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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. - PowerPoint PPT Presentation
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Marco Feroci SAIT 2009 INAF/IASF RomeMarco Feroci (INAF/IASF Roma)
Astrofisica X e Gammadopo due anni di AGILE (ed uno di GLAST)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
OutlineGamma Ray Astronomy todayThe AGILE MissionHighlights of Scientific Results from AGILE:
AGNsGamma-ray PulsarsGalactic compact sourcesGalactic TransientsGamma Ray Bursts
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Gamma-ray Astrophysics Missions (above 30 MeV)
SAS-2 NASA Nov. 1972 – July 1973
COS-B ESA Aug. 1975 – Apr. 1982
CGRO NASA Apr. 1991 – Jun. 2000
AGILE ASI April 23, 2007 -
GLAST NASA June 11, 2008 -
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
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
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
From EGRETFrom EGRET to AGILEFrom EGRET to AGILE to GLAST
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The AGILE Mission
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The AGILE Payload: the most compact
instrument for high-energy astrophysics
It combines for the first time a gamma-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
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The AGILE challenge…
• only ~100 kg of Payload
• only ~100 W of PL absorbed power
• only 350 kg of satellite…
• Small Mission budget and resources
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE: inside the cube…
ANTICOINCIDENCE (INAF/IASF Milano)
HARD X-RAY IMAGER (SUPERAGILE)
INAF/IASF Roma
GAMMA-RAY IMAGER SILICON TRACKER
INFN-Trieste INAF/IASF Milano, Roma
(MINI) CALORIMETERINAF/IASF Bologna
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE in context…EGRET AGILE GLAST
Eff. Area (0°, 100 MeV) 1000 500 3800
Eff. Area (0°, 1 GeV) 1000 500 8500
Eff. Area (40°, 100 MeV) 40 400 2700
Field of View 0.5 sr 2.5 sr >2 sr
Weight - 350 4000
Budget - 50M€ $690+foreign contr.s
Pointing strategy Staring Staring Survey
Angular Resolution 100 MeV 6 deg 4 deg 4 deg
Dead Time 100 ms <200 µs <100 µs
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GLAST
AGILE
Dr Evil
Mini-Me
from “Austin Powers” (1999)
AGILE in context…
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE in orbit:• launched April 2007• > 10.000 orbits • > 94% in nominal scientific observation• no sign of instrument degradation• approved through April 2011
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
2-year -ray exposure
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
2-year -ray sky by AGILE
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE First Catalog of -ray sources
Average flux above 100 MeV
Pittori et al., 2009
AGILE First Catalog of X- and -ray sources
Pittori et al. 2009
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE Fast Reactions
39 Astronomers’ Telegrams (ATel):27 on Gamma-ray Transients12 on X-ray Transients
37 GRB Coordinate Network (GCN) Telegrams:21 on Gamma Ray Bursts 4 on Magnetars12 with InterPlanetary Network (IPN)
One fast communication every ~10 days
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Papers on Refereed JournalsDel Monte et al. GRB 070724B A&A 478 (2008) L5Vercellone et al. 3c 454.3 ApJ 676 (2008) L13Giommi et al. S 0716+714 A&A 487 (2008) L49Bulgarelli et al. 3EG J1835+5918 A&A 489 (2008) L17Chen et al. S 0716+714 A&A 489 (2008) L37Marisaldi et al. MCAL GRBs A&A 490 (2008) 1151Pucella et al. PKS 1510-089 A&A 491 (2008) L21Giuliani et al. GRB 080514B A&A 491 (2008) L25Halpern et al. PSR J2021+3651 ApJ 688 (2008) L36Vercellone et al. 3c 454.3 ApJ 690 (2009) 1018 Donnarumma et al. Mkn 421 (w/TeV) ApJ 691 (2009) L13Pellizzoni et al. Known Pulsars ApJ 691 (2009) 1618Pacciani et al. 3c 273 A&A 494 (2009) 49Giuliani et al. 3c 279 A&A 494 (2009) 509Pellizzoni et al. New Pulsars ApJ 695 (2009) L115Tavani et al. Eta Carinae ApJL 2009 in pressPittori et al. First GRID Catalog A&A submittedDonnarumma et al. 3c 454.3 ApJ, to be submittedVercellone et al. 3c 454.3 ApJ, to be submittedFeroci et al. SA results A&A, to be submittedTavani et al. IC 443 ApJ, in preparationEvangelista et al. GX 301-2 (X-rays) A&A, in preparationDel Monte et al. Cyg X-1 (X-rays) A&A, in preparation
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE Results on Active Galactic Nuclei
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
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
A Multi- Approach
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE detected at least one object for each blazar category:
FSRQ 3C 454.3 LBL 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)
The Blazar Flavours
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Donnarumma et al., 2009, ApJL, 691, L13<F> = (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 -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
Mkn 421
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The longest monitoring so far of a -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).
