Cosmic co-evolution Black holes/galaxies Françoise Combes

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1 Chaire Galaxies et Cosmologie Cosmic co-evolution Black holes/galaxies Françoise Combes

2 Tight relation between masses Mass of the black hole M ~ 0.5 % Mass of the bulge M Gultekin et al 2009 It is not the total mass but only that of the spheroid «Classical» bulge, not the pseudo-bulge of barred spirals Does not depend on the dark matter V ou M bulbe 2

3 Bar in the plane of the sky Exception for barred spirals cacahuète boîte Bar along the line of sight Graham et al

4 Known black holes (~50) r infl = Radius of the black hole sphere of influence GM /r infl = <V 2 > * is the spatial resolution 4

5 Mbulge ~ 4 But attention, M Better correlation with? is calculated partially from! Kormendy & Ho

6 Exception for ongoing mergers The signatures of merger are tidal tails, shells, loops, and all perturbations in the morphologies: NGC4382, NGC2960, IC1481 a NGC 4382= M85 S0pec Sa LINER S? LINER 6

7 Smaller black holes for ongoing mergers May be we see only one black hole out of the two, and after merger, BH coalesce Mass x 2 Or, the merger occurs late, when all the gas has been consumed by star formation! Searches only at center? 7

8 M black hole Bulge mass (or ), at z~6 Early black holes? Ma ass of th he black hole QSO at z=6 The mass of the black hole is larger than expected But: Uncertain inclination Mass of bulge ALMA will yield morphology and inclination 8

9 Outsiders to the relation M -M bulge N1277 M bulge ~700 M Sometimes, objects a little above, in galaxy clusters Cannibal galaxies at the center The BH swallows the hot gas before star formation? 9

10 NGC 1277: an obese black hole? Gas dynamics M = M Scharwaechter et al

11 Too massive black holes? May be it is only ignorance on their bulge mass? Some measure a higher velocity dispersion 11

12 Ratio M -M bulge Bt Between 0.2 and 1%, according to mass 12

13 Cause or effect? Light distribution in ellipticals and bulges De Vaucouleurs (1948) in r 1/4 Sersic (1968) in r 1/n n=1 exponential disk, n=4 Elliptical But sometimes flat profiles in the center core Log (r) 13

14 Dichotomy: core vs. cusp NGC 4621 E5 Cuspy stellar distribution (power law, ~r ) NGC 720 Flat stellar light distribution, or core E5 14

15 Correlations of the fundamental plane distinguishing elliptical galaxies and spheroidals Surface Bright tness Ell E Sph S,Im globular clusters Kormendy (1985, 1987) Luminosity 15

16 Dichotomy: core vs. cusp M87, cd Gebhardt et al (1996) N4472, E2 The core is a true truncation (Kormendy 1999) 16

17 The cores are due to the merger of black holes? r b (pc) Slow rotation Boxy Log Faber et al (1997), Kormendy (1999), Nieto et al (1991) Kormendy (1987) Luminosité M32 Luminosité Dichotomy: core vs. cusp Galaxies with cores are boxy & slow rotators Galaxies without core have a disk & rotate fast 17

18 How does the black hole influences the bulge? Rdi Radius of fthe black khl hole sphere of fifl influence GM/ /r infl = <V 2 > r infl = GM /<V2 > Correlation observed M ~ M bulbe Bulge mass M 5<V bulbe ~5 2 >R bulbe /G r ~10-2 infl R bulbe Volume of influence = 10-6 Volume of the bulge Difficult to imagine gravitational exchange of information 18

19 How does the black hole influences the bulge? Energy delivered at the black hole growth ~0.1 L = dm acc /dt c2 dm /dt = (1- ) dm acc/dt Growth energy E c = M c2 Gravitational energy of bulge E bulge ~ M bulge <V 2 > E /M ) c /E bulge = M bulge) c 2 /<V 2 > ~ 400! The active nucleus radiates enough energy to destroy the bulge Even if a large part of this energy is lost to intergalactic space, this is enough to moderate the bulge growth 19

20 How to follow the evolution of black holes? 1- Study active nuclei (AGN) as a function of z: luminosity function, mass derived from the BLR 2- Comparison with the black hole mass function of today z=0, based on M -M bul and function of L bul 3- Background radiation accumulated, mainly in X-rays Radiation rate mc 2? L/L edd? role of mergers? Obscured or low efficiency phases? When do the black holes form? 20

21 dn/dm = (M ( ) Black hole mass function = M (M ) dm = M /Mpc 3 (M M ) Marconi et al 2004 Shankar

