the monster roars: agn feedback & co-evolution with galaxies

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The Monster Roars: AGN Feedback & Co-Evolution with Galaxies Philip Hopkins Saturday, September 14, 13

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Page 1: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

The Monster Roars:AGN Feedback & Co-Evolution with Galaxies

Philip HopkinsSaturday, September 14, 13

Page 2: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Ø (Nearly?) 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.)

Saturday, September 14, 13

Page 3: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

McConnell et al.

BHs and Bulges Co-evolve

Saturday, September 14, 13

Page 4: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Num

ber D

ensit

yProblems?

Spheroid & BH Formation Times:

Oppenheimer & Dave

Observed

No AGN FB

Marconi et al.

Ø Sharp color bimodalityØ Lowering mass of >M* galaxiesØ Removing/heating gas in groups

Saturday, September 14, 13

Page 5: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Quasar Feedback as a Means to Regulate BHsSANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE

Saturday, September 14, 13

Page 6: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Quasar Feedback as a Means to Regulate BHsSANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE

Frad ⇠ L

c⇠ MBH c

tSalpeter

Saturday, September 14, 13

Page 7: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Quasar Feedback as a Means to Regulate BHsSANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE

Fgrav ⇠ GMgal Mgas

R2gal

⇠ fgas�4

G

Frad ⇠ L

c⇠ MBH c

tSalpeter

Saturday, September 14, 13

Page 8: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Quasar Feedback as a Means to Regulate BHsSANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE

Fgrav ⇠ GMgal Mgas

R2gal

⇠ fgas�4

G

Frad ⇠ L

c⇠ MBH c

tSalpeter

Shut down accretion when: Frad & Fgrav

Saturday, September 14, 13

Page 9: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Quasar Feedback as a Means to Regulate BHsSANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE

Fgrav ⇠ GMgal Mgas

R2gal

⇠ fgas�4

G

Frad ⇠ L

c⇠ MBH c

tSalpeter

Shut down accretion when: Frad & Fgrav

MBH ⇠ fgas tSGc

�4 ⇠ 108 M�

⇣ �

200 km s�1

⌘4

Saturday, September 14, 13

Page 10: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Star Formation

BH Growth

Saturday, September 14, 13

Page 11: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Saturday, September 14, 13

Page 12: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

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

Wada et al.

Saturday, September 14, 13

Page 13: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

M-sigma Suggests Self-Regulated BH Growth

FEEDBACK PREVENTS RUNAWAY BLACK HOLE GROWTH

Di Matteo et al., PFH et al. 2005

Black hole growth

without feedback

with feedback

Saturday, September 14, 13

Page 14: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

• MBH- evolution:• Hosts more gas rich/compact at high-z more “work” for the BH before self-regulation

Size evolution of spheroid hosts

Corresponding increasein MBH/Mhost

• Doesn’t mean that BHs grew “before” their hosts PFH et al. 2006, 2007

PFH, Murray et al. 2009

Predictions?

Saturday, September 14, 13

Page 15: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

BH mass of an L* QSO

BH accretion rate (x1000)

SFR (points)

PFH, Richards, & Hernquist 2007Merloni et al. 2007

“Downsizing” in BHs and Galaxies is the same:

Co-Evolution falls out naturally:

Ø Provided self-regulation exists, average correlations are independent of fueling

Saturday, September 14, 13

Page 16: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

With AGNFeedback

No AGN Feedback

Springel et al. 2005

Helps Ensure Ellipticals are “Red and Dead” Gas Density

Gas Temperature

Saturday, September 14, 13

Page 17: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Cox et al. 2005

Feedback-Driven Winds METAL ENRICHMENT & BUILDING THE X-RAY HALO

X-Ray Emission

Saturday, September 14, 13

Page 18: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Quasar Outflows May Be Significant for the ICM & IGM

SHUT DOWN COOLING FOR ~ COUPLE GYR. PRE-HEATING?

without AGN feedback

with AGN feedback

simulated vs. observed profiles

McCarthy et al., Schaye et al. 2011

Saturday, September 14, 13

Page 19: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

AGN or Starburst-Driven Winds?WHICH ARE MORE IMPORTANT?

Halo Mass [Msun]

BHs Dominate Feedback

Stars Dominate Feedback

Saturday, September 14, 13

Page 20: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

AGN or Starburst-Driven Winds?WHICH ARE MORE IMPORTANT?

