Coevolution of massive black holes and galaxies

This lecture is part of the course "physics of active galactic nuclei" offered to graduate students in astrophysics by Rodrigo Nemmen and Joao Steiner at IAG USP.

https://rodrigonemmen.com/teaching/active-galactic-nuclei/

Transcript

1. Rodrigo Nemmen Massive Black Holes as Cosmic Bullies AGA5727 - Active Galactic Nuclei Credit: Randall, …, Bulbul et al. 2015 ApJ
2. Cosmic radiation background Frequency [Hz] Flux density [nW/m2 sr] microwaves IR optical X-rays γ-rays big bang stars/AGN AGN G. Ghisellini log (radiation flux) log (frequency / Hz)
3. Cosmic radiation background Frequency [Hz] Flux density [nW/m2 sr] nuclear fusion / accretion X-rays big bang stars/AGN AGN black hole accretion ?? log (radiation flux) log (frequency / Hz)
4. Evidence for coevolution between massive black holes and galaxies AA52CH13-Heckman ARI 4 August 2014 10:48 1010 109 108 107 106 60 80 100 200 300 400 Elliptical/classical bulge Pseudobulge AGN Quiescent M BH /M Velocity dispersion/km s–1 log 10 (M BH /M ) a Figure 9 ualreviews.org sonal use only.
5. log dρ./dt (M year–1 Mpc–3) z t (Gyr) 2.0 × 10–4 0.3 12 10 8 6 4 2 0.5 1.0 2.0 5.0 1.5 × 10–4 1.0 × 10–4 5.0 × 10–5 Black hole growth dρ STAR /dt*8.0e–4 (Fardal et al. 2007) dρ STAR /dt*8.0e–4 (Hopkins & Beacom 2006) Cosmic history: growth of massive black holes and stars Shankar et al. 2009 ⟨black hole accretion rate⟩ star-formation rate
6. M-σ relation: Black hole mass related to large scale properties of galaxies MBH = 2 ⇥ 108M ✓ 200 km s 1 ◆5.6 Woo+13; McConnell & Ma 13; Heckman & Best ARA&A 14 1010 109 108 107 106 60 80 100 200 300 400 Elliptical/classical bulge Pseudobulge AGN Quiescent 9.0 6 7 8 9 10 M BH /M Velocity dispersion/km s–1 log 10 (M BH /M ) M a b Figure 9 nnualreviews.org ersonal use only.
7. MBH = 2 ⇥ 108M ✓ 200 km s 1 ◆5.6 Woo+13; McConnell & Ma 13; Heckman & Best ARA&A 14 1010 109 108 107 106 60 80 100 200 300 400 Elliptical/classical bulge Pseudobulge AGN Quiescent 9.0 6 7 8 9 10 M BH /M Velocity dispersion/km s–1 log 10 (M BH /M ) M a b Figure 9 nnualreviews.org ersonal use only. central black hole host galaxy property: grav. potential of spheroid M-σ relation: Black hole mass related to large scale properties of galaxies
8. M-σ : Fundamental link between assembly of black holes and galaxy formation or coincidence? MBH = 2 ⇥ 108M ✓ 200 km s 1 ◆5.6 Woo+13; McConnell & Ma 13; Heckman & Best ARA&A 14 1010 109 108 107 106 60 80 100 200 300 400 Elliptical/classical bulge Pseudobulge AGN Quiescent 9.0 6 7 8 9 10 M BH /M Velocity dispersion/km s–1 log 10 (M BH /M ) M a b Figure 9 nnualreviews.org ersonal use only. central black hole host galaxy property: grav. potential of spheroid
11. Motivation for some kind of “AGN feedback” process in galaxies
12. Slide: Simon White 1)
13. Slide: Simon White 1)
14. 2) The cooling flow riddle
15. T ~ 106 - 107 K bremsstrahlung radiation Dbrem / ⇢2 2) The cooling flow riddle
16. Dbrem / ⇢2 2) The cooling flow riddle
17. http://chandra.harvard.edu/photo/2003/perseus/animations.html
18. Consequences of cooling flows in galaxy clusters High accretion rates ~1000 M‒ yr-1 Large reservoir of cold gas: T < 1 keV Lots of star formation
19. Consequences of cooling flows in galaxy clusters High accretion rates ~1000 M‒ yr-1 Large reservoir of cold gas: T < 1 keV Lots of star formation ~30 M‒ yr-1 And what Chandra and XMM-Newton saw Little star formation, <10 M‒ yr-1 Much less cold gas than expected Something is heating up the gas in galaxy clusters
20. How can massive black holes affect galaxies? i.e. how cosmic bullies work
21. How can massive black holes affect galaxies? i.e. how cosmic bullies work
22. Hydra A McNamara et al. X-rays (Chandra) Optical
23. 1’ = 22 kpc X-rays (Chandra) Fabian et al. Perseus cluster a b c Optical
25. MS0735 McNamara+05 Nature, McNamara+ 09 1’ = 210 kpc
