Investigating silk yield and morphological changes in silk ...
The Golden Mass of Galaxies and Black Holes with Deep Learning … · 2019-04-24 · Larson 74 ,...
Transcript of The Golden Mass of Galaxies and Black Holes with Deep Learning … · 2019-04-24 · Larson 74 ,...
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Avishai Dekel The Hebrew University of Jerusalem & UCSC
The Golden Mass of Galaxies andBlack Holes with Deep Learning
Ofer Lahav’s 60th Birthday, April 2019
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A Characteristic Mass for Galaxy Formation
low-mass quenching
high-mass quenching
Black HolesEfficiency of galaxy formation
Behroozi+ 2013
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A Characteristic Time for Galaxy Formation
low-mass quenching
high-mass quenching
Mass
Star-formation density
typical halos at z~2 are ~1011-12M
�
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AGN Activation at the Critical MassForster-Schreiber+18 KMOS3D z=0.6-2.7 599 galaxies
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Why do galaxies like to form at the golden mass (and time)?
Why do black holes grow rapidly Why do black holes grow rapidly once their host galaxies are above
the golden mass?
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A Characteristic Mass for Galaxy Formation
Mstar~1010.5M�Mvir~1012M�
Vvir~100 km/s
- Supernova feedback efficient at M<Mcrit (Vcrit)
- Hot halo (virial shock heating) at M>Mcrit
Larson 74, Dekel & Silk 86
Rees & Ostriker 77, Silk 77, Binney 77, Dekel & Birnboim 06
-> Compaction to Blue Nuggets + quenching at ~Mcrit (any z) Zolotov+15, Tacchella+16, Dekel+17
Larson 74, Dekel & Silk 86
-> Black Holes suppressed by supernovae at M<Mcrit, Black hole growth at M>Mcrit
-> Quenching of star formation at M>Mcrit triggered by compaction, maintained by hot halo & black hole
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2. Virial Shock Heating in Massive Halos
Dekel & Birnboim 06, Rees & Ostriker 77, Silk 77, Binney 77
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Hot Halo Scale: shutdown of cold gas supply
slow cooling -> shock
critical halo mass ~~1011.8Mʘ
11 −−< compresscool tt
Dekel & Birnboim 06, Rees & Ostriker 77, Silk 77, Binney 77
log T
Kravtsov+
log T
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Mvir [Mʘ]
1013
1012
shock heating
cold streams
hot CGM
Mcrit by Shock Heating: Mvir~1011.5-12M
�
hot CGM
Dekel & Birnboim 06
Simulations:Ocvirk, Pichon, Teyssier 08;
Dekel+ 09
Mvir [Mʘ]
typical halos
redshift z
1011
0 1 2 3 4 5
cold CGM
Press & Schechter 74
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Empirical Model From Observations
Fraction of star-forming galaxiesBehroozi+
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3. Supernova Feedback in Low-mass Halos
Larson 74, Dekel & Silk 86
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Supernova Fdbk Scale Vvir~100 km/s
Energy fed to the ISM by supernova bubble before fading:
Gas binding energy:
Dekel & Silk 86
km/s120, SN2
SNSN ≈≈∗
VVME
RGMVVME /, 2vir
2virgasgas =≈
ESN ~ Egas & star formation at peak efficiency M*~Mgas
--> an upper limit for efficient supernova feedback:
)0at(107km/s120 11SNvir,SNvir, =×≈→≈
⊗zMMV
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Mvir [Mʘ]
1013
1012
shock heating
cold streams
hot CGM
Mcrit by SN Feedback: Mvir~1011.5-12M
�
hot CGM
Dekel & Birnboim 06
Mvir [Mʘ]
typical halos
redshift z
1011
0 1 2 3 4 5
cold CGM Dekel & Silk 86
Press & Schechter 74
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Dekel & Burkert 14, Zolotov+15, Tacchella+16a,b, Dekel, Lapiner+18
4. Wet Compaction to Blue Nuggets
Blue Nugget
Red Nugget
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wet compaction max density core: blue nugget
gas + young stars
vela v2 07
vdi disk core depletion: a hole and a ring
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wet compaction max density core: blue nugget
stars
vela v2 07
green nugget red nugget + envelope
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gas
stars
dark matter
1 kpc10
8
M
Compaction -> quenching in the inner 1 kpc
star-formation rate
time
M
2
0
diffuse compaction quenching
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Compaction and Quenching in Simulations
blue nuggetstar formingdiffuse
diffuse compact
quenched red nugget
Zolotov+15Tacchella+16Dekel+17
L-shape track
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Observed L-Shape Track Barro+17
compactionBN
star forming
quenching
diffuse compact
quenched
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Blue Nugget --> Red Nugget
blue nugget red nugget
gas stars gas stars
gas depletion from core, gas ring may form, -> inside-out quenching
stellar core remains dense from BN to RN
dense gas core -> dense stellar core
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What is the Trigger of wet Compaction?
