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The first black holes and AGN Marta Volonteri Institut d’Astrophysique de Paris M. Habouzit, Y. Dubois, M. Latif (IAP) A. Reines (NOAO) M. Tremmel (University of Washington) F. Pacucci (SNS)

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  • The first black holes and AGN

    Marta VolonteriInstitut d’Astrophysique de Paris

    M. Habouzit, Y. Dubois, M. Latif (IAP)A. Reines (NOAO) M. Tremmel (University of Washington)F. Pacucci (SNS)

  • As massive as the largest MBHs today, but when the Universe was ~ Gyr old

    Wu et al. 2015

    z>6

    High-redshift quasars and local MBHs

    POX 52, NGC 4395: stellar mass 4x108 Msun, MBH~3x105 Msun

    Galaxies without MBHs too

    RGG18: MBH~5x104 Msun

  • Very bright quasars in SDSS, CFHQ, UKIDDS with z>6 (Willott et al., 2003; Fan et al., 2006; Jiang et al., 2009)

    Detection of a 2x109 Msun BH at z=7 and a 1010 Msun BH at z=6.3 (Mortlock et al., 2011, Wu et al. 2015)

    Requirement:-  Need to grow at the Eddington limit for the whole time (M0~300 Msun) or 60% of the time (M0~105Msun)

    High-redshift quasars

  • Eddington limit?Gas infalls from the galaxy: how does the galaxy know that it has to feed the MBH exactly at the Eddington limit?

    Super-Eddington accretion does not imply highly super-Eddington luminosity

    Trapping of radiation: photons are advected inward with the gas, rather than diffuse out

    Luminosity highly suppressed

    Only short periods needed to ease constraints (e.g. MV & Rees 2005; MV, Silk & Dubus 2015; Pacucci, MV et al. 2015a,b; Lupi et al. 2016)

    L∝ ln(M•

    )L∝M•

  • No detection in X-ray stacking of LBGs at z>6: LX

  • The billion solar masses MBHs powering the observed z>6 quasars are the tip of the iceberg

    Very biased, dense halos

    What do we expect for normal MBHs in normal galaxies?

    High-redshift MBHs

  • How do MBHs form?

    MetalFree

    -5

    0

    -3

    -4

    -2

    -1

    10 102 103 104 105 106

    Pop III remnants

    Stellar mergersin nuclear clusters

    BH mergers in nuclear clusters

    Dynamics-driven gas collapse

    Thermodynamics-driven gas collapse

    MBH (Msun)

    log(Z/Z☉)

    Cosmic string loopsInflationary black holes

    Popular today

  • A physical approach to seed cosmological simulations with MBHs

    Ramses: Grid-based hydro solver with mesh refinement (Teyssier 2002) - Cooling/Star formation (Rasera & Teyssier 2006)

    - Supernova feedback (Dubois & Teyssier 2008, Teyssier et al. 2013, Dubois et al. 2015)- BH accretion + AGN feedback (Dubois et al. 2012)

    MBH seeds (sink particles) formed in: •  overdense bound collapsing regions •  metal-poor (Z

  • Habouzit, MV, Dubois 2016

    Density mapBHs form only in high gas-density regions

    Metallicity mapBHs form in low-metallicity regions

    (10 Mpc)3 cosmo hydro simulation:Spatial resolution 80 pcDM resolution 2 106 Msun

  • How do galaxies ���feed normal MBHs?

    Low-mass BHs in low-mass galaxies: fragile environment

    Interplay between SN feedback and MBH accretion: SN feedback is sufficient to energize the gas and suppress accretion (Dubois+14)

  • SETH, Ramses Cosmological Zoom, ~5pc resolution, Dubois, MV+14

  • How do galaxies ���feed normal MBHs?

    z=0 BHs and AGN (Reines & Volonteri 2015)

    10 Mpccosmological volume, ~80pc resolution

    Habouzit, MV, Dubois 2016

  • How do galaxies ���feed normal MBHs?

  • Growing black holes in growing galaxies

    Galaxy

    Massiveblack hole

    Early universe

    Today

  • (Willott 2011; Fiore et al. 2012; Cowie et al. 2012; Treister 2013; Giallongo et al. 2015; Weigel et al. 2015; Cappelluti et al. 2016)

    Bulge mass�B

    lack

    hol

    e m

    ass�

    Kormendy & Ho 2013

    Expect MBH ~106 Msun

    Searches for AGN in galaxies with stellar masses ~109 Msun at z > 6 have found very few, if any, black holes

  • BH mass vs. total galaxy stellar mass

    (341 nearby galaxies)

    MBH vs galaxy at high redshift

    Reines & MV 2015

    Log

    Blac

    k H

    ole

    Mas

    s

    Log Total Stellar Mass

  • Log

    Blac

    k H

    ole

    Mas

    s

    Log Total Stellar Mass

    MBH vs galaxy at high redshift

    MBH ~10-3 Mgal

    MBH ~10-4 Mgal

    Reines & MV 2015

  • MBH ~10-3 MgalMBH ~106 Msun

    MBH ~10-4 MgalMBH ~105 Msun

    MBH vs galaxy at high redshift

    MV & Reines 2016

    stellar mass ~109 Msun

    AGN expected to be less luminous

    Expect 0-3 AGN with LX >1042 erg/s in the 4Ms CDFS

    Consistent with current limits/candidates

  • High-redshift MBHs

    Current limits/candidates high-z AGN compatible with a population of MBHs similar to low-z counterpart in galaxies of similar mass

    How about the high-z quasars?

  • Current large-shallow surveys select only the most luminous quasars, Lbol>1046 erg/s

    MBH vs galaxy at high redshift

    Lauer et al. 2007; MV & Stark 2011; MV & Reines 2016

    ⇒ the most massive holes at a given stellar mass

  • Growing black holes in growing galaxies

    Galaxy

    Massiveblack hole

    Early universe

    Today

  • Galaxies form stars and emit ionizing photons

    MBHs accrete and emit ionizing photons

    Relative Role of Stars and Quasars in Cosmic Reionization

    MBHs predicted to contribute 20-50% of ionizing photons (MV & Gnedin 2009)

    Growing black holes in growing galaxies:contribution to reionization

  • Growing black holes in growing galaxies:contribution to reionization

    MV & Gnedin 2009

  • High-redshift MBHs

    “Ab-normal” MBHs in “normal” galaxies are those that grow fast and can be detected as luminous quasars

    “Normal” MBHs in “normal” galaxies may grow slowly

    Current limits/candidates high-z AGN compatible with a population of MBHs similar to low-z counterpart in galaxies of similar mass

    Relative role of stars and MBHs in cosmic reionization


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