26. (a)]: A 3D rendering of our MAD a = 0.99 model at t = ). Dynamically-important magnetic fields are twisted in the image) at the center of an accre ly dominates the jet structure ets with cyan-blu xima Jet simulation: Tchekhovskoy
27. Jet power OUT jet bubble age / P E t = Credit: Chandra Chandra observations of nearby radio-loud elliptical galaxies provide jet powers and BH accretion rates BH bub ( / ) s R c bub (4 ) PV X-ray cavities McNamara+05, Nature How to estimate the power required to heat up/ create the cavities in clusters Fabian 12 ARA&A Heating rate
28. ADAF & kpc ⇠ few pc ~10 R s ~100 AU ~10 -3 pc M ckinney+ Black hole jets affect the growth/ formation of galaxies, groups and clusters “AGN feedback” “Radio mode” AGN feedback
29. Simulation of AGN feedback via jets (“radio mode”) in a cluster atmosphere Omma et al. 2004
30. Brüggen et al. 2005 0.4 Mpc Simulation of AGN feedback via jets (“radio mode”) in a cluster atmosphere
31. Observational considerations • Feedback on cluster scales is more easily observable (larger physical scales, denser atmospheres, brighter diffuse emission from the hot gas in the X-rays) • Feedback on galactic scale is hard to resolve and a smoking gun is still needed Slide courtesy of M. Volonteri
32. Observational considerations • Feedback on cluster scales is more easily observable (larger physical scales, denser atmospheres, brighter diffuse emission from the hot gas in the X-rays) • Feedback on galactic scale is hard to resolve and a smoking gun is still needed Slide courtesy of M. Volonteri was
33. molecular outflow: OH absorption (Herschel) Ultraluminous infrared galaxy IRAS S F111191+3257: evidence for quasar feedback Tombesi et al. 2015, Nature
34. ultra-fast outflow: X-ray absorption line (Suzaku) molecular outflow: OH absorption (Herschel) Ultraluminous infrared galaxy IRAS S F111191+3257: evidence for quasar feedback Tombesi et al. 2015, Nature
35. Credit: NASA Tombesi et al. 2015, Nature “Quasar mode” AGN feedback”: Black hole winds important when there are no jets
36. 0.99 model at t = sted vs. Jets Winds “radio mode” “quasar mode”
37. Di Matteo+ 05, Nature
38. AGN feedback quenches star formation → redder galaxies her assume s energy is k holes on on between size of the edback are growth and also Sup- ur panels). laxies soon orces have oles in the gnificantly erate level. affected by ch plots the on rate and on of time. he galaxies as distorted is shocked as into the bursts and vident that the gas, as accretion rates are both quenched in the remnant, and black hole growth saturates owing to feedback provided by accretion energy. However, the damping of star formation and black hole activity is also Sup- ur panels). laxies soon orces have oles in the gnificantly erate level. affected by ch plots the on rate and on of time. he galaxies as distorted is shocked as into the bursts and vident that the gas, as perature of black holes. centres. ird pair of y converted ing to the ge to form ose to the Figure 2 Black hole activity, star formation and black hole growth plotted as a function of time during a galaxy–galaxy merger. The star formation rate (SFR), black hole accretion Di Matteo+ 05, Nature relation between starbursts and AGNs
39. ULIRG! Hopkins et al. 2006 ApJ
40. Galaxy formation and evolution Affect thermodynamic state of galaxy clusters Reionization of the universe Larger impact of AGNs http://www.nature.com/nature/journal/v468/n7320/full/nature09527.html
41. Cosmological evolution of massive black holes
42. High-redhift quasars Sloan Digital Sky Survey: SDSS pioneered the optical selection of z=6 quasars with the first large area survey in the i’ and z’ filters Shallow-wide survey: find rare bright quasars SDSS Deep finds 11 fainter quasars over 300 sq deg Fan et al.(2000-2006) Jiang et al.(2008;2009) courtesy of C. Willott M. Volonteri
