Future Directions in High Resolution AstronomyA Celebration of the 10th Anniversary of the VLBA

June 8-12, 2003, Socorro, New Mexico, USA

Marc Ribó CEA-SACLAY

MICROQUASARSMICROQUASARS

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

An X-ray binary is a binary system containing a compact object (either a neutron star or a stellar-mass black hole) accreting matter from the companion star. The accreted matter carries angular momentum and on its way to the compact object usually forms an accretion disk, responsible for the X-ray emission. A total of 280 X-ray binaries are known (Liu et al. 2000, 2001).

High Mass X-ray Binaries (HMXBs). Optical companion with spectral type O or B. Mass transfer via decretion disk (Be stars) or via strong wind or Roche-lobe overflow (OB SG). There are 131 known HMXBs.

Low Mass X-ray Binaries (LMXBs). Optical companion with spectral type later than B. Mass transfer via Roche-lobe overflow. 149 known LMXBs.

X-RAY BINARIESX-RAY BINARIES

An X-ray binary is a binary system containing a compact object (either a neutron star or a stellar-mass black hole) accreting matter from the companion star. The accreted matter carries angular momentum and on its way to the compact object usually forms an accretion disk, responsible for the X-ray emission. A total of 280 X-ray binaries are known (Liu et al. 2000, 2001).

High Mass X-ray Binaries (HMXBs). Optical companion with spectral type O or B. Mass transfer via decretion disk (Be stars) or via strong wind or Roche-lobe overflow (OB SG). There are 131 known HMXBs.

Low Mass X-ray Binaries (LMXBs). Optical companion with spectral type later than B. Mass transfer via Roche-lobe overflow. 149 known LMXBs.

X-RAY BINARIESX-RAY BINARIES

Radio Emitting X-ray Binaries (REXBs) are X-ray binaries that display radio emission, interpreted as synchrotron radiation. Around 43 of the known 280 X-ray binaries (15%) are REXBs, including 8 HMXBs and 35 LMXBs. Abundances:

Total Galaxy No X-ray pulsarsHMXBs 8/131 ( 6%) 8/86 ( 9%) 8/37 (22%)LMXBs 35/149 (23%) 35/147 (24%) 34/142 (24%)

QUASARS MICROQUASARS

Mirabel et al. (1992)

Quasar 3C 223 Microquasar 1E1740.7-2942

radio (VLA) observations at 6 cm

VLA at 1477MHz ~ 20 cm

MICROQUASARSMICROQUASARS

REXBs displaying relativistic radio jets.

Compact object may be a Neutron Star or a Black Hole (BH).

In BH, the length and time scales are proportional to the mass, M.

The maximum color temperature of the accretion disk is Tcol 2107 M1/4.

(Mirabel & Rodríguez 1998)

MICROQUASARSMICROQUASARS

REXBs displaying relativistic radio jets.

Compact object may be a Neutron Star or a Black Hole (BH).

In BH, the length and time scales are proportional to the mass, M.

The maximum color temperature of the accretion disk is Tcol 2107 M1/4.

(Mirabel & Rodríguez 1998)

Microquasars had to wait the era of high energy astrophysics

MICROQUASARS : ARTIST’S VIEW

Each source is interesting by itself.Only 15 confirmed cases with resolved jets, but probably all REXBs are microquasars!

Why study jets ?

• Outflows may be important for the structure of accretion flow.

• Jets may dissipate a large fraction of the total accretion energy.

• Jets may be a source of light element nucleosynthesis

• ….• They look cool ….

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

COMPACTS JETS: radio

GRS 1915+105

Dhawan et al. (2000)Fuchs et al. (2003)

GRS 1915+105

flat spectrum

emission = optically thicksynchrotron from radio IR

flat or inverted spectrum model:

conical jet cut 1/Rmin

shock accelerated e--

Observations : image in radio or spectrum: radio flat

Falcke et al. (2002)

ISOLATED (SUPERLUMINAL) EJECTIONS

• Move on the plane of the sky ~103 times faster• Jets are two-sided (allow to solve equations max. distance)• Advantage of AGN at <100 Mpc: collimation at 30-100 Rsh (M87, Junor et al. 1999)

same Lorentz factor as in Quasars : ~ 5-10

Mirabel & Rodriguez (1994)

VLA at 3,5 cm

VLBI at 22 GHz ~ 1,3 cm

~ arcsec. scale ~ milliarcsec.

scale

GRO J1655-40 (VLBA at 1.6 GHz)

Hjellming & Rupen (1995) (also Tingay et al. 1995)

= 0.92 , = 85

18-19 Aug. 1994

22-23 Aug. 1994

25-26 Aug. 1994

1-2 Sep. 1994

8-9 Sep. 1994

12-13 Sep. 1994

EPISODIC (SUPERLUMINAL) EJECTIONS

VLBA+VLA map of LS 5039 at 5 GHz (Paredes et al. 2000).

