1. S. Chaty (University Paris 7 / CEA Saclay) Moriond Very High Energy Phenomena La Thuile, 14 March 2005 Microquasars and jets

2. S. Chaty - Moriond - 14 March 20052 Summary 0. Prelude to microquasars 0. Prelude to microquasars I. Youth of microquasars I. Youth of microquasars II. Maturity of microquasars II. Maturity of microquasars III. Microquasar land… III. Microquasar land… Accretion/ejection, jets and surroundings… Accretion/ejection, jets and surroundings…

3. S. Chaty - Moriond - 14 March 20053 0. Prelude to microquasars: SS 433 1979: Microquasar prototype: SS 433, or how a galactic object ejects matter at 0.26c (  =1.04 Margon 1984) 1979: Microquasar prototype: SS 433, or how a galactic object ejects matter at 0.26c (  =1.04 Margon 1984) Observations of emission lines in optical: content of jets is baryonic Observations of emission lines in optical: content of jets is baryonic Properties too special to be classified in a family Properties too special to be classified in a family SS433 & W50: 2°x2° (Dubner et al., 1998)

4. S. Chaty - Moriond - 14 March 20054 1990: SIGMA, orbiting on Granat, observes galactic black hole candidates 1990: SIGMA, orbiting on Granat, observes galactic black hole candidates 1992: First microquasar: 1E 1740.7-2942: bipolar radio jets spread over several light-years (jets/ISM interaction) 1992: First microquasar: 1E 1740.7-2942: bipolar radio jets spread over several light-years (jets/ISM interaction) Analogy with quasars Analogy with quasars The great annihilator of the Galaxy The great annihilator of the Galaxy I. Youth of microquasars: 1E 1740.7-2942 1E1740, 1’x1’: Mirabel et al. 1992 M87

5. S. Chaty - Moriond - 14 March 20055 Binary system of the Galaxy, black hole or neutron star, surrounded by an accretion disc, and a companion star Binary system of the Galaxy, black hole or neutron star, surrounded by an accretion disc, and a companion star Necessity of multi- wavelength observations to understand various components, at different scales of the system Necessity of multi- wavelength observations to understand various components, at different scales of the system Now ~20 microquasars in our Galaxy Now ~20 microquasars in our Galaxy I. Youth of microquasars: the scenario

6. S. Chaty - Moriond - 14 March 20056 1992: Discovery of the black hole candidate GRS 1915+105, archetype of microquasars 1992: Discovery of the black hole candidate GRS 1915+105, archetype of microquasars 1994: Observations of superluminal motion at v~0.92c 1994: Observations of superluminal motion at v~0.92c Advantages compared to quasars: Advantages compared to quasars: Closer Closer Observation of both jets: approaching and receding Observation of both jets: approaching and receding Ejection timescale much shorter Ejection timescale much shorter Physical analogy: microquasars really become “micro”-quasars Physical analogy: microquasars really become “micro”-quasars Now only microblazars miss to the family… Now only microblazars miss to the family… I. Youth of microquasars: GRS 1915+105 10 000AU=800mas Mirabel & Rodriguez 1994

7. S. Chaty - Moriond - 14 March 20057 Fruitful analogy quasars/ microquasars Fruitful analogy quasars/ microquasars Advantage microquasars: accretion/ejection timescale proportional to black hole mass Advantage microquasars: accretion/ejection timescale proportional to black hole mass Advantage quasars: Application of jet models from active galaxies to describe ejection in microquasars Advantage quasars: Application of jet models from active galaxies to describe ejection in microquasars I. Youth of microquasars: analogy with quasars Chaty, PhD, 1998

8. S. Chaty - Moriond - 14 March 20058 I. Youth of microquasars: analogy with quasars Marscher et al. 2002 (3C120 observed during 3 years) GRS 1915+105 observed during 1 month

9. S. Chaty - Moriond - 14 March 20059 1997: First observations of link between accretion- ejection in GRS 1915+105 1997: First observations of link between accretion- ejection in GRS 1915+105 Disappearance of internal part of accretion disc, followed by ejection of relativistic plasma clouds Disappearance of internal part of accretion disc, followed by ejection of relativistic plasma clouds Recurrent ~30-45mn cycles Recurrent ~30-45mn cycles I. Youth of microquasars: GRS 1915+105 Chaty, PhD, 1998 Mirabel, Dhawan, Chaty et al. 1998

10. S. Chaty - Moriond - 14 March 200510 Standard model: thermal emission of multicolour accretion disc + non- thermal emission of plasma corona Standard model: thermal emission of multicolour accretion disc + non- thermal emission of plasma corona Low/hard and high/soft states Low/hard and high/soft states Concurrent models: jet synchrotron emission from radio to X Concurrent models: jet synchrotron emission from radio to X I. Youth of microquasars: accretion Fender 2001