- Mergers (major, minor) (Barnes, Hernquist 91; Hopkins+ 06)
- VDI-driven inflow (Dekel, Burkert 15)
Drastic loss of angular momentum
- Counter-rotating streams (Danovich+ 15)
- Tidal compression (Dekel+ 03; Renaud+ 14; Mandelker+ 16)
- Triaxial halo core (Ceverino+ 15; Tomassetti+ 16)
- Return of recycled low-AM gas (Elmegreen+ 14; DeGraf+ 16)
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Counter-rotating Streams
Rv
Danovich+15
1/3 streams are counter-rotating
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A Critical Mass for Blue Nuggets (at all z)
Mstar~1010M�Mvir~1011.5M�
Hot CGM
Origin of BN scale? SN fdbk + hot CGM
SN fdbk
time
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Identify BNs in 3D simulations (gas, stars)
Deep Learning: BNs inTheory vs Observations Pre BN Blue Nugget Post BNHuertas-Company+ 18
Train CNN on mock images of simulations
Classify BNs in HST images
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Blue Nuggets at a Golden Mass in CANDELS
Deep Learning: Huertas-Company+ 18
Luminosity (mass) eliminated
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Convoluted Neural Network
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Transition in Galaxy Properties at the BN
- Star forming -> quenched
- Oscillations across the Main Sequence -> quenching
- Diffuse -> compact core + extended disk
- Dark-matter -> baryon dominated core
- Prolate -> oblate stellar system
- V/σ~1 -> V/σ~4, dispersion -> rotation dominated
- …
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4. Compaction and Black-Hole Growth
Dekel, Lapiner, Dubois+ 2017
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Interplay between SNe and BHsRAMSES Simulation SN+BH by Dubois+ 15
merger
z=3.60 z=3.44
no SN
merger compactionwith SN
- M<Mcrit: strong SN fdbk suppresses BH growth- Compaction overcomes SNe -> rapid BH growth- M>Mcrit: AGN fdbk helps quenching
time
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gas
stars
dark matter
1 kpc10
8
M
Compaction -> BH Growth
star-formation rate
time
M
2
0
diffuse compaction quenching
black hole
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Compaction driving BH GrowthNew Horizon simulations SN+BH Dubois+ Lapiner+
gas 1kpc
stars 1kpc
BHx104
stars
compaction DM 1kpc
gas 1kpc
BH growth
rBH
gravity
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Compaction driving BH Growth
New Horizon simulations SN+BH Dubois+ Lapiner+
BHx104stars 1kpc
BHx104stars 1kpc
stars
stars
compaction compactiongas 1kpc
gas 1kpc
stars 1kpccompaction compaction
BH growth
BH growth
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BH Below the Linear Relation for MBH~105M
�
Lapiner+
New Horizon Simulation
Blue Nugget
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Magic Mass for BH is Robust in Simulations
EAGLEBower+ 16
no SN
w SN
Illustris TNGHabouzit+18
FIREAngeles-Alcazar+17
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BH Growth by Compaction at Mvir~1011.5-12M
�
-Mvir < Mcrit, pre-compaction SN phase: Vesc < 100 km/s -> SN winds of 100 km/s evacuate the core -> BH growth is suppressed , Blue-Nugget formation is suppressed
-Mvir ~ Mcrit, compaction overcoming SN fdbk:The compressed gas activates rapid BH growth The compressed gas activates rapid BH growth
-Mvir > Mcrit, post-compaction hot CGM phase: Vesc > 100 km/s -> SN winds are bound (by halo potential and hot gas)-> gas falls back in -> BH growth continues-> AGN self-regulates with the accretion, AGN fdbk keeps the CGM hot and suppresses SFR long term
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Observed High Fraction of AGN in BN PhaseKocevski+17
SFR RN
comactnesss
-> Compaction triggers BH growth and AGN -> quenching
BN diffuse
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AGN Activation at the Critical MassForster-Schreiber+18 KMOS3D z=0.6-2.7 599 galaxies
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Fraction of AGN
L = 0.1 dMbh/dt c2
BH accretion rate
simulations
dM/dt L
L=1042.5
KMOS3D
New Horizon sims
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AGN Correlate with CompactnessForster-Schreuer+18 KMOS3D z=0.6-2.7 599 galaxies
incidence
M*=10-10.75
M*=10.75-11.3
incidence
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A Characteristic Mass for Galaxy Formation
Mstar~1010.5M�Mvir~1012M�
Vvir~100 km/s
- Supernova feedback efficient at M<Mcrit (Vcrit)
- Hot halo (virial shock heating) at M>Mcrit
Larson 74, Dekel & Silk 86
Rees & Ostriker 77, Silk 77, Binney 77, Dekel & Birnboim 06
-> Compaction to Blue Nuggets + quenching at ~Mcrit (any z) Zolotov+15, Tacchella+16, Dekel+17
Larson 74, Dekel & Silk 86
-> Black Holes suppressed by supernovae at M<Mcrit, Black hole growth at M>Mcrit
-> Quenching of star formation at M>Mcrit triggered by compaction, maintained by hot halo & black hole
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Conclusions
Wet compaction to a Blue Nugget is a dramatic event in the history of many galaxies (~40% by mergers, 30% counter-rotating streams)
The major compaction is typically at the golden mass, when SN fdbkbecomes ineffective and cold streams penetrate the hot CGM
The golden mass M*~1010M�(and z~2) is due to suppression of SFR
by SN fdbk at low masses and CGM heating at high masses (+AGN)
The Blue Nugget marks transitions in most galaxy properties:mass, size, SFR, gas fraction, metallicity, dust,dark-matter dominance, shape, kinematics, …
BH growth is suppressed by SN feedback in M<Mcrit halos, and is triggered by Wet compaction in M>Mcrit halos, where SNe are ineffective & the CGM is shock heated. The resulting AGN helps maintaining the quenching
Deep Learning is a tool for confronting simulations with observations
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Mvir [Mʘ]
1013
1012
shock heating
cold streams
hot CGM
The Golden Mass Mvir~1011.5-12M
�
hot CGM
Dekel & Birnboim 06
BH growth
SF quenching
Mvir [Mʘ]
typical halos
redshift z
1011
0 1 2 3 4 5
Dekel & Silk 86
SN-suppressed BH
SN-suppressed SF
Press & Schechter 74
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Cosmic Velocity Fields, 9th IAP Colloquium, 1993
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