Chaire Galaxies et Cosmologie. Feedback of black holes on star formation. Françoise Combes NGC 4258

Transcription

1 Chaire Galaxies et Cosmologie Feedback of black holes on star formation Françoise Combes NGC 4258

2 Symbiosis between Black Holes and Galaxies M ~0.5% M bulge M Up to which maximum mass? Max mass of bulges M M ~ M M Read & Trentham

3 Maximum mass of an AGN? The outer radius of the accretion disk, at the origin of theagn is a function almost independent of the mass R disk ~0.01pc ~ 2000 AU Horizon~ 20 (M /109 M ) AU The disk can no longer exist between the last stable orbit and R disk, for M > M King 2016 a : Spin du TN BH can be more massive but invisible 3

4 IR An AGN has enough energy to destroy the bulge SFR X-ray M BH = M gal E gal ~M gal 2 BHAR x3300 E BH ~0.1M BH c 2 E BH /E gal > 80 But this assumes an efficient radiation! Above the limiting mass M > M No influence any more on the galaxy 4

5 Necessity of AGN to stop star formation Formation of supernovae, Stellar winds Relativistic winds from AGN Radio jets Baugh 2006, Eke et al 2006, Jenkins et al

6 Outline 1- Two modes of feedback 2- Discovery of molecular flows 3- Conservation of Energy or Momentum? 4- Is AGN feedback efficient? 6

7 1- Two modes for the feedback The Quasar mode: radiation or relativistic winds When luminosity is close to Eddington, young QSO, high z L Edd = 4 GM BH m p c/ T M BH ~f T V4, f gas fraction Same consideration with radiation pressure on dust grains with d d / T ~1000, limitation it ti for Mbulge to 1000 M BH? The Radio mode, or kinetic, jets When L < 0.01 L Edd, low z, Massive galaxies, Radio ellipticals Non destructive: heating-cooling balance Radiatively inefficient i flow ADAF Cooling flows in galaxy clusters Low luminosity AGN, Seyferts.. CenA 7

8 Eddington limit in details When the luminosity of an object (star or AGN) is so intense that all the gas around begins to be ejected L Edd = maximum luminosity which can cross the gas in equilibrium, Above, the equilibrium is broken For a star, the limit is reached for 120 M, then the enveloppe is blown away this is the stellar wind Gravity force = GM /r2 ( A N H m) Radiation force= L/c A/4 r 2 (1-e ) In general <<1, 1-e ~ = N H F AN grav = F rad L Edd = 4 c GM m/ M M(cloud)= A N H m M If L Edd = 4 c GM mn H 8

9 Conditions of winds around the AGN F grav is computed with M alone: works very close to the black hole If the gas is ionized, Thomson cross section T for electron scattering If the gas is neutral, and there exist dust grains, the cross section will be dust = 1000 T, in compensation F grav of M bulge Coincidence? id M bulge ~1000 M Radiation pressure L Edd /c balances and ejects the gas M gas = fm gal at the outer parts of the galaxy M bulge ~2 V2 r /G (Virial) L Edd /c = GM bul M gas /r 2 = Gf/r 2 (2 V2 r /G) 2 = 4f V4 /G L Edd /c = 4 GM m/ M ~f T V 4 close to the relation M- this order of magnitude supports the idea of feedback 9

10 Quasar mode: relativistic winds 10

11 UFO: «Ultra-Fast Outflow» Lines Fe XXV/XXVI in absorption Gas highly ionized, relativistic Outflow of gas seen in X-rays V > km/s Jet UFO Tombesi et al Black hole Accretion disk 11

12 Destruction of gas clouds If the medium is very fragmented in small dense clouds, the surface A is insufficient to have an effect. On the contrary, even a weak wind can disintegrate the clouds, and thus increase their surface Instabilities Kelvin-Helmholtz N H decreases, A increases Hopkins & Elvis

