1. MICROQUASARS Felix Mirabel European Southern Observatory. Chile on leave from CEA-Saclay. France Five international workshops VI in Como, Italy (18-22 Sept. 2006)

2. HIGH ENERGY SOURCES IN THE GALACTIC CENTRE Mirabel, Rodriguez, et al, 1992 Black Hole Wang et al. ApJ 2002 Belanger, Goldwurm, Goldoni, ApJ 2003 INTEGRAL Chandra

3. QUASAR-MICROQUASAR ANALOGY The scales of length and time are proportional to M BH R sh = 2GM BH /c 2 ;  T  M BH Unique system of equations: The maximum color temperature of the accretion disk is: T col  M/ 10M  ) -1/4 (Shakura & Sunyaev, 1976) Waited era of space astronomy For a given accretion rate: L Bol  M BH ; l jet  M BH ;  M BH -1 ; B  M BH -1/2 (Sams, Eckart, Sunyaev, 96; Rees 04) QUASAR MICROQUASAR Mirabel & Rodriguez (Nature 1998) APPARENT SUPERLUMINAL MOTIONS IN  QSOs AS IN QSOs ?

4. SUPERLUMINAL EJECTION IN A  QSO 1 arcsec Mirabel & Rodriguez, 1994 V app > C for a DISTANCE > 8 Kpc  cm THE PLASMA THAT RADIATES IN THE HARD X-RAYS IS BLOWN IN SUPERLUMINAL JETS VLA GRS 1915+105

5. SUPERLUMINAL MOTIONS IN THE GALAXY 1) ASYMMETRIES DUE TO RELATIVISTIC ABERRATION IN TWIN JETS 2)  QSOs HAVE SAME BULK LORENTZ FACTORS AS QSOs & BLAZARS 3) JET COLLIMATION @ 30-100 R sh IN M87 IS CONSISTENT WITH THE BLANDFORD-PAYNE MODEL (Biretta et al., 2004).  HADRONIC JETS ?

6. DARK JETS FROM BLACK HOLES Radio (Dubner et al); X-rays: (Brinkmann et al) SS433/W50 ATOMIC NUCLEI MOVING AT 0.26c  MECHANICAL LUMINOSITY > 10 39 erg/sec NON RADIATIVE JETS = “DARK” JETS >50% OF THE ENERGY IS NOT RADIATED 1 o = 60 pc  arcsec VLA 20cm

7. LARGE-SCALE JETS IN CYGNUS X-1 Gallo, Fender et al. Nature 2005 ring diameter = 5 pc LARGE-SCALE JETS IN GRS 1915+105 ? Rodriguez & Mirabel (2006) hot spots at ~ 50 pc > 50% OF THE RELEASED ENERGY IS NOT RADIATED IS IT A VHE SOURCE ?

8. MOVING X-RAY JETS IN A  QSO  QSOs XTE J1550-564 &  Corbel et al. Science 2002, 05 X-rays are produced by synchrotron  electrons accelerated to TeV energies

9. ACCRETION–JET CONNECTION - THE ONSET OF THE JET IS AT THE TIME OF A X-RAY “SPIKE” - SUDDEN REFILL OF THE INNER DISK & INJECTION INTO THE JETS - SHOCK THROUGH A MILDLY RELATIVISTIC COMPACT JET  T  M BH Mirabel, Dhawan, Rodriguez (1998 )1 hr = 30 yr in SgrA* GRS 1915+105

10. COMPACT STEADY JETS ~100 AU IN LENGTH PRESENT DURING PLATEAU STATE SPEED OF THE FLOW < 0.4c ( Ribo, Dhawan & Mirabel 2005) LARGE SCALE JETS ARE SHOCKS PROPAGATING  c THROUGH THE SLOWER MOVING COMPACT JET Ribo, Dhawan & Mirabel (2005) Mirabel, Dhawan, et al. 1998 2.0 cm 3.6 cm GRS 1915+105

11.  QSOs & ULTRALUMINOUS X-RAY SOURCES Microquasars in external galaxies X-ray (Chandra) Antennae Fabbiano et al. ISOTROPIC BUT M BH > 30 M  (Pakull et al. 2002) ANISOTROPIC BUT NOT BEAMED ( King et al 2001) ANISOTROPIC & BEAMED (Mirabel & Rodriguez, 1999; Koerding & Falke 2002) IMBHs DO NOT CONSTITUTE A LARGE FRACTION OF ULXs

