the role of feedbackin galaxy formation models

rachel somerville (STScI/JHU)rachel somerville (STScI/JHU)

feedback1 information about reactions to a

product, a person's performance of a task, etc., used as a basis for improvement.

2 the modification or control of a process or system by its results or effects, e.g., in a biochemical pathway or behavioral response.

feedback1 information about reactions to a

product, a person's performance of a task, etc., used as a basis for improvement.

2 the modification or control of a process or system by its results or effects, e.g., in a biochemical pathway or behavioral response.

types of feedbacktypes of feedback

thermal: add heat to gas kinetic: move gas around radiative: destroy molecular

clouds, ionize neutral gas

thermal: add heat to gas kinetic: move gas around radiative: destroy molecular

clouds, ionize neutral gas

here, i will discuss only thermal & kinetic feedback from Type II SNae and accreting black holes

feedback invoked to solvefeedback invoked to solve

overcooling/overmassive galaxy problem

massive galaxy quenching problem overabundance of low-mass galaxies

(slope of MF/LF); satellite problem ‘global’ and ‘local’ angular momentum

problems cooling flow problem/entropy floors in

galaxy clusters strong correlation of black hole mass

and galaxy properties

overcooling/overmassive galaxy problem

massive galaxy quenching problem overabundance of low-mass galaxies

(slope of MF/LF); satellite problem ‘global’ and ‘local’ angular momentum

problems cooling flow problem/entropy floors in

galaxy clusters strong correlation of black hole mass

and galaxy properties

empirical mapping between halo mass & stellar mass

empirical mapping between halo mass & stellar mass

Moster, rss et al. 2009

stellar masses of cluster galaxies (Lin & Mohr 2004)

Milky Way(Klypin, Zhao & rss 2003)

special scaleMh~1012 Msun

fraction ofhalo baryonsin stars

also matchesgalaxy

clusteringas fcn of

stellar mass

z=5.7 (t=1.0 Gyr)z=5.7 (t=1.0 Gyr)

z=1.4 (t=4.7 Gyr)z=1.4 (t=4.7 Gyr)

z=0 (t=13.6 Gyr)z=0 (t=13.6 Gyr)

Springel et al. 2006Springel et al. 2006 Wechsler et al. 2002

shock heating & atomic cooling

photoionization squelching

merging star formation

(quiescent & burst) SN heating & SN-

driven winds chemical evolution stellar populations &

dust

shock heating & atomic cooling

photoionization squelching

merging star formation

(quiescent & burst) SN heating & SN-

driven winds chemical evolution stellar populations &

dust

e.g. White & Frenk 1991Kauffmann et al. 1993Somerville & Primack 1999Cole et al. 1994; 2000

outflow rate ~ few times SFRvW ~200-800 km/s(e.g. Martin 1999, 2005)

implementing supernova feedback

implementing supernova feedback

thermal energy from Type II SNae dumped into gas; cooling/hydro forces often switched off for some time after injection (e.g. Thacker & Couchman 2000)

large-scale winds sometimes put in by hand (e.g. “constant velocity” or “momentum driven” winds (Springel & Hernquist 2003; Oppenheimer & Dave’ 2006)

thermal energy from Type II SNae dumped into gas; cooling/hydro forces often switched off for some time after injection (e.g. Thacker & Couchman 2000)

large-scale winds sometimes put in by hand (e.g. “constant velocity” or “momentum driven” winds (Springel & Hernquist 2003; Oppenheimer & Dave’ 2006)

in hydro simulations

supernova feedbacksupernova feedbackdmrh/dt = (Vc) dm

*/dt

(Vc) = SN (V0/Vc)

typically = 2 (“energy driven”)

gas may be ejected from halo (e.g., if Vc>Vthresh)

gas may re-enter halo on e.g. mass doubling timescale

dmrh/dt = (Vc) dm*/dt

(Vc) = SN (V0/Vc)

typically = 2 (“energy driven”)

gas may be ejected from halo (e.g., if Vc>Vthresh)

gas may re-enter halo on e.g. mass doubling timescale

in SAMs...