13 Radiative mode in simulations SFR ~ n with n=1, 1.5, 2 Feedback of supernovae+ black hole growth and associated feedback Sub-grid physics Is the feedback efficient? Does not stop star formation! Springel et al. ( ), Hopkins et al Gabor & Bournaud 2014: 13

14 The different steps: starburst- quasar Cox et al

15 Respective role Supernovae - AGN Energy integrated over the whole active phase x10 59 erg The star formation concerns extended disk regions 5 times more feedback energy from the AGN 15

16 Cooling flows In galaxy clusters, density is so high in the center tcool << thubble The gas cools down, loses its support and falls to the center Gas cycle and black hole + radio jet Very little star formation! 16

17 ne ~0.1 cm-3, T = 10 8 K dm/dt ~ M /yr Star formation of only 1% Filaments of ionized gas (H ) Peak of cooling L(X) = erg/s much larger Than radio synchrotron radiation erg/s 17

18 Rayons X Perseus A, Fabian et al 2003 Gas flows in galaxy clusters Star formation (green) Ionized gas (pink) Canning et al 2014 Cavities and sound waves 18

19 Cold molecular gas in filaments Inflows and Outflows Co-exist The cooled gas infalls and feeds the AGN Salome et al

20 Cooling and buoyancy y 20

21 Cavities digged out by multi-scale jets The intra-cluster hot gas looks like a swiss cheese 21

22 Radio cavity Energy of the jet (cavity) versus radio energy Mach~1.2 Ene ergie PdV de la ca avité P cav ~1000 L radio pv cavity shocks 20kpc Nucleus Accretion, spin Birzan et al

23 The radio jet can compensate the cooling Comparison with X-ray luminosity Equilibrium Heating- cooling Luminosity X Hlavacek-Larrondo et al 23

24 Characteristic time-scales t-cool (10 9 yr) t-cool > tcav t-cool (10 8 yr) Age of Universe t c =10 8 yr t c =t cav Voigt & Fabian 2004 Rayon (kpc) Age de la cavité (10 8 yr) t-cool larger than age of cavities The feedback is intermittent, and the black hole can 24 be fueled by the cooled gas

25 Accretion of cold gas, hot gas, or spin? Transition mode Radio Quasar at 0.1 Eddington For weak luminosities, Bondi accretion of hot gas could be sufficient Cold gas Hot gas Russell et al 2013, McNamara et al

26 ALMA: cold gas in galaxy clusters H 2 mass M between km/s around Vsys + a cloud at high V at -570km/s (outflowing jet if in front of the nucleus? A1664 : CO(3-2) at V=systemic and high velocity cloud Russell et al

27 ALMA, cold gas in groups Molecular clouds in CO (blue & red shifted), on the Chandra image HST image Masses of fragments, or GMA, to 10 7 M, 10-50km/s No disk in rotation, but clouds also in absorption David et al

28 Large variety of simulations For galaxy clusters or massive elliptical galaxies Cooling rate ~ Bondi amplified, + cold gas accretion Radiation pressure insufficient Mechanical feedback with jets or winds Succeed to moderate the cooling + Distribution of hot gas Efficiency scaling with the objects (E-gal) (cluster) 28 Gaspari et al 2012

29 2- Molecular gas outflows J1148 Z=6.4 CII Mrk 231 AGN + nuclear starburst, M Outflow of 700M /yr Extended over ~kpc, Affects the whole galaxy Maiolino et al 2012 IRAM Ferruglio et al 2010 Blue wing Red wing CO Cicone et al 2012 dm/dt = 3v M F /R F ~1000 M /yr, (5xSFR) Kinetic power ~ erg/s AGN 29

30 dm/dt Correlations of outflows with AGN V dm/dt L AGN L AGN /c For the AGN, the outflow rate V dm/dt ~20 L AGN /c is proportionnal to L(AGN) May be explained by an energy conserving mechanism Cicone et al 2014 (Zubovas & King 2012) 30

