FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera

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1 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 these theories, an introduction to Black Hole (BH) and SMBH properties is given, along with a brief explanation of the different techniques used to find SMBH. Also a description of what we know about SMBH is in here. In this part are of remarkably importance the facts that: High Z and Low Z quasar have similar properties: Then they should have a common origin. Mass of SMBH proportional to the mass of the bulge: Exceptions M33 and NGC205. rest of their life at Eddington rate. B. Mergers: Again the process is thought to star with a Population III star as a seed in the earlier Universe which collapse and form a BH. This BH will grow by mergers with others BH and Intermediate BH (IBH). The total number of mergers depends on the mass of Seeds and the mass of Dark Matter Halos. In a normal case a total of dark matter halos are needed to form a SMBH. This big number tells us that the theory is not valid alone. The formation of SMBH is a not clear process. It has not been explained yet what was first: Stars or BH s,, the Galaxy or the central SMBH. Here the three most plausible explanation of formation of SMBH are given: Population III stars: Accretion, Mergers or Accretion + Mergers Collapse of Gas Clouds Collapse of Stellar Clusters 1. Population III stars: A. Accretion: The process is thought to start with a Population III star as a seed in the earlier Universe. These stars collapse at the end of their r lives to form BH s.. These BH s emitting at Eddington luminosity and accreting gas at Eddington limit with a efficiency of 10% would last about 7x108 yrs. to become a SMBH of mass 3x109 M. M. SMBH at high Z cannot be explained by this theory. A plausible explanation for these SMBH s at high Z is that some period of time they accrete at Super-Eddington rate and the C. Accretion + Mergers: The most plausible theory is the combination of Accretion and Mergers. In this case some authors claim that the proportions would be: 10% Mergers + 90% Accretion 2. Collapse of Gas Clouds: This theory is based in that a gas cloud can collapse to form a SMBH via a supermassive star or via a disk. This theory is only valid if fragmentation of the gas cloud into stars can be avoided. Conditions necessary to avoid star formation in the gas clouds are given, along with a possible outcome for the formation of the SMBH. 3. Collapse of Stellar Clusters: This theory is based in the possibility of that a stellar cluster collapse to form a SMBH. Conditions necessary for the collapse are a given, so as other possible variation of this theory.

2 FORMATION OF SUPERMASSIVE BLACK HOLES NESTOR M. LASSO CABRERA AST 7939 High Energy Astrophysics Jonathan Tan

3 Outline What is a Black Hole? What is a SMBH? How to find SMBH What do we know about SMBH? Formation of SMBH Population III Stars: Accretion and Mergers Collapse of Gas Clouds Collapse of Stellar Clusters

4 What is a Black Hole? Stars with M > 5-6 M Ceases to sustain a nuclear fusion reaction Collapses under its own gravitational field Supernova Black Hole Nothing escapes its gravitational field Well known: Formation Localization Mass

5 What is a SMBH? SuperMassive Black Hole Mass ~ M Nothing escapes its gravitational field NOT well known: Quasars Mass Localization: Center of galaxies?? Formation?????????

6 How to find a SMBH? X-Ray Emission Radial Velocity Rotational Velocity Gravitational lensing M NO STAR Centaurus A Radio Light ~1350 Km s Mpc Visible Light

7 What do we know about SMBH? Present in nearly all active and non-active luminous galaxies Quasar population High z and Low z quasar similar properties indistinguishable Mass proportional to the mass of bulge M ~ 0.2% M galaxy (Miyaji et al. 2000)

8 What do we know about SMBH? Mass proportional to the mass of bulge EXCEPTIONS: M33 and NGC 205 (Ferrarese et al. 2006)

9 Formation of SMBH Not clear: First nonlinear objects: Stars or BH? Galaxies or Central BH? THEORIES: Population III stars: Accretion Mergers Accretion + Mergers Collapse of Gas Clouds Collapse of Stellar Clusters

