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
   

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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)
   

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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)
   

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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.
   

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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
   

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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.
   

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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
   

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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
   

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9. View Slide

10. View Slide

11. Motivation for some kind
    of “AGN feedback”
    process in galaxies
    

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12. Slide: Simon White
    1)
    

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13. Slide: Simon White
    1)
    

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14. 2) The cooling flow riddle
    

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15. T ~ 106 - 107 K
    bremsstrahlung
    radiation
    Dbrem
    / ⇢2
    2) The cooling flow riddle
    

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16. Dbrem
    / ⇢2
    2) The cooling flow riddle
    

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17. http://chandra.harvard.edu/photo/2003/perseus/animations.html
    

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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
    

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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
    

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20. How can massive black
    holes affect galaxies?
    i.e. how cosmic bullies work
    

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21. How can massive black
    holes affect galaxies?
    i.e. how cosmic bullies work
    

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22. Hydra A
    McNamara et al.
    X-rays (Chandra)
    Optical
    

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23. 1’ = 22 kpc
    X-rays (Chandra)
    Fabian et al.
    Perseus cluster
    a
    b c
    Optical
    

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24. View Slide

25. MS0735
    McNamara+05 Nature,
    McNamara+ 09
    1’ = 210 kpc
    

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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
    

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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
    

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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
    

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29. Simulation of AGN feedback via jets (“radio mode”) in
    a cluster atmosphere
    Omma et al. 2004
    

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30. Brüggen et al. 2005
    0.4 Mpc
    Simulation of AGN feedback via jets (“radio mode”) in
    a cluster atmosphere
    

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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
    

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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
    

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33. molecular outflow:
    OH absorption (Herschel)
    Ultraluminous infrared galaxy
    IRAS S F111191+3257:
    evidence for quasar feedback
    Tombesi et al. 2015, Nature
    

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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
    

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35. Credit: NASA
    Tombesi et al. 2015, Nature
    “Quasar mode” AGN feedback”: Black hole
    winds important when there are no jets
    

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36. 0.99 model at t =
    sted
    vs.
    Jets Winds
    “radio mode” “quasar mode”
    

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37. Di Matteo+ 05, Nature
    

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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
    

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39. ULIRG!
    Hopkins et al. 2006 ApJ
    

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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
    

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41. Cosmological evolution
    of massive black holes
    

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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
    

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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
    

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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
    

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45. Where do the seeds of
    massive black holes
    come from?
    Volonteri
    

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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
    

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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
    

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48. HOW
    can you make a
    massive black hole ‘seed’?
    M. Volonteri,
    Brera 2013
    

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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
    

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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
    

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51. How do massive black
    holes grow?
    Volonteri
    

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52. How does large scale structure evolve in the
    universe? Hierarchical scenario
    http://www.illustris-project.org
    

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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
    

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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
    

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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
    

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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
    

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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
    

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58. MBH
    - host relations:
    co- evolution of MBHs and galaxies
    early universe
    today
    today
    adjustment
    symbiosis
    dominance
    M. Volonteri,
    Brera 2013
    

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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
    

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60. Vogelsberger et al. 2014, Nature
    Vogelsberger et al.
    2014, Nature
    

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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
    

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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)
    

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63. http://www.illustris-project.org
    

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64. http://www.illustris-project.org
    

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65. http://www.illustris-project.org
    

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66. http://www.illustris-project.org
    

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67. http://www.illustris-project.org
    

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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
    

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