11. S. Chaty - Moriond - 14 March 200511 II. Maturity of microquasars: spectral energy distribution XTEJ1118+480 accretion disc + non- thermal emission + stellar emission Non-linear Monte- Carlo simulation with hot spherical plasma in the centre Chaty et al. 2003 Markoff et al. 2001 What is the jet contribution??? (need sensitivity + temporal resolution)

12. S. Chaty - Moriond - 14 March 200512 II. Maturity of microquasars: spectral energy distribution: comparison with GRS 1915+105 Flat radio spectrum, Plateau (low-hard) state Flat radio spectrum, Plateau (low-hard) state Jet emission -> NIR Jet emission -> NIR XTE J1118+480 & GRS 1915+105 have an accretion/outflow energy ratio falling into the regime of radio-quiet quasars XTE J1118+480 & GRS 1915+105 have an accretion/outflow energy 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) 1 st simultaneous observations with INTEGRAL Fuchs, Rodriguez, Mirabel, Chaty et al. 2003, A&A, 409, L35

13. S. Chaty - Moriond - 14 March 200513 III. Microquasar land: Ks Polarimetry of H1743-322 H1743-322 observed in outburst in 2003 and 2004 H1743-322 observed in outburst in 2003 and 2004 Average interstellar polarisation p=1.4-3.5%. Average interstellar polarisation p=1.4-3.5%. Linear polarisation of H1743- 322: p=2.25 +/- 0.75% Linear polarisation of H1743- 322: p=2.25 +/- 0.75% Polarisation is interstellar consistent with a large extinction: A V ~ 11 Polarisation is interstellar consistent with a large extinction: A V ~ 11 line-of-sight close to the Galactic centre line-of-sight close to the Galactic centre During outbursts: propitious to detect polarisation from IR jet, but no sign of intrinsic polarisation During outbursts: propitious to detect polarisation from IR jet, but no sign of intrinsic polarisation Dubus & Chaty, MNRAS subm.

14. S. Chaty - Moriond - 14 March 200514 Mini-outburst ESO/NTT 2003 observations: Ks 3.2 mag brighter than 2MASS (K S ~ 15.6 in quiescence) ESO/NTT 2003 observations: Ks 3.2 mag brighter than 2MASS (K S ~ 15.6 in quiescence) RXTE ASM light curve: small amplitude outburst with 4.5 counts/s peak lasting about a month (). RXTE ASM light curve: small amplitude outburst with 4.5 counts/s peak lasting about a month (Sturner & Shrader 2005). Our observations on the decline at ~2.5 counts/s. Our observations on the decline at ~2.5 counts/s. III. Microquasar land: Polarimetry of XTE J1550-564

15. S. Chaty - Moriond - 14 March 200515 Ks polarimetry of XTE J1550-564 & field stars (ESO/NTT 2003 during weak outburst). Stars cluster around the origin, dispersion of 0.5%. Ks polarimetry of XTE J1550-564 & field stars (ESO/NTT 2003 during weak outburst). Stars cluster around the origin, dispersion of 0.5%. Position of XTE J1550-564 inconsistent with other stars at the 2.5  level=> Intrinsic infrared polarization p=0.9-2.0%. Position of XTE J1550-564 inconsistent with other stars at the 2.5  level=> Intrinsic infrared polarization p=0.9-2.0%. Reddening E(B-V)=0.7=> Reddening E(B-V)=0.7=> expected interstellar polarisation: p K ~0.7% expected interstellar polarisation: p K ~0.7% Association with outburst? Association with outburst? Dubus & Chaty, MNRAS subm. III. Microquasar land: Polarimetry of XTE J1550-564

16. S. Chaty - Moriond - 14 March 200516 Some microquasars emit at high energy, emission dominated by power law (spectral index 2.5-3), no cut-off. Some microquasars emit at high energy, emission dominated by power law (spectral index 2.5-3), no cut-off. What is the underlying physical process: comptonization or synchrotron? What is the underlying physical process: comptonization or synchrotron? Need polarization… Need polarization… High-energy observations: Constraints on accretion-ejection models: Blandford-Payne, Blandford-Znajek, MRI… Constraints on accretion-ejection models: Blandford-Payne, Blandford-Znajek, MRI… Jets made of e - /e + or e - /p? Jets made of e - /e + or e - /p? Answer with detection of (Doppler) shifted or annihilation emission lines?=> need sensitivity Answer with detection of (Doppler) shifted or annihilation emission lines?=> need sensitivity III. Microquasar land: accretion-ejection Grove et al. 1998

17. S. Chaty - Moriond - 14 March 200517 III. Microquasar land: accretion-ejection Gallo, Fender, Pooley (2003) Coupling: F rad  F X +0.7 1 kpc Important to understand accretion/ejection coupling and model constraints No strong Doppler amplification: low velocity jet (  <0.8c,  <2) Coupling at higher energy???

