1. ARTIST VIEW OF BLACK HOLES by Jean-Pierre Luminet

2. ACCRETION/JET CONNECTION IN MICROQUASARS: AS IN AGN THE JETS COME IN DIFFERENT TYPES 1) DOUBLE-SIDED RADIO SOURCE WITH STATIONARY LOBES ASSOCIATED TO PERSISTENT X-RAY SOURCES 2) DOUBLE OR SINGLE SIDED MOVING JETS THAT APPEAR AT TRANSITIONS FROM LOW-HARD TO HIGH-SOFT X-RAY STATES. FORMATION OF TERMINAL LOBES AT RADIO & X-RAYS. 3) TRANSIENT “BABY-JETS” DURING FAST TRANSITIONS FROM LOW-HARD TO HIGH SOFT STATES. FLUENCE-  T CONNECTION ? 4) COMPACT STEADY JETS DURING LONG LOW-HARD STATES SEEN IN ALL STEADILY ACCRETING BHs: Cyg X-1… Sgr A * IN  QSOs ASSOCIATED TO SPECIFIC X-RAY STATES

3. X/GAMMA-RAY SPECTRA OF BLACK HOLE BINARIES GRO (Grove et al 98) DIFFERENT FROM SPECTRA OF NEUTRON STAR X-RAY BINARIES

4. Grebenev et al. 93 Low/Hard and High/Soft states in Black Holes Accretion disk structure and spectrum described by Shakura & Sunyaev 73 Compact jet Corbel et al. 2001

5. The Power-Evolution of Black Hole XRBs Accretion DiskRadio & X-ray SpectrumRadio Jet Fender (2001)Sunyaev Sunyaev Sunyaev

6. Falcke et al. & Fender et al. 2002 X-RAY STATES AND JETS MAJOR EJECTIONS TAKE PLACE DURING X-RAY TRANSITION FROM LOW- HARD TO HIGH-SOFT STATE (Mirabel et al. 1994, 1998; Fender et al. 2002). Microquasar GRS 1915+105 VLBA ALLOWS ASTROMETRY AND PROPER MOTIONS WITH SUB-MAS PRECISION ! (Pooley with Ryle) RXTE 100 AU Dhawan, Mirabel, Rodriguez, 2000

7. MICROQUASARS AS PROBES OF BLACK HOLE FORMATION HOW ARE STELLAR-MASS BLACK HOLES FORMED ? IS IT BY PROMPT COLLAPSE OR DELAYED/FAILED COLLAPSE ? ARE BLACK HOLES BORN WITH NATAL KICKS AS NEUTRON STARS ? IS THIS A FUNCTION OF THE PROGENITOR AND BLACK HOLE MASS ? ANSWERS ARE IMPORTANT TO: 1) CONSTRAIN THE PHYSICAL MODELS, 2) FOR ASTRONOMY PROJECTS THAT USE GRB’s FOR COSMOLOGY. IS THE FORMATION OF BH’s ALWAYS ASSOCIATED TO SN AND GRB’s ? THE BIRTH PLACE AND MECHANISM OF FORMATION CAN BE INFERRED FROM THE KINEMATICS. BUT IT IS NOT POSSIBLE TO KNOW THE SPACE VELOCITY OF SOLITARY BLACK HOLES.

8. MULTIWAVELENGTH TOOLS TO TRACK THE PATH OF MICROQUASARS 1) RADIAL VELOCITY OF THE CENTRE OF MASS FROM SPECTROSCOPY OF THE DONOR STAR 2) PROPER MOTION FROM ASTROMETRY OF COMPACT JETS (VLBI) OR DONOR STAR (OPTICAL) THE GALACTOCENTRIC ORBIT CAN THEN BE COMPUTED USING A GALACTIC MASS MODEL 3) DISTANCE BY CLASSIC METHODS IN ASTRONOMY

9. BLACK HOLE IN THE HALO Mirabel, Dhawan, Rodrigues, Mignani, Guglielmetti (Nature, September 13, 2001) XTE J1118+480: M BH =7 M  @ l =158 o b=+62 o ; D=1.9 kpc V pec =150 km/sec Proper Motions: Radio with VLBA Optical on 43 years POSS DRIFTING AT A VELOCITY OF 150 km/sec

10. Animacion

11. POPULAR VIEW OF BLACK HOLES AS “CANNIBAL STARS”

12. Irapuan

13. THE PATH OF SCORPIUS X-1 A GALACTIC BULGE X-RAY BINARY WITH A “CHAOTIC” ORBIT

14. THE RUNAWAY BLACK HOLE GRO J1655-40 (Mirabel, Rodrigues, et al. 2002) DISTANCE = 1-3 Kpc RUNAWAY VELOCITY: 116 +/- 12 km/sec LINEAR MOMENTUM = 550 +/- 100 M SUN km/s as neutron stars BH FORMED IN A SN Consistent with (Israelian et al. Nature 2001) PROPER MOTION WITH HST

15. THE BIRTH SITES OF HMXBs LSI +61 303 Cygnus X-1 Rodrigues & Mirabel 2003 THE AGES, RUNAWAY VELOCITIES, PROGENITOR MASS LIMITS ETC… CAN BE CONSTRAINED

16. RESULTS In proceedings of 4 th Microquasar workshop ON 7 INDIVIDUAL SOURCES. THE RUNAWAY KINETIC ENERGY OF X-RAY BINARIES IS < 1% OF THE KINETIC ENERGY OF SUPERNOVAE. ALTHOUGH THE SAMPLE IS STILL NOT STATISTICALLY SIGNIFICANT TO DRAW MUCH GENERAL CONCLUSIONS. IN THE FUTURE IT WILL BE POSSIBLE TO CONSTRAIN WITH MORE PRECISION WHICH BLACK HOLES ARE FORMED IN THE EXPLOSION OF MASSIVE STARS AND WHICH ARE FORMED BY IMPLOSION, AS A FUNCTION OF THE PROGENITOR AND BLACK HOLE MASSES. CAVEAT: SELECTION EFFECT IN THE SAMPLE BECAUSE THE MOST ENERGETIC NATAL EXPLOSIONS MAY UNBOUND THE BINARIES, AND THEREFORE NOT ABLE TO SEE THOSE HIGH SPEED REMNANTS.