Prof Chris Done University of Durham amp ISASJAXA AGN feedback MagorrianGebhardt relation gives BH mass Big black holes live in host galaxies with big bulges Either measured by bulge luminosity or bulge mass stellar velocity dispersion or ID: 1045022
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1. The nature of the accretion flow in AGN Prof Chris DoneUniversity of Durham & ISAS/JAXA
2. AGN feedbackMagorrian-Gebhardt relation gives BH mass!! Big black holes live in host galaxies with big bulges! Either measured by bulge luminosity or bulge mass (stellar velocity dispersion) or BLR105-10M Black hole mass Stellar system mass1031091061012
3. AGN black holes grow by accretionGas supply to nucleusGalaxy disc instabilitiesMajor mergersMinor mergersCooling flow of hot gas from haloRegulated by feedback SupernovaeKinetic energy from jetMomentum from wind and/or radiationNeed to understand accretion to understand feedback Di Matteo et al 2005
4. Large scale radio jetsTransport AGN power to halo scales, keeping gas hot and preventing runaway star formation at late timesjet power determined by black hole mass, mass accretion rate and spinRadio mode (jet) feedback
5. Large scale radio jetsTransport AGN power to halo scales, keeping gas hot and preventing runaway star formation at late timesjet power determined by black hole mass, mass accretion rate and spinRadio mode (jet) feedback
6. Wider angle than jetDissipate energy in bulge? Perhaps this sets the M-s relation (King 2008)Wind power determined by black hole mass, mass accretion rate and spinQuasar mode (winds) feedback
7. Dramatic changes in continuum – single object, different daysUnderlying pattern in all systemsHigh L/LEdd: soft spectrum, peaks at kTmax often disc-like, plus tailLower L/LEdd: hard spectrum, peaks at high energies, not like a disc (McClintock & Remillard 2006)Gierlinski & Done 2003BHB: mass accretion rate L/LEddvery high
8. Scale up to AGN Bigger mass! Timescales MUCH longer. Disc temp lower – peaks in UVATOMIC PHYSICSLarger RANGE in mass –from 105-1010M And maybe bigger range in spin??Scaling black hole accretion flow
9. AGN/QSO Zoo!!! Multitude of different optical line ratios
10. And InclinationAGN: complex environment From now on take only UNOBSCURED AGN
11. Dramatic changes in continuum – single object, different daysUnderlying pattern in all systemsHigh L/LEdd: soft spectrum, peaks at kTmax often disc-like, plus tailLower L/LEdd: hard spectrum, peaks at high energies, not like a disc (McClintock & Remillard 2006)Gierlinski & Done 2003Spectral states - BHBvery high
12. ‘Spectral states in AGN’1001010.10.01Disc BELOW X-ray bandpass. Only see tail.
13. Unobscured AGN: LINERS-S1-NLS1Increasing L/LEddSimilar mass. Different L/LEdd Different ionisationdiscHot inner flow, no disc – true Seyfert 2sLINERS1/QSONLS1Boroson 2002
14. Unobscured AGN: LINERS-S1-NLS1Increasing L/LEddSimilar mass. Different L/LEdd Different ionisationdiscHot inner flow, no disc – true Seyfert 2sLINERS1/QSONLS1Boroson 2002
15. Medhipour et al 2011Classic QSO – most common shape Mkn 509 - 108M L/LEdd~0.1 (take out warm abs!)Not disc dominated - far too low temperature! Plus strange soft X-ray excess….What is this????
