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On Dichotomies in Active Galaxies or The Jet-Accretion Connection

On Dichotomies in Active Galaxies or The Jet-Accretion Connection. Annalisa Celotti - S.I.S.S.A. [celotti@sissa.it]. Jets/outflows in accreting systems. Active Galactic Nuclei ~10% AGN 'radio-loud' extended / compact jets aligned up to 10 8 decades q < few degrees

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On Dichotomies in Active Galaxies or The Jet-Accretion Connection

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  1. On Dichotomies in Active Galaxies or The Jet-Accretion Connection Annalisa Celotti - S.I.S.S.A. [celotti@sissa.it]

  2. Jets/outflows in accreting systems Active Galactic Nuclei ~10% AGN 'radio-loud' extended / compact jets aligned up to 108decades q < few degrees G~ 10 L ~ 1043- 1048erg/s SMBH + disc Gamma-ray Bursts 102 < G < 104 q ~ ? L ~ 1052 erg /s BH + torus X-ray Binaries up to ~ 20% (?) a few SL G ~ few - >> 1 (?) L ~ 1038- 1040 erg /s BH / NS + disc

  3. RQ Quasars + Sey 1 ~30%(?) outflows radio BAL outflows: ~10% QSO Tb > 108 K + compact (< pc) SMHB + disc PG 1407 + 263 z=0.94 Blundell et al. 03 Low Luminosity AGN ~20-60% unresolved radio + Tb > 108K SMHB + disc Pulsars Chandra jets (e.g. Crab) G= ? v =0.5 c (HST) magnetized rotating NS no disc ? Crab Young Stellar Objects v ~ vesc~ 100- 400 km /s L ~ 10-2 - 10-1 Lstar protostar + disc HST archive And… Jets/outflows are easy to form

  4. How/Why jets form? Qs: - How/where/why are they formed, accelerated and collimated? - How do they relate to gas inflow? - In which form is energy extracted and transported? - How/where/why do they dissipate? JETSenergetically important COMPACT OBJECTrequired? v~v esc potential, i.e. BHnecessary for relativistic jets? DISCnecessary? different accretion regimes? OUTFLOWS: necessary?

  5. BH vs DISC ?Jet content(pairs, el.m.,e-p) MBH, accretion mode, relative power The jet – disc connection Mirabel et al 98 Possible answers Hydromagnetic B provides link jet-disc/hole (rotational) power + symmetry from : spinning BH:low barion loading - no radiation drag disc:more power (depending on accretion regime) ? are jets needed? both?:relativistic el.m./pair core + collimating e-p `slow’ MHD flow

  6. Jet-disc connection in AGN Which is the connection between accretion rate/accretion regime and jets? 1. Jetted vs non jetted AGN with similar accretion propertiesRL-RQ quasars 2. Jetted AGN with different accretion properties FRI-FRII Radio Galaxies 3. Non-jetted AGN with different accretion properties LINERS and Seyfert galaxies

  7. RL RL Radio Power Radio-to-optical ratio: R*º Lr / Lo RQ RQ Elvis et al. ‘94 Elvis et al. ‘94 Optical Optical 1 - Radio loudness of quasars RL ~ 10% AGN (opt. surveys) : dichotomy?

  8. R*5 GHz ~ 10 Log10 P5 GHz ~ 25 Miller et al. 1990 1 - Evidence for RQ/RL dichotomy Padovani1993

  9. FIRST + Large Bright Quasar Survey New large complete samples FIRST + 2dF Quasar Redshift Survey Lr vs L opt 2dF + LBQS Large spread between optical and radio luminosities Cirasuolo et al. 02 2dF + LBQS No evidence for a gap Hewitt et al. 00 R 1- Is the RQ/RL dichotomy real ? The fraction of radio detected quasars depends on apparent and absolute optical magnitudes