22 Argument of Soltan (1982) L = dm acc /dt c 2 dm /dt = (1- )dm acc /dt dm /dt = (1- )/ L/c2 accumulates in all nuclei Andrzej Soltan By integrating the luminosity function of AGN (L, z) One obtains = M /Mpc 3 with = 0.1 The same result should be obtained in integrating today the mass function of all sleeping black holes = M /Mpc 3, or larger The AGN are obscured, or radiate inefficiently Or the calculation is inexact 22

23 Cosmic background radiation CMB CIB COB Galaxies CXB Primordial Universe AGN G. Hasinger 23

24 X-ray spectrum of quasars X-rays allow us to detect obscured AGN But up to a column density of cm -2 Beyond, even X-rays cannot get out, sources are then called «Compton-thick» Gilli et al

25 Taking into account the «Compton-thick thick» Once the most obscured quasars are taken into account Assuming that ttheir luminosity function is the same as for the others (with only a factor of proportionality) Observations can be reproduced Gilli et al

26 Luminosity functions versus z dn = (L,z) ) dv dl AGN census at a given L, at a given z To correct for the Malmquist bias, due to object detection only above a limit flux F lim, one uses the maximum volume V max based on the distance D 2 max (z) = L /4 F lim V max < V, corr (L,z) = dn/(dvmax dl) > (L,z) = dn/(dv dl) Li, Ho, Wang

27 Luminosity function of AGN Function in double power law and Different from the galaxy function Schechter law Power law + exponential 27

28 Several models to reproduce the observations Not only a Pure Lum Evolution PLE Pure Density Evolution PDE Reference z=0 28

29 Evolution in density or luminosity? Density Luminosity Density, as a function of luminosity (LDDE) The slopes change 29

30 Distribution in Mag (or L) and redshift redshift Lum agnitude Luminosity The dependency in Luminosity and redshift are two indissociable aspects 3D Function 30

31 Downsizing The slopes must change Mêmes pentes Lum If the observations show that the AGN of higher masses and luminosities form earlier («downsizing»orantihierarchical anti-hierarchical formation), then this implies coupled evolutions between Luminosity and density The slopes and must change with z 31

32 Evolution of the slopes with z The luminosity function becomes flatter at high z This should be reproduced by models Hopkins et al

33 Distribution of luminosity of QSO with z The peak is at z=2.15 As is the star formation peak, Even more marked as a function of time! The most surprising is at z=6 Richards et al

34 Distribution N and L in X-rays Eid Evidence of «downsizing i»: the most massive black holes form first, more rapidly Lum Lum PLE Pure luminosity evolution LDDE Lum-dependent density evolution Hasinger et al

35 Models and Downsizing quasars, < z < 2.6 PLE..; LDDE LE +DE best fit z z Lum Croom et al

36 Anti-hierarchical growth of black holes 50% of the final mass The massive BH are formed in the deepest potential wells and grow the first The less massive BH form in shallow potentials they form afterwards They are sensitive to feedback and take a long time to grow Marconi et al

$gas fraction$

37 Model: quasars are activated during galaxy mergers Interaction between two spiral galaxies Drags the gas to the center Triggers starbursts After the starburst, activity of the nuclei,agn Color: gas fraction Episode Quasar Merger of BH (2Gyr) Hopkins et al

38 Temporal evolution of the activity Integrated life-time of the quasar, t Q, above the Luminosity L Reference: Lum constant ~L Edd Light-bulb ON ouroff quasar Hopkins et al

39 New interpretation of the luminosity function (and of its 2 slopes) Long gphases at low luminosity quasars at low or high luminosity are the same sources, viewed at different epochs of their life The cut is determined by the peak of dn (L pic )/dt Very different from a model at cst luminosity light-bulb On or OFF Hopkins et al

40 Several interpretations possible: duration of the activity and L duration of the activity and L max Luminosity function observed Activity rate of quasars of a givenl-peak Boyle et al 2000 Model ON/OFF at constant Lum Possible origin of the two slopes Limited by Eddington With Eddington Life time depending on Luminosity Observed luminosity Max luminosity of quasars 40

41 Quasars formed in mergers Obscured period, NH 2, starburst, t 100 Myr Feedback ejects gas & dust. Quasar visible during Myr NGC 6240, Keel

42 The most FIR luminous are the most obscured N H N H function of Luminosity L temps Hopkins et al

43 Even more possibilities Free parameters: efficiency, and Eddington ratio = L/L edd Grey curve: density of black holes at z=0 43 Shankar et al 2009