e.g. Kauffmann, White & Guiderdoni 1993; rss & Primack 1999

AGN feedback: ‘quasar mode’AGN feedback: ‘quasar mode’

observational signatures: X-ray bright, UV/IR excess, broad emission lines, high-ionization narrow lines

radiatively efficient rare and short-lived high accretion rates (0.1-1 LEdd),

fueled by cold gas via thin accretion disk

triggered/fed by mergers or secular (bar) instabilities?

may drive winds that can shut off further accretion onto the BH and sweep the cold gas out of the galaxy

observational signatures: X-ray bright, UV/IR excess, broad emission lines, high-ionization narrow lines

radiatively efficient rare and short-lived high accretion rates (0.1-1 LEdd),

fueled by cold gas via thin accretion disk

triggered/fed by mergers or secular (bar) instabilities?

may drive winds that can shut off further accretion onto the BH and sweep the cold gas out of the galaxy

Hydrodynamic simulations of galaxy mergers including black hole growth and feedback

di Matteo, Springel & Hernquist 2005

self-regulated BH growth, reproducing MBH- relation (di Matteo et al. 2004)

AGN-driven wind removes nearly all cold gas at the end of the merger, leading to lower SFR and redder colors in the spheroidal remnant (Springel et al. 2004)

characteristic AGN ‘lightcurve’ (Hopkins et al. 2006)

self-regulated BH growth, reproducing MBH- relation (di Matteo et al. 2004)

AGN-driven wind removes nearly all cold gas at the end of the merger, leading to lower SFR and redder colors in the spheroidal remnant (Springel et al. 2004)

characteristic AGN ‘lightcurve’ (Hopkins et al. 2006)

momentum-driven winds:galactic outflows

momentum-driven winds:galactic outflows

€

wind EBH

c= Moutvesc

€

EBH = ηdmacc

dtc 2

€

dMout

dt= εwindη

c

vesc

dmacc

dt

from hydrodynamic simulations of galaxy mergers (Springel, di Matteo & Hernquist; Hopkins et al.)rss et al. 2008

condition for halting accretion: sufficient injection of momentum within a dynamical time near the sphere of influence of the BH

deeper potential well requires a more massive BH to shut off accretion

condition for halting accretion: sufficient injection of momentum within a dynamical time near the sphere of influence of the BH

deeper potential well requires a more massive BH to shut off accretion

€

˙ p Δt ∝ MBH2 /σ 3 ∝m*σ

→ MBH ∝m*1/ 2σ 2

Hopkins et al. 2007 astro-ph/0701351

self-regulated BH growthself-regulated BH growth

€

tdyn ∝ RBH /σ ∝ MBH /σ 3

observed “black hole fundamentalplane”

gas rich progenitors dissipate energy and produce more compact remnants (Dekel & Cox 2005; Cox et al. 2006; Robertson et al. 2006)

deeper potential well requires a more massive BH to shut off accretion

higher gas fraction --> more compact remnant --> more massive BH (‘BH fundamental plane’)

gas rich progenitors dissipate energy and produce more compact remnants (Dekel & Cox 2005; Cox et al. 2006; Robertson et al. 2006)

deeper potential well requires a more massive BH to shut off accretion

higher gas fraction --> more compact remnant --> more massive BH (‘BH fundamental plane’) Hopkins et al. 2007a,b, 2008

consequences of self-regulated BH growthconsequences of self-regulated BH growth

gas fraction

AGN feedback: ‘radio mode’

AGN feedback: ‘radio mode’

observational signatures: radio emission/jets, bubbles in X-ray images

radiatively inefficient common in massive galaxies,

especially in groups/clusters low accretion rates (low Eddington

ratio, <10-3 Bondi accretion or ADAF?)

fueled by ‘drizzles’ of gas from hot halo?

jets may heat surrounding hot gas, offsetting or quenching cooling flow

observational signatures: radio emission/jets, bubbles in X-ray images

radiatively inefficient common in massive galaxies,

especially in groups/clusters low accretion rates (low Eddington

ratio, <10-3 Bondi accretion or ADAF?)

