rachel somerville (STScI/JHU)
description
Transcript of rachel somerville (STScI/JHU)
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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