“quasar” feedback in galaxies
TRANSCRIPT
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Philip Hopkins
“Quasar” Feedback in Galaxies
Lars Hernquist, Norm Murray, Eliot Quataert, Todd Thompson, Dusan Keres, Chris Hayward, Stijn Wuyts,
Kevin Bundy, Desika Narayanan, Ryan Hickox, Rachel Somerville, & more
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Ø Every massive galaxy hosts a supermassive black hole
Ø Mass accreted in ~couple bright quasar phase(s) (Soltan, Salucci+, Tremaine+, Yu & Lu, PFH, Shankar, et al.)
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Scatter in MBH
Scatter in the mass that “gets down to” MBH
BHs must somehow self-regulate
PFH, Murray, & Thompson 2009
Gebhardt et al.Ferrarese et al.Haring & RixTremaine Marconi & Hunt
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Num
ber D
ensit
yWhat can AGN Feedback Do For You?
Spheroid & BH Formation Times:
PFH, Lidz, et al. 2007
Oppenheimer & Dave
Observed
No AGN FB
Marconi et al.
Ø Sharp color bimodalityØ Lowering mass of >M* galaxiesØ Removing/heating gas in groups
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Ø “Quasar” mode (high mdot)
Ø Move mass from Blue to Red?
Ø Rapid (~107 yr)
Ø Small(er) scales (~pc-kpc)
Ø Morphological Transformation
Ø Gas-rich/Dissipational Mergers?
Ø Regulates Black Hole Mass
Ø “Radio” mode (low mdot)
Ø Keep it Red
Ø Long-lived (~Hubble time)
Ø Large (~halo) scales
Ø Subtle morphological change
Ø Hot Halos & Dry Mergers
Ø Regulates Galaxy Mass
“Transition” “Maintenance”vs.
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Star Formation
BH Growth
Sanders, Scoville, many subsequent
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What Can Quasar Feedback Do?
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Feedback Energy:
SILK & REES ‘98
L = �r MBH c2 (�r ⇠ 0.1)
! Erad ⇠ 0.1MBH c2 ⇠ 1061 erg(MBH ⇠ 108 M�)
Egal ⇠ Mgal �2 ⇠ (1011 M�) (200 km/s)2 ⇠ 1059 erg
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M-sigma Suggests Self-Regulated BH Growth
PREVENTS RUNAWAY BLACK HOLE GROWTH
Di Matteo et al. 2005
Black hole growth
without feedback
with feedback
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Quasar Outflows: Heating Halo Gas
SHUT DOWN COOLING AND/OR “SET UP” RADIO MODE
No Quasar
With Quasar
Quasar Feedback
No Feedback
Cox et al. 2006
McCarthy et al. 2010,11
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With AGNFeedback
No AGN Feedback
Springel et al. 2005
Expulsion of Gas Turns off Star Formation
ENSURES ELLIPTICALS ARE SUFFICIENTLY “RED & DEAD”?
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But Does Quasar Mode Feedback Exist?
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Optical (Stars)
OIII Ionization Cone
NGC 5728
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Arav et al.Wampler et al. 1995Hamann et al. 2001de Kool et al. 2001&2Korista et al. 2008Moe et al. 2009Dunn et al. 2010Aoki et al. 2011Kaastra et al. 2011
Rwind � 1� 20 kpcv � 1000 km s�1
Mwind � 100� 600 M� yr�1
Broad Absorption Line Quasars
Ø Preferentially in high-L quasarsØ Covering factor ~20%
Ø ~12 (16) objects now, 10/12 confirmed:
Lwind & 0.01LAGN
Mwind v & LAGN/c
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|DVBLUE||DVRED|
Green & Zakamska et al. 2011
Shen et al. 2011 (Double-Peaked NLRs)
Laor et al., Crenshaw et al. (lower-luminosity, v ~ 100-400 km/s)
Humphrey et al. 2010
“Broad wings in Narrow Lines” in Type-2 (Narrow-Line) Quasars
M ⇠ 50� 1000M�/yr
M v ⇠ 1� 30LAGN/c
Lwind ⇠ 0.01LAGN
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Lehnert et al. 2009,2011Nesvadba et al. 2010,2011
Alexander et al. 2010
Ionized Gas Tracers At High-Redshift
> 1000 km/s
“Pushed” By Radio Jets
No Radio Jets / Radio Quiet
Lwind ⇠ 0.1LAGN
Rwind ⇠ 5 kpc
v ⇠ 1000 km/s
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Molecular+Ionized Outflows:
Mwind � 1000 M� yr�1
v > 500 km s�1
Rwind � 1� 4 kpc
Rupke & Veilleux 2005,2011Fischer et al. 2010 (Mrk 231)Feruglio et al. 2010 (Mrk 231)Alatalo et al. 2011 (NGC 1266)
CO:
kpc
Molecular Outflows in AGN ULIRGs
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Sturm et al. 2011:Molecular Outflows in AGN ULIRGs
M ⇠ 100� 1000M�/yrM v ⇠ 5� 30LAGN/c
Lwind ⇠ 0.03� 0.10LAGN
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Where to now? How Do We Model This?
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Step 1: Inflow
R < 0.1 pc: ~ few M⊙ yr-1Ø Beginning to directly follow inflow
to sub-pc scales
PFH & Quataert 2009,10,11Levine, Gnedin, Kravtsov 09,10Mayer, Callegari, 09,10
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Step 1: Inflow
R < 0.1 pc: ~ few M⊙ yr-1Ø Beginning to directly follow inflow
to sub-pc scales
PFH & Quataert 2009,10,11Levine, Gnedin, Kravtsov 09,10Mayer, Callegari, 09,10
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Bars w/in Bars(Shlosman et al. 1989)
“It’s Bars all the Way Down ...”
