some results…

Galactic Gamma-Ray sources:
Microquasars and new transients

M. Tavanion behalf of the AGILE TeamFermi Symposium, Nov. 5, 2009

The AGILE gamma-ray sky (E > 100 MeV)
2 year exposure: July 2007 – June 2009

hard -X ray sources (18- 60 keV), 2 years• AGILE combination of co-aligned
gamma-ray (50 MeV – 5 GeV) andhard X-ray (20-60 keV) imagers isoptimal for Galactic source studies• AGILE-GRID is optimized near 100 MeV– good PSF (~3º at 100 MeV)
– typical daily exposure of ~ 107 cm2 sec(at 100 MeV)

AGILE “Galactic” science topics• new (soft) gamma-ray Pulsars• PWNe• microquasar studies, Gamma-ray emission
from Gal. compact objects• “new” gamma-ray transient candidates• SNRs and origin of cosmic rays
• Molecular clouds, CR propagation

Galactic microquasars
New transientsGalactic microquasars
New transientsmany results
many surprises

AGILE 2-year GRID exposure (100 MeV – 10 GeV)AGILE 2-year Super-A exposure (20-60 keV)

Galactic “Micro-QSOs” (radio “jet” sources)
Exposure
Cyg X-1~ 1 year
Cyg X-3~ 1 year
SS 433~ 6-8 months
GRS 1915+104~ 6-8 months
GRO J1655-40~ 4-5 months
GRS 1758-258~ 4-5 months
XTE J1550-564~ 6-8 months
Sco X-1~ 4-5 months
LS I 61 303~ 4-5 months
LS 5039~ 4-5 months

Galactic “Micro-QSOs” (radio “jet” sources)Θ (degrees) βΓ LX/LE γ/TeV
MeV
Cyg X-1?
?
? 0.1-1 ~5yes
Cyg X-3
SS 433
GRS 1915+104
GRO J1655-40
GRS 1758-258
XTE J1550-564
Sco X-1
LS I 61 303
LS 5039< 14< 7070> 70?
60-70> 70?
< 80> 0.8 > 1.6 0.1-1
0.26 1.03 0.01
0.92 2.5 0.1-1
0.9 2.5
10.1-1> 0.8 1.5 0.1-1> 0.8 > 1.6 0.1-1?
?
10-4> 0.2 ?
10-4?
nono
no
no
nono
yes
yes

MAGIC single isolated
detection of Cyg X- 1,
24 Sept. 2006,~ 79 min. TeV flare

Cyg X-1 hard X-ray flux, Swift/BAT (15-50 keV)

Cygnus -X 1 monitoring

14 passes a day: adetailed lightcurve

AGILE-GRID telemetry on Nov. 3, 2008

The AGILE 1-day exposure (E > 100 MeV)
(30 Nov. 2008)

a comparison: 1-day exposure
AGILE FERMI(GRID) (LAT)FOV (sr)

2.5

2.5

sky coverage

1/5whole sky

Source livetime fraction~ 0.5~ 0.16

1- day exposure (30 degreeoff- axis, 100 MeV)

~ (1-2) 107~ 2 107
cm2 sec cm2 sec
fixedvariable

Attitude

AGILE Ground Segment

Satellite~0.5 hrMalindi Ground Station

Fucino TZP MOC~0.5 hr
ASDC

Automatic
data processing~0.5 hr

AGILE Team~(1.5 - 2) hr
Guest Observers

Public data accessMultifrequency science• AGILE, FERMI• Radio Telescopes (VLA, Mojave,Michigan, AMI-LA, RATAN)• Optical Obs. Networks (GASP, REM, …)• SWIFT, Suzaku, XMM• INTEGRAL• TeV (MAGIC, HESS, VERITAS)

Carina-Vela Regions

Cygnus Region
Galactic Center

The Galactic CenterGC region, AGILE B19b,FM (E > 400 MeV)Example: October 1, 2009 view of the Galactic Center region
with Super-A (20-60 keV)SKYBINSKYCOORDDIRECTION

ZONE

RATE

ERR_RATE

CTS cm-2 s-1

EXPOSURE

1428.88
1891.711370.05
1857.82
1597.11766.9201574.64
1982.021610.881085.47
1708.841503.75
1329.26-6.6805715.4799-9.49395
13.9335
1.49684-34.2576
0.400699
19.4848
2.16789-22.2762
6.91432-3.05522-11.4187

X
X
X
X
X
X
X
X
X
X
X
X
X

15
128
12
9
3
7
12
9
10
8
9
7

1.39655
0.586521
0.495455
0.3601080.429247
0.312803
0.331132
0.248696
0.253957
0.271741
0.202768
0.170617
0.181133