16. Unobscured AGN: LINERS-S1-NLS1Increasing L/LEddSimilar mass. Different L/LEdd Different ionisationdiscHot inner flow, no disc – true Seyfert 2sLINERS1/QSONLS1Boroson 2002ATOMIC PHYSICS
17. Unobscured AGN: LINERS-S1-NLS1Increasing L/LEddSimilar mass. Different L/LEdd Different ionisationdiscHot inner flow, no disc – true Seyfert 2sLINERS1/QSONLS1Boroson 2002
18. Unobscured AGN: LINERS-S1-NLS1Similar mass. Different L/LEdd Different ionising SEDBoroson 2002discHot inner flow, no disc – true Seyfert 2sLINERS1/QSONLS1Ljet
19. AGN spectral states: LINERSNemmen et al 2014 Look like hot flow – truncated disc + G~1.5 jet No strong UV bump from disc (Elvis et al QSO SED) Radio from G~1.5 jetLower UV
20. AGN/QSO Zoo!!! Radio loudEnormous, powerful, relativistic jets on Mpc scalesFRI (fuzzy) - BL lacs FRII (hot spots) – FSRQUrry & Padovani 1992; 1995
21. FRI is top of ADAF branch (low/hard state BHB) but G=15!BHBL/LEddGhisellini et al 2010
22. BHBGhisellini et al 2010FRI is top of ADAF branch (low/hard state BHB) but G=15!
23. Spin-jet paradijmGhisellini et al 2010Uncontroversial – very high spin to get G=10-15?Mdot<0.01Radio large scale structure – depends on environment Fermi GeV flux does not! From base of jet
24. Black hole mass & mdotCosmological simulations gives number densities (M, mdot)……With cosmic time (Fanidakis et al 2011) Colours are luminosity density ASSUME all RIAF (mdot<0.01) produce BL Lac jet Log MLog mdot
25. Black hole mass & mdotLog MLog mdotCosmological simulations gives number densities (M, mdot)……With cosmic time (Fanidakis et al 2011) Colours are luminosity density ASSUME all RIAF (mdot<0.01) produce BL Lac jet
26. Black hole mass & mdotLog MLog mdotCosmological simulations gives number densities (M, mdot)……With cosmic time (Fanidakis et al 2011) Colours are luminosity density ASSUME all RIAF (mdot<0.01) produce BL Lac jet
27. Black hole mass & mdot L/LEdd Gardner & Done 2014aSync-self-Compton (SSC)Inject e-, coolAverage jet parameters (Ghisellini et al 2010) G=15Scale jet kinetic power to M and mdot - LBL to HBL (Heinz & Merloni 2004)
28. 1000x more Fermi BL Lacs!!Paste scaled jet onto all mdot<0.01 AGNRandom directionPredicted Fermi numbers of BL Lacs Gardner & Done 2014a
29. 1000x more Fermi BL Lacs!!WRONG!! Gardner & Done 2014aObserved!!
30. Spin-jet paradijm BL LacsGhisellini et al 2010Scaling breaks for jets! G=1.5 not 15 in BHB and most AGNSo high G jets RARENeed to pick preferentially high mass?
31. Chaotic accretionFanidakis et al 2011Gas has random angular momentum directionLow BH spin BH – BH mergers spin UP the most massive BH to 0.76<logM<77<logM<88<logM<99<logM<10
32. Prolonged accretionFanidakis et al 2011Gas all has same angular momentum directionSpin BH up to a ~ 1BH – BH mergers spin DOWN the most massive BH to 0.76<logM<77<logM<88<logM<99<logM<10
33. Spin-jet paradijm BL LacsGhisellini et al 2010Scaling breaks! G=1.5 not 15 in BHB So high G jets RARENeed to pick preferentially major mergersHigh spin rare, a>0.8 for G=15 jetBut iron line – high spin in low mass, radio quiet AGN
34. But most AGN are high spin?From Fe line fits… Majority of high spin in high L/Ledd (NLS1)Reynolds et al 2013
35. Spin-jet paradijm BL LacsGhisellini et al 2010Scaling breaks! G=1.5 not 15 in BHB So high G jets RARENeed to pick preferentially major mergersHigh spin rare, a>0.8 for G=15 jetBut iron line – high spin in low mass, radio quiet AGNHigh spin common, accretion of B flux from halo is rare (Sikora & Begelman (2013)
36. NLS1 don’t look like this!! Jin et al 2012Same L but lower M, higher L/LEdd (107, L~LEdd )
37. Jin et al 2012‘simple’ NLS1‘simple’ NLS1 not ‘complex’ NLS1! (Gallo 2006)Dominated by disc, not soft x-ray excess
38. NLS1 – disc in soft X-rays2-10 keV spectrum has enormous soft X-ray excess ??Low M and high L/LEdd so highest AGN disk temperature Done, Davis, Jin, Blaes Ward 2011
39. Disc spectra 2x106 M L/LEdd ~1Done, Davis, Jin, Blaes Ward 2011Low M and high L/LEdd so highest AGN disk temperature REJ1034 2x106, L~LEdd – scale up by factor 2!No! mostly the disc!