(PFH & Quataert 2010)
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Derive ‘Instability’ Rate:
M � 10 M� yr�1� Disk
Total
�5/2M�1/6
BH, 8 Mgas, 9 R�3/20,100
Bars w/in Bars(Shlosman et al. 1989)
“It’s Bars all the Way Down ...”
(PFH & Quataert 2010)
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Derive ‘Instability’ Rate:
M � 10 M� yr�1� Disk
Total
�5/2M�1/6
BH, 8 Mgas, 9 R�3/20,100
Bars w/in Bars(Shlosman et al. 1989)
“It’s Bars all the Way Down ...”
More accurately ...
“It’s Non-axisymmetric Features all the Way Down ...”
(PFH & Quataert 2010)
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ESA
Step 2: Stellar Feedback & the ISM
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ESA
Step 2: Stellar Feedback & the ISM
Ø High-resolution (~1pc), molecular cooling (<100 K), SF only at highest densities (nH>1000 cm-3)
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ESA
Step 2: Stellar Feedback & the ISM
Ø High-resolution (~1pc), molecular cooling (<100 K), SF only at highest densities (nH>1000 cm-3)
Ø Heating:Ø SNe (II & Ia)Ø Stellar WindsØ Photoionization (HII Regions)
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ESA
Step 2: Stellar Feedback & the ISM
Ø High-resolution (~1pc), molecular cooling (<100 K), SF only at highest densities (nH>1000 cm-3)
Ø Heating:Ø SNe (II & Ia)Ø Stellar WindsØ Photoionization (HII Regions)
Ø Explicit Momentum Flux:Ø Radiation Pressure
Ø SNe
Ø Stellar Winds
Prad ⇠ L
c(1 + �IR)
PSNe ⇠ ESNe v�1ejecta
PW ⇠ M vwind
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ESA
Step 2: Stellar Feedback & the ISM
Ø High-resolution (~1pc), molecular cooling (<100 K), SF only at highest densities (nH>1000 cm-3)
Ø Heating:Ø SNe (II & Ia)Ø Stellar WindsØ Photoionization (HII Regions)
Ø Explicit Momentum Flux:Ø Radiation Pressure
Ø SNe
Ø Stellar Winds
Prad ⇠ L
c(1 + �IR)
PSNe ⇠ ESNe v�1ejecta
PW ⇠ M vwind
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With QuasarFeedback
No Quasar Feedback
Springel et al. 2005
Do we still need ‘Quasar Mode’ Feedback?
100
10
1
0.1
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With QuasarFeedback
No Quasar Feedback
Springel et al. 2005
Do we still need ‘Quasar Mode’ Feedback?
100
10
1
0.1
Stellar Feedback, No Quasar
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ESA
Step 3: Physical Sources of AGN Feedback
mechanical (jets & winds) & radiative
• Jets• heat IGM/ICM (low ρ), but not dense ISM
• Winds• BAL-QSO winds✓ equatorial
✓ Ṗ up to ~ 5L/c (Arav+)
• Photons• UV: Ṗ ~ L/c (absorbed by dust): κUV ~ 103 cm2 g-1 ~ 103 e scatt
• FIR: Ṗ ~ τL/c (τ ~ dust FIR optical depth ~ 10-100): κFIR ~10 e scatt
• Compton Heating (only low density gas)
• Outstanding Problem: Which Dominates?• Physics very difft for ISM & IGM
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ESA
BAL Winds as a Quasar Feedback Mechanism
R
z
z
Proga et al. 00-07; Kurosawa et al. 08-11
Ø L/LEdd >~ 0.1Ø Covering factor ~10-30%
Ø ~12 (16) objects now, 10/12 confirmed:
Lwind & 0.01LAGN
Mwind v & LAGN/c
Ø Launched at < pc
Mlaunch ⇠ MBH
vlaunch ⇠ 30, 000 km/s
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BAL Winds on ~1pc - 1kpc scales:
Mlaunch(0.1 pc) = 0.5 MBH
vlaunch(0.1 pc) = 10, 000 km/s
No BAL Winds With BAL Winds
PFH in prepWada et al.
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BAL Winds as a Quasar Feedback MechanismSILK & REES 1998, MURRAY ET AL. 2005, MANY MORE
Lc
>GMMg
r2
Momentum Flux:
L
c& Fgrav ⇠ GM Mg
r2
Lmax / MBH / �4Shut Down Accretion When:
if momentum flux ~ few L/c, predicts normalization of M-s
MBH ⇠ 108 M�
⇣ �
200 km/s
⌘4
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BAL Winds on Galactic ScalesCAN IT REALLY AFFECT STAR FORMATION?
Debuhr, Ma, Quataert 2010,11
Only Long-Range Feedback
with BAL winds
Ø Recover M-sØ Normalization ~ (efficiency)-1
Ø Launch ~1000 km/s “tail” in winds
Ø Suppress SFR
Novak et al. 2010,11
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SummaryØ Quasar feedback is here to stay
• BAL Winds + Jets + Radiation Pressure on Dust + ??? = ???
Ø Strong arguments that this regulates BH Mass: Sets MBH-s • Less clear how it impacts the galaxy• BUT, depletion times ~1 Myr are hard to ignore!
Ø Inflows: “Stuff within Stuff”: Cascade of instabilities with diverse morphology• Nuclear starbursts & powering of SMGs & ULIRGs• Determines structure & kinematics of elliptical galaxies
Ø Outflows: Towards a Predictive Modell BAL Winds:
• CAN explain MBH-s• WILL suppress SFRs • SHOULD heat & clear IGM & Proto-Group Environments
l (Quasar) Jets:• WHEN PRESENT, probably even stronger effects• Probably jet-driven winds, not “direct” jet heating
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