0.279310
0.117304
0.0990910
0.0720216
0.0858494
0.0625605
0.0662264
0.0497392
0.0507915
0.0543482
0.0405536
0.0341235
0.0362266

0.457440
0.0465814
0.0171424
0.0270270
0.0139616
0.0589205
0.00958806
0.0222842
0.00847812
0.0174138
0.00648387
0.00582340
0.00669337

45017.2
46703.643871.646456.044629.1
43524.2
44375.747381.2
44675.743800.044998.644294.843824.1

NAME
Sco X-1
4U 1700-377
GX 17+2
GX 349+2
GX 5-1
GRS 1915+105
Ginga 1826-24
OAO 1657-415
GRS 1758-258
SWIFT J1753.5-0127
4U 1820-303
GX 9+1
1M 1812-121

One-day automatic integration on the GC: 13 sources from 38 mCrab to 3 Crab,

SIGN
34.9787
15.1582
13.59869.33134
9.159808.73901
8.261597.986176.53055
6.49230
6.39260
5.16577
4.80630

AGILE capabilities• Semi-continuous monitoring of sources in theFOV (14 passes/day)– SAA and Earth occultation• Good sensitivity near 100 MeV• Simultaneous hard X-ray and gamma-ray
monitoring• Careful statistical analysis: likelihood and FDR
methods, post-trial significanceGamma-Ray Galactic Transients• Big issue since EGRET, some detection/hints– example: GRO J1838- 04• AGILE discovery of several gamma-raytransients in the plane (usually low-energy)– Examples:• 24 Nov. 2007
• Crux Region transients• Carina Region transients• Eta-Car• Galactic Center transients (March 09)• L= 17• L = 8 (Easter-09 transient)• Cygnus transients

GRO J1838-04 (blazar-less EGRET transient)

EGRET

AGILE (all data)

Galactic gamma-ray transients:• GC region• Cygnus region• Carina region• Crux region
AGILE observes variability and detects newtransients on time scales of 1-2 days at flux
levels of 10-6 cm-2s-1 , even in crowded, highdiffuse emission Galactic plane regions.
NO detectable simultaneous hard X-rayemission (F < 20-30 mCrab, 18-60 keV, 1-dayintegration)

AGILE facts and surprises•

in general, no obvious X-ray or hard Xray strong source (above 10 mCrab)•some SWIFT follow-ups: no obvious
detections, (except one…)•

but…Eta-Car and Cygnus X-3 examples

Energetics…
• Gamma-ray luminosity above 100 MeV
L = 7 x 1034 d2kpc erg/s

Energetics…
• Gamma-ray luminosity above 100 MeV
L = (a few) x 1034 d2kpc erg/s• Compatible with WR/CWB expectations– It could be a class of WR/CWB or flaringstars• But also it could be a NEW CLASS of(non-accreting or low X-ray) sourcesEaster 2009 transientEaster transient: 10-13 April 2009, 1014310180, bin =0.2, B16, FM, E>100 MeV

Easter transient: 10-13 April 2009, 1014310180, bin =0.2, B16, FM, E>100 MeV

Easter transient: 10-13 April 2009, 1014310180, bin =0.2, B17b, FT

E > 100 MeV

E > 400 MeV

The Carina Region: AGILE at 100 MeV

AGILE discovery of gamma- ray emission from theEta Carinae region

AGILE-GRID, Eta Carinae at 400 MeV

The Eta Carinae system:a colliding wind binary

Transient gamma-ray emission from EtaCarinae (12-13 Oct., 2008)
10-11 Oct.

12-13 Oct.

14-15 Oct.

16-17 Oct.

monitored Micro-QSOs• Cyg X-1
• Cyg X-3
• GRS 1915+105• SS 433• ….

Challenges…

• are Cyg X-1-like fast transients common ?
• AGILE did not detect (yet) Cyg X-1 above
100 MeV• detect gamma-ray variability within
1 day…or even less

Cyg X-1 monitoring (2007-mid 2009): in hard state, no gamma-ray
flaring
44 days

20 days 51 days

45 days

160 days, 6.1 x 106 s

SuperAGILE(20 – 50 keV)

RXTE/ASM(2 – 12 keV)

2 Nov 2007

1 Dec 2008

Del Monte et al. Submitted to A&A

Cygnus -X 1 monitoring

14 passes a day: adetailed lightcurve

GRS 1915+105

GRS 1915+105: historical radio flaring(J.C.A. Miller-Jones, 2007)

