S. Chaty (University Paris 7 / CEA Saclay) Moriond Very High Energy Phenomena

S. Chaty S. Chaty (University Paris 7 / CEA Saclay)

Moriond Very High Energy Moriond Very High Energy PhenomenaPhenomena

La Thuile, 14 March 2005La Thuile, 14 March 2005

Microquasars and jets

S. Chaty - Moriond - 14 March 2005S. Chaty - Moriond - 14 March 2005 22

SummarySummary

0. Prelude to microquasars0. Prelude to microquasars I. Youth of microquasarsI. Youth of microquasars II. Maturity of microquasarsII. Maturity of microquasars III. Microquasar land…III. Microquasar land…

Accretion/ejection, jets and surroundings…Accretion/ejection, jets and surroundings…


0. Prelude to microquasars: SS 4330. Prelude to microquasars: SS 433

1979: 1979: Microquasar prototypeMicroquasar prototype: SS : SS 433, or how a galactic object ejects 433, or how a galactic object ejects matter at 0.26c (matter at 0.26c (=1.04 =1.04 Margon 1984)Margon 1984)

Observations of emission lines in Observations of emission lines in optical: content of jets is baryonicoptical: content of jets is baryonic

Properties too special to be Properties too special to be classified in a familyclassified in a family

SS433 & W50: 2°x2° (Dubner et al., 1998)SS433 & W50: 2°x2° (Dubner et al., 1998)


1990: SIGMA, orbiting on 1990: SIGMA, orbiting on Granat, observes galactic Granat, observes galactic black hole candidatesblack hole candidates

1992: 1992: First microquasarFirst microquasar: : 1E 1740.7-2942: bipolar 1E 1740.7-2942: bipolar radio jets spread over radio jets spread over several light-years several light-years (jets/ISM interaction)(jets/ISM interaction)

Analogy with quasarsAnalogy with quasars The great annihilator of the The great annihilator of the

GalaxyGalaxy

I. Youth of microquasars: 1E 1740.7-2942I. Youth of microquasars: 1E 1740.7-2942

1E1740, 1’x1’: Mirabel et al. 1992

M87


Binary system of the Binary system of the Galaxy, black hole or Galaxy, black hole or neutron star, surrounded neutron star, surrounded by an accretion disc, by an accretion disc, and a companion starand a companion star

Necessity of multi-Necessity of multi-wavelength observations wavelength observations to understand various to understand various components, at different components, at different scales of the systemscales of the system

Now ~20 microquasars Now ~20 microquasars in our Galaxyin our Galaxy

I. Youth of microquasars: the scenarioI. Youth of microquasars: the scenario


1992: Discovery of the black hole 1992: Discovery of the black hole candidate GRS 1915+105, candidate GRS 1915+105, archetype of microquasarsarchetype of microquasars

1994: Observations of 1994: Observations of superluminal motion at v~0.92csuperluminal motion at v~0.92c

Advantages compared to quasars: Advantages compared to quasars: CloserCloser Observation of both jets: Observation of both jets:

approaching and recedingapproaching and receding Ejection timescale much shorterEjection timescale much shorter

Physical analogy: microquasars Physical analogy: microquasars really become “micro”-quasarsreally become “micro”-quasars

Now only microblazars miss to the Now only microblazars miss to the family…family…

I. Youth of microquasars: GRS 1915+105I. Youth of microquasars: GRS 1915+105

10 000AU=800mas Mirabel & Rodriguez 1994


Fruitful analogy Fruitful analogy quasars/ microquasarsquasars/ microquasars

Advantage Advantage microquasars: microquasars: accretion/ejection accretion/ejection timescale proportional timescale proportional to black hole massto black hole mass

Advantage quasars: Advantage quasars: Application of jet Application of jet models from active models from active galaxies to describe galaxies to describe ejection in microquasarsejection in microquasars

I. Youth of microquasars: analogy with I. Youth of microquasars: analogy with quasarsquasars

Chaty, PhD, 1998


I. Youth of microquasars: analogy with I. Youth of microquasars: analogy with quasarsquasars

Marscher et al. 2002

(3C120 observed during 3 years)GRS 1915+105 observed during 1 month


1997: First observations 1997: First observations of link between accretion-of link between accretion-ejection in GRS ejection in GRS 1915+1051915+105

