The bluetides simulation Tiziana DiMatteo (CMU ) Yu Feng (Berkeley), - - PowerPoint PPT Presentation
The next quasars and galaxies frontier: The bluetides simulation Tiziana DiMatteo (CMU ) Yu Feng (Berkeley), Rupert Croft (CMU ), Aklant Bhowmick, Kuan-Wei Hunag, (CMU) Simeon Bird (JHU), Steve Wilkins (Sussex),Ananth Tenneti (CMU ) Nick
The next quasars and galaxies frontier:
The bluetides simulation
Tiziana DiMatteo (CMU)
Yu Feng (Berkeley), Rupert Croft (CMU), Aklant Bhowmick, Kuan-Wei Hunag, (CMU) Simeon Bird (JHU), Steve Wilkins (Sussex),Ananth Tenneti (CMU) Nick Battaglia (Princeton),Mark Straka (NCSA)
http://bluetides- project.org
The cosmic dawn - a largely unexplored frontier
300Myrs 800Myrs
z =8 z =6 z =7
1Billion yrs
A few (tens) of compact, clumpy irregular galaxies two quasars
room for discovery
The first 800 million years
http://bluetides-project.org/
The challenge: first objects are rare and tiny..
A sketch of Cosmic History
300Myrs 800Myrs The Universe First Billion Yrs
BTii
(renewal/ current BW project)
BT
( initial BW project)
BlueTides Simulation:
NCSA BlueWaters 0.7 million cores 0.7 trillion particles full hydrodynamics Resolves galaxies and large-scale structure of the Universe
Hybrid TreePM (gravity) SPH (Hydrodynamics – ideal fluid, baryons)
N-Body Method
à FFTW + Boltzmann Eq for collisionless DM
Euler Continuity 3rd law of thermodynamics
Hybrid TreePM (gravity- dark matter) SPH (Hydrodynamics – ideal fluid, baryons)
Cosmological expanding gasà a is the scale factor Euler Continuity 3rd law of thermodynamics
à FFTW + Boltzmann Eq for collisionless DM system
BlueTides Simulation: Technology
BlueTides Simulation: Science
calibrated from rad. Hydro sims (Battaglia+13)
BlueTides 400 x volume of HubbleUltraDeepField,
Galaxy Luminosity Function in BlueTides consistent with Hubble Legacy Fields
Cosmic variance
Feng et al., 2015a (star formation rate) Galaxy luminosity bright
J J
1.3x1010M¤ @ z=6.3 ¢ ¢
Wu+15, Nature
2x109M¤ @ z=7
(Mortlock+11)
A few (Gpc)-3
¢ ¢ 2x109M¤ @ z=7
(Mortlock+11)
BH as massive as most massive at z=0 (t> 13 billion yrs)
McConnel&Ma13 Galaxy mass
h``11111 ¡
1 QSO
z=6 qsos are this rare
J1342+0928
ALLWISE/Ukidss
Banados+17, Nature
MBH=8x108M¤ …. And after 6 years
BH Seeds
Small Large Grow Massive BHs
BH Seeds
Small Grow
PopIII remnants
ü First stars (metal free) are massive M★ ~O(100) M¤ ü When they die they leave a remnant BHs of MBH,seed ~ M★ ~ O(100) M¤
BH Seeds
Large Grow
Direct gas collapse
ü Deep potential well for gas infall and collapse require inflow rate > 0.1M¤ ü Form a supermassive star, that accretes envelope forms MBH,seed ~ O(104-6) M¤
1.E+00 1.E+01 1.E+02 1.E+03 1.E+04 1.E+05 1.E+06 1.E+07 1.E+08 1.E+09 100 500 1000
BH Mass in Solar Masses
DC/supermassive Star Seed PopIII Seed Myrs since the BigBang
Observed..
How/ where do MBHs seeds grow?
BH-BH mergers
Mayer et al.
Gas Accretion
Total mass density of BHs grows with time.
How/ where do MBHs seeds grow?
Gas Accretion
Total mass density of BHs grows with time. LBH = efficiency Macc c2 BH Growth = Gas Supply = Energy liberated
AGN feedback
SMBHs Stars (bulges) /galaxies DM halos? RSch=2GMBH /c2 Rgrav=2GMBH
/σ2 microparsec/parsec
RSch=2GM*/σ2
kiloparsec
RSch=2GMHalo/σ2
megaparsec
Resolution demands to do BH growth in simulations
Uniform Cosmological Simulations with BHs ü rare regions Large Volumes ü galaxy scales High Resolution ü gas accretion Hydrodynamics …
+ star formation BH accretion feedback
subgrid
that probes high-z quasars
Example:
6x108Msun
Most massive BHs at z=8, M ~ 108Msun
Fastest growing, massive black holes are not in disky galaxies!
First quasars beyond z=7
The environment of the most massive BH: compact, spheroidal host galaxy with strong radial inflows
BT: First Massive stuff: tidal fields/IC
MBH=4x108 Msun
Primordial ‘Milky Way’ galaxies
∂i∂ jFirst billion solar mass BHs
disc spheroid HIGH TIDAL FIELD LOW TIDAL FIELD
Di Matteo+17
Strong enough inflow in rare region of low tidal fields rates can sustain critical growth rates (+)
1.E+00 1.E+01 1.E+02 1.E+03 1.E+04 1.E+05 1.E+06 1.E+07 1.E+08 1.E+09 100 500 1000
BH Mass in Solar Masses
DC/supermassive Star Seed PopIII Seed Myrs since the BigBang
109Msun
J1342+0928
ALLWISE/Ukidss
Banados+17, Nature
MBH=8x108M¤ ….current PRAC meets observations
quasar
quasar
Tenneti, TDM+18
MBH=7x108M¤ M*= 3e10M¤ …. In BlueTides
Does the BH ever stop growing?
Evidence for BH feedback/winds in z=6 quasars
Maiolino et al. 2013
The outflow at z=7.5
Z=7.54 Quasar outflows
Quasar outflows Few 100 Solar Mass/yr
Does the BH ever stop growing? YES
BT predicts z=7.54 quasar has strong
Ni+2018
co-evolution
BHs from high-z?
Who is the host ?
Who grows first? Galaxy or BH?
Courtesy of M. Volonteri
Giant BH, tiny dusty host galaxy for z=7.54 QSO
Tenneti+2018 BT predicts host for JWST observation: qso galaxy Webb telescope
Webb telescope
The environment of the first quasar in Bluetides Synthetic JWST observation of the host galaxy
Tenneti, TDM+18
MBH=7x108M¤ …. In BlueTides
JWST FOV(~100”)
DARK MATTER
Tiny host galaxy for the first giant quasar
Bluetides z=7.54 quasar host galaxy M87: another host of billion solar mass black hole
co-evolution
BHs from high-z
BH ‘grows’ first
Courtesy of M. Volonteri
co-evolution
BHs from high-z
Courtesy of M. Volonteri
Bluetides makes contact with data:
first galaxies and quasars