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Microquasars as seen with SIMBOL-X. J. Rodriguez (CEA/SAp & AIM; France). Ultra soft X-rays 0.1-3 keV: absorption, local conditions, circumstellar material. }. Self absorbed or not synchrotron emission: very long -> infra red/Optical. soft X-rays ~1keV-10 keV: -Thermal emission, disc - PowerPoint PPT Presentation
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1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Microquasars as seen with
SIMBOL-X
J. Rodriguez (CEA/SAp & AIM; France)
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Hard X-rays >10 keV:-Inverse Compton,
thermal vs non thermal-Non-thermal emission,
jet corona, reflection
Hard X-rays >10 keV:-Inverse Compton,
thermal vs non thermal-Non-thermal emission,
jet corona, reflection
soft X-rays ~1keV-10 keV: -Thermal emission, disc-Iron complex (lines, edge)
soft X-rays ~1keV-10 keV: -Thermal emission, disc-Iron complex (lines, edge)
Self absorbed or not synchrotron emission: very long -> infra red/Optical}
Ultra soft X-rays 0.1-3 keV: absorption, local conditions, circumstellar material
Ultra soft X-rays 0.1-3 keV: absorption, local conditions, circumstellar material
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
12 Years of RXTE
• Evolution along the outburst (mainly <20 keV PCA)=>disc, iron, corona (but only
• Short term (>16s) evolution=> disc,
• Phase spectroscopy and link Fe <-> QPO
Remillard et al. ‘06
Rodriguez et al. ‘02
QuickTime™ et undécompresseur TIFF (non compressé)
sont requis pour visionner cette image.
Miller & Homan ‘06
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Where do we stand?
• Spectral evolution between states: LS->HIMS->SIMS->SS
• Hysteresis: extra parameter to dm/dt needed
• Connection with radio behaviour (the jet line)
• The fundamental plane: X-ray/radio correlation in LS
• Tight connection with temporal behaviour
=> The Q-shaped pattern Belloni, Fender, et al.
BH knowledge greatly increased, especially behaviour of disc, but still lacks understanding
of the so-called corona and drivers of state changes
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Some (key) questions
• Interplay between spectral components• Emitting process(es) at high energies• Connection with jets• Iron complex : reflection, and also a
probe of the metric close to the BH
=> Need for high sensitivity, good spatial and spectral resolution, broad band coverage, high time resolution (D. Barret’s talk)
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Bright BH in outburst (1)• E.g. XTE J1550-564: In soft state, not detected
with HEXTE > 20 keV (Sobczak et al. ‘00)
NH = 0.907±0.003 1022 cm-2
kT = 0.759±0.001 keV= 2.50±0.03Line= 6.6 ±0.1 keVdof)
NH = 0.91±0.01 1022 cm-2
kT = 0.760±0.003 keV= 2.6±0.1dof)
• 1 ks => good determination of the spectrum up to ~80 keV, and precise estimate of all parameters
• 100s => good spectrum up to ~80 keV, main parameters well constrained
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Bright BH in outburst (2)• E.g. XTE J1550-564: In hard state, power law and cut off
(Rodriguez et al. ‘03)
FTEST gives 3e-18 chance improvement for the inclusion of the cut-off
NH = 0.88±0.02 1022 cm-2
Ecut = 40-5+7 keV
Efold = 51 -19 +27 keV= 1.48±0.011.03 (295dof)
100 s spectra
Extension beyond 80 keV?
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Why do we need short times in bright BHs?
Each blue point = 1 dayEach arrow = a few ks obsWhat happens in between?E.g when do ejections occur?
In ~12 ks : 2 sequences of correlated X-ray radio behaviour: short times => constraints on the physics triggering the ejection
GRS 1915+105
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Short times: the 1915 caseF TEST => 5e-20 chance
F TEST => 2e-11 chance
1s accumulation !!
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Accretion-ejection links today• With e.g. INTEGRAL integration of few hundreds of sec
=> averaging of spectra to get decent SNR
• R. et al. ‘06 => spike = trigger of ejection, ejected material is corona BUT low statistics >25 keV and accumulation over several 10s of seconds
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Accretion-ejection links with SIMBOL-X
• Method: follow the evolution of spectral parameters along the sequence on s time scale
• Aim: identify the real trigger of ejection, confirm the origin of the ejected material, understand how ejections take place (the disk-corona-jet connection)
• Advantage of SX: the 10-80 keV at 1s resolution… never done so far => tight constraints on corona
kT=1.48 ± 0.09 keVRin= 380 ± 60 km = 2.8 ± 0.4
F1-100 keV disk~F1-100 keV pl F1-100 keV disk~10 * F1-100 keV pl
kT=1.74 ± 0.07 keVRin= 255-12
+40km = 2.1 ± 1.2
=> What happens between both : formation of the jet in X-rays
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
External Galaxies: LMC
• Typical LHS, ~1037 erg/s (~10-10erg/s/cm2), powerlaw and cut-off, 10 ks observation
NH = 0.063±0.003 1022 cm-2
Ecut = 27.7±1.2 keV= 1.47±0.01dof)
Physics of outburst evolution => do source behave the same?Disc-corona connection in LMC, the Q shape?
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
LMC: Physical models
• Comptt and reflection: 10 ks, kTinj=0.2 keV, kTe=67 keV, relrefl=0.25
Comptt alone not satisfactory
NH = 0.05±0.02 1022 cm-2
Relref = 0.22 ± 0.06kTinj= 0.21-0.02
+0.003 keVkTe = 59.51-9
+13 keV= 2.2±0.2dof)F TEST => 8e-9 chance
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
External Galaxies: M 33
• Typical LHS, ~1037 erg/s (~10-10 erg/s/cm2), powerlaw and cut-off, 10 ks observation @ 795 kpc, 50 ks flux (20-100 keV)=2.6e-13 erg/s/cm2
NH = 0.05±0.02 1022 cm-2
Ecut = 33 -10 +24 keV= 1.5±0.1dof)F TEST => 5e-5 chance
NEVER BEEN OBSERVED
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
Quiescent microquasars
• 10-10 erg/cm2/s <=> 1035 erg/s @ 6kpc =>early and late stages of outbursts, evolution of corona, connection with disc, jets, reflection component
• 10-13 erg/cm2/s <=> 4.3 1032 erg/s @ 6 kpc <=>broad band spectra of quiescent sources behaviour of >10 keV emission for the 1st time: – physics of low luminosity accretion: physical properties of
plasma, ADAF, ..– study of populations of hard quiescence vs. soft
quiescence (Corbel et al. ‘05)
• Valid for all transient sources of the Galaxy (~40 BH(C)s, + transient NSs) => ¿ a criterion to distinguish NS and BH based on quiescent spectra ?
1st SIMBOL-X workshop, Bologna, May 14-16, 2007
To summarise• Bright sources
– Better characterisation of hard X-rays in Soft States => better estimate the disc parameters, identification “true” disc (e.g. Mc
Clintock et al. ‘06 vs. Middleton et al. ‘06) => measure of BH spin– Spectral monitoring of GRS 1915+105 like object on s time scale
Formation of jets in the X-rays Approach of disc and ejection of corona, does one cause the other ?
• Quiescent microquasars– Behaviour of >10 keV emission
Better constraints on the physics of low luminosity accretionStudy of source population: hard vs soft quiescence
• External Galaxies– Non biased study of source populations
Transient sources low luminosity hard state BHsCharacterisation up to quite high distance (~1 Mpc)
– Physical properties of extragalactic microquasars:Do they behave the same? study of the Q-shape (spectral transitions) patternPhysics of corona, reflection in external galaxies
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