Disappearance of internal Disappearance of internal part of accretion disc, part of accretion disc, followed by ejection of followed by ejection of relativistic plasma cloudsrelativistic plasma clouds

Recurrent ~30-45mn Recurrent ~30-45mn cyclescycles

I. Youth of I. Youth of microquasars: GRS microquasars: GRS

1915+1051915+105

Chaty, PhD, 1998Mirabel, Dhawan, Chaty et al. 1998


Standard model: Standard model: thermal emission of thermal emission of multicolour accretion multicolour accretion disc + non-thermal disc + non-thermal emission of plasma emission of plasma coronacorona

Low/hard and Low/hard and high/soft stateshigh/soft states

Concurrent models: Concurrent models: jet synchrotron jet synchrotron emission from radio emission from radio to Xto X

I. Youth of microquasars: accretionI. Youth of microquasars: accretion

Fender 2001


II. Maturity of microquasars:II. Maturity of microquasars: spectral energy spectral energy distributiondistribution

XTEJ1118+48XTEJ1118+4800

accretion accretion disc + non-disc + non-thermal thermal emission + emission + stellar stellar emissionemission

Non-linear Non-linear Monte-Carlo Monte-Carlo

simulation with simulation with hot spherical hot spherical

plasma in the plasma in the centrecentre

Chaty et al. 2003

Chaty et al. 2003

Chaty et al. 2003Markoff et al. 2001

What is the jet contribution???(need sensitivity + temporal resolution)


II. Maturity of microquasars:II. Maturity of microquasars: spectral energy spectral energy distributiondistribution: comparison with GRS 1915+105: comparison with GRS 1915+105

Flat radio spectrum, Plateau (low-hard) stateFlat radio spectrum, Plateau (low-hard) state Jet emission -> NIRJet emission -> NIR XTE J1118+480 & GRS 1915+105 have an accretion/outflow XTE J1118+480 & GRS 1915+105 have an accretion/outflow

energy ratio falling into the regime of radio-quiet quasarsenergy ratio falling into the regime of radio-quiet quasars

Study of the largest multiwavelength campaign(Ueda, Yamaoka, Sanchez, Dhawan, Chaty et al., 2002, ApJ, 571, 918)

1st simultaneous observations with INTEGRAL Fuchs, Rodriguez, Mirabel, Chaty et al. 2003, A&A, 409, L35


III. Microquasar land: III. Microquasar land: Ks Polarimetry of Ks Polarimetry of

H1743-322H1743-322 H1743-322 observed in H1743-322 observed in

outburst in 2003 and 2004outburst in 2003 and 2004

Average interstellar Average interstellar polarisation p=1.4-3.5%.polarisation p=1.4-3.5%.

Linear polarisation of Linear polarisation of H1743-322: p=2.25 +/- H1743-322: p=2.25 +/- 0.75%0.75%

Polarisation is interstellar Polarisation is interstellar consistent with a large consistent with a large extinction: Aextinction: AVV~ 11 ~ 11 line-of-sight close to the line-of-sight close to the

Galactic centreGalactic centre

During outbursts: During outbursts: propitious to detect propitious to detect polarisation from IR jet, polarisation from IR jet, but no sign of intrinsic but no sign of intrinsic polarisationpolarisation Dubus & Chaty, MNRAS

subm.


Mini-outburstMini-outburst

ESO/NTT 2003 ESO/NTT 2003 observations: Ks 3.2 observations: Ks 3.2 mag brighter than mag brighter than 2MASS (K2MASS (KSS~ 15.6 in ~ 15.6 in quiescence)quiescence)

RXTE ASM light curve: RXTE ASM light curve: small amplitude small amplitude outburst with 4.5 outburst with 4.5 counts/s peak lasting counts/s peak lasting about a month about a month ((Sturner & Shrader 2005). ).

Our observations on Our observations on the decline at ~2.5 the decline at ~2.5 counts/s. counts/s.