In the model where quasars are activated by mergers, L_peak is correlated with the halo mass, but not the instantaneous luminosity

44 Test of the clustering of quasars Two models reproduce (L): many quasars with short life-time or rare quasars of long lifetime? Distinction by their clustering rate with the dark matter distribution! In the model where quasars are activated by mergers, L_peak is correlated with the halo mass, but not the instantaneous luminosity Detailed study of simulated light curves, of the degree of correlation with the halo mass Depends very little on the luminosity, compatible with the préedictions of the model Lidz et al

45 Comparison with galaxies Quasars cluster less than elliptical galaxies (red) but more than spiral galaxies (blue) They constitute an intermediate population p At z~2.5, similar to starbursts Amp pmitude de corrél lation redshift 45 Hopkins et al. 2007

46 Descendents of quasars The amplitude at z=0 and z are linked by cosmology M Mbulge l The amplitude corresponds to that of ellipticals, but not to spirals corrélation Ampl litude de Luminosity Quasars live in halos M~ 4x10 12 Mo, whatever z and L 46 Hopkins et al. 2007

without metals M * ~10 3 M, explode in supernovae M ~102

in the center Collapse in a supermassive star, which

47 How can massive black holes form early? Remnant of super-stars Pop III Super-massive stars, sine without metals M * ~10 3 M, explode in supernovae M ~102 M Direct collapse Gas clouds, massive and dense, pile up in the center Collapse in a supermassive star, which never stops growing, until the collapse into a black hole M * >10 6 M M >104 M 47

48 Formation of quasars at z=6 M (z=6) Peaked gas distribution Continuous growth at L Edd Or a flat distribution, more difficult TIS =Truncated Isothermal sphere z(form) Tanaka & Haiman

49 Sketch from Martin Rees Rees, Physica Scripta,

50 Updated 32 yrs later Avoid the sling-shot effect d Ejection of the 3 rd black hole Begelman & Rees, Gravity s Fatal Attraction 2 nd Edition,

51 Sling-shot effect: ejection of a 3 rd BH One of the BH (type 1) has a velocity~ 1200km/s with respect to the host galaxy Type 2: absorption and emission i of ionized i gas, variability Or 3 BH one ejected, or the merger remnant of a binary BH can recoil (after the emission of gravitationnal waves) Civano et al 2010 CID42: HST Blue=X-rays 51

52 Formation of the first seeds Metallicity=0 We must suppress H 2 with the UV of nearby galaxies? (but without metals??) Also evacuate L with gravity torques in a disk Volonteri

53 Formation of Pop III stars Abel et al

54 Formation of a QUASISTAR Similar to a red giant A convective enveloppe, supported by pressure Photospheric temperature decreases with the BH growth Central Temp.~10 6 K Radius~ 100 AU T phot decreases Direct collapse when BH M = 104 M radius grows 54

Death of a QUASISTAR : explosion in supernova Critical

enveloppe (details very uncertain) Final mass of the

55 Death of a QUASISTAR : explosion in supernova Critical ratio: R M =(enveloppe mass)/(bh mass) R M < 10: opacity crisis (Hayashi path) R M < 100: powerful winds, difficult to make compatible accretion and enveloppe (details very uncertain) Final mass of the black hole: M BH 7 2 M ~ 10 RM -1 1M Sol yr 4 ~ 10 M 10 Sol 6 M Sol 55

56 Core collapse of a globular cluster Two-body relaxation Log de ensité Log r The energy transfer from the center to the outskirt produces the core collapse, in 10 t relax At the center, stellar collisions produce a run away, and the formation of a black khole 56

57 In summary: 2/ 3 possible ways Regan & Haehnelt

58 Masses formed in the various processes Star clusters Devecci & Volonteri 2008 Direct collapse Pop III remnants 58

59 Conclusions Relation M - Mbulge -- Tighter with -- exceptions: mergers, pseudo-bulges, bl bars, -- origin of this relation? -- History of the formation, or feedback? -- Argument from Soltan, make the census of the whole activity? Obscured activity (Compton-thick) Or accretion with inefficient radiation? (ADAF, RIAF..) Models of galaxy mergers: starburst obscured quasar Then quasar visible with a narrow range of max Luminosity How are formed the super-massive BH? -- Very early, very rapidly, z=6 T < 1 Gyr -- Direct gas collapse, or quasi-star, or stellar cluster 59

FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera

FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera In this presentation the different theories that can explain the formation of Supermassive Black Holes (SMBH) are presented. Before focus on