fueled by ‘drizzles’ of gas from hot halo?

jets may heat surrounding hot gas, offsetting or quenching cooling flow

radio jets and hot bubbles

radio jets and hot bubbles

Allen et al. 2006; see also Birzan et al. 2004

• bubbles seen in ~70% of “cooling flow” clusters (Dunn & Fabian 2006) • can estimate jet powerusing PdV argument• total heating rate may be ~x10 higher (Binney & Omma 2007)

assume radio mode powered by Bondi accretion from hot halo (Nulsen & Fabian 2000)

energy offsets cooling in “hot mode” halos

required heating rates consistent with observational constraints

assume radio mode powered by Bondi accretion from hot halo (Nulsen & Fabian 2000)

energy offsets cooling in “hot mode” halos

required heating rates consistent with observational constraints

“radio mode” heatingenergy budget “radio mode” heatingenergy budget

Allen et al. & Rafferty et al. groups & clusters; Best et al. study

rss et al. 2008

halos with primarily “cold” vs. “hot” flows separated by a critical mass of few x 1012 Msun at low redshift (e.g. Birnboim & Dekel 2003; Keres et al. 2004; 2008);

typical to assume heating processes only effective when a quasi-static hot gas halo is present (i.e. in large mass halos)

halos with primarily “cold” vs. “hot” flows separated by a critical mass of few x 1012 Msun at low redshift (e.g. Birnboim & Dekel 2003; Keres et al. 2004; 2008);

typical to assume heating processes only effective when a quasi-static hot gas halo is present (i.e. in large mass halos)

hot vs. cold flowshot vs. cold flows

Dekel & Birnboim 2006

redshift dependence of dominant gas accretion mode

redshift dependence of dominant gas accretion mode

Ocvirk et al. 2007

more difficult to quench massive galaxies at highredshift (Dekel & Birnboim 2006)

top-level halos start with a ~100 Msun seed

BH mergers trigger bursts of star formation

and accretion onto BH; based on hydrodynamical merger simulations (Cox et al., Robertson et al.)

following a merger, BH accrete at Eddington until they reach ‘critical mass’, then enter ‘blowout’ (power-law decline) phase (Hopkins et al. lightcurves)

energy released by accretion drives a wind BH merge when their galaxies merge; mass

is conserved ‘Bondi’ accretion mode fed by hot halo gas

top-level halos start with a ~100 Msun seed

BH mergers trigger bursts of star formation

and accretion onto BH; based on hydrodynamical merger simulations (Cox et al., Robertson et al.)

following a merger, BH accrete at Eddington until they reach ‘critical mass’, then enter ‘blowout’ (power-law decline) phase (Hopkins et al. lightcurves)

energy released by accretion drives a wind BH merge when their galaxies merge; mass

is conserved ‘Bondi’ accretion mode fed by hot halo gas

model for the co-evolution of galaxies, black holes, and AGN

rss, Hopkins, Cox, Robertson & Hernquist 2008

rss, Hopkins, Cox, Robertson & Hernquist 2008

importance of different FB modes is mass-dependent: SN-driven winds remove baryons from small-mass halos some process(es) prevent cooling in large-mass halos (radio

jets, clumps, conduction, cosmic ray pressure?)

importance of different FB modes is mass-dependent: SN-driven winds remove baryons from small-mass halos some process(es) prevent cooling in large-mass halos (radio

jets, clumps, conduction, cosmic ray pressure?)

