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STEADY JETS AND TRANSIENT JETS Characteristics and Relationship  

Max-Planck-Institut für Radioastronomie, 7th - 8th April 2010, Bonn

Radio jets and high energy emission in microquasars

Radio jets and high energy emission in microquasars

Josep M. Paredes

Josep M. Paredes

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XB: A binary system containing a compact object (NS or a stellar-mass BH) accreting matter from the companion star. 299 XB in the Galaxy (HMXB, Liu et al. 2006, A&A 455,1165 and LMXB 2007, A&A 469, 807).

HMXBs: (114) Optical companion with spectral type O or B. Mass transfer via decretion disc (Be stars) or via strong wind or Roche-lobe overflow.

LMXBs: (185) Optical companion with spectral type later than B. Mass transfer via Roche-lobe overflow.

Microquasars: X-ray binaries with relativistic jetsMicroquasars: X-ray binaries with relativistic jets

At least 15 microquasarsMaybe the majority of RXBs are microquasars (Fender 2001)

299 XB 65 (22%) REXBs 9 HMXBs

56 LMXBs

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MICROQUASARS IN OUR GALAXY

Name System D Porb Mcomp Activity app θ Jet Size Remarks

type (kpc) (d) (M) radio (AU)

High Mass X-ray Binaries

LS I +61 303 B0V+NS? 2.0 26.5 p 0.4 10 700 Precession ?

V4641 Sgr B9III+ BH ~10 2.8 9.6 t 9.5

LS 5039 O6.5V+NS? 2.9 4.4 1 3 p 0.15 < 81º 10 1000 Precession?

SS 433 evolved A?+BH? 4.8 13.1 11± 5? p 0.26 79º ~104 106 Precession,Hadronic, X-ray jet

Cygnus X-1 O9.7I+ BH 2.5 5.6 10.1 p 40º ~ 40

Cygnus X-3 WNe+BH? 9 0.2 p 0.69 73º ~ 104 Radio outbursts

Low Mass X-ray Binaries

Circinus X-1 Subgiant+NS ~ 6.5 16.6 t > 15 < 5º >104

XTE J1550-564 G8+BH 5.3 1.5 9.4 t 2 ~ 103 X-ray jet

Scorpius X-1 Subgiant+NS 2.8 0.8 1.4 p 0.68 44º ~ 40

GRO J1655-40 F5IV+BH 3.2 2.6 7.02 t 1.1 72º85º 8000 Precession ?

GX 339-4 ?+ BH ~ 4 1.76 5.8 ± 0.5 t < 4000

1E 1740.7-2942 ?+BH ? 8.5? 12.5? p ~ 106

XTE J1748-288 ?+BH ? 8 ? > 4.5? t 1.3 > 104

GRS 1758-258 ?+ BH ? 8.5? 18.5? p ~106

GRS 1915+105 K-MIII+BH 12.5 33.5 14 ± 4 t 1.2 1.7 66º70º ~10 104 Precession?

Leptonic models: SSC Atoyan & Aharonian 1999, MNRAS 302, 253 Latham et al. 2005, AIP CP745, 323

EC Kaufman Bernadó et al. 2002, A&A 385, L10 Georganopoulos et al. 2002, A&A 388, L25

SSC+EC Bosch-Ramon et al. 2004 A&A 417, 1075

Synchrotron jet emission Markoff et al. 2003, A&A 397, 645

Hadronic models: Pion decay Romero et al. 2003, A&A 410, L1 Bosch-Ramon et al. 2005, A&A 432, 609

MQs as high-energy γ -ray sourcesTheoretical point of view

The VHE gamma-ray Sky MapThe VHE gamma-ray Sky Map

LS I+61 303

LS 5039 PSR B1259-63

At HE LSI+61303, LS5039 and Cygnus X-3: Fermi and AGILE (E > 100 MeV)

Cygnus X-1: AGILE 5

Cygnus X-1

38 extragalactic

60 galactic

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Parameters PSR

B1259-63

LS I +61 303

LS 5039 Cygnus X-1

Cygnus X-3

System Type B2Ve+NS B0Ve+NS? O6.5V+BH? O9.7I+ BH WR+ BH?