43. Optical luminosity function Luminosity functions: Tools to study evolution of AGN population through cosmic time S. M. Croom et al. The binned 2SLAQ LF for six redshift intervals from z = 0.4 to 2.6. The filled points are those derived using the model-weighted estimator d Croom et al. 2009, ApJ
44. Schematic luminosity functions for AGNs 9.7. Mass and luminosity evolution of the AGN population 311 z=0 z=0 z=0 z=0 z=1 z=1 z=1 z=2 z=2 z=2 Luminosity evolution L-dependent density evolution Density evolution L Space Density Φ (L,Z) Figure 9.12. Various schematic luminosity functions for AGNs showing how such objects can vary in luminosity and space density through cosmic time. Luminosity functions: Tools to study evolution of AGN population through cosmic time Netzer
45. Where do the seeds of massive black holes come from? Volonteri
46. Quasars have been detected at very large distances, corresponding to a very young age of the Universe. As massive as the largest SMBHs today, but when the Universe was 0.75 Gyr old! WHEN do you make the first massive black holes? Gultekin et al. 2009 The farthest quasar currently known, ULASJ112010641, at z=7.1, has estimates of the MBH mass MBH~2 x109 Msun (Mortlock et al. 2011) M. Volonteri, Brera 2013
47. Mfin =2x109 Msun tH (z=7)~0.75 Gyr fEdd =0.3-1; ε~0.1 㱺 Min >300-ish Msun ULASJ112010641 M(t) = M in e ( 1−ε ε fEdd t 0.45Gyr ) M. Volonteri, Brera 2013
48. HOW can you make a massive black hole ‘seed’? M. Volonteri, Brera 2013
49. HOW can you make the first massive black holes? PopIII stars remnants Gas-dynamical collapse Stellar-dynamical collapse M. Volonteri, Brera 2013 Slide: M. Volonteri
50. Testing MBH seed formation: 
 two techniques 1. Semi-analyical modelling - Analytical “recipes” for MBH formation and growth - Monte-Carlo realizations of the merger history of dark matter halos in a LCDM cosmology - computationally inexpensive =>statistical samples 1. Cosmological simulations - No need to use global quantities or smooth functions - Gravity and hydrodynamics naturally included - Either high resolution or large volume due to computational costs MV, Haardt & Madau 2003,MV & Natarajan 2009, MV & Begelman 2010 M. Volonteri, Brera 2013
51. How do massive black holes grow? Volonteri
52. How does large scale structure evolve in the universe? Hierarchical scenario http://www.illustris-project.org
53. z=5.7 (t=1.0 Gyr) z=1.4 (t=4.7 Gyr) z=0 (t=13.6 Gyr) Hirschmann et al. 2012 Millennium Simulation mass assembly in a hierarchical universe Slide: Rachel Somerville
54. MBHS are grown from seed BHs. These seeds are incorporated into larger and larger halos, accreting gas and coalescing after galaxy mergers. time local galaxy high-z protogalaxies local galaxy high-z protogalaxies Cosmic evolution of MBHs M. Volonteri, Brera 2013
55. The growth of MBHs in galaxies Galaxy Massive black hole Early universe Today How do MBH seeds grow to become supermassive? The seeds at high redshift are small, ∼100-105 Msun M. Volonteri, Brera 2013
56. How do MBH seeds grow to become supermassive? BH-BH mergers vs gas accretion The seeds at z>20 are small, ∼100-105 Msun Total mass density in MBHs is constant in time: just reshuffle the mass function Total mass density in MBHs grows with time M. Volonteri, Brera 2013
57. MBH - host relations: how are they established? Is the correlation regulated by the galaxy or by the MBH? Feedback: The MBH regulates the process: when it reaches a limiting mass and luminosity it drives outflows that sweep away the surrounding gas, thus halting both its own growth and star formation in the galaxy. Feeding: the galaxy sets the MBH mass by regulating the amount of gas that trickles to the MBH Casuality: central-limit-theorem, i.e., a large number of mergers will average out the extreme values of MBH /Mbulge towards the ensemble average M. Volonteri, Brera 2013