The asymmetry in the brightness of the components, and in their distance to the core, can be explained by Doppler boosting, implying:

0.15 , 81

The jet seems to be persistent, because radio emission is always detected at similar levels as the ones found when this map was obtained.

PERSISTENT JETS WITH NO OUTBURST

0.17 , 80

Persistent nature of the LS 5039 jets thanks to EVN and MERLIN observations on 2000 March 1 (Paredes, Ribó, Ros, Martí, & Massi 2002).

ONE-SIDED / TWO SIDED JETS

CYG X-3 (VLBA at 15 GHz)

Mioduszewski et al. (2001)

0.81 , 14

CYG X-3 (VLBA at 15 GHz) 0.81 , 14

CYG X-3 (VLA at 5 GHz)

Marti et al. (2000)

ONE-SIDED / TWO SIDED JETS

Mioduszewski et al. (2001)

= 0.48 , = 73

CYG X-3 (VLA at 5 GHz)

LS I +61 303 (EVN at 5 GHz)

LS I +61 303 (MERLIN at 5 GHz)

Massi et al. (2002)

Massi et al. (2001)

QuickTime™ et undécompresseur TIFF (non compressé)sont requis pour visionner cette image.

ENERGY TRANSFER FROM THE CORE TO THE RADIO JETS

Sco X-1 (Global VLBI at 5 GHz)

Fomalont et al. (2001)

= 0.45 , = 44Energy transfer at 0.95

JETS AT LARGE SCALES

• Steady jets in radio at arcminute scale

• Sources found to be nearly always in the low/hard state long-term action of steady jets on the interstellar medium

1E1740.7-2942

GRS 1758-258

VLA at 6 cm

LARGE SCALE JETS ex: XTE J1550-564

• 20 Sept. 1998: strong and brief X-ray flare

• Mbh= 10.5 +/- 1.0 M ; d ~ 5 kpc (Orosz et al. 2002)

RXTE/ASM lightcurve (1998-99)

20 Sept. 1998 one day X-ray flare

Hannikainen et al. (2001)

Superluminal relativistic ejection (Hannikainen et al. 2001)

VLBI2 –10 keV

XTE J1550-564 : LARGE SCALE X-RAY JETS !

Chandra images 0.3 - 8 keV

23 arcsec 

Related to the brief flare of Sept. 1998

Discovery of X-ray sources associated with the radio lobes

• Moving eastern source • Alignment + proper motion

First detection of moving relativistic X-ray jets !

Corbel et al. (2002)

• evidence for gradual deceleration• radio-X-ray spectrum: compatible with synchrotron emission from the same e-

distribution

• external shocks with denser medium? Particle acceleration, to TeV ?

Is it a lonely case ? No!

XTE J1748-248: a cosmic jet hits the wall ? (Hjellming, unpublished).

Jet/ISM interaction ? The jets stoped when it possibly hits a cloud.

Radio (VLA)

A fossil X-ray jet in 4U 1755-33

Angellini & White (2003)

• XMM-Newton observations of 4U 1755-33 in 2000 (in quiescence since 1995).• Large (7’) scale two-sided X-ray jets.• BHC active for > 25 years.• If v=c, it would have taken 13 yr to extend to its current length.

SUMMARY ABOUT JETS

• compact jets milli-arcsecond

• isolated ejections caused by state changes in the source

sometimes: superluminal ejections 0.1 to 1 arcsecond

• large scale jets: interaction with the interstellar medium

arcminute

• composition ?e-/e+, p+, ions ?

Paragi et al. (1999)

Equatorial emission inSS 433:

wind-like equatorial outflow

or

extension of the accretion disk

ANOMALOUS EQUATORIAL EMISSION

Equatorial emission with flat spectral index:

either thermal radiation

or

self-absorbed synchrotron.

More news soon…

Blundell et al. (2001)

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

Low/Hard

High/Soft

Grebenev et al. (1993)

VARIABILITY: Low/Hard and High/Soft states

• 2 main X-ray states for the black hole X-ray binaries

• Correlation between radio and hard X-ray emission

Fender, Corbel et al. (1999)

VARIABILITY : state changes

Fender (2001)Fender (2001)

•

“Classically” : soft X-rays disc (thermal), hard X-rays corona (IC of therm. phot.)

Some state changes transient ejections, ex: off high/soft

VARIABILITY: accretion / ejection coupling

• cycles of 30 minutes in GRS 1915+105 : ejections after an X-ray dip disappearance / refilling of the internal part of the disc ? transient ejections during changes of states

same phenomenon in the quasar 3C 120 ? far slower !

