Françoise CombesFebruary 13, 2014

AGN-driven outflows

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Perseus cooling flow

Mrk 231

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Gaibler et al 2011

Inefficient star formationBehroozi et al 2013

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MS0735.6+7421 cluster (McNamara et al. 2009)

Outline

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1- AGN feedback: cooling flows

2- SN+AGN inflow/outflow in galaxies

3- Mechanisms -- Energetics

4- ALMA and NOEMA perspectives

Very frequently, inflow and outflow occurs simultaneously -- more difficult to see the inflow

1- Gas flow in coolcore clusters

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Salomé et al 2006

Perseus A , Fabian et al 2003

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Cold CO in filaments

Salome et al 2008

Velocity much lower than free-fall

Inflow and outflow coexist

The molecular gas coming from previous cooling is dragged out by the AGN feedback

The bubbles create inhomogeneities and further cooling

The cooled gas fuels the AGN

Numerical simulations (Revaz, Combes, Salome 2007)

7Log Temperature (150kpc) Log density (25x50kpc)

Buoyant bubbles, compressionand cooling at the surfaces+Cold gas dragged upwards

Turbulence triggered by SF

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Perseus cluster simulated by Falceta-Goncalves et al 2010MHD

AGN heating reduces the cooling

OI, CII with Herschel

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Same morphology +Same spectrabetween CO(2-1) and OI

Same gas, cooling throughdifferent phases?

No rotation, but inflows

Edge et al 2010Mittal et al 2010

10Dasyra & Combes 2011, 2012

4C12.50 SFR ~400-1000 Mo/yrOutflow ~130 Mo/yr

6 out of 300systems searchedshow H2 outflows

2-Feedback in nuclei: H2 & CO

AGN-driven molecular outflows

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Mrk 231AGN and also nuclearStarburst, 107-108MoOutflow 700Mo/yr

IRAM Ferruglio et al 2010

Aalto et al 2012

high-densitymolecular tracers (HCN, HCO+HNC, HC3NCN, …

Molecular outflows: excitation

12Cicone et al 2013Search in 7 ULIRGs and QSO: 100Mo/yr outflows found in 4

In additionof several CO lines:

More excited gasIn the outflowCicone et al 2012

Spatial extension in Mrk231

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Blue wing Red wing

Cicone et al 2012

On kpc scales, affects the galaxy

dM/dt = 3v MOF/ROF ~1000 Mo/yr, while SFR ~200 Mo/yrKinetic power ~2 1044 erg/s AGN

Dense gas in the base of the outflow

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Mrk 231

Cicone et al 2013

Outflows in 4 out of 7

Relations outflow AGN, SFR

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Starburst galaxies are on the lineMass loading factor ~1For AGN-hosts, dM/dt is larger

For AGN-hosts, the outflow rateCorrelates with the AGN power

Comparison with AGN models

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dM/dt v ~20 LAGN/cCan be explained by energy-driven outflows(Zubovas & King 2012)

Lower efficiency in LinersHigher in SB

Molecular outflows are massive

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N1377

Aalto et al 2012

Some outflows are more massive thentheir dense nuclear disk, e.g. N1377 (S0)200pc extent with modest 140km/sMout= 1-5 107Mo, disk mass ~2 107 Mo

Outflows due to SN: M82, Mout ~ 5107Mo V~200km/s (Nakai et al 1987)

N3256 merger, Mout ~ 107Mo 10 Mo/yr, V~420km/s (Sakamoto et al 2006)

Arp220, Pcygni profiles 100pc, HCO+, Mout ~ 108Mo (Sakamoto et al 2009)

More violent outflows due to AGN: V> 1000km/s, up to 1200 Mo/yrOH, H2O abs Herschel, Sturm et al (2011), ULIRG+AGNMrk231 (Feruglio et al 2010) 700 Mo/yr, depleted in 107 yrsN1266 (Alatalo et al 2011) Mout ~ 2 107Mo, depleted in ~108 yrs

Ionized flows, more frequent

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Statistics on 200 galaxies 0.4 < z <1.4 (Martin C. et al 2012)2% of FeII absorption outflow at 200Km/s, 20% at 100km/sStrong function of SFR (FeII, MgII, Keck)

Outflow and also inflow

Fraction of outflowsIndependent of stellar mass, color, or luminosity.

CollimatedAngle smaller with larger V

Ionised or atomic gas (Na I D abs)

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Rupke et al 2005

All SB with SFR> 10Mo/yr

Less frequent in AGNBut Vel higher

Differ only in vmax

Mrk 231: both a high-velocity, small-scale and low-velocity, extended outflow

Correlations with SFR, AGN

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Martin et al 2012

Larger outflows at high zand at higher M

But also higher SFR and M

More frequent for SN than AGN

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Stacking by Chung et al 2011Even in starburst, flows of 1000km/sDifficult to disentangle SN and AGN(only may be in N1266?)Energy of SF: sufficient

Mass involved: depends a lot on conversion ratios. In the future: many CO lines, withHCN/HCO+ will give clues

Stacked spectrum = 120h-antennaALMA will get it in 2hours

OH-119 absorption by Herschel

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43 mergers, ULIRGS & QSO, Veilleux et al 2013

OH wind detection rateAs a function of Starburst LumAnd AGN fractionNot significant..

