Marco Feroci (INAF/IASF Roma)

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



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 -



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



SAIT 2009

From EGRETFrom EGRET to AGILEFrom EGRET to AGILE to GLAST



SAIT 2009

The AGILE Mission



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



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



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



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



SAIT 2009

GLAST

AGILE

Dr Evil

Mini-Me

from “Austin Powers” (1999)

AGILE in context…



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



SAIT 2009

2-year -ray exposure



SAIT 2009

2-year -ray sky by AGILE



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



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



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



SAIT 2009

AGILE Results on Active Galactic Nuclei



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



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



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



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!



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



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



SAIT 2009

AGILE Observation of Sources in our

Galaxy



SAIT 2009

Gamma-ray Pulsars



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!



SAIT 2009

Rotation-powered pulsars

Vela

Geminga

Crab

Pellizzoni et al. 2009



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)



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?



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.



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.



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)




SAIT 2009

Eta Carinae



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.



SAIT 2009

The SNR IC 443



SAIT 2009

Geminga

Crab

Proton acceleration in IC 443?

AGILE

MAGIC

Solid: hadronsDashed:

electrons



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



SAIT 2009

X-ray Binaries



SAIT 2009

Cyg X-3



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



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



SAIT 2009

Gamma Ray transients on the Galactic Plane



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



SAIT 2009

1AGL J2020+4032 April 27-28, 2008



SAIT 2009

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



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.



SAIT 2009

GRS 1915+105

Variable sources: GRS 1915+105



SAIT 2009

GRS 1915+105

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



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



SAIT 2009

GX 301-2



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



SAIT 2009

SuperAGILE & ASM: GX 301-2

D.A Lehay

Y. Evangelista et al.



SAIT 2009

GX 301-2

And the 680s X-ray Pulsar: pulse shape at all orbital phases

Evangelista et al. in preparation



SAIT 2009

The Galactic Center



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



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)



SAIT 2009

Short X-ray Transients



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



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



SAIT 2009

Gamma Ray Bursts



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)




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



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




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



SAIT 2009

2009 - Anno dell’Astronomia

Emissione 7 maggio 2009



SAIT 2009

Thank You !



SAIT 2009

Spare slides



SAIT 2009

AGILE AGILE



SAIT 2009

The AGILE Tracker (INFN-Trieste)



SAIT 2009IASF Roma

2 x 1-D

1-D

1-D107°

SuperAGILE (IASF Roma)



SAIT 2009

The AGILE Mini-Calorimeter (IASF/Bologna & Thales-Alenia

Space – Laben)



SAIT 2009

GRB 090423



SAIT 2009

Cyg X-1



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)



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



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



SAIT 2009

GRB 090401B: prompt MeV emission

The AGILE MCAL detected GRB 090401B up to the MeV region. Detailed analysis is still ongoing.



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



SAIT 2009

(Flaring) Active Galactic NucleiMrk 421 NGC 4151 Cen A3C 273

SuperAGILE & AGNs



SAIT 2009

GRS 1915+105 LSI +61°303



SAIT 2009

GRID Galactic anticenter observation

LSI +61°303



SAIT 2009

GRB 090401B: extended prompt emission

Swift/BAT, 15 – 150 keV




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




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



SAIT 2009


Rotation-powered pulsars

Vela Geminga Crab



SAIT 2009

Terrestrial Gamma Ray Flashes




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.




<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




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.




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

)

Documents

Marco Feroci (INAF/IASF Roma)