12. VHE (>100 GeV) FROM    RAY BINARIES LSI +61 303 with MAGIC (Albert et al. Science 2006) VHE emission is variable LS 5039 with HESS (Aharonian et al. Science 2005) Both have compact objects with masses M < 4 M  Both are runaway HMXBs formed < 2 x 10 6 yrs ago

13. LS 5039 WAS EJECTED FROM THE GALACTIC PLANE A VHE (> 100 GEV) SOURCE Paredes, Ribo et al. 2002Ribo, Paredes et al. 2002 V = 100-140 km/s; e~0.5; Mj = 2000-5000 Km/s M  ; M ejected in SN = 5-15 M 

14. LSI +61 303 WAS EJECTED FROM A CLUSTER THE COMPACT OBJECT IN LSI +61 303 WAS FORMED < 2 Myr AGO IN AN ASYMMETRIC SN EXPOLSION V ~ 27 km/s  < 2 M  were blown away Linear momentum = 430 M  km/s, as in runaway neutron stars Mirabel, I. Rodrigues & Lu (A&A, 2004) Massey et al. 1995 IC 1805 A VHE ( > 100 GEV) SOURCE

15. MODELS FOR  -RAY BINARIES 1)IC of e - jets on UV photons (Paredes et al. 2002) or hadrons in the jets (Romero et al. 2005) with matter of the stellar wind. Microblazars (Mirabel & Rodriguez,1999) 2) e - from pulsar wind on UV Photons (e.g. PSR B1259-63, Maraschi & Treves, 1981) Mirabel (Science 309, 714, 2006)

16. VHE FROM COMPACT BINARIES PULSAR WIND MODEL: Power by rotational energy (Dubus, 2006) PSR B1259-63, LS 5039 & LSI +61 303 have compact objects with M < 4 M SUN Time variability & x-ray spectrum of LSI +61 303 resemble those of young pulsars LSI +61 303 is a Be star like PSR B1259-63 & all known Be/X-ray binary are NSs But does not satisfactorily fit the GeV  radio wavelength fluxes in LSI & LS 5039 Definitive proof: Detection of pulsations in LS 5039 & LSI +61 303 MICROQUASAR JET MODELS: Power by accretion (Bosch-Ramon) Particle energy in QSOs and  QSOs are comparable (blazar-microblazar analogy) The kinetic power in  QSOs is equal or larger than the radiated power Electrons in the jets are accelerated up to TeV energies LS 5039: jets are steady, two-sided, seem to have bulk motions of 0.2-0.3c as compact  QSO jets, and no radio outbursts have been observed (Paredes et al.) Definitive proof: VHE emission from confirmed BHs (e.g Cyg X-1, V 4641,GRS 1915) RADIO IMAGES WITH HIGHER SENSITIVITY AND RESOLUTION

17. GAMMA-RAY BURSTS OF LONG DURATION MARK THE BIRTH OF BLACK HOLES AT COSMIC DISTANCES They are detected at large redshifts, up to z = 6.4 They are exploding massive stars of low metallicity Associated with SN Ic & super-relativistic jets

18. QSO -  QSO -  GRB ANALOGY HAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, S&T 2002) AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ? no no ?

19. SUMMARY Microquasars have provided insight into: THE PHYSICS OF RELATIVISTIC JETS FROM BH’s THE CONNECTION BETWEEN ACCRETION & EJECTION Microquasars could provide insight into: A LARGE FRACTION OF ULXs IN NEARBY GALAXIES GRBs OF LONG DURATION IN DISTANT GALAXIES THE PHYSICS IN THE JETS OF DISTANT BLAZARS

20. HOW ARE BLACK HOLE BINARIES FORM ? THERE ARE THEORETICAL MODELS e.g. Fryer & Kalogera ; Woosley & Heger (2002) BUT FEW OBSERVATIONS ! Mirabel & I. Rodrigues (2001-05) used the kinematics of  QSOs to find out: BIRTH PLACE & NATURE OF THE PROGENITOR STARS WHETHER THE PROGENITOR STAR ALWAYS EXPLODES AS AN ENERGETIC SUPERNOVAE