z=0

quenching of massive galaxies

(note the slope is wrong for low mass galaxies.this is not due to AGN FB, & cannot be easily solved by ‘tweaking’)

rss, Hopkins, Cox, Robertson & Hernquist 2008

SS

FR

stellar mass

z=0

global sf history & stellar mass assembly history

global sf history & stellar mass assembly history

rss et al. 2008(updated version)

bursts

solid: MORGANAdash: Munich Mill.dot-dash: rss08

stellar mass function evolution

“raw” model predictions with convolved errors

Fontanot, de Lucia, Monaco, rss, Santini2009, MNRAS (arXiv:0901.1130)

stellar mass assemblywithout mass errors with errors (0.25 dex)

solid: MORGANAdash: Munich Mill.dot-dash: rss08

data: integrated composite MF

Fontanot et al. 2009

in models, mass in low mass galaxies evolves little; mass in high mass galaxies evolves more

data:red square: Drory et al. 2008blue: Bell et al. 2007cyan: Martin et al. 2007green: Grazian et al. 2006magenta: Noeske et al. 2007red x: Chen et al. 2008blue diamond: Dunne et al. 2008

Fontanot et al. 2009

evolution of the SF sequence

SFR from different indicators/surveys differ by up to x10

models do pretty well for massive galaxies; low-mass galaxies are too low at all z

SFR from different indicators/surveys differ by up to x10

models do pretty well for massive galaxies; low-mass galaxies are too low at all z

archeological downsizingarcheological downsizing

data: Gallazzi et al. 2007

Fontanot et al. 2009

stellar populations in low mass model galaxies are too old, downsizing is too weak

partly, but not wholly, due to biases intrinsic to age estimates from Balmer lines (see Trager & rss 2008)

stellar populations in low mass model galaxies are too old, downsizing is too weak

partly, but not wholly, due to biases intrinsic to age estimates from Balmer lines (see Trager & rss 2008)

halo mass

stellar mass

Moster, rss et al. 2009

evolution of stellar-to-halo mass relationship

evolution of stellar-to-halo mass relationship

low mass halos were less efficient at converting baryons into stars at high redshift

in SAMs, galaxies move along z=0 SMHM relation -- no evolution

SN FB more efficient at high z?

low mass halos were less efficient at converting baryons into stars at high redshift

in SAMs, galaxies move along z=0 SMHM relation -- no evolution

SN FB more efficient at high z?

multi-wavelength properties multi-wavelength properties

rss, Gilmore & Primack; Gilmore, rss & Primack (in prep)

UV-optical IR-sub-mm

Springel & Hernquist 2005Robertson et al. 2006Hopkins, rss et al. 2009

efficiency of spheroid formation in mergersefficiency of spheroid formation in mergers

usual assumption in SAMs: all mergers with mass ratio above some value (1:3-1:4) produce spheroidal remnants

simulations show: gas rich mergers are less efficient at producing starbursts and forming spheroids (& BH)

i.e. even major mergers between gas rich galaxies can produce disk-dominated remnants

usual assumption in SAMs: all mergers with mass ratio above some value (1:3-1:4) produce spheroidal remnants

simulations show: gas rich mergers are less efficient at producing starbursts and forming spheroids (& BH)

i.e. even major mergers between gas rich galaxies can produce disk-dominated remnants gas fraction

dis

k m

ass

fra

ctio

n

Hopkins et al. 2008

mass functions by typemass functions by type

standard spheroidformation recipe

new spheroid formation recipe

Hopkins, rss et al.MNRAS 2009arXiv:0901.4111

the ‘bulgeless galaxy problem’the ‘bulgeless galaxy problem’

Weinzirl et al. 2008: H-band bulge-disk decompositions of 146galaxies from the OSU Bright Spiral Galaxy Surveylog (m*/msun)>10; B/T<0.75

old spheroid model new model

Weinzirl et al. data

stellar massH-band

why does it work?why does it work?gas fractionin mergerprogenitors

radio modequenching

time since Big Bang

bulge mass vs. bh massbulge mass vs. bh mass

rss et al. 2008

BH were more massive relativeto their spheroids in the past

• ‘old’ model still peaks at too high a redshift• ‘new’ spheroid model does pretty well

BH accretion history

rss et al. in prep

spheroid potential tells BH how much it can grow

gas cools to rotation supported disk

hot halo?yes no gas accretion mode depends

on DM halo mass and redshift

BH mass determines how much galaxy can grow

cooling continuesstays quenched

mergers drive starburst and accretion onto SMBH; leave behind spheroidal remnant

summarysummary current models rely on gas ejection by SN-

driven winds to achieve small baryon fractions in low mass halos. however, current FB recipes do not reproduce SF histories of low-mass galaxies.