Distance (kpc) 1.5 2.0±0.2 2.5 2.0±0.2 ≈7

Orbital Period (d) 1237 26.5 3.9 5.6 4.8h

Eccentricity 0.87 0.72 0.35 ~0

Inclination (º) 36 30 20 20? 33 5

Periastron-apastron (AU)

0.7 - 10 0.1 - 0.7 0.1 - 0.2 0.2

Activity Radio Periodic (48 ms and 3.4 yr)

Periodic (26.5 d and 4 yr)

Persistent Persistent Persistent

and Bursts

Radio Structure (AU) <2000 ~Jet-like

10-700

Jet

10 -103

Jet

40 + ring

Lradio(0.1−100GHz) (erg s−1)

(0.02 −0.3)× 1031

(1 − 17) × 1031 1 × 1031 0.3 × 1031

LX(1−10keV) (erg s−1)

(0.3 − 6) ×1033 (3 − 9) × 1033 (5 − 50) × 1033

1 × 1037 ≈1038

LVHE (erg s−1) 2.3 × 1033 8 × 1033 7.8 × 1033 12 × 1033

Γ VHE 2.7 ± 0.2 2.6 ± 0.2 2.06 ± 0.05 3.2 ± 0.6

Large luminosity and

strong stellar wind

Radio emitters

might be a BH if i<25° (Casares et al. 2005)

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Gallo et al. 2005, Nature

Martí et al. 1996, A&A 306, 449

5 pc (8’) diameter ring-structure of bremsstrahlung emitting ionized gas at the shock between (dark) jet and ISM.

VLAWSRT

Stirling et al. 2001, MNRAS 327, 1273

VLBA+VLA

Stellar Mass Black Hole Cygnus X-1Cygnus X-1

15 mas 30 AU

● HMXB, O9.71+BH

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● Strong evidence (4.1 post trial significance) of intense short-lived flaring episode

● Orbital phase 0.9-1.0, when the black hole is behind the star and photon-photon absorption should be huge: flare in the jet?

MA

GIC

Albert et al. 2007, ApJ 665, L51

TeV source: Cygnus X-1

Hard x-rays ==> base of the jet (non-thermal e in the hot comptonising medium, McConnell et al. 2002)

-rays ==> further away by interaction with stellar wind (shocks located in the region where the outflow originating close to the BH interacts with the wind of the star, Perucho & Bosch-Ramon 2008, A&A

482, 917)

Malzac et al. 2008, A&A 492, 527

INTEGRAL

Flaring Activity

9Sabatini et al. 2010, ApJ 712, L10

AGILE 2-years integrated map

AGILE 1-day map

Black circle: optical position Green contour: AGILE 2sig confidence level

October 16, 2009

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RXTE2-10 keV

Swift15-50 keV

Super-AGILE(gray dots)

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AGILE 2 sig U.L. above 100 MeVA: 2 weeksB: 4 weeks

C: 315 d

AGILE data flaring episode

Hard stateSoft state

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Second AGILE detection of a gamma-ray flare from the Cygnus X-1 region (24-25 March 2010) Bulgarelli et al. 2010, Atel 2512

Fe

rmi

Public data. V. Zabalza

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Strong radio outburstsStrong radio outbursts

Modelling Cyg X-3 radio outbursts: particle

injection into twin jets Martí et al. 1992, A&A 258, 309

Exhibits flaring to levels of 20 Jy or more

In 1972 was first “caught” flaring above 20 Jy. These events are amongst the best-known examples of observed expanding synchrotron-emitting sources (21 papers in Nature Phys. Sci. 239, No. 95 (1972))

VLBA

Cygnus X-3Cygnus X-3

VLA, 5 GHz

Martí et al. 2001, A&A 375, 476

Miller-Jones et al. 2004, ApJ 600, 368

● HMXB, WR+NS?

Orbital modulation of X-ray emission lines i>60 NS, i<60 BH Vilhu et al. 2009, A&A 501,679

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RXTE ASM 3–5 keV —BATSE 20–100 keV ┼GBI 8.3 GHz ….

Strong radio flares occur only when the source is in the soft state

Szostek et al. 2008, MNRAS 388, 1001

If the non-thermal electrons responsible for either

the hard X-ray tails or

the radio emission during major flares

were accelerated to high enough energies then detectable emission in the γ-ray range, e.g., the GeV or TeV band, would be possible.