GRS 1915+105

15 April, 2008
Hard X-ray re-activation of GRS 1915+105

GRS 1915+105 during a radio flareRadio monitoring

Historical radio mapping(Trushkin S. et al., ATel #1509)(J.C.A. Miller-Jones, 2007)

Cygnus region

Cassiopeia-Cygnus Region

Cyg X-3

Cygnus X-3• erratic and powerful microquasar (not clear
yet whether BH or unusual NS)• radio and X-ray spectral state studies(G.Pooley, R.Hjellming’s group, S. Trushkin,
M. McCollough, D. Hannikainen et al.)• difficult to find a pattern, soft and hard X-ray
emission is anticorrelated

Koljionen et al., in prep. (see also Szostek, Zdziarski,
Mc Collough et al., 2008)

AGILE and Cygnus X-3(recent paper accepted by Nature)• AGILE detects several gamma-rayflares from Cygnus X-3, and also weakpersistent emission above 100 MeV• very interesting correlations with radioand X-ray spectral state changes• gamma-ray flares usually before radioflares• a pattern emerges !

Cyg X- 3long timescale monitoring (Swift- BAT)

example: very strong radio flare ofCygnus X-3 in April 2008
• Strong radio-flare reaching ~20 Jy on Apr. 18,2008 (RATAN)• good exposure by AGILE before, during andafter the radio flare, both in hard X-rays andgamma-rays• gamma-ray flare detected at the onset of theradio flare

RATAN Obs. (S. Truskhin et al.)Apr. 13 – Apr. 27, 2008

very strong radioflare, presumably
with jet ejection

strong gamma-rayflare

X-ray (1-10 keV)
flare

Hard X-ray flux
state change(Super-Amonitoring)

”quenched” radio state !

Dec. 2008 gammaray flareMajor gamma-ray flares in special transitional
states in preparation of radio flares !

figure adaptedfrom Szostek
Zdziarski &McCollough(2008)

Gamma-ray flaring of Cyg X-3:
average AGILE spectrum (preliminary)Cygnus X-3 and other micro-qso’s• deep theoretical implications: optically thickComptonized models inadequate (hybridmodels: quasi-thermal + PL)• microquasar jet formation (and preparation)
associated with extreme high-energy particle
acceleration above GeV energies• correlation with hard X-ray/soft X-ray/radio
states,– in the inner accretion disk region– in outwardly propagating shocks

Implications…
• Cygnus X-3 can teach about BH systems andpossibly also about blazars• Its jet is pointing at us, it is a “micro-blazar”• “preparation” for a major jet ejection andnon-thermal extreme particle acceleration
with GeV emission before plasmoid
production is suggested also in someblazars• Bright future for understanding BHs

Galactic “Micro-QSOs” (radio “jet” sources)Θ (degrees) βΓ LX/LE γ/TeV
MeV
Cyg X-1?
?
? 0.1-1 ~5yes
Cyg X-3
SS 433
GRS 1915+104
GRO J1655-40
GRS 1758-258
XTE J1550-564
Sco X-1
LS I 61 303
LS 5039< 14< 7070> 70?
60-70> 70?
< 80> 0.8 > 1.6 0.1-1
0.26 1.03 0.01
0.92 2.5 0.1-1
0.9 2.51
0.1-1> 0.8 1.5 0.1-1> 0.8 > 1.6 0.1-1?
?
10-4> 0.2 ?
10-4?
nononononono
yesyesGalactic “Micro-QSOs” (radio “jet” sources)Θ (degrees) βΓ LX/LE γ/TeV
MeV
Cyg X-1?
?
? 0.1-1 ~5yes
Cyg X-3
SS 433
GRS 1915+104
GRO J1655-40
GRS 1758-258
XTE J1550-564
Sco X-1
LS I 61 303
LS 5039< 14< 7070> 70?
60-70> 70?
< 80> 0.8 > 1.6 0.1-1
0.26 1.03 0.01
0.92 2.5 0.1-10.9 2.5
10.1-1> 0.8 1.5 0.1-1> 0.8 > 1.6 0.1-1?
?
10-4> 0.2 ?
10-4

YES
nono
no
no
no
no
yesyesConclusions• very exciting time for Galactic gamma- ray source
studies, AGILE and FERMI• detections by AGILE of Galactic transients– no hard X-ray outbursts– low flux X-ray sources• the Cyg X- 3 “clock”, a clear pattern of gamma- rayemission• FAST alerts and follow- up multi- freq. observations !
• Archival long
- baseline studies and cross- correlation