“radio mode” AGN feedback seems to be a promising mechanism for stopping cooling in massive halos -- but many details remain to be worked out.

AGN driven winds may be responsible for regulating BH growth and imprinting the BH mass-galaxy scaling relations. direct effect on galaxy properties is minor.

current models rely on gas ejection by SN-driven winds to achieve small baryon fractions in low mass halos. however, current FB recipes do not reproduce SF histories of low-mass galaxies.

“radio mode” AGN feedback seems to be a promising mechanism for stopping cooling in massive halos -- but many details remain to be worked out.

AGN driven winds may be responsible for regulating BH growth and imprinting the BH mass-galaxy scaling relations. direct effect on galaxy properties is minor.

summarysummary observed mass assembly history and

SFR history reproduced (w/in observational errors) for massive galaxies (M*>few 1010 Msun)

low mass galaxies form too early, are too passive at all redshifts (z<2), and have stellar pops that are too old at z~0

may indicate that modelling of SN FB in current models needs to be modified

possible dearth of both very rapidly SF galaxies and quenched galaxies at z~2

latest models still fail to reproduce enough bright SMGs

observed mass assembly history and SFR history reproduced (w/in observational errors) for massive galaxies (M*>few 1010 Msun)

low mass galaxies form too early, are too passive at all redshifts (z<2), and have stellar pops that are too old at z~0

may indicate that modelling of SN FB in current models needs to be modified

possible dearth of both very rapidly SF galaxies and quenched galaxies at z~2

latest models still fail to reproduce enough bright SMGs

Devriendt, Guiderdoni & Sadat 1999

emission from starsemission from stars

models predict distribution of stellar ages and metallicities in each galaxy

convolve with ‘simple stellar population’ (SSP) models

models predict distribution of stellar ages and metallicities in each galaxy

convolve with ‘simple stellar population’ (SSP) models

modeling dust absorption and emission

modeling dust absorption and emission

full (3D) radiative transfer in post-processing (refs)

full radiative transfer applied within simplied geometries

analytic recipes for dust absorption, templates for dust emission

full (3D) radiative transfer in post-processing (refs)

full radiative transfer applied within simplied geometries

analytic recipes for dust absorption, templates for dust emission

dust absorptiondust absorption

optical depth of ‘cirrus’ dust proportional

to column density of metals in disk HI ~ Zgas NH

stars and dust assumed uniformly mixed in a ‘slab’

two-component model:diffuse ‘cirrus’dense ‘birthclouds’

optical depth of ‘birthclouds’ proportional to HI

stars within birthclouds enshrouded within a ‘screen’ of duststars are freed from birthclouds on timescale ~107 yr

Charlot & Fall 2000; de Lucia & Blaizot 2007; etc

dust emissiondust emission

energy emitted = energy absorbed

empirical template emission spectra: Ldustdetermines shape of emission spectrum (ratio of warm/cold dust)

Sanders & Mirabel ; Devriendt &Guiderdoni; Chary & Elbaz;

improved dust emission templates from spitzer irsimproved dust emission

templates from spitzer irs

Rieke et al. 2009

check of methodcheck of method

Fontanot, rss et al. 2009

Fontanot, rss & Silva in prep

for most statistical quantities (such as LF and counts), the analytic dust recipe gives similar results to full RT with GRASIL!

lum

i nos

it y d

ens i

t y

log wavelengthredshift

The Bolometric Luminosity History of the Universe

Gilmore, Madau, Primack, rss & Haardt 2009, MN in press“GeV gamma-ray attenuation and the high-redshift UV background”

rss, Gilmore & Primack in prep“Panchromatic Galaxy Properties in Hierarchical Models”

