M87 interaction between a SMBH and gas rich atmosphereShocks, Buoyant plasma bubbles, Jet, Cavities, Filaments

Outbursts from Supermassive Black Holes Forman, Churazov, Jones, Bohringer, Begelman, Owen,

Eilek, Nulsen, Vihlinin, Markevitch, Heinz, Kraft

Unambiguous signature of an AGN triggered shockOutburst energyOutburst durationEnergy channels for heating

Cool X-ray filamentary structureClear evidence for bubbles

•Outbursts from galaxies to (M87 to) rich clusters

•Outbursts range from 1055 < ∆E < 1062 ergs

•See growth of SMBHs - ∆MSMBH ∝ ∆ EOUTBURST / c2

•∆MSMBH up to 3x108 solar masses per outburst

2

Hot X-ray emitting atmospheres - “fossil record” of SMBM activity •Observe outburst frequency •Measure total power - mechanical vs. radiative (cavities)•Understand interaction of outburst with surroundings•Insight into high redshift, early universe •Growth/formation of galaxies•Growth of SMBH

SMBH and Parent Galaxy

Mbulge-M

M -

Magorrian et al.Gebhart et al.Ferrarese & Merritt

M

MVelocity Dispersion

MBulge

3

Millenium Run + Semi-analytic Galaxy Evolution

•1010 particles of 109 Msun

• extract merger trees of dark matter halos from z=20 to z=0

•z=0 dark matter •z=0 light

Croton et al. 2006

Croton et al. 2006“The many lives of active galactic nuclei: cooling flows, black holes and the luminosities and colours of galaxies”

4

Millenium Run + Semi-analytic Galaxy EvolutionCroton et al. 2006

For massive galaxies/halos, AGN feedback into hot coronae is long-lived phase

Study this long-lived phase of outbursts and feedback into the hot coronae

Rapid Cooling

Hot Halo

Massive halos/galaxies •Form hot gas coronae at early times•Growth/merging continues with little star formation•Oldest systems become “red and dead” - but still growing via mergers•AGN heating is key•Downsizing - more massive galaxies end star formation at higher z; appears “anti-hierarchical”

5

Setting the stage Family of increasing mass, temperature, and luminosity

E/S0 Galaxies Groups Clusters

Lx (ergs/sec) 1040-42 1042-43 1043-46

Gas Temp 0.5-1.0 keV 1-3 keV 2-15 keV

Mgas/Mstellar 0.02 1 5

6

Hot gas seen ONLY in X-ray band - thermal bremsstrahlung + lines

•Gas provides a fossil record of mass ejections and energy outbursts•For clusters, 16% of mass is luminous baryons (mostly hot gas)

•Measure heavy element enrichment - history of star formation

•See reflections of energy outbursts in cavities over cosmic times

Setting the stage Family of increasing mass, temperature, and luminosity

7

Cooling Flows

• Cowie & Binney (1977) Fabian & Nulsen (1977) “Cooling gas in the cores of clusters can accrete at significant rates onto slow-moving central galaxies”

• Strong surface brightness peak dense gas short cooling time

• Hot gas radiates – gas must cool unless reheated, then compressed by ICM

• Mass Deposition rates are large (100 -1000 M/yr) - more than 50%

• But large amounts of cool gas were not detected

• Emission lines from cooling gas NOT SEEN byXMM-NEWTON OGS (cool gas only 10% of prediction) (e.g., Peterson et al. 2001, 2002; Peterson & Fabian 2005)

Allen/Fabian

Virgo Cluster - X-ray/Optical

1’=4.65 kpc; 2o=0.5 Mpc Central galaxy in Virgo cluster D=16 Mpc

•3x109Msun supermassive black hole•Spectacular jet (e.g. Marshall et al.)•Nearby (16 Mpc; 1’=4.5 kpc, 1”=75 pc)•Classic cooling flow (24 Msun/yr)•Ideal system to study SMBH/gas interaction

Chandra-XMM-VLA View• Two X-ray “arms”

• X-ray (thermal gas) and radio (relativistic plasma) “related”

• Eastern arm - classical buoyant bubble with torus (Churazov et al 2001) – XMM-Newton shows cool arms of uplifted gas (Belsole

et al 2001; Molendi 2002)

• Southwestern arm - less direct relationship - radio envelops gas

M87

Chandra-XMM-VLA View

M87

Churazov et al. 2001

Density and Pressure Maps

Central Piston Shock Filamentary arms

Gas Pressure (3.5-7.5 keV)

Gas Density (1.2-2.5keV)

12

Shock

Bubble

ICM

ICM

Schematic

Central Region of M87 - the driving force

• Nucleus, jet (knots)• Cavities surrounding the jet and the (unseen)

counterjet• Bubble breaking from counter jet cavity

– Perpendicular to jet axis; – Radius ~1kpc. – Formation time ~4 x106 years

• Piston driving shock• X-ray rim is low entropy gas

uplifted/displaced by relativistic plasma

6 cm

6cm VLA

SMBH 3x109Msun

Shock Model I - the dataHard (3.5-7.5 keV) pressure soft (1.2-2.5 keV) density profiles