AGILE & 3C 454.3Vercellone et al. 2008, 2009, in prep.; Donnarumma et al. in prep.
FluxPhoton Index3c 454.3 is rebrightening again!
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Multi—: 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…
The Multi- View of 3C 454.3
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
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
PKS 1510-089
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE Observation of Sources in our
Galaxy
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Gamma-ray Pulsars
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
VELACRAB
GEMINGAB1706-44J2021+3651
J2229+6114B1509-58
B1821-24
J1016-5857
J1357-6429J2043+2740
J1524-5625
J0737-3039
AGILE Pulsars… two years after…
AGILE doubled the EGRET pulsar sample in only two years!
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Rotation-powered pulsars
Vela
Geminga
Crab
Pellizzoni et al. 2009
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
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).
• Cglitch=1011 counts,
where is the unknown conversion efficiency of the glitch energy to gamma-ray emission (Pellizzoni et al., 2009)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Small Vela glitch in August 2007: burst emission possibly detected by AGILE
Vela glitch=54,312.5+/-3 MJD
E>50
MeV
15 photons in 4 minutesCglitch=1011 counts
Gamma-ray emission from pulsar glitches?
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE Discovery of –ray pulsations from PSR J2021+3651
Halpern et al. 2008
-ray-pulse separation vs -ray-radio lag: data vs outer gap model (Romani & Yadigaroghu 1995). Relation holds for many Fermi new pulsars.
Viewing
Angle
Phase-resolved images resolve a region including confused EGRET sources.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
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
Pelliz
zoni
et a
l., 2
009
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.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
PRELIMINARY
Double neutron star system 0737-3039
Orbital period: 2.4 h eccentricity=0.09(Burgay et al., 2003; Lyne et al., 2004)
Pellizzoni et al. 2009
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Eta Carinae
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
HST image of -Car
A Gamma-ray source in the Carina Region
11-13 Ott 08
2 days integration maps - counterclockwise
Gamma light curve vs RXTE lught curve
Tavani et al., 2009
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).
<F>=(37±5)e-8, 7.8L=3.4x1034 erg s-1
Jul 2007 – Oct 2008 -Car: Binary system (orbit 5.5 yr) including a LBV and an O star. Strong wind ejection (10-410-5 Msun yr-1) by both stars.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The SNR IC 443
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Geminga
Crab
Proton acceleration in IC 443?
AGILE
MAGIC
Solid: hadronsDashed:
electrons
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Proton acceleration in IC 443?
• 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
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
X-ray Binaries
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Cyg X-3
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
15 - 18 April 2008Giant 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 !
Cygnus X-3
In the same period SuperAGILE
revealed an X-ray flare
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Cygnus X-3
GRID Images (50 MeV – 3 GeV) around day 18 April 2008
-2 days-4 days-6 days
+2 days18 April 2008
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Gamma Ray transients on the Galactic Plane
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 200944
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
Variable Sources in the Galactic Plane: e.g., 1AGL J2020+4032
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
1AGL J2020+4032 April 27-28, 2008
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Variable Sources in the Galactic Plane: possible counterparts to 1AGL J2020+4032
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 200947
The variable gamma-ray sources are very bright ( Crab). SuperAGILE simultaneous observation: upper limits between 10 and 40 mCrab. Weak and steady hard X-ray source in Swift/BAT survey.
L/Lx » 1Interpretation models based on leptonic jet emission from Microquasars predict large emission at X-rays, so they are excluded by the simultaneous SuperAGILE upper limits.