10 1 - Population III stars: Accretion Seed: Early massive star - Population III stars Free metal ~100 M (Abel et al and Bromm et al. 2002) BH (Heger et al and Carr et al. 1984) Gas Accretion: Eddington limit = 10 L Edd / c 2 Eddington Luminosity. M Edd Radiative Efficiency of 10% η = 0.1 L Edd = (4πm p cgm)/σ Th M SMBH = 3x10 9 M t SMBH ~ 7x10 8 yr. (Haiman et al. 2001) t ΛCMD Uni (z=6) ~ 8x10 8 yr. SEEDS at z 15 SMBH at high z NO PAUSIBLE

11 1 - Population III stars: Accretion Eddington rate: M BH = 10 8 M. M Edd Radiative Efficiency of 10% η = 0.1 = 10 L Edd / c M yr -1 Super-Eddington rate: SMBH at high z PLAUSIBLES Thick disk (Radiative inefficient flow RIAF) Eddington luminosity Energy not radiate away. M >>. M Edd (Begelman et al. 1982)

12 1 - Population III stars: Accretion Super-Eddington rate + Eddington rate (Cavaliere et al. 2000).. If M >> M Edd Outflows of mass Little mass reach the BH (Stone et al. 1999) SMBH at high z NO PAUSIBLE.. M ~ M (Begelman 2002) Edd SMBH at high z PAUSIBLE

13 1 - Population III stars: Mergers Seed: Early massive star - Population III stars Free metal z ~ 20 In dark matter halos of 10 6 M (min. to form stars) ~100 M (Abel et al and Bromm et al. 2002) BH (Heger et al and Carr et al. 1984) Mergers: Total Mergers depend on: mass of Seeds and mass of Dark Matter Halos Mergers of ~ 10 4 IMBH (10 5 M ) Dark Matter Halos NO VALID ALONE

14 1 - Population III stars: Mergers NGC 6240 First evidence of SMBH Mergers 3000 light years apart

15 1 - Population III stars: Accretion + Mergers 10% Mergers (Combes 2005) 90% Accretion

16 2 Collapse of Gas Clouds Could form SMBH s directly at high z via: Supermassive Star (SMS) Disk Only if fragmentation of the gas cloud into stars can be avoided Contracting gas becomes: Optically thick Radiation pressure supported Less susceptible to Star Formation (Loeb et al. 1994) If self-gravitating Prone to Star Formation (Goodman 2003)

17 2 Collapse of Gas Clouds How to stabilize the cloud and avoid Star Formation? Keep disk at high temperature: Only in metal free, high z halos H 2 dissociated by UV light No cooling No molecules No star formation Gas collapses at ~ 8000K ~ 10 6 M SMBH (Oh et al. 2003) Angular momentum (even with cooling particles): From gravitational instabilities, spiral waves, bars, Drive a fraction of the gas to smaller scales in nucleus

18 2 Collapse of Gas Clouds A possible outcome for the formation of the SMBH: Gas flows in Disk becomes optically thick Radiation pressure dominates for sufficiently massive objects Radiation pressure may temporarily balance gravity Forming a SMS SMS radiates at Eddington limit and continue contracting When SMS sufficiently compact, star becomes dynamically unstable For M 10 5 M Start stops collapsing and explode For M > 10 5 M Start collapses directly to a SMBH (Shapiro 2004)

19 3 Collapse of Stellar Clusters Negative heat capacity of self-gravitating stellar systems makes them vulnerable to gravitational collapse (Binney & Tremaine 1987) If core collapse continues SMS SMBH Depends on number of stars in cluster N stars (Lee 1987) A different theory: (Begelman et al. 1978) Massive stars dominate the dynamics of the cluster Massive stars collapse faster than cluster as a whole IMBH IMBH + Accretion + Mergers

20 References: Haiman, Z arxiv:astro-ph/ v1 Greenwood, C.J. Supermassive Black Holes at the Center of Galaxies Kormendy et al arxiv:astro-ph/ v1 Miyaji, T., Hasinger, G., & Schmidt, M. 2000, A&A, 353, 25 Begelman, M. C., & Meier, D. L. 1982, ApJ, 253, 87 Combes, F arxiv:astro-ph/