21. A BLACK HOLE IN THE GALACTIC HALO XTE J1118+480 M BH ~7 M  M * =0.1–0.5 M  ; l =158 o b=+62 o ; D=1.9 kpc WAS THE BH FORMED IN THE HALO, THICK DISK OR IN THE GALACTIC THIN DISK BY A VIOLENT NATAL KICK ? GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs Yellow: Sun White: BH binary Orbit typical of globular clusters (Mirabel, Dhawan et al Nature 2001) but Solar abundances in the star imply that the black hole formed in a SN that polluted the donnor (astro-ph by Gonzalez et al. 2006)

22. A RUNAWAY BLACK HOLE A LIKELY FOSSIL OF A GRBs FORMED IN AN HYPER-NOVA (Israelian et al. Nature 2001) Mirabel, Irapuan Rodrigues et al. (A&A 395, 595, 2002) Proper motion with HST + radial velocity from ground RUNAWAY VELOCITY ~120 km/s MOMENTUM = 550 M  km/s as in runaway neutron stars LOW-MASS BLACK HOLE FORMED IN A LUMINOUS SUPERNOVA GRO J1655-40 M BH ~ 4 M  ORBITS FOR THE LAST 230 Myrs Yellow: Sun White: BH binary

23. THE GALACTIC TRIP OF SCORPIUS X-1 SCO X-1 FORMED IN A GLOBULAR CLUSTER OR GALACTIC BULGE The best determined XRB path. Parallax and proper motion from Fomalont et al. (Mirabel & I. Rodrigues, 2003) GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs Yellow: Sun Red: BH binary

24. THE ~10 M  BLACK HOLE IN Cyg X-1 WAS BORN IN THE DARK V < 9 +/- 2 km/s  < 1 M  ejected in SN Otherwise it would have been shot out from the parent association of massive stars MASSIVE STELLAR BH FORM PROMPTLY Mirabel & I. Rodrigues, Science (2003)

25. FORMATION OF THE BH IN GRS 1915+105 Moves in the Galactic plane with V b = 0 +/- 4 km/sec V BH = (33 to 70) +/- 12 km/s for D = 9 to 12 kpc (Chapuis & Corbel,2004) But dispersion velocity of 6x10 9 yr old disk population is ~50 km/s THE BH WAS FORMED PROMPTLY IN THE DISK Black hole of 14 +/-4 M  with a ~1 M  donnor (Greiner et al. 2002-3) VLBA astrometry during 7 years: 6.8+/-0.2 mas/yr (Dhawan & M., 2005)

26. QPOs AND GENERAL RELATIVITY GRS 1915+105 (Strohmayer) XTE & INDIAN SAT. max = f(M BH, Spin)  DETERMINE THE SPIN OF BLACK HOLES THE BLACK HOLE SPIN & DISK TEMPERATURE SUGGEST THAT JETS MAY BE POWERED BY THE BLACK HOLE SPIN High frequency QPOs (e.g. 40 & 67 Hz repeat in GRS) This 3:2 ratio now found in 4 BHXBs (Remillard et al.)  must depend on fundamental properties of black hole Jerome Rodriguez et al.

27. SUMMARY Microquasars have provided insight into: THE PHYSICS OF RELATIVISTIC JETS FROM BH’s THE CONNECTION BETWEEN ACCRETION & EJECTION THE FORMATION OF STELLAR-MASS BLACK HOLES Microquasars could provide insight into: A LARGE FRACTION OF ULXs IN NEARBY GALAXIES GRBs OF LONG DURATION IN DISTANT GALAXIES BLACK HOLE ASTROPHYSICS IS TODAY IN AN ANALOGOUS SITUATION AS WAS STELLAR ASTRONOMY IN THE FIRST HALF OF LAST CENTURY, WHEN THE HR DIAGRAM WAS CONSTRUCTED FOR FIRST TIME

28. IF THE EMPIRICAL CORRELATIONS X-ray/radio/mass QPOs/mass Noise-spectrum/mass Gallo et al. 2004 Abramovics, 2005 Uttley et al. 2004 BECOME MORE ROBUST, INDEPENDENTLY OF THE MODELS, THE MASS AND SPIN OF BLACK HOLES WILL BE DETERMINED

29. THE BLACK HOLE FUNDAMENTAL PLANE Merloni et al. Falke, Koerding et al.

30. SUPERLUMINAL MOTIONS IN QSOs & AGN OBSERVED IN > 30 QSOs & AGN IN RADIO & OPTICAL WAVES PROPER MOTION SEEN IN YEARS V app UP TO 30c in blazars One sided because of Doppler boosting WHAT IS THE NATURE ? “PLASMONS” OR SHOCKS ?