III. Microquasar land:III. Microquasar land: Polarimetry of XTE J1550-Polarimetry of XTE J1550-

564564


Ks polarimetry of XTE Ks polarimetry of XTE J1550-564 & field stars J1550-564 & field stars (ESO/NTT 2003 during (ESO/NTT 2003 during weak outburst). Stars weak outburst). Stars cluster around the origin, cluster around the origin, dispersion of 0.5%.dispersion of 0.5%.

Position of XTE J1550-564 Position of XTE J1550-564 inconsistent with other inconsistent with other stars at the 2.5stars at the 2.5 level=> level=> Intrinsic infrared Intrinsic infrared polarization p=0.9-2.0%.polarization p=0.9-2.0%.

Reddening E(B-V)=0.7=>Reddening E(B-V)=0.7=> expected interstellar expected interstellar

polarisation: ppolarisation: pKK~0.7%~0.7% Association with Association with

outburst?outburst? Dubus & Chaty, MNRAS subm.

III. Microquasar land:III. Microquasar land: Polarimetry of XTE Polarimetry of XTE

J1550-564J1550-564


Some microquasars emit at Some microquasars emit at high energy, emission high energy, emission dominated by power law dominated by power law (spectral index 2.5-3), no cut-(spectral index 2.5-3), no cut-off.off.

What is the underlying What is the underlying physical process: physical process: comptonization or comptonization or synchrotron?synchrotron?

Need polarization…Need polarization…

High-energy observations:High-energy observations: Constraints on accretion-Constraints on accretion-

ejection models: Blandford-ejection models: Blandford-Payne, Blandford-Znajek, Payne, Blandford-Znajek, MRI…MRI…

Jets made of eJets made of e--/e/e++ or e or e--/p?/p? Answer with detection of Answer with detection of

(Doppler) shifted or (Doppler) shifted or annihilation emission lines?annihilation emission lines?=> need sensitivity=> need sensitivity

III. Microquasar land: accretion-ejectionIII. Microquasar land: accretion-ejection

Grove et al. 1998


III. Microquasar land: accretion-ejectionIII. Microquasar land: accretion-ejection

Gallo, Fender, Pooley (2003)

Coupling:Frad FX

+0.71 kpc

Important to understand accretion/ejection coupling and model constraints

No strong Doppler amplification: low velocity jet (<0.8c, <2)

Coupling at higher energy???


Observation of a steady Observation of a steady compact jet in GRS compact jet in GRS 1915+105, 1mas=10AU 1915+105, 1mas=10AU (Dhawan et al. 2000)(Dhawan et al. 2000)

Observation of sporadic Observation of sporadic ejections at large scaleejections at large scale

III. Microquasar land: multi-scale observations of jetsIII. Microquasar land: multi-scale observations of jets

Fuchs, Rodriguez, Mirabel, Chaty et al. 2003

0.2’’/week


Microquasar Microquasar community: jet = community: jet = propagation of plasma propagation of plasma cloudsclouds

Extragalactic Extragalactic community: jet = community: jet = propagation of shock propagation of shock wavewave

Application of 3C273 Application of 3C273 model to GRS model to GRS 1915+105: Propagation 1915+105: Propagation of shock wave forming of shock wave forming at 1AU, with dissipative at 1AU, with dissipative stream at v=0.6cstream at v=0.6c

III. Microquasar land: jetsIII. Microquasar land: jets

Turler, Courvoisier, Chaty, Fuchs, 2004


1E 1740.7-2942: steady 1E 1740.7-2942: steady jet: braking of jet in jet: braking of jet in interstellar medium?interstellar medium? signature: narrow signature: narrow

annihilation lines at 511 annihilation lines at 511 keV? need better keV? need better sensitivity?sensitivity?

XTE J1550-564: Jets in X-XTE J1550-564: Jets in X-rays => Acceleration of rays => Acceleration of particles up to TeV: particles up to TeV: analogy with quasarsanalogy with quasars

What is the e- maximal What is the e- maximal energy???energy???