31 Molecular outflows are massive Aalto et al 2012 N1377 More massive than the dense nuclear disk in e.g. NGC1377 Size 200pc with V= 140km/s M out = M, disk mass ~ M Outflows due to supernovae: less massive, lower velocities M82, Mout ~ M V~200km/s Merger NGC3256, Mout ~ 10 7 M, 10 Mo/yr, V~420km/s Arp220, + absorption 100pc, Mout ~ 10 8 M Outflows due to AGN: V> 1000km/s, up to 1200 M /yr Mrk M /yr, gas will be consumed in 10 7 yrs NGC1266 Mout ~ M, gas has disappeared in ~10 8 yrs 31

32 Ionized gas outflows more frequent Statistics on 200 galaxies 0.4 < z <1.4 (Martin C. et al 2012) 2% of the FeII absorption outflow at 200Km/s, 20% at 100km/s Depends on the star formation rate (FeII, MgII, Keck) Inflow or outflow Collimated t d Angle smaller at large V Blue: outflow Red: inflow Green: no flow Atomic gas (abs Na I D) Rupke et al

33 Molecular winds seen by Herschel Absorption lines blueshifted in 70% of objects Outflow with a large angle (145 ) Veilleux et al 2013 Only 10% of redshifted absorption: Accretion from filaments, plane geometry Vmax ~-1000km/s, Vmoy -200km/s, increases with L AGN 33

34 Molecular vs ionized outflows dm dt 6 QSO at z=2.4 Carniani et al 2015 Only one object in common AGN varies in amplitude L AGN Moment =VdM/dt Kinetic power of ionized gas <0.1% LAGN L AGN /c Molecular gas outflow 50x ionized gas outflow Different acceleration mechanisms 34

35 Offcentered nucleus and outflow in NGC1068 Black V=-50km/s White V=50km/s Outflow of 63M /yr 10x the star formation rate in this region Garcia-Burillo et al

36 Jet in the disk plane NGC 4258 Cecil et al

37 Positive AGN feedback: jet-induced star formation AGN radio source 4C12.50: young or rejuvenated The gas flow starts at 100 pc from the nucleus Or the jet interacts with the gas medium Morganti et al 2013, Dasyra & Combes

38 Radio jet action in IC5063 CO contours on dust emission Molecular l flow at V=600km/s Seyfert galaxy, weak in radio ALMA maps, Morganti et al

39 IC5063: multiple winds along the jet VLT SINFONI, NIR H 2, Iron lines Molecular flows in 4 points, where the jet is deviating Dasyra et al

40 Feedback in low luminosity AGN NGC 1433: barred spiral, CO(3-2) with ALMA The molecular gas feeds the AGN, + flow // minor axis M H2 = M in 1kpc Flow of 100km/s 7% of the mass= M The smallest flow detected L kin =0.5 dm/dt v 2 ~ erg/s L 43 bol (AGN)= erg/s Momentum of the flow > 10 L AGN /c Combes et al

41 ALMA observations of NGC 1377 Resolution 0.2 arcsec MH 2 in the cone 10 8 M In the jet 10 7 M 41 Aalto et al 2015

42 Precessing jet in NGC 1377? Projected density Velocity Dispersion Model of a simple precession The jet changes sign symmetrically North/South V= km/s The flow starts at r < 10pc Aalto et al

43 Jet precession in micro-quasars SS433 VLBA 15GHz 1mas= 3AU Mioduszewski et al Inner jet 5mas Advance of 7-10mas Per day 1E close to Galactic center Luque-Escamilla et al

44 Why molecules in the outflows? Zubovas & King 2014 Shock heated gas at K Dissociated molecules? V in V s Efficient cooling Multiphase, with instabilities Rayleigh-Taylor t-cool << 1Myr induces star formation This implies a luminosity comparable to L AGN 100M /yr! Difficult to distinguish outflows due to starburst or to the AGN 44

45 3- Energy conserving outflows? If the cooling is efficient momentum conserving flow (mv) For fast winds > km/s, very little radiative losses Energy conserving flow (Faucher-Giguère & Quataert t 2012) The molecular gas at Vs, receives a boost of momentum Conservation of in of the order of 1 Boost of v in /2 Vs ~50! Explains why the momentum >> L AGN /c 45