Gilmore, rss & Primack in prep“The Extragalactic Background Light and Implications for Gamma-ray Spectra”

the next set of slides are taken from work with UCSC graduate student Rudy Gilmore & Joel Primack:

luminosity densityluminosity density

z=0

luminosity density evolutionluminosity density evolution

z=0z=0.5z=1.0z=1.5z=2.0z=2.5

extragalactic background lightextragalactic background light

multi-wavelength counts:UV and optical

multi-wavelength counts:UV and optical

FUV

NUV

multi-wavelength counts: IRmulti-wavelength counts: IR

multi-wavelength counts: sub-mm

multi-wavelength counts: sub-mm

star formation rate density as function of galaxy mass

green: GOODS; blue: Zheng et al. (COMBO-17)red: Conselice et al.; cyan: Mobasher et al. 2008

solid: MORGANAdash: Munich Mill.dot-dash: rss08

Fontanot et al. 2009

agrees for low mass galaxies by accident (too many, but SF too low)

agrees for low mass galaxies by accident (too many, but SF too low)

Baugh et al. 2005

Baugh et al. (2005) invoked a model with an extreme top-heavyIMF in merger-triggered bursts in order to solve the problem withunderproduction of SMGs in their models...

observations:Sanders et al. 2003Le Floch et al. 2005Caputi et al. 2007

Lacey et al. (2008) argued that the same model with a top-heavyIMF in bursts was favored by Spitzer observations

z=5.7 (t=1.0 Gyr)z=5.7 (t=1.0 Gyr)

z=1.4 (t=4.7 Gyr)z=1.4 (t=4.7 Gyr)

z=0 (t=13.6 Gyr)z=0 (t=13.6 Gyr)

dark matter ‘halos’

‘merger tree’

N-body simulation

8.5 < log m* < 9.59.5 < log m* < 10.510.5 < log m* < 11.511.5 < log m* < 12.5

standard model new model

distribution of B/Tdistribution of B/T

black hole and galaxy seem to ‘know about’ each otherblack hole and galaxy seem to ‘know about’ each other

BH mass correlates with spheroid: velocity dispersion mass/luminosity inner light profile

remarkably small scatter

BH mass correlates with spheroid: velocity dispersion mass/luminosity inner light profile

remarkably small scatter

Gultekin et al. 2009

Kormendy & Richstone 1995;Magorrian et al. 1998; Ferrarese & Merritt 2000; Gebhardt et al. 2000; Marconi & Hunt 2004Haring & Rix 2004; Graham et al. 2001; Kormendy & Bender 2009

spheroid velocity dispersion

blac

k ho

le m

ass

The Angular Momentum CatastropheThe Angular Momentum Catastrophe

Navarro & Steinmetz 2000

halos

real g

alaxies

real g

alaxies

hydrospec

ific

ang

ular

mom

entu

m

rotation velocity

but see Governato et al. 2008, 2009

van den Bosch & Burkert 2001

comparison of theoretical angular momentum profiles j(r) with observed dark matter dominated dwarf galaxies

theory predicts too much large j and too much small j material

comparison of theoretical angular momentum profiles j(r) with observed dark matter dominated dwarf galaxies

theory predicts too much large j and too much small j material

the ‘local’ angular momentum problem

the ‘local’ angular momentum problem

see also Bullock et al. 2001

simulations of ‘radio mode’ heating

simulations of ‘radio mode’ heating

intermittent jet with a duty cycle of ~107 yr

leads to efficient heating of a large fraction of the cluster gas (Ruszkowski et al. 2004)

combination of sound waves, weak shocks and bubble interface

heating rate able to balance radiative cooling for reasonable input luminosities

intermittent jet with a duty cycle of ~107 yr

leads to efficient heating of a large fraction of the cluster gas (Ruszkowski et al. 2004)

combination of sound waves, weak shocks and bubble interface

heating rate able to balance radiative cooling for reasonable input luminosities

Bruggen, Ruszkowski & Hallen 2005see also Reynolds et al. (2002; 2005)Vernaleo & Reynolds (2006, 2007)Sijacki & Springel 2005; Sijacki et al. 2007

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