III. Microquasar land: jet-interstellar medium III. Microquasar land: jet-interstellar medium interactioninteraction

Jets at large distance: 45’’ (Corbel et al. 2002)

1E1740.7-2942


III. Microquasar land: Jet-interstellar III. Microquasar land: Jet-interstellar medium interaction: GRS 1915+105’s medium interaction: GRS 1915+105’s

outburstoutburst

Mirabel, Rodriguez, Chaty et al. 1996, ApJ, 472, L111Mirabel, Rodriguez, Chaty et al. 1996, ApJ, 472, L111

Strong & long X-ray outburst Strong & long X-ray outburst of GRS 1915+105 in 08/1995of GRS 1915+105 in 08/1995

Radio source resolved in 2 Radio source resolved in 2 jetsjets

Increase of NIR emission Increase of NIR emission between 2 and 5 days after between 2 and 5 days after the radio burstthe radio burst

Presence of extended cocoon Presence of extended cocoon of dust, heated by ejectionsof dust, heated by ejections

Cocoon created by previous Cocoon created by previous ejections, jets, ISM dust???ejections, jets, ISM dust???

Dust later confirmed by Dust later confirmed by CHANDRA and ISO CHANDRA and ISO observationsobservations


III. Microquasar land: III. Microquasar land: What about the What about the

surroundings of GRS surroundings of GRS 1915+105???1915+105???

Low-resolution cm Low-resolution cm map: 2 sources aligned map: 2 sources aligned with central sourcewith central source

Strange non-thermal features in the south-east lobe

Synchrotron signature=> interactions between jets and ISM?

Chaty et al. 2001, A&A, 366, 1035


Microblazar = Microquasar Microblazar = Microquasar whose jet points towards the whose jet points towards the observerobserver

V=0.98c: time/10, flux*1000, V=0.98c: time/10, flux*1000, increase of photon energyincrease of photon energy

BUT sources difficult to BUT sources difficult to observe since flares, although observe since flares, although strong, are shortstrong, are short

Jet Precession: intermittent Jet Precession: intermittent microblazarmicroblazar

V4641 Sgr: at distance of 6 V4641 Sgr: at distance of 6 kpc, jets exhibit apparent kpc, jets exhibit apparent velocity of v~10c: velocity of v~10c: microblazar?microblazar?

III. Microquasar land: observation of III. Microquasar land: observation of microblazars…microblazars…

V4641 SGR: 1 day flare, 1.6->12.2 Crab, 148.8mag, wind velocity 5000km/s

Chaty et al. 2003


III. Microquasar land: observation of ULXs…III. Microquasar land: observation of ULXs…

ULXs: ultra-luminous sources ULXs: ultra-luminous sources observed near active galactic nuclei at high stellar formation observed near active galactic nuclei at high stellar formation

raterate

Beamed jets from microquasars?Beamed jets from microquasars? Or black holes of intermediate mass (~1000 MOr black holes of intermediate mass (~1000 Msolsol)?)?

Are there ULXs in our Galaxy?Are there ULXs in our Galaxy? 3 associations between galactic microquasars and gamma-3 associations between galactic microquasars and gamma-

ray sources: e.g. LS 5039…ray sources: e.g. LS 5039… ……and hundreds of unidentified gamma-ray sources exist…and hundreds of unidentified gamma-ray sources exist…

Need better angular resolution for ULXs Need better angular resolution for ULXs


With better sensitivity:With better sensitivity: Low/hard emission related to presence of jet?Low/hard emission related to presence of jet? Annihilation line emitted by microquasars, from jet or from Annihilation line emitted by microquasars, from jet or from

e+ colliding the interstellar medium?e+ colliding the interstellar medium? What is the nature of the jet?What is the nature of the jet?

With better angular resolution:With better angular resolution: Distinguish sources, in particular ULXsDistinguish sources, in particular ULXs

With temporal resolution:With temporal resolution: Correlation between high-energy and radio (jet) emissionCorrelation between high-energy and radio (jet) emission

With polarization:With polarization: Infrared & high-energy synchrotron emission: Infrared & high-energy synchrotron emission:

synchrotron???synchrotron??? Link Theory/model/observations:Link Theory/model/observations:

Propagation of jetPropagation of jet Accretion-ejection mechanismsAccretion-ejection mechanisms Quasi-periodic oscillationsQuasi-periodic oscillations

IV. The key questionsIV. The key questions

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S. Chaty (University Paris 7 / CEA Saclay) Moriond Very High Energy Phenomena

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