21 THE LOW MASS END OF THE SUPERMASSIVE BLACK HOLE POPULATION M33 Nestor M. Lasso Cabrera This presentation is base in the low mass end of the SMBH population. In particular it is based on M33 and its particular nuclei. After see in the former presentation the particularities of the nuclei of M33 compare with other luminous galaxies, here is presented a study of M33 compare with M32, a galaxy with bulge, and with NGC4395, a similar galaxy with bulge. Curves of Surface brightness profile, radial velocity and velocity dispersion of M33 are compared with that of M32, a typical galaxy with bulge. This curves place the upper limit of M33 in 3000M for Merrit et al.,2001 and in 1500 M for Gebhardt et al., Also the relation mass BH vs. velocity dispersion is shown for different galaxy and both upper limits of M33 are place in the plot, p showing that M33 does not follow the relation. Finally M33 is compare with NGC A galaxy pretty similar to M33 but that shows a BH of about x 105M.

22 THE LOW MASS END OF THE SUPERMASSIVE BLACK HOLE POPULATION M33 NESTOR M. LASSO CABRERA AST 7939 High Energy Astrophysics Jonathan Tan

23 FORMATION OF SUPERMASSIVE BLACK HOLES What is a SMBH? How to find SMBH X-Ray Emission Radial Velocity Rotational Velocity Gravitational Lensing What do we know about SMBH? Present in almost all luminous galaxies Quasar Population High and Low z quasar with similar properties Mass proportional to the mass of bulge M ~ 0.2% M galaxy

24 FORMATION OF SUPERMASSIVE BLACK HOLES Formation of SMBH Population III Stars: Accretion and Mergers Collapse of Gas Clouds Collapse of Stellar Clusters Mass proportional to the mass of bulge EXCEPTIONS: M33 and NGC 205

25 Brightest Galaxies => SMBH Intermediate and Lowest Galaxies => Stellar Nucleus 50%-70% late-type galaxies contain Stellar Nucleus (Balcells et al. 2003) Stellar Nuclei ~20 times brighter than typical globular cluster (Ferrarese et al. 2006)

26 M33

27 Surface brightness profile M32 Gebhardt et al., 2001 Michard & Nieto, 1991

28 M33 M33 M32 Merrit et al.,2001 Gebhardt et al., 2001 Bender, Kormendy & Dehnen km/s σ 35km/s σ ~ 24km/s M 7x10 4 M סּ Upper limit: M 3000 M סּ M 5x10 4 M סּ M 1500 M סּ

29 Gebhardt Merrit et al.,2001 M =1.3x10 8 M סּ (σ/200) 3.65 Gebhardt et al., 2001 M =1.3x10 8 M סּ (σ/200) 4.8 Ferrarese & Merrit 2000

30 σ < 35Km/s ~ Glob. cluster σ => No evidence BH (Merrit et al., 2001) σ ~ 24Km/s ~ Glob. cluster σ => No evidence BH (Gebhardt et al., 2001) Upper limit on the Mass ~3000M Merrit et al.,2001 Upper limit on the Mass ~1500M Gebhardt et al.,2001 Stellar central ρ ~ 10 6 M /pc 3 ~ BH ρ >> Globular cluster ρ Stellar Nuclei ~20 times brighter than typical globular cluster NO BH or Globular cluster in Bulgeless galaxies => WHAT????

31 Barth et al. 2005

32 Filippenko & Ho, 2003 σ 30km/s THERE IS A BH!!! M ~ 3-4x10 5 M סּ Reverberation Mapping

33 Conclusions Some Bulgeless galaxies have BH Other Bulgeless galaxies: NO BH or Globular cluster => WHAT???? Luminous Galaxies with Bulge (L, σ ): SMBH M - σ relation for luminous galaxies with bulges M - σ relation for bulgeless galaxies????

34 References: Ferrarese et al. 2006, ApJ 644,L21 Merritt et al. 2001, arxiv:astro-ph/ v2 Gebhardt et al. 2001, ApJ 122:2469 Greene and Ho 2007, arxiv:astro-ph/ v1 Barth et al. 2005, ApJ 619:L151

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