Chaire Galaxies et Cosmologie Galaxies with radio and optical jets Françoise Combes
The jet: component of the standard model Less than 10% of galaxies have an active nucleus. 10% of AGN have Radio jets («Radio-Loud») Every galaxy has a black hole but the activity time-scale is short, ~ 10-40 million yrs According to the angle of the line of sight: the jet is seen, or relativistic motions, broad lines exist, or are hidden by the molecular torus (type 2, scattering, polarisation) 2
jet Distinction between jet and wind wind The wind comes from the heated disk, which can evaporate Or the magnetic pressure is too strong star BH disk Turbulence in the disk MRI instability magnetic lines 3
Activity cycles Separation of lobes ~ 100 kpc, V ~ 1000 km/s age t ~ 10 8 yrs Several cycles? Other way to estimate the duration of the activity cycles of AGN t ~ (galaxy life)(% active time) ~ (10 10 yrs)(1% of galaxies active with jets) ~ 10 8 yrs 4
Two types of morphologies for the radio jets High luminosity 3C 219 FR II (left) &FR I (right) 3C 33.1 3C 31 Low luminosity 3C 296 3C 47 Hot spots at the end 3C 465 Hot spots in the center 5
3C133 Image VLA Why only one jet? Faraday depolarisation~ 2 3C133 Polarisation Polarisation The visible jet is always towards the observer Laing, 1988 Eliminated hypothesis --The jet is alternatively on one side or the other --Absorbing medium 6
Relativistic aberration, Doppler boost Reference frame of the fluid Isotropic emission Reference frame of observer Lorentz transformation Already aberration at small speed (ex. rain) -- For AGN ~5 Flux multiplied by D 2 7
Total relativistic Doppler effect Doppler factor ~5 v/c ~ 0.98, D ~ 9.9 Aberration, Flux multiplied by D 2 Effect of time dilatation, Flux multiplied by D Time 1 Time 2 Time 3 Time 1 Time 2 Time 3 Source at rest Source in motion Doppler effect on frequencies, Flux in (synchrotron = 1) Flux multiplied by D 3+ ~D 4 ~ 9600 Some up to 100, D~200, and D 4 ~ 16 10 8!! S 8
Optical jets, various wavelengths Martel et al 2003
Superposition with Radio Jet radio: contours // optical jet (HST) 67kpc long HST+Merlin 10
HST Chandra Merlin 3C273, the most nearby quasar Jet detected at all wavelengths Superposition of optical jet (HST) in X-rays (Chandra) and in radio cm (Merlin) 11
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Jets can be super-luminal P at velocity v, with respect to O y = r sin t = r/v J et radio dans 3C C279 Light coming from P reaches us in less time than light coming from O. Time observed for the object to go from O to P t app = t - x/c t app = (r/v) - (r/c) cos t app = (r/v) (1 - cos ) V apparent on the sky v app = y/t app v app = (v sin )/(1 - cos ) For v<<c c, =v/c ~0 v app =vsin For v ~ c, v app >> v and even larger than c To observer
Relativistic jets: a large range of scales High resolution Space Telescope + radio jet (VLA) 14
Black hole in rotation: origin of Radio jets? If the black hole is rotating, energy can be extracted from it, by the Penrose process 15
Penrose process E2 > E1 E<0 up to 29% E1 Jean-Pierre Luminet 16
Mechanism of Blandford-Znajek The goal is to extract energy and angular momentum from the black hole in rotation. The electromagnetic field around the hole is perturbed by magneto-spherical currents, which produce a torque Slow down the black hole Pair creation e+ - e- Poloidal B field, and B same sense Described by the potential vector A H Horizon Particules in T can only fall in the hole disk The positrons are quickly absorbed by the hole, The atmosphere is of negative charge 17
Blandford-Znajek (following) disk Poynting vector S= E x B / 18
Electromagnetic extraction of rotational energy S horizon Plasma dominated by magnetic energy ergosphere S S B B Flux of Poynting vector S Blandford and Znajek 1977 B Equatorial plane 19
Extraction MHD and not only MD Plasma dominated by magnetic energy S horizon v ergosphere Flux of vector of Poynting B S v v v S B Region dominated by particules Negative flux of particules Punsly & Coroniti 1990 S B Equatorial plane 20
Torque slowing down the black hole: Jx B Meridian plane Punsly & Coroniti 1990 Angular momentum L 21