40. BHB Disc spectra:10 M L/LEdd ~1Kolehmainen et al 2013 LMC X-3Peak at 3.5 keV for ~0.8LEdd3.5 x (10/107)1/4~0.1keV for 107 AGN (Ross, Fabian & Mineshige 1991)
41. Disc spectra 2x106 M L/LEdd ~1Done, Davis, Jin, Blaes Ward 2011Enormous soft excess in REJ1034?No – mostly disc! Plus a little soft X-ray excessAGN – changing mass as well as L/LEdd
42. Jin et al 2012‘simple’ NLS1‘simple’ NLS1 not ‘complex’ NLS1! (Gallo 2006)
43. Complex vs simpleFe 7-20 Fe 2-3Maximal spin maximal spinHeight small height largeri~60 i~30
44. Similar line Hb widths and LoptSimilar mass and mass accretion rate (and iron abundance)
45. Do we have a clean view?1H07072e6M a=0, 0.9, 0.998L/Ledd = 20, 63 150 (30 degrees)L/Ledd = 44, 123 270(60 degrees)Done & Jin 2015Clean disc??
46. Spectra of accretion flow: discLog nLog n f(n) Thermal emission: L = AsT4Last stable orbit sets maximum temperature – X-ray
47. Spectra of accretion flow: discLog nLog n f(n) Thermal emission: L = AsT4Last stable orbit sets maximum temperature – X-rayDepends on spin!
48. Do we have a clean view - Winds1H07072e6M a=0, 0.9, 0.998L/Ledd = 20, 63 150 (30 degrees)L/Ledd = 44, 123 270 (60 degrees)Done & Jin 2016Clean disc??
49. Simple NLS1Complex NLS1
50. SimpleComplex
51. SimpleComplex
52. SimpleComplex
53. SimpleComplex
54. SimpleComplex
55. Wind models for Ka line!Monte-Carlo bipolar (smooth) wind – Hagino et al 2015a, b
56. Wind models for Ka line!PDS456 Hagino et al 2015a1H0707 Hagino et al 2015b
57. PDS456 Wind opening angle O/2p=0.15 i=48-56 Hagino et al 2015aUse zxipcf to make low E spectral variabilityWind models for Ka line in 1H0707
58. Wind models for Ka line in 1H0707Use same model for 1H0707 Hagino et al 2015bNeed i=60-75Extrapolates to NuSTAR
59. Wind models for Ka line in 1H0707Hagino et al 2015b
60. ConclusionsZoo of AGN must be based on mass, mass accretion rate, spin and inclinationScale from BHB to AGN – disc peaks UV so atomic physics much more important! Breaks scaling for normal quasars.Low L/Ledd scale as still plasma physics from hot inner flowLINERS – look like hot flow BUT FRI/BL Lacs are low L/Ledd flow with highly relativistic jetHigh spin = highly relativisitc jet ? But iron lines spins in NLS1 say all AGN have high spin…..BUT NLS1 look quite like disc dominated BHB. Extreme NLS1 have L/Ledd>>1. Winds?? So can get from simple to complex via inclination??