Given that major radio flares indicates the presence of hard X-ray tails, GeV and TeV emission should be searched for during those radio flares.

15Tavani et al. 2009, Nature 462, 620

AGILE

16Abdo et al. 2009, Science 326, 1512

Fermi

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Dubus et al. 2010, MNRAS

Jet launched around a BH- moderate bulk relativistic speed- oriented not too far from the light of sight

• The e− emit synchrotron radio beyond the γ-ray emission zone on much larger scales

• A shock occurs in the wind because (Perucho et al. 2010, A&A) - wind mass-loss rate is very large - orbit very tight

Jet IC emission Jet IC emission >100 MeV γ-ray modulation in Cyg X-3>100 MeV γ-ray modulation in Cyg X-3

Anisotropic IC e± pair cascade model. The optical depths for γ-rays created inside the binary system are huge. Escape of γ-rays with energies above a few tens of GeV is not very likely.

Bednarek, 2010, MNRAS

Anisotropic IC by jet relat. e− with stellar photons along the orbit produces a modulation in the gamma-ray lightcurve (Khangulyan et al. 2008, MNRAS)

Most μqs jets will interact much further away when their pressure matches that of the ISM. Any HE particles will find a much weaker radiation environment and will be less likely to produce a (modulated) IC γ-ray

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First high-energy (> 100 MeV)COS-B gamma-ray source:

CG/2CG 135+01 Hermsen et al. 1977, Nature 269, 494

The radio emitting X-ray binary LS I+61 303, since its discovery as a variable radio source, has been proposed to be associated

with the γ-ray source 2CG 135+01 (= 3EG J0241+6103) (Gregory & Taylor 1978, Nature 272, 704)

LS I +61 303LS I +61 303Historical association with a γ-ray sourceHistorical association with a γ-ray source

26.5 days periodicityRadio (P=26.496 d) Taylor & Gregory 1982, ApJ 255, 210; Gregory 2002, ApJ 575, 427

Optical and IR Mendelson & Mazeh 1989, MNRAS 239, 733; Paredes et al. 1994 A&A 288, 519

X-rays Paredes et al. 1997 A&A 320, L25

HE gamma-rays Abdo et al. 2009, ApJ 701, L123

VHE gamma-rays Albert et al. 2009, ApJ 693, 303

Periodic emissionPeriodic emission

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0.8-0.5

0.5-0.8

Tavani et al. 1998, ApJ 497, L89

3EG J0241+6103

EG

RE

TF

erm

i

Abdo et al. 2009, ApJ 701, L123

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0.5-0.8

Albert et al. 2009, ApJ 693, 303

FermiMAGIC blue, 0.5-0.7VERITAS black, 0.5-0.8

MAGIC

Albert et al. 2006, Sci 312, 1771

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Accretion onto a compact object (NS or BH) embedded in mass outflow of the B-star

Taylor & Gregory 1982, ApJ 255, 210; Taylor et al. 1992, ApJ 395, 268

LS I +61 303LS I +61 303

Resolved radio emission pointed towards the microquasar scenario (Massi et al. 2001 A&A 376, 217)

Non-accreting young pulsar in orbit around a mass-losing B star

Powered by the spindown of a young pulsar (Maraschi & Treves 1981, MNRAS 194,1)

Revived after the discovery of PSR B1259-63 (Tavani et al. 1994, ApJ 433, L37)

EVN at 5 GHz

MERLIN at 5 GHz

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Jet-like features have been reported several times, but show a puzzling behavior (Massi et al. 2001, 2004). VLBI observations show a rotating jet-like structure (Dhawan et al. 2006, VI Microquasars Workshop, Como, Setember 2006)

3.6cm images, ~3d apart, beam 1.5x1.1mas or 3x2.2 AU. Semi-major axis: 0.5 AU

VLB

A

A

B C

D

E

FGH

I

J

Observer

NOT TO SCALE

Pulsar scenario: Interaction of the relativistic wind from a young pulsar with the wind from its stellar companion. A comet-shape tail of radio emitting particles is formed rotating with the orbital period. We see this nebula projected (Dubus 2006, A&A 456, 801). UV photons from the companion star suffer IC scattering by the same population of non-thermal particles, leading to emission in the GeV-TeV energy range

Zdziarski et al. 2010, MNRAS

Not resolved yet the issue of the momentum flux of the pulsar wind being significantly higher than that of the Be wind, which presents a problem for interpretation of the observed radio structures (as pointed out by Romero et al. 2007).