  10. * Radio properties Lr Radio and optical luminosities related andunrelated Shapes Log10 R*1.4 or Log10 Pradio distributions: Distributions of radio-to-optical ratios and radio powers Dependence of the fraction on apparent/absolute magnitude Number counts: radio and optical band Redshift and absolute magnitude distributions N LBQS 2dF PG R 1- Bypass selection effects: A new approach * Optical Luminosity Function: Lopt,z * Monte Carlo simulations + Observational cuts * Comparison with data(KS and c2)

  11. X1 = -0.5 ± 0.3 s1 = 0.75 ± 0.3 Monotonic distribution: no gap X2 = 2.7 ± 0.2 s2 = 0.7 ± 0.2 97±2 % Cirasuolo et al. 02 R Lr 1 - Result: No dichotomy Uniqueness of the solution using only a simple prescription for R*1.4 Radio luminosity depends on optical one, even though with a large scatter. The dependence of the fraction of RL quasars on apparent and absolute magnitude results from selection effects. Continuity in jet formation mechanism(s) ?

  12. Ivezic et al 02, 03 R Radio Optical Ivezic et al 02 Ivezic et al 03 Optical R R Cirasuolo et al See also Jester & Kron: SDSS+FIRST 1- What about SLOAN results?

  13. 3c31 Cyg A Fanaroff & Riley 74; Ledlow & Owen 96 Images courtesy of NRAO/AUI Morphology radio power 2 - Phenomenology of radio galaxies: FRI - FRII

  14. Ghisellini & Celotti 01 + MB - MBH[McLure & Dunlop 01] m Lr - LNLR - Lacc[Willott et al 01] Transition FRI-FRII : ~ const ~ 6 10-2 /e0.1 2- Transition FRI-FRII

  15. Radio gal: direct look at nucleus at HST resolution 3CR RG (z<0.3) Lopt vs Lr FRI Chiaberge, Capetti & Celotti 99, 01, 02; Verdoes Kleijn ea 01 * Compact core (< tens-hundreds pc) in majority of sources * In FRI optical luminosity correlates with radio 2 - Estimate of nuclear luminosity - I

  16. FRI + FRII Lopt Unification RL AGN Relativistic beamingRadio gal vs blazar Obscuring ‘torus’Broad vs Narrow lines BRLG(Broad Line Galaxy) QUASAR LIKE HEG (High-Excitation Galaxy) OBSCURED OBJECTS LEG(Low-Excitaton Galaxy)FRI LIKE BLRG + QSO Lradio FRII 2 - Estimate of nuclear luminosity II

  17. Marchesini, Capetti & Celotti 04 • FRI + FRII/LEG:no optically and geometrically thick torus • FRII/HEG: obscured • FRII/BLRG + QSO:‘’extra’ thermal/disc emission OPT IR OPT IR 2 - Nuclear optical emission * Nuclear transition for: continuum + lines + torus * Nuclear properties do not match extended radio: on-off episodes/evolution?

  18. m in Eddington units= L / LEdde D(log ) ~ 0.45 m m 2 - Accretion properties MBH from MB-MBH LBOLfrom Lopt (HST) + bolometric correction (caveat RG) Main sample, iscomplete and not selected on nuclearproperties

  19. MBH FRII/HEG absorbed e = 1 m Marchesini, Celotti & Ferrarese 04 10-3 • FRII/LEG FRII/BLRG 2 - MBH and Accretion rate QSO FRI Indication for bimodal accretion rate distribution

  20. Discontinuous distribution in * On-off switching of the nuclear accretion? * Evolutionary sequence from FRII to FRI-like regime? m m • Continuos distribution, allpossible • * Unstable flow at intermediate rates: radiation pressure dominated accretion regime ? • * Gap due to inhibition of jet formation: spin energy via Blandford & Znajek – • efficient for rates >> 1 and << 1 (H~R)? • *Transition due to a change ine: e.g transition to radiatively- • inefficient, geom thick, optically thin flow? • * Decrease in the effective mass accretion: mass loss ? • m 2 - Why ? Speculations Complete 3CR subsample (at same z): two peaks ~ equally populated

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