Projected Deprojected

Deprojected Gas Temperature

Rarefaction

Shock

No hot shocked region interior to shock

Consistent density and temperature jumps

T2/T1= 1.19

M~1.2yield same Mach number: (MT=1.20 Μρ.24)

Rankine-Hugoniot Shock Jump Conditions

€

ρ2 /ρ1 =γ +1( )M 2

γ +1( ) + γ −1( ) M 2 −1( )

€

ρ2 /ρ1 =1.34

€

T2 /T1 =γ +1( ) + 2γ M 2 −1( )[ ] γ +1( ) + γ −1( ) M 2 −1( )[ ]

γ +1( )2M 2

Outburst Energy

Series of models with varying initial outburst energy2, 5, 10, 20 x 1057 ergs

Match to dataE = 5 x 10 57 ergsDetermined by jumps

Fast - large shock heated region

Absence sets outburst duration 2-5 million yrs

Slow - cool rim

Shock-heated gas if τoutburst is too short Absence of hot region limits duration of outburst

Must be longer than 2 million years

Derive outburst timescale

19

Fast/Slow Cartoon

Fast

Fast SlowRadio Lobes

Radio bright

X-ray dim

Small Large

Shock heated gas

Radio dim

X-ray dim

Yes No

Cool rims No Yes

Rarefaction region Yes Yes

Outer shock Yes Yes

Slow

RadioLobes

RadioLobes

Hot, dim

Cool, bright

20

Where does the energy go ?

Sedov Slow (2-5 Myr)Slow (2-5 Myr)

Kinetic energy in the shock

~6x1056 ergs

(11%)

~6x1056 ergs

(11%)

Will be carried away

~12x1056 ergs (22%)

~12x1056 ergs

(22%)

Enthalpy of the central bubble

~1.7x1056 ergs (3.4%)

~2.3-3.7x1057

ergs (46%-64%)

Heating 100-22=78% >100-22=78%

(eventually)

Sequence of buoyant bubbles Many small bubbles (comparable to “bud”)

Effervecent heating - Begelman•PV ~ 1054 - 1055 ergs τrise ~ 107 yearsArms - resolved

Eastern arm - classical buoyant bubbleSouthwestern arm - overpressured and “fine” (~100pc, like bubble rims) - limit bulk gas velocities in core

4.65 kpc

90 cm (Owen et al.)

1.2-2.5 keV

M87

Soft Filamentary Web

22

Organized and Disorganized

4.65 kpc

Ruszkowski/BegelmanSimulation for Perseus

Both large scale bubblesAND

Small scale chaotic bubbles

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are needed to see this picture.

QuickTime™ and aYUV420 codec decompressor

are needed to see this picture.

Radio (blue) Chandra X-ray (red)

M87 shocks and bubbles contribute to heatingBoth naturally arise from AGN outburstsShock carries away ≤ 20-25% of energy75% of outburst available to heat (eventually)

Filaments Cool thermal rims of bubbles Southwestern arm - interaction with radio plasmaShock (and trailing rarefaction region) R, jump in T or ρ => Total deposited energy 5x1057 erg Lobes and shock radius => Age ≈ 14x106 yrCool/bright rims => “slow” energy deposition 2-5x106 yearsAverage energy release: few x 1043 erg/s ≈ Cooling losses Dunn et al. - 55 cluster sample, 20 have τ<3x109 yrs and 75% show bubblesRafferty - 33 clusters; 50% withbubbles and sufficient energy to quench cooling

Pre-Einstein early type galaxies •Gas free - Stellar mass loss removed by SN driven winds.

Einstein Observatory images showed extended, hot coronae:•~1 keV temperatures; masses to 1010 M , •Strong correlation of LX and LB but much scatter.

(e.g. Forman et al. 1979, 1985, Canizares et al. 1987)•High central gas densities => short cooling times •Accretion rates of 0.02-3 Msun/year (Nulsen et al. 1984, Thomas et al. 1986 )

Hot Gas in Early-type Galaxies - The Einstein Era

A Chandra survey of ~160 early type galaxies to measure outburst energy, age, frequency, plus diffuse/gas luminosity

and nuclear emission (Jones et al.)

Study hot gas - as a function M, velocity dispersion, ….Measure cavities - determine outburst energies (PV) and timescalesDerive nuclear luminosities - correlate with gas density

Chandra resolution required!

