. Eta Carinae

  35. A Gamma-ray source in the Carina Region -Car: Binary system (orbit 5.5 yr) including a LBV and an O star. Strong wind ejection (10-410-5 Msun yr-1) by both stars. Jul 2007 – Oct 2008 IF the association is true, this would be the first detection of a colliding wind binary above 100 MeV (in qualitative agreement with IC and/or pion decay model by Reimer et al. 2006). HST image of -Car <F>=(37±5)e-8, 7.8 L=3.4x1034 erg s-1 Gamma light curve vs RXTE lught curve 11-13 Ott 08 Tavani et al., 2009 2 days integration maps - counterclockwise

  36. The SNR IC 443

  37. Proton acceleration in IC 443? Solid: hadrons Dashed: electrons AGILE Geminga MAGIC Crab

  38. 100 MeV source and TeV source are non coincident ! Absence of IC emission above 10-100 GeV at the gamma-ray peak: 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 The Northeastern SNR shock environment provides the target for proton-proton interaction and pion production/decay Hadronic model at the NE shock is the only viable Proton acceleration in IC 443?

  39. X-ray Binaries

  40. Cyg X-3

  41. 15 - 18 April 2008 Giant radio flare of Cygnus X-3 detected by RATAN-600 radio telescope Radio flux increasing of a factor ~103, from ~10 mJy to ~10 Jy S.A.Trushkin et al., ATel #1483 10 Jy is typical flux for plasmoids emission ! In the same period SuperAGILE revealed an X-ray flare Cygnus X-3

  42. Cygnus X-3 GRID Images (50 MeV – 3 GeV) around day 18 April 2008 -4 days -2 days -6 days +2 days 18 April 2008

  43. Gamma Ray transients on the Galactic Plane

  44. Variable Sources in the Galactic Plane: e.g., 1AGL J2020+4032 • Cygnus Region • Persistent Emission • (1.20 ± 0.07) × 10-6 cm-2 s-1 at 23,4 σσ • Position: (l,b) = (78.37, 2.04)°, error ~ 0.12° • 1-day flare on April 27-28, 2008 [ATel #1492] • (2.9 ± 0.8) × 10-6 cm-2 s-1 at 3.7 σ • Position: (l,b) = (78.1, 2.0)°, error ~ 0.8° • 1-day flare on June 20-21, 2008 [ATel #1585] • (2.5 ± 0.7) × 10-6 cm-2 s-1 at 4.9 σ • Position (l,b) = (78.6, 1.6)°, error ~ 0.7° • 1-day flare on November 16-17, 2008 [ATel #1848] • (2.5 ± 0.7) × 10-6 cm-2 s-1 at 4.8 σ • Position (l,b) = (78.6, 2.1)°, error ~ 0.7° • Gamma association: 3EG J2020+4017 - 0FGL J2021.5+4026 44

  45. 1AGL J2020+4032 April 27-28, 2008

  46. Variable Sources in the Galactic Plane: possible counterparts to 1AGL J2020+4032

  47. Variable Sources in the Galactic Plane: a possible interpretation • The variable gamma-ray sources are very bright ( Crab). • SuperAGILEsimultaneous observation: upper limits between 10 and 40 mCrab. Weak and steady hard X-ray source in Swift/BAT survey. • L/Lx » 1 • Interpretation models based on leptonic jet emission from Microquasars predict large emission at X-rays, so they are excluded by the simultaneous SuperAGILE upper limits. • Romero & Vila (2009) propose interpretation in terms of emission from hadronic jets in Galactic microquasars. This model is able to reproduce a Spectral Energy Distribution (SED) where the luminosity at X-rays is very small, consistent with the AGILE observations. 47

  48. GRS 1915+105 Variable sources: GRS 1915+105

  49. GRS 1915+105 15 April 2008 “reactivation” of the microquasar GRS 1915+105

  50. GRS 1915+105 Radio monitoring (Trushkin S. et al., ATel #1509) Historical radio mapping (J.C.A. Miller-Jones, 2007)

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