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

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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