Mirabel et al. (1998)

Marscher et al. (2002)

Spectrum of a Microquasar

If jet emission extends up to the visible band, the jet has > 10% of the total power

Markoff et al. (2001)

If jet emission dominates the X-ray band, the jet has > 90% of the total power

Synchrotron(jet)

Synchrotron(jet)

Synchrotron(jet)

Synchrotron(jet)

thermal(disc)

thermal(disc)

?

• MeV emission due to Synch. Self-Compton from the compact jet ? (GLAST)

• shocks with the ISM TeV ?

39

The INTEGRAL mission

Launched on October 17, 2002NEW HORIZONS ON BLACK HOLE ASTROPHYSICS

MULTIWAVELENGTH INTEGRAL NETWORK (“MINE”)

R & DhawanQPO at 2.5 HzJEM-X

Y.Fuchs (Sap), G. Pooley, S. Trushkin ...

GRS 1915+105: INTEGRAL and Multi-

P. Goldoni, P. Sizun (SAp)

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

Astrometry and Stellar Evolution…… before GAIA

Two options for the final stages of the progenitor of the compact object:

• Mass loss or kick produce changes in the orbital parameters runaway binary systems.

• Prompt collapse produces no runaway.

Approach:

• Radial velocity curve provides radial velocity of the system.

• VLBI, HST or archives provide the proper motions in the plane of the sky.

• Classic methods in astronomy (also VLBI parallaxes!) provide the distance.

With all this information we can compute the space velocity. Assuming a mass model for the Galaxy we can compute the Galactocentric orbit of the system!

Up to now:

XTE J1118+480: a black hole formed ~7 Gyr ago in a Globular Cluster of the Galactic Halo, with vpec=150 km/s (Mirabel et al. 2001).

LS 5039: a runaway system with vpec=150 km/s and an amazingly huge linear momentum of ~ 6000 M km/s !!! (Ribo et al. 2002). Kick? Under study.

GRO J1655-40: a runaway low-mass black hole formed in a SN explosion with runaway velocity of vpec ~ 120 km/s and linear momentum of 550 M km/s, as seen in neutron star systems with kicks (Mirabel et al. 2002).

Sco X-1: a runaway system formed in a Globular Cluster (Mirabel & Rodrigues 2003).

Cyg X-1: a high-mass black hole formed by prompt collapse, or formed in the dark, with no SN explosion (Mirabel & Rodrigues 2003).

LS I +61 303: a runaway system that lost ~ 90 M !!! (Rodrigues & Mirabel, submitted).

GRS 1915+105: a black hole formed by prompt collapse? (Dhawan et al. in preparation).

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

RBSC: X-ray catalog at 0.1-2.4 keV, 18806 sources, Voges et al. (1999).NVSS: radio catalog at 1.4 GHz, 40, 1.8106 sources, Condon et al. (1998).

We assumed reasonable selection criteria for sources with b 5 and 40(NVSS limit) and ended up with a sample containing 17 sources.Among them:

4 already known sources:

The well known microquasars LS 5039, SS 433 and Cyg X-3

The new microquasar LS I +61 303.

We recovered all HMXB persistent microquasars except Cyg X-1.

THE CROSS-IDENTIFICATION METHODTHE CROSS-IDENTIFICATION METHOD

SUMMARY OF RESULTS AFTER OBSERVATIONSSUMMARY OF RESULTS AFTER OBSERVATIONS

Summary of the obtained results after the VLA, optical and EVN+MERLIN observations. An asterisk indicates a non-expected behavior for microquasars.

(Paredes, Ribó, & Martí 2002)(Ribó, Ros, Paredes, Massi, & Martí 2002)

SUMMARYSUMMARY

Summary of the obtained results after the VLA, optical and EVN+MERLIN observations. An asterisk indicates a non-expected behavior for microquasars.

(Paredes, Ribó, & Martí 2002)(Ribó, Ros, Paredes, Massi, & Martí 2002)

Optical spect. (Martí, Paredes, Bloom, Casares, Ribó, & Falco submitted)

SUMMARY OF RESULTS AFTER OBSERVATIONSSUMMARY OF RESULTS AFTER OBSERVATIONS

SUMMARYSUMMARYSUMMARY OF RESULTS AFTER OBSERVATIONSSUMMARY OF RESULTS AFTER OBSERVATIONS

Summary of the obtained results after the VLA, optical and EVN+MERLIN observations. An asterisk indicates a non-expected behavior for microquasars.