46 Slow cooling high momentum VdM/dt UFO Faucher-Giguère & Quataert 2012 c b v/c Tombesi 10, 14 a Costa, Sijacki, Haehnelt,

47 Momentum ratio 1Myr 3Myr Other possibilities 10Myr Outflows >1000 km/s with a high momentum p (10 L/c) Could be obtained considering Optical thickness effects in the infrared R(kpc) And mainly the variability of AGN It is possible that the AGN has disappeared, when we see the flow Relics of passed episodes of the AGN Ishibashi & Fabian (2015) 47

48 Impact of an ultra-fast outflow (UFO) Two phases 1- At beginning, M BH is below the M- relation the wind v=0.1c is stopped by a shock << 1kpc outflow momentum conserving, energy radiated away Not sufficient to stop the gas, the black hole grows 2- Then M BH reaches the M- relation, the flow extends over large radii > 1kpc, and becomes energy conserving The pressure is >> v 2, the medium is easily ejected, with Vesc (as the observed molecular outflows) Regulation of M bulge The disk is a too massive obstacle, the jet is deviated bipolar King & Pounds

49 UFO+ molecular outflow in Mrk231 Mrk 231 AGN + starburst Gas ejected Mo Flow of 700M /yr Feruglio et al

50 Several simulated modes Quasar mode, when dm BH /dt > 0.01 Edd Spherical symmetric energy Radio mode: V= 10 4 km/s, in a cylinder perp. tothedisk the Energy conserving, mechanism much more efficient AGN flow with > 10 L Edd/c Entrained cold gas > 10 9 M after the shock cooling by metals Costa et al 2014 Comparison between realistic cosmological simulations and idealised models in spherical symmetry y the AGN feedback is efficient only with outflows 10 times 50 higher

51 Quasar mode: multi-phase simulations Most of the kinetic energy of the flow is lost in voids Feedback: positive and negative The cold gas is pushed by the ram pressure More feedback on the diffuse gas Could explain the M- relation Nayakshin

52 4- AGN feedback: efficient or not? If AGN trigger star formation feedback of SN? Starburst in a ring The AGN winds are not sufficient to stop SF Positive feedback by gas compression Gaibler et al

53 Efficiency of feedback (models) The feedback both thermal and kinetic builds the M- relation Twice less baryons in stars Feedback mecanical +radiative is efficient to reduce star formation Choi et al

54 or inefficient (models) Feedback is negligible in simulations with ionisation +radiative transfer Roos et al

55 Negligible effect on star formation Ionisation and heating of the diffuse phase Dense clouds little affected Negligible impact on SF L AGN = erg/s Only r<40pc is concerned, and only diffuse gas Even with outflows of 3-10 x SFR Roos et al 2015, Vogelsberger et al 2013, 2014, Illustris Rosdahl et al 2013, RAMSES-RT 55

56 Sometimes AGN trigger star formation The AGN provides a pressure excess leading to more fragmentation of molecular gas Bieri et al

57 Radio mode: fractal structure 2pc-1kpc Efficient i relativistic i jets; Influence of porosity Wagner & Bicknell

58 Inefficient feedback (observations) L(FIR) SFR SFR Starbursts AGN Vblue Voffset L(AGN) SFR SFR 224 quasars z<1 no relation bt between SFR and V flow AGN feedback no obvious Either two different time-scales or positive feedback also 58

59 Conclusions Mechanisms: Quasar mode (relativistic wind), luminous AGN Or radio mode (jets), for low-luminosity AGN, low z Molecular l outflows very frequentlyobserved, around AGN, v= km/s M, outflow/star formation= 1-5 Energy conserving flow: boost of momentum p ~ 20 L AGN /c However, not efficient to stop star formation The radio mode is very efficient in galaxy clusters to moderate the cooling: mechanical energy of fjets, cold gas accretion 59