Numerical simulations: MD & MHD Monopole field (Komissarov 2001, McKinney 2005) Z H Le flux of Poynting corresponds to model of Blandford-Znajek stationnary state a=0.5 a=0.1 a=0.9 t=120 Lorentz factor 0 Z R The energy is extracted from BH, the introduction of particules MHD does not change the phenomenon MD R MHD very similar to MD model a=0.9 from 0 to 14 22
Ergosphere and B field in simulations Simulations MD, uniform field (Komissarov 2004) B 2 D 2 h All field lines entering the Ergosphere are in rotation up to 0.5 times of hole horizon ergosphere The dissipative layer in the equatorial plane is the source of energy Dissipative layer The energie is extracted from the region between The energie is extracted from the region between horizon and ergosphere (=processus of Penrose) 23
Jets are confined by magnetic fields Collimation over 8 orders of magnitude in scales 24
MHD and jet confinement The differential rotation twists the field lines which slows down rotation and allows more accretion Magnetic pressure and thermal pressure accelerate the jet Magnetic tension collimates Uchida et al 1999 25
Ejection mechanisms A black hole in rotation (a~1) accretes ionized and magnetized gas The gas falls in the hole, and some Electromagnetic energy is ejected along the rotation axis This energy flux (Poynting) will be charged with particules, to form a relativistic jet Similarity with the processus of Blandford-Znajek The reaction of the magnetic field is to accelerate the plasma in counter-rotation rotation of the hole Magnetic field lines Ergosphere Black hole Arrival of L < 0 Koide et al 2002 26
The radio galaxies are in general Ellipticals, may b b M M be because M BH ~M bulbe NGC 7052 NGC 4261
Galaxies host Cen A of FR-Is and FR-IIs The radio galaxies FR I and FR II are Giant ellipticals with dust lanes The FRI are often cd galaxies at the center of rich clusters M87 28
The majority of quasars are observed in galaxy mergers Violent gas shocks fueling of the black hole
Ejection of plasma: radio lobes in ellipticals, results of merers Cygnus A Image radio, VLA Optical mage, HST 30
A double quasar, just merging: 3C75, z=0.023 Image radio, VLA Optical limage HST 25,000 ly 31
Radio lobes, galaxies in motion 3C129 Galaxies move at a velocity up to 1000km/s in galaxy clusters 3C465 32
How two radio lobes can merge in a signle one NGC 1265, Perseus cluster 33
Weaker radio sources: more diffuse lobes Radio, VLA NGC 1316 in Fornax HST
Origin of radio mission : Power-law spectrum decreasing with frequency (slope 0 at nucleus, then -1) linearly polarised emission (at least 30%, which is a lot) Synchrotron radiation emitted by electrons in relativistic motion in a magnetic field For an electron of energy 2 2 v E m e c avec γ 1 1 γ 2 The characteristic frequency of emission is 6 2 c ~ 4.2 10 γ B Hz With B in Gauss c 35
Emission gamma (TeV) from a blazar Very high energy photons are emitted by radio AGN, when their jet is oriented towards the observer blazar & «Flat Spectrum Radio Quasar» (FSRQ) Doppler factors of 20-50! 36 Marscher 2005
Jets in Gamma: high variability Radiation mechanisms: synchrotron, SSC (synchrotron (y self-compton) & EIC (external inverse Compton) At low power: SSC At high power: EIC Variability on time scales down to minutes 37
The blazar sequence The highest luminosity blazars have the softest spectra Electrons of high energy In low power objects injection between min =10 4-5 to 10 6-7 At high L, min is smaller 38
Mechanisms of photons in culture B-field 2. Pair production 3. Compton scattering 3. Compton scattering 1. Seed high- 5. Compton 4. Pair energy photon scattering production Multiplication of high energy rays, as soon as (1) high energy photons are injected (2) there exists a B field transverse or chaotic (3) () an isotropic radiation field (BLR at 10 17 cm) (4) the Lorentz factor of the jet ~4-10 Stern & Poutanen (2006, 2008) 39
Why some AGN have radio jets and not others? Frequency and circumstances: Most AGN have no jet, 90% are «Radio-Quiet» 10% of «Radio-Loud»: a true dichotomie Are these different phases of an universal evolution? R=Radio/Optical Centaurus A Blue: X-rays Red: Radio Kellerman 1989 40