(Paredes, Ribó, & Martí 2002)(Ribó, Ros, Paredes, Massi, & Martí 2002)

Optical spect. (Martí, Paredes, Bloom, Casares, Ribó, & Falco submitted)

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

MICROBLAZARS (Mirabel & Rodriguez, ARA&A 1999)

Due to relativistic beaming: t

e.g. If = 5, t < 1/50 and I > 103

SHOULD APPEAR AS SOURCES WITH FAST

AND INTENSE VARIATIONS OF FLUX

DIFFICULT TO FOLLOW AND TO FIND

First microblazar: V4641 Sgr: a BH in a HMXB Vapp>10c & (Hjellming et al. 2000; Orosz et al.

2001)

PRECESSING MICROBLAZARS

Possible gamma-ray sources by inverse Compton of the electron jets and external photon fields

Kaufman-Bernado, Romero, Mirabel (A&A, 2002)

Romero, Kaufman-Bernado, Mirabel (A&A, 2002)

Cyg X-1 MAY BE A PRECESSING MICROBLAZAR • Possible gamma-ray transients seen by BATSE (Golenetskii et al. 2002 & Scmidt 2002)

• One-sided jet with possible variable ejection angle (Stirling et al. 2001)

• V > 0.5c with transient lasting a few hours

UNIDENTIFIED EGRET SOURCES (>100 MeV)

1) Relics from core-collapsed SN correlated with

the tilted Gould Belt (Grenier, 1998;Gehrels et al. 2000)

TWO MICROQUASARS IN THE ERROR BOX OF EGRET SOURCES:

TWO GALACTIC SUBSAMPLES (Grenier, 2001)

2) Variable, soft and faint population at a scale

high of ~2 kpc with a distribution of halo objects

LS 5039 (Paredes et al. 2000)

LS I +61 303 (Kniffen et al. 1997)

QSO CANDIDATES ARE HMXBs JET SOURCES (Paredes et al; Romero et al.)

ULTRALUMINOUS X-RAY SOURCESMicroquasars in external galaxies ?

X-ray (Chandra) AntennaeFabbiano et al.

SUPER-EDDINGTON X-RAY SOURCES

SHORT-LIVED HMXBs (MICROQUASARS) ?

WITH ANYSOTROPIC EMISSION: BEAMED (Mirabel & Rodriguez, 1999) ANISOTROPIC BUT NOT NECESARILY BEAMED (King et al. 2001)

WITH ISOTROPIC EMISSION BUT MBH > 60 M (Pakul et al. 2002)

MULTIWAVELENGTH OBSERVATIONS (Ward et al. 2001-03)

M82 seen by ChandraLx ~ 1040 erg/sec when Eddington limit Lx ~ MBH x 1038 erg/s

INTERMEDIATE MASS BHs > 200 M?

claimed by NASA press releases. However:

•Photon spectra similar to Galactic stellar-mass black holes

•Mostly seen in starburst galaxies (e.g. The Antennae)

•Where such Intermediate-mass BHs would accrete from ?

•Why none was found in the Milky Way ?

First radio counterpart of a ULX

Chandra

ATCA: source + radio contours

In the NGC 5408 galaxy:

HST image

Kaaret et al. (2003)

Origin of this ULX :• X-ray spectrum + radio and optical counterpart:

compatible with beamed emission from a relativistic jet (angle < 10°)

First extragalactic microblazar ???• Intermediate mass black holes in question ?

ULX

1. Introduction

2. Types of jets

3. State changes and accretion/ejection coupling

4. Astrometry and stellar evolution

5. A search for new microquasars

6. ULXs as microblazars

7. Conclusions

OUTLINEOUTLINE

Some major questions about jets

• What fraction of the total power output of compact objects is in jets versus radiated energy?

• Are jets electron/proton or electron/positron?• Are jets purely accretion powered or can jets

extract energy from the rotation of a bh?• How are jets formed and collimated?• What is the role of magnetic fields?• Are jets re-energized at large distances from

origin?

CONCLUSIONS Microquasars allow to gain insight into:

• THE PHYSICS OF RELATIVISTIC JETS AND THE INTERACTION WITH THE ISM

• THE CONNECTION BETWEEN ACCRETION DISK INSTABILITIES AND THE FORMATION OF JETS

• CONSTRAIN THE ORIGIN AND EVOLUTION OF BHs

NEW PERSPECTIVES• DETERMINE THE SPIN OF BLACK HOLES (QPOs)

• GAIN INSIGHT INTO ULTRALUMINOUS X-RAY SOURCES

• DEEPER SURVEYS TO DISCOVER NEW SOURCES

• GAIN INSIGHT INTO GRB AFTERGLOWS ?

• SOURCES OF GAMMA-RAYS AND TeV NEUTRINOS ?