Molecular winds in mergers & QSO

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Blue-shifted fast absorption is seen in 70% of objectsWide angle geometry of outflow (145°) Veilleux et al 2013Only 10% of redshifted absorption:inflow in filamentary, planar geometry

Vmax ~-1000km/s, mean -200km/s, larger in high LAGN

HERUS, 24 ULIRGS, 2/3 of them have V> 600km/s AGN drivenSpoon et al 2013

OH emission decreases as the silicate absorption increasesOH is located in the nuclear cocoon, up to 2-4 108 Mo of outflow

Radio MOHEGs (MOlecular Hydrogen Emission Galaxies)

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A way to disentangle SN and AGN actions: outflows in nonStar-forming objects30% of 55- 3C radio sources have enhanced H2 lines (Spitzer)H2/PAH 10 x normal, off the KS law (no SF) Ogle et al 2010

H2 lines narrower than mid-IR ionised lines (Guillard et al 2012)HI-outflow RG have bright H2 mid-IR lines not accounted for by UV or X-ray heating.

CO-detections in radio MOHEG Casasola et al 2012

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Guillard et al 2012

High Spatial resolution

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Larger velocities close to the nuclear StarburstOH, H2O absorption lines -Herschel, V~1000km/sCO velocities: slow down to 100-400km/s

N3079

M82

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Alatalo et al 2011

Spatial resolution of ~300pc

N1266

Molecular disk, concentratedR<200 pc of the nucleus SF rate ≈ 2 M ⊙ yr-1

Signs of quenching in theH lines, etc..ETG (Sauron)

3-Why molecular outflows?

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Outflowing gas is accelerated by a shock, and heated to 106-107K Molecules should be dissociated at such temperaturesEven if cold clumps are carried out in the flow shock signature?

Radiative cooling is quick enough to reform molecules in alarge fraction of the outflowing material (Zubovas & King 2014)

With V~1000km/s, and dM/dt ~1000 Mo/yr, efficient coolingproduces multi-phase media, with triggered star formation

AGN winds more than SF outflows?

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Cooling efficient (free-free, metals)Flow unstable, if R=Prad/Pgas<0.5(Krolik 1981), and R~0.07 MBH/Mcrit fEDD ~0.07Multiphase, with RT instabilities

Time-scale for cooling << 1MyrAt kpc scales, SF induced

The SF results in a Luminosity Comparable to LAGN 100Mo/yr!

This means that SB or AGN outflowsare difficult to disentangleAll could be due to AGN

Zubovas & King 2014

Energy-conserving outflows?

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If the cooling is very efficient, momentum-conserving outflow

But for very fast winds > 10 000km/s, radiative losses are slowenergy-conserving flow (Faucher-Giguère & Quataert 2012)

In some cases, even slow winds vin ~1000km/s driven by radiation pressure on dust, could be energy-conservingPush by the hot post-shock gas, boost the momentumVs of the swept-up material

Boost of vin /2 Vs ~50! Explains why momentum flux >> LAGN/c

// Adiabatic phase, or Sedov-Taylor phase in SN remnant

Slow cooling --High momentum fluxes

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Faucher-Giguère & Quataert 2012

Full: protonsDash: electronsTComp= 2 107K

Minimal e-heatingTe=me/mpTpat the shock2-temp plasma

T behind SW

Outflow solutions

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Faucher-Giguère & Quataert 2012

Represent the typical case of Mrk231, face-on, R~3kpcV~1000km/s

Momentum flux =15 LAGN/c

Momentum boost

Winds launch

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From accretion disks, as seen in UV absorption linesBAL quasars, or from X-rays coronaeThermal heating (Compton) makes the gas reach VescRadiation on electrons ( > Eddington)Or even radiation pressure on dust

Or magnetic driving (Proga 2003, 2005)More realistically, all driving mechanisms together!

Schematic view

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Need for AGN feedback

M/L = 80

Standard CDM model: Too many galaxies at both ends

35Observations: lower number of dwarfs, and of giants

N

Mass

N M/L

Mass

MBH-Mbulge relation

Gultekin et al 2009

AGN wind feedback

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Near the BH cooling is efficient (inv. Compton), and an outflow providesefficient feedback, if

MBH > 3.67 108 (fg/0.16) (/200km/s)4

Silk & Rees 1998, King (2003, 2010), Nayakshin & Power (2010)

Since the outflow can reach kpc, where the radiation is much lowerThe critical value is slightly above the M- relation, for fg=0.16,But the gas fraction could be lower.

It might need sometimes after the critical mass is reached to clear upthe bulge from gas the BH has time to grow by a factor up to 10Zubovas & King (2012

The MBH- relation

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Mass ratio between SMBH and bulge~1/700

Sometimes higher, in galaxyclusters (cD galaxy)McConnell et al 2011

Cannibal galaxies, fueledBy cooling flow, without SF?

There could be severalM- relationsFor spirals, ellipticalsor clusters

Different M- relations

38Zubovas & King 2012

Feedback loop?

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Angles-Alcazar et al 2013

Torque limited growth

Mostly gas accretion, sometimesMergers (but not essential)

Numerical evolutionM- relations for seeds

Effects of initial conditions are Quickly erased

dMBH/dt ~SFR with scatterNo feedback loop required

Positive AGN feedback

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SFR

L*

-Mgas

3Myr

10Myr

30Myr

Zubovas et al 2013

Silk 2005, Dubois et al 2013

Two-phase simulations

41Nayakshin 2013

Most of the outflow kinetic energy escapes through the voidsPositive and negative feedbackCold gas is pushed by ram-pressureMore feedback on