Two sequences in the plane L B L R 41
Same sequences in (L B /L Edd )-(L R /L Edd ) This time normalised to L Edd 10 38 (M BH /M ) erg/s 42
R~ L R /L B, accretion rate ~ L acc /L Edd 43
Criteria for radio jets 1) The parameter R increases when the accretion rate L acc /L Edd decreases 2) This is verified for both sequences «radio-loud» and «radio-quiet» 3) A saturation of the parameter R occurs at low accretion rate λ < 10-3 44
Dependence of R on the mass of the BH For powerful radio jets, M BH must be > 10 8 M 45
The micro-quasars in our Galaxy: nearby, variable at human time-scale SS433: micro-quasar Objects of stellar masses The end of life for massive stars Rotation of the BH 1000 times 46 per second
Microquasars & Quasars 47
Micro-quasar GRS 1915 superluminal velocity Scale: one month X-Rays: red Gamma-rays: grenn Radio : blue Ejection cycles of about one hour A dizain per day 48
Radio versus X for micro-quasars S radio S X S X For low accretion rates, the radio luminosity increases with the accretion rate (L X ) like L R L 0.7 X (Gallo et al. 2003) But for higher accretion rates 001Edd 0.01, the jet production becomes intermittent (Fender et al., 2004) 49
The accretion phases vary for example Cyg X-1 Accretion High (H) (small truncation radius) Accretion low (L) (higher truncation radius) Transitions Energy emitted in photons Compton H L 50
Fender 1999 1.0? 0.1? The different phases Instable Intermittent Micro-quasars & AGN The hard X are correlated with the radio emission In the high luminosity phase, the disk radiates efficiently, and electrons are not emitted Disque mince In the low phase, ADAF Pas de jet ni Truncation of the disk, formation de couronne of a corona where photons are comptonized (hard X-rays) Disque tronqué Couronne et jet continu The corona is the jet base51
Several phases for the Seyfert Seyferts 1 in general accrete at the Eddington limit this corresponds to a high accretion rate, unstable -- oscillation time-scale of ~ 2 yr (M/10 6 M ) Some Seyfert galaxies have no longer broad lines Narrow Line S1 example NLS1 PKS 2004-447 M = 5 10 6 M ; could become a classical S 1 in < 10 yr A brighter AGN, broader lines 52
Criteria for radio jets For AGNs as for micro-quasars, L R and L acc are related for the low accretion rates, and for high accretion rates, the production of jets become intermittent (e.g., Merloni et al., 2003, Nipoti et al., 2005) But the relations are verified separately for spirals and ellipticals, as for two parallel relations there exists an other parameter, related to the formation of these galaxies, and of their central black hole The spin of the black hole? 53
The role of the black hole spin If jets are produced by the extraction of the rotational energy of black holes and if elliptical galaxies have more luminous radio jets -- does this mean that ellipticals have not enough gas to stop the jets? -- or ellipticals have higher spin parameters (a)? Ellipticals are formed by mergers of smaller galaxies, but more frequently by major mergers Alargenumber of minor mergers could arrive in the same final mass state, but the spin would be cancelled statistically 54
Minor & major mergers The final angular momentum coming from several BH of random orientation cancels out Aresidual spin is expected for the black hole resulting from amajormerger merger 55
Simulations of jet formation Brinkmann & Brinkmann Camenzind 2004 & Camenzind LSW 2004 56
Esin et al. 1995 A. Müller (2004) 57
Unstable: Oscillations sity Luminos Fender & Belloni 2004 ARAA Frequency 58
Conclusions Properties of jets -- relativistic boost, disymmetry y -- superluminal jets -- analogy with micro-quasars -- The radio power is 3 orders of magnitude larger in ellipticals relative to spirals How are jets formed? -- Extraction of the rotational energy of the BH (Blandford-Znajek) (processus of Penrose + B field) -- the radio power increases when the accretion rate decreases Ellipticals have black holes with a larger spin ( a~1) Could be due to their formation in major mergers 59