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Romero, Okazaki et al. (A&A 474, 15) apply a “Smoothed Particle Hydrodynamics” (SPH) code in 3D dynamical simulations for both the pulsar-wind interaction and accretion-jet models.

When orbital effects are included, even the most favourable assumptions toward a large Be/pulsar wind momentum ratio do not produce the simple elongated shape inferred in the VLBI radio image, which was previously cited as strong evidence in favour of a pulsar wind interaction scenario

Be starPulsar

Massi & Zimmermann 2010 (arXiv:1003.3693)

Massi & Kaufman Bernadó 2009, ApJ 702, 1179

Lense-Thirring precession induced by a slowly rotating compact object could be compatible with the daily variations of the ejecta angle observed in LS I +61◦303.

6.7yr GBI dataPeriodic outbursts: two consecutive outbursts (opt. thick and opt. thin)

Shock-in-jet model:The opt. thin spectrum is due to shocks caused by relativistic plasma (transient jet) traveling through apreexisting much slower steady flow (steady jet)

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VLBA+VLA, 5 GHz

3EG J1824-1514

Paredes et al. 2000, Science 288, 2340

LS 5039LS 5039EGRET HESS

Aharonian et al. 2005 , Science 309, 746

Aharonian et al. 2006, A&A 460, 743

3.9 day orbital modulation in the TeV -ray flux● HMXB, O6.5V+NS?

The γ-ray data require a location of the production region at the periphery of the binary system at ~1012 cm (Khangulyan et al. 2008, MNRAS; Bosch-Ramon et al. 2008, A&A)

25Abdo et al. 2009, ApJ 706, L56

Black points (dotted line): phase-averaged spectrum Red points (dotted line): spectrum (fit) at inferior conjunction (0.45-0.9)Blue data points (dotted line): spectrum (fit) at superior conjunction (<0.45 and >0.9)

Fermi and H.E.S.S.Fermi

BP051(1999)

BR127 (2007)

GR021 (2000)

0.02 0.14 0.27 0.47 0.53 0.75 0.78 0.04Phase

To observerTo observer

The orbital plane has two degrees of

freedom:

0 10.5

Longitude of the ascending node

Inclination of the orbit

Preliminary!

[Moldón et al., in preparation]

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27Skilton et al. 2009, MNRAS 399, 317

Binary system?-Coincident with Be star MWC 148

- No companion yet detected; no information on period

-Variable X-ray and radio emission

Acciari (for the VERITAS Col.), arxiv:0905.3139

A new gamma-ray binary?A new gamma-ray binary? HESS J0632+057HESS J0632+057

Hinton et al. 2009, ApJ 690, L101

MWC 148: star XMMU J063259.3+0548: open circlePos. uncertainty of CoG of HESS J0632+057: square marker with error bar

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Instrument PSR

B1259-63

LS I +61 303 LS 5039 Cygnus X-1 Cygnus X-3

EGRET >100 MeV

__ 3EG

J0241+6103

3EG

J1824-1514

__ __

AGILE 30 MeV-50 GeV

__ yes __ yes yes

FERMI30 MeV-300 GeV

__ yes yes __ yes

HESS>100 GeV

yes not visible yes __ __

MAGIC>60 GeV

not visible yes __ yes __

VERITAS>100 GeV

not visible yes __ __ __

Period

ic

Period

ic

Period

ic

Period

ic

Period

ic

All of them are HMXBs All of them are radio emitters All of them have a bright companion (O or B star) source of seed

photons for the IC emission and target nuclei for hadronic interactions NS and BH are among these detected XRBs VLBI monitoring of the jets along the orbit is crucial to understand some of these

systems Multi-wavelength (multi-particle) campaigns are of primary importance HESS J0632+057: New gamma-ray binary?

SummarySummary