Variable Sources in the Galactic Plane: a possible interpretation
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.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRS 1915+105
Variable sources: GRS 1915+105
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRS 1915+105
15 April 2008“reactivation” of the microquasar GRS 1915+105
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRS 1915+105
(Trushkin S. et al., ATel #1509)
(J.C.A. Miller-Jones, 2007)
Hist
orica
l rad
io
map
ping
Radio monitoring
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GX 301-2
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Long-term Monitoring of the HMXB GX 301-241.5 d orbital period The regular flares 1-2 days before periastron…
RXTE/ASM data
Evangelista et al. in preparation
41.5 days
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
SuperAGILE & ASM: GX 301-2
D.A Lehay
Y. Evangelista et al.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GX 301-2
And the 680s X-ray Pulsar: pulse shape at all orbital phases
Evangelista et al. in preparation
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The Galactic Center
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Postcards from GC - I
GX 340+04U 1700-
377
4U 1820-303
AX J1749.1-2639GX 5-1
Ginga 1826-24Sco X-1
GX 17+2
Sco X-1
4U 1700-377
AX J1749.1-2639GX 5-1
Ginga 1826-24
4U 1820-303
4U 1820-303
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Ginga 1826-24
4U 1820-303
GX 17+2
GRS 1758-258
Sco X-1
GX 1+4
GRS 1758-258
GX 17+2
Ginga 1826-24
Ginga 1826-24
GX 1+44U 1820-
303
Postcards from GC - II
4U 1700-377 Ginga 1826-24Sco X-1
GX 17+2
4U 1700-377
AX J1749.1-2639GX 5-1
Ginga 1826-24
4U 1820-303
Ginga 1826-24
4U 1820-303
GX 17+2
GRS 1758-258
Sco X-1
Daily variability in the Galactic Center (counts image)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Short X-ray Transients
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
IGR J17473-2721/XTE J1747-274
Confirmed by later observations(ATels# : 1459, 1460, 1461, 1468)
IGR J17473-2721/XTE J1747-274 is an X-ray Burster ! ATel #1445 (Del Monte et al.) – 27 Mar 2008
SuperAGILE detection of the first known
type-I X-ray burst
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
SAX J1750.8-2900
Sudden outburst of the X-ray Transient SAX J1750.8-2900
(Pacciani et al., ATel #1428)
4U 1700-377 AX J1749-2639
Sco X-1
4U 1700-377 GX 17+2 ~1 day
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Gamma Ray Bursts
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
The main feature of GRB 080514B is the extended emission in gamma rays (Giuliani et al., 2008). It is the first gamma-ray bright GRB after EGRET and is also associated to an afterglow and a photometric redshift measure of 1.8 (A. Rossi et al., 2008).
Gamma Ray BurstsGRB 080514B: the first gamma-ray bright GRB associated to an afterglow
SuperAGILE – Mars Odyssey
IPN annulus
SuperAGILE 1-D(37° off-axis)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
A single model for the whole spectrum
The same Band model fits the spectrum from 20 keV up to 50 MeV. The spectacular GRB 080916C detected by Fermi shows that this holdsup to 1 GeV. Same emission mechanism at work.
= -0.599
= -2.48
Epeak = 224 keVGRID fluence
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The extended emission in gamma rays
A common feature of the GRBs detected in gamma rays by AGILE is the extended emission; this property was already known after the EGRET observation;The feature is confirmed by the Fermi/LAT detections: notably GRB 080916C (up to 200 s after trigger), 090328 (up to 900 s after trigger), 090323 (up to 2 ks after trigger) and 080825C (up to 35 s after trigger);
GRB 080514B
1/32/3
GRB 090401B
1/54/5
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
Population studies and the gamma-ray emission
11 GRBs localized by SuperAGILE with spectral parameters in 20 keV – 2 MeV (by Konus-Wind, Suzaku/WAM or Fermi/GBM) and GRB 080721 (in the GRID FoV).GRB 080514B and GRB 090401B firmly detected by GRID;GRB 080721 and GRB 081001 with smaller significance in GRID;
GRB 080613B with a peak flux of ~5x10-6 erg cm-2 s-1
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
2009 - Anno dell’Astronomia
Emissione 7 maggio 2009
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Thank You !