In luminous ellipticals, most of the X-ray emission is from hot gas, In fainter systems, emission from LMXBs makes nearly all of the

“diffuse” emission

Gas dominates “diffuse” emission

Correlation of Lx with L

and Land

Mostly unresolved LMXB’s (hard specta)

Galaxies with little hot ISM

Exploding Elliptical -NGC4636

•Strange X-ray structure in an otherwise normal Virgo elliptical galaxy•Double pin wheel-like structure in X-rays! X-ray arms ~8 kpc long.•Nuclear outburst 3 x 106 years ago with energy 6 x 1056 ergs•But small weak radio source

Jones et al 2001

29

Bubbles in a galaxy -- M84

For Perseus, M87, M84, and for almost all others

Gas surrounding bubble is cool

Usually no shock heating in lobe H-shaped gas has

kT~ 0.6 keV

Ambient gas temperature increases from 0.6 to 0.8 keV with increasing radius

.

Lobes ~ 4 kpc diameter

outburst ~ 4 - 6 x 106 yrs ago

Interaction with radio lobes of 3C272.1

Tail to south & northern lobe compression

motion of M84 to the north

X-ray Radio

Galaxy rims are (generally) cool (like cluster) - no shocksBubbles (seen as cavities) gently uplift and impart energy to the gas

NGC4636

3 106 years

2 106 years5 106 years

107 years

NGC5846

5 106 years

3 106 years

5 107 years

NGC507

Galaxies with diffuse gas

How Common are AGN Outbursts in Galaxies?Determine fraction of Galaxies with Cavities

Galaxies with cavities

In luminous ellipticals (including some poor groups), 30% have cavities

In galaxies, outbursts are recent (=> frequent) and

impart significant energy to the ISM

AGE of outbursts

Ages and outburst energy for the 27 systems with cavities

PV (ergs)1053 1055 1057 1059

•X-ray emission detected from the nucleus for ~80% of early-type galaxies

Nuclear activity - “AGN”Determine fraction with nuclear X-ray emission

In “normal” early-typegalaxies

ConclusionsEnergy input from AGN is common in galaxies- reheats cooling gas, drives gas from their halos,

and is important for galaxy evolution

In luminous ellipticals, ~30% have cavities => recent outbursts

- typical ages are 3x106 to 6x107 years

- typical outburst energies (estimated from cavity sizes) are 1055 - 1058 ergs

~80% of all early type galaxies have weak X-ray “AGN”

35

Hydra A (Nulsen et al 2005)

Small cavities in core, medium cavities and a shock Shock front 200-300 kpc from AGN

Shock energy 1061 ergs -- 1.4 X 108 years since outburst

Hydra A (Nulsen et al 2005)

Chandra radio contours on X-ray

Small cavities in core , medium cavities and a shock Shock front 200-300 kpc from AGN

Shock energy 1061 ergs -- 1.4 X 108 years since outburst

Cluster Scale Outbursts MSO735.6+7421 6 X 1061 ergs driving shock

(McNamara et al 2005)

Cluster Lx = 1045 ergs/sec z=0.22X-ray bright region - edge of radio cocoon lies at location of shockRadio lobes fill cavities (200 kpc diam) - displace and compress X-ray gas Work to inflate each cavity ~1061 ergs; age of shock 1 X 108 years Average power 1.7 X 1046 ergs/sec

Growth of SMBH by accretion in “old” stellar population systems(Rafferty et al. 2006 - solar mass/yr) with star formation to maintain MBH-Mbulge relation

Mechanical power balances cooling in 50% of clusters AGN outbursts deposit energy into gas through shocks and bubbles

Outbursts from Clusters to GalaxiesSOURCE SHOCK

RADIUS(kpc)

ENERGY

(1061 erg)

AGE

(My)

MEAN POWER

(1046 erg/s)

∆M

(108 Msun)

MS0735.6Hercules A

Hydra AM87

NGC4636

230160210145

5.73

0.90.0005

0.00006

10459

136143

1.71.60.2

0.00120.0007

31.70.5

0.00030.00003

€

˙ M BH ≈ 0.1−1

Impact of AGN outbursts on hot gas

•M87 outburst τ~14x106 years, τ~2-5x106 years; inflates inner region “classical shock - seen in density/temperature & rarefaction region slow expansion of “piston” (no large shock heated region)

Outburst energy matches cooling • M87 arms from buoyant bubbles; soft filamentary web; complex (magnetic field) interactions of radio plasma bubbles with ISM•Galaxy outbursts and mini AGN are common (see talk by Christine Jones) •Outbursts from galaxies to clusters 1055-1062 ergs which grow SMBH

NGC4636M87Hydra A

Impact of AGN outbursts on hot gas

NGC4636M87Hydra A

•Reheat cooling gas through shocks/buoyant bubbles in all gas rich systems i.e. those with bulges and black holes•Critical to galaxy evolution/downsizing models

•Massive galaxies are “red and dead”•Evolution continues but not (appreciable) star formation

•Hot coronae “contain” AGN feedback energy over cosmological times•X-ray observations allow study of the outbursts and exactly how energy is injected into the hot surrounding atmosphere•Critical to understanding the new view of galaxy and black hole evolution

41