58. MBH - host relations: co- evolution of MBHs and galaxies early universe today today adjustment symbiosis dominance M. Volonteri, Brera 2013
59. The Illustris Cosmological Simulation ARTICLE doi:10.1038/nature13316 Properties of galaxies reproduced by a hydrodynamic simulation M. Vogelsberger1, S. Genel2, V. Springel3,4, P. Torrey2, D. Sijacki5, D. Xu3, G. Snyder6, S. Bird7, D. Nelson2 & L. Hernquist2 Previous simulations of the growth of cosmic structures have broadly reproduced the ‘cosmic web’ of galaxies that we see in the Universe, but failed to create a mixed population of elliptical and spiral galaxies, because of numerical in- accuracies and incomplete physical models. Moreover, they were unable to track the small-scale evolution of gas and stars to the present epoch within a representative portion of the Universe. Here we report a simulation that starts 12 million years after the Big Bang, and traces 13 billion years of cosmic evolution with 12 billion resolution elements in a cube of 106.5 megaparsecs a side. It yields a reasonable population of ellipticals and spirals, reproduces the observed distribution of galaxies in clusters and characteristics of hydrogen on large scales, and at the same time matches the ‘metal’ and hydrogen content of galaxies on small scales. Theinitialconditionsfor structureformationintheUniversearetightly constrained from measurements of anisotropies in the cosmic micro- wave background radiation1. However, previous attempts toreproduce the properties of the observed cosmological structures with computer modelshaveshownonlylimitedsuccess.Nosingle,self-consistentsim- ulation of the Universe was able to simultaneously predict statistics on large scales, such as the distribution of neutral hydrogen or the galaxy population of massive galaxy clusters, together with galaxy properties onsmallscales,suchasthemorphologyanddetailedgasandstellarcon- tentofgalaxies.Thechallengelies infollowingthe baryonic component of the Universe using hydrodynamic simulations2–4, whichare required volumeandimprovedresolution,oursimulationisevolvedwiththenovel hydrodynamic algorithm AREPO5, which uses a moving unstructured Voronoi tessellation in combination with a finite volume approach (Methods).Finally,weemployanumericallywell-posedandreasonably complete model for galaxy formation physics, which includes the for- mationofbothstarsandSMBHs,andtheireffectsontheirenvironments in forms of galactic super-winds driven by star formation, as well as radio bubbles and radiation proximity effects caused by active galactic nuclei (AGNs; see Methods). Unlike previous attempts, we find a mix of galaxy morphologies ranging from blue spiral galaxies to red ellipticals, with a hydrogen and
60. Vogelsberger et al. 2014, Nature Vogelsberger et al. 2014, Nature
61. Start from early universe initial conditions Build simulation which includes relevant physics Allow galaxies to “self-consistently” evolve Challenge: Push toward a predictive theory of galaxy formation
62. Incorporate comprehensive physics/feedback model: Radiative Cooling Star formation Stellar Evolution Galactic Winds AGN Feedback Illustris Project Methods Full description of physical model in: Vogelsberger et al., (2013 arXiv: 1305.2913)
63. http://www.illustris-project.org
64. http://www.illustris-project.org
65. http://www.illustris-project.org
66. http://www.illustris-project.org
67. http://www.illustris-project.org
68. Black holes in Illustris 9 Figure 4. Central panel: stellar half-mass of all galaxies at z = 0 versus their central black hole mass. Colour-coding is according to the g r colours of galaxies. The thick black line denotes the best-fit MBH - Mstar , HM relation from Kormendy & Ho (2013) fitted to ellipticals and galaxies with bulges only. Symbols with error bars are from Kormendy & Ho (2013) as well, where circles are for ellipticals, Sijacki et al. 2015, MNRAS