18. S. Chaty - Moriond - 14 March 200518 Observation of a steady compact jet in GRS 1915+105, 1mas=10AU (Dhawan et al. 2000) Observation of a steady compact jet in GRS 1915+105, 1mas=10AU (Dhawan et al. 2000) Observation of sporadic ejections at large scale Observation of sporadic ejections at large scale III. Microquasar land: multi-scale observations of jets Fuchs, Rodriguez, Mirabel, Chaty et al. 2003 0.2’’/week

19. S. Chaty - Moriond - 14 March 200519 Microquasar community: jet = propagation of plasma clouds Microquasar community: jet = propagation of plasma clouds Extragalactic community: jet = propagation of shock wave Extragalactic community: jet = propagation of shock wave Application of 3C273 model to GRS 1915+105: Propagation of shock wave forming at 1AU, with dissipative stream at v=0.6c Application of 3C273 model to GRS 1915+105: Propagation of shock wave forming at 1AU, with dissipative stream at v=0.6c III. Microquasar land: jets Turler, Courvoisier, Chaty, Fuchs, 2004

20. S. Chaty - Moriond - 14 March 200520 1E 1740.7-2942: steady jet: braking of jet in interstellar medium? 1E 1740.7-2942: steady jet: braking of jet in interstellar medium? signature: narrow annihilation lines at 511 keV? need better sensitivity? signature: narrow annihilation lines at 511 keV? need better sensitivity? XTE J1550-564: Jets in X- rays => Acceleration of particles up to TeV: analogy with quasars XTE J1550-564: Jets in X- rays => Acceleration of particles up to TeV: analogy with quasars What is the e- maximal energy??? What is the e- maximal energy??? III. Microquasar land: jet-interstellar medium interaction Jets at large distance: 45’’ (Corbel et al. 2002) 1E1740.7-2942

21. S. Chaty - Moriond - 14 March 200521 III. Microquasar land: Jet-interstellar medium interaction: GRS 1915+105’s outburst Mirabel, Rodriguez, Chaty et al. 1996, ApJ, 472, L111 Strong & long X-ray outburst of GRS 1915+105 in 08/1995 Strong & long X-ray outburst of GRS 1915+105 in 08/1995 Radio source resolved in 2 jets Radio source resolved in 2 jets Increase of NIR emission between 2 and 5 days after the radio burst Increase of NIR emission between 2 and 5 days after the radio burst Presence of extended cocoon of dust, heated by ejections Presence of extended cocoon of dust, heated by ejections Cocoon created by previous ejections, jets, ISM dust??? Cocoon created by previous ejections, jets, ISM dust??? Dust later confirmed by CHANDRA and ISO observations Dust later confirmed by CHANDRA and ISO observations

22. S. Chaty - Moriond - 14 March 200522 III. Microquasar land: What about the surroundings of GRS 1915+105??? Low-resolution cm map: 2 sources aligned with central source Low-resolution cm map: 2 sources aligned with 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

23. S. Chaty - Moriond - 14 March 200523 Microblazar = Microquasar whose jet points towards the observer Microblazar = Microquasar whose jet points towards the observer V=0.98c: time/10, flux*1000, increase of photon energy V=0.98c: time/10, flux*1000, increase of photon energy BUT sources difficult to observe since flares, although strong, are short BUT sources difficult to observe since flares, although strong, are short Jet Precession: intermittent microblazar Jet Precession: intermittent microblazar V4641 Sgr: at distance of 6 kpc, jets exhibit apparent velocity of v~10c: microblazar? V4641 Sgr: at distance of 6 kpc, jets exhibit apparent velocity of v~10c: microblazar? III. Microquasar land: observation of microblazars… V4641 SGR: 1 day flare, 1.6->12.2 Crab, 14  8.8mag, wind velocity 5000km/s Chaty et al. 2003

24. S. Chaty - Moriond - 14 March 200524 III. Microquasar land: observation of ULXs… ULXs: ultra-luminous sources ULXs: ultra-luminous sources observed near active galactic nuclei at high stellar formation rate observed near active galactic nuclei at high stellar formation rate Beamed jets from microquasars? Beamed jets from microquasars? Or black holes of intermediate mass (~1000 M sol )? Or black holes of intermediate mass (~1000 M sol )? Are there ULXs in our Galaxy? Are there ULXs in our Galaxy? 3 associations between galactic microquasars and gamma-ray sources: e.g. LS 5039… 3 associations between galactic microquasars and gamma-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

25. S. Chaty - Moriond - 14 March 200525 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 e+ colliding the interstellar medium? Annihilation line emitted by microquasars, from jet or from 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 ULXs Distinguish sources, in particular ULXs With temporal resolution: With temporal resolution: Correlation between high-energy and radio (jet) emission Correlation between high-energy and radio (jet) emission With polarization: With polarization: Infrared & high-energy synchrotron emission: synchrotron??? Infrared & high-energy synchrotron emission: synchrotron??? Link Theory/model/observations: Link Theory/model/observations: Propagation of jet Propagation of jet Accretion-ejection mechanisms Accretion-ejection mechanisms Quasi-periodic oscillations Quasi-periodic oscillations IV. The key questions