Halo Mass [Msun]

BHs Dominate Feedback

Stars Dominate Feedback

Efficient star formation

Inefficient star formation

Saturday, September 14, 13

Page 21: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

AGN or Starburst-Driven Winds?WHICH ARE MORE IMPORTANT?

Halo Mass [Msun]

BHs Dominate Feedback

Stars Dominate Feedback

Efficient star formation

Inefficient star formation

How is this inefficient star formation *maintained*?

Saturday, September 14, 13

Page 22: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Ø “Quasar” mode (high mdot)

Ø Move mass from Blue to Red?

Ø Rapid (~107 yr)

Ø Small(er) scales (~pc-kpc)

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 Hot Halos & Dry Mergers

Ø Regulates Galaxy Mass

“Transition” “Maintenance”vs.

Saturday, September 14, 13

Page 23: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Maintenance Mode IS IT ALSO “RADIO”-MODE?

• Observational constraints on the power involved are leading the way

Allen: P(jet) versus P(accretion):Ho: P(radio) versus Eddington ratio:

Saturday, September 14, 13

Page 24: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Maintenance Mode IS IT ALSO “RADIO”-MODE?

• Know that (non-cooling flow) clusters do look “pre-heated”... but we also see radio jets doing work:

• What is “typical”?

Fabian (Perseus Cluster)

Allen (X-ray Ellipticals)

Saturday, September 14, 13

Page 25: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Saturday, September 14, 13

Page 26: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Saturday, September 14, 13

Page 27: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Log(L/Lsun)

Ø Observed luminosity function: populations at different evolutionary stages

“Blowout” (Bright Mergers)

“Fading” Mergers (post-starburst spheroids)

“Seyferts” (disk-dominated, secular/minor mergers)

“Dead” Bulges (stellar wind/hot gas halo accretion)

Log(

Num

ber D

ensit

y)

Seyferts Quasars

Saturday, September 14, 13

Page 28: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Where to From Here?

Saturday, September 14, 13

Page 29: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

ESA

Step 1: Stellar Feedback & the ISM

6=multi-phase ISM with outflows

sub-grid ISM

cutting-edge analytic models

Saturday, September 14, 13

Page 30: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

ESA

Step 1: Stellar Feedback & the ISM

6=multi-phase ISM with outflows

sub-grid ISM

cutting-edge analytic models

Ø Non-linear QSO-Stellar feedback interactions matter

Saturday, September 14, 13

Page 31: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Step 2: InflowR < 0.1 pc:

~ few M⊙ yr-1

Ø Beginning to directly follow inflow to sub-pc scales

PFH & Quataert 2009,10,11Levine, Gnedin, Kravtsov 09,10Mayer, Callegari, 09,10

Saturday, September 14, 13

Page 32: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Step 2: InflowR < 0.1 pc:

~ few M⊙ yr-1

Ø Beginning to directly follow inflow to sub-pc scales

PFH & Quataert 2009,10,11Levine, Gnedin, Kravtsov 09,10Mayer, Callegari, 09,10

Ø NOT:Ø Bondi-HoyleØ Viscous (-Disk)

Saturday, September 14, 13

Page 33: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Bars w/in Bars(Shlosman et al. 1989)

“It’s Bars all the Way Down ...”

(PFH & Quataert 2010)

Saturday, September 14, 13

Page 34: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

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)

Saturday, September 14, 13

Page 35: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

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)

Saturday, September 14, 13

Page 36: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Step 3: Observed Sources of AGN Feedback

• Jets• heat IGM/ICM (low-density), but not dense ISM?

Fabian (Perseus Cluster)

Saturday, September 14, 13

Page 37: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Step 3: Observed Sources of AGN Feedback

• Jets• heat IGM/ICM (low-density), but not dense ISM

• Radiation Pressure• LAGN >> Lstars

Roth, Kasen, Quataert, PFH 2012 + in prepSaturday, September 14, 13

Page 38: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Step 3: Observed Sources of AGN Feedback

• Jets• heat IGM/ICM (low-density), but not dense ISM

• Radiation Pressure• LAGN >> Lstars

Roth, Kasen, Quataert, PFH 2012 + in prep

• Accretion Disk Winds• Broad Absorption Line Winds

Proga et al., Novak et al.

Saturday, September 14, 13

Page 39: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Saturday, September 14, 13

Page 40: The Monster Roars: AGN Feedback & Co-Evolution with Galaxies

Put all of this into a cosmological simulation, and.... (?)

Saturday, September 14, 13