Early Growth of typical Massive Black Holes - Muhammad Latif - Physics Department
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Early Growth of typical Massive Black
Holes
Muhammad Latif
Physics Department,
United Arab Emirates University
Luminosities of high z quasars
★ Supermassive black holes
9
with ~10 solar masses have
been observed at z>6.
Figure 4:
14
★ The highest-redshift black
hole currently observed is at
z=7.085 and has 2x10 M9
⦿
(Mortlock et al. 2011).
★ The most massive black of
1.3 x 10 10 M at z=6.3
⦿
(Wu et al. Nature 2015)
Direct collapse scenario
Direct collapse scenario
Direct collapse of a massive
★ Provides
alo of 107-10massive
8
M☉ seeds of
105-106 M⦿
ey requirements
★Key requirement is to have large
rimordial composition
inflow rate of > 0.1 M⦿/yr
uench H2 formation
★Isothermal direct collapse with
ragmentation
T~ 8000 K
remains
uppressed
★ Primordial gas composition
rovides massive seeds of 105
106 M☉
★ Requires strong LW flux to
he quench
role ofHturbulence
2 formation remains
nexplored See review by Latif & Ferrara 2016
Regan et al 2009
Supergiant protostar
“Supergiant Protostar”
TH+12
stellar+radius+: R*+(+R!)
HIburning+starts
ZAMS
HIburning+starts
stellar+mass +M*+(+M!)
" The+protostar+never+contracts+to+reach+the+ZAMS+stage,+but+
+++++largely+expands+with+very+rapid+accreDon,++>+0.01+M!/yr.+
" large+radius+→+low+effecDve+temperature+→+weak+UV+feedback+
Hoskawa et al. 2012, Schleicher, ML et al. A&A 2013
Outcome of an Isothermal collapse
Turbulent, magnetized black hole formation 7
ILES-B12 ILES-B10 LES-B12 LES-B10
halo 1 281 & 384 * 1335 & 1680 * no no
halo 2 no no no 831 & 588
halo 3 no no no no
halo 4 no no no no
halo 5 no no no 356 & 156 *
halo 6 no no no 2&4*
halo 7 5589 & 5185 no no no
halo 8 no 28 & 42* no 3833 & 1753
halo 9 no no 128 & 121 no
Turbulent, magnetized black hole formation 9
Table 1. Fragmentation results of all 36 simulations, i.e., 9 different halos
(with slightly different initial conditions) each with 4 different setups. The
masses of the clumps are given in M . The asterisk indicates whether the
fragmentation was first identified at a peak density of 10 9 g/cm3 and not
yet at a peak density 10 12 g/cm3 . The two snapshots are ⇡ 150 years apart
(compared to a free-fall time of ⇡ 50, 000 years at 1 pc).
which encompasses all (turbulent and non-turbulent) contributions
from scales larger than the grid resolution scale. The ratio of the
three non-ideal hydrodynamic pressures to the thermal pressure for
all LES is illustrated in Fig. 6.
In the case of weak initial seed fields (LES-B12, left panel),
both resolved and turbulent magnetic pressures are weak (
BH growth: simulation setup ➡ 3D radiation hydrodynamics cosmological simulation ➡ Halo mass of 3 × 1010 M⦿ at z = 7.5 ➡ Coming periodic box of 8 Mpc/h ➡ DM resolution of ∼ 53,000 M⦿ ➡ Physical resolution of 3.6 pc
Pop III/II Star Formation
★ An Overdensity of 5 x 105 (~ 103 cm-3 at z =10)
★ A converging gas flow (∇·Vgas < 0)
★ Molecular hydrogen fraction (fH2 > 5 x 10-4)
★ The mass is randomly sampled from IMF with mass range
between 1-300 M⦿
★ For Z/Z⦿ > 10-4 Pop II star cluster of ~1000 solar masses
are allowed to form
Wise & Abel 2012
Stellar feedback
★ Radiative feedback is modelled using the ray tracing scheme
★ We take a monochromatic spectrum with an energy of 29.6 eV for Pop III
stars
★ For Pop II stars, we take a fixed spectrum of 21.6 eV appropriate for low
metallicity stars
★ BH seeds from the First stars
We model both Type II and PINSN
Massive black hole feedback
★ Insert a massive black hole (MBH) seed of 105M⦿ at the
halo center at z = 12
★ We model both UV and X-ray feedback from an accreting
MBH
★ Four energy bins at 13.6 eV, 24.6 eV, 54.4 eV and 1 keV
are used when generating the photons
★ We model the gas accretion onto the MBH following the
prescription of Kim et al. (2011) and estimate mass
accretion onto BH using the Bondi-Hoyle recipe
Growth of a DCBH in Atomic cooling halo
3D Radiation Hydrodynamical simulations
Include both UV & X-ray feedback (0.1eV-1.1 KeV) from a BH
10-3
1.15
10-4
Accretion Rate [M O• /yr]
10-5
MBH[104 M O• ]
1.10
10-6
10-7
1.05 10-8
10-9
1.00 10-10
0 2 4 6 8 10 0 2 4 6 8 10
Time [Myrs] Time [Myrs]
Also see Johnson et al. 2011
Aykutalp et al. 2014Stellar mass
Latif, Volonteri & Wise 2018Star formation rate
Salmon et al. 2015 at z=6.5
Latif, Volonteri & Wise 2018Metal distribution gure 2. Projections of density-weighted temperature along the y-axis at various redshifts for the central 14 kpc region. The nel shows the moment when first SN goes off while other panels depict the epochs when large outflows are produced by the ndem with MBH feedback. gure 3. Projections of density-weighted metallicity originating from Pop III SNe along the y-axis at the same redshifts as figu e central 14 kpc region. Latif, Volonteri & Wise 2018
Growth of a typical DCBH
re 4. Projections of density-weighted gas density along the y-axis at the same redshifts as figure 2 for the central 14 kpc region.
e 5. The black hole mass evolution (top panel) Latif,Volonteri
and the mass accretion&rate
Wise 2018
onto the MBH (bottom panel) over the cosmic timeComparison of BHAR vs SFR
Black hole growt
Latif et al. 2018
Figure 6. The MBH accretion rate against star formation rate is shown here. The green squares represent Pop III SFRs whil
triangles correspond to Pop II SFRs. They are plotted for all halo progenitors at all redshifts. The grey-shaded region shows thKey Findings
★ SNe in combination with feedback from MBH quench its
growth
★ PISNe are more effective in removing the gas from BH
vicinity
★ The average SFR during the simulation is ∼ 1 M⊙/yr
★ This may explain the paucity of low luminosity AGN at z>6Formation of the First Black Holes
Formation
Forthcoming
Formation of the First Black Holes
of the First
The formation of the first supermassive black holes is one of the
main open questions in our understanding of high-redshift structure
formation. In this book, we aim to provide a summary on the state
Black Holes
of art of modern research on this topic, exploring the formation of
massive black holes from a fluid dynamical, stellar dynamical and
Thank you
chemical perspective. The book thus provides a solid theoretical
foundation, and includes a comparison with current observations and
future perspectives, including modern topics such as the potential of
the Square Kilometre Array, the European Extremely Large Telescope,
the Euclid satellite or possible detections via gravitational waves.
Muhammad Latif
Dominik Schleicher
Schleicher
Latif
Editors
World Scientific ISBN 978-981-3227-94-1
www.worldscientific.com World Scientific
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