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Spare slides
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
AGILE AGILE
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The AGILE Tracker (INFN-Trieste)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009IASF Roma
2 x 1-D
1-D
1-D107°
SuperAGILE (IASF Roma)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
The AGILE Mini-Calorimeter (IASF/Bologna & Thales-Alenia
Space – Laben)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRB 090423
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Cyg X-1
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Cyg X-1
Likely the longest continuous hard X-ray monitoring of Cyg X-1 Total Observation Time: ~ 4.5 Ms(1196 Orbits)
1 Month~1.3 Crab Flare
(see also INTEGRAL ATels #1533,1536)
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Cyg X-1
Del Monte et al., in preparation
SuperAGILE
GRID
SuperAGILE light curve LE (20-25 keV): Yellow HE (25-50 keV): Cyan
Γ~ 1.61 +/- 0.13Low/Hard State Monitoring State
Transitions…
…and possible gamma-ray emission
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Cygnus Field
Cyg X-1
Cyg X-3Cyg X-2
EXO 2030+375
GRS 1915+105
EXO 2030+375
Cyg X-3
Cyg X-1
Cyg X-2
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRB 090401B: prompt MeV emission
The AGILE MCAL detected GRB 090401B up to the MeV region. Detailed analysis is still ongoing.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Yesterday’s GRB: 080625
SuperAGILE: L. Pacciani et al., GCN 7903
Afterglow:OSN: I>21.5mag A. de Ugarte Postigo et al., GCN 7904, 7907UVOT: mag~19.6-20 WUVB M.C. Stroh et al. GCN 7905Swift/XRT: 1.5 arcmin, F~10-12 cgs S. Immler et al. GCN 7906
NO GRID detection
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
(Flaring) Active Galactic NucleiMrk 421 NGC 4151 Cen A3C 273
SuperAGILE & AGNs
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRS 1915+105 LSI +61°303
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRID Galactic anticenter observation
LSI +61°303
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
GRB 090401B: extended prompt emission
Swift/BAT, 15 – 150 keV
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
GRB 090401B: afterglow emission
Automatic Plot from the UK Swift Science Data Centre at the University of Leicester (Evans et al. 2007).
See the talk by P. Romano
F t-, 1.4
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
GRBs as seen in gamma rays by EGRET
GRB 930131
Five GRBs coincident in time with BATSE GRBs were detected by EGRET;Most of them showed extended emission of gamma rays, until few hundreds of seconds from trigger;The spectrum of GRB 930131 for example is modeled by the same powerlaw, extending from 1 MeV up to 1 GeV;The afterglow emission was not yet discovered, thus the redshift was not known.
Sommer et al., 1994, ApJSchneid et al., 1992, A&A
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Pellizzoni et al. 2009
Rotation-powered pulsars
Vela Geminga Crab
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009
Terrestrial Gamma Ray Flashes
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
Candidate TGFs detected by the AGILE/MCAL
~4 TGF candidates/month triggered by MCAL. The rate almost doubled since the onset of the trigger on the 1 ms time scale.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
<0.7 MeV
0.7-1.4 MeV
1.4-2.8 MeV
>2.8 MeV
All range
Light curve Position distribution
Energy vs time
Bar address vs time
Event of 2008-11-04 10:22:33 UT in details
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
High energy electrons in the upper atmosphere BATSE and RHESSI detected
TGFs in the MeV region. The study of the atmosphere in radio at ELF/VLF (30 Hz – 30 kHz) reveals powerful emission from lightning discharges.A correlation is established between the BATSE and RHESSI TGFs and the ELF/VLF data. The lightning discharges creates strong fields above the thunderclouds which generate the runaway electron avalanche producing gamma rays. AGILE/MCAL is following this study in collaboration with M. Fullekrug (Univ. Bath, UK).A timing issue of 2 – 5 ms in the coincidence is raised with RHESSI. The AGILE/MCAL time resolution of 2 µs can help solving the problem.
Marco Feroci INAF/IASF Rome
Astronomia X e Gamma
SAIT 2009Ettore Del Monte, INAF IASF Roma
Geographical distribution of the candidate TGFsSelection criteria: HR>0.2 AND fluence > 7 counts: 44 candidates / 8
monthsClustering
over Africa as expected
from RHESSI results
0 <= HR < 11 <= HR < 22 <= HR < 33 <= HR < 4
4 <= HR
HR = NE>1.4 MeV / NE<1.4MeV
Spot radius proportional
to fluence (7-24 counts)
Longitude (deg)
Latit
ude
(deg
)
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