1
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
6
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)
7
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
10
RXTE2-10 keV
Swift15-50 keV
Super-AGILE(gray dots)
11
AGILE 2 sig U.L. above 100 MeVA: 2 weeksB: 4 weeks
C: 315 d
AGILE data flaring episode
Hard stateSoft state
12
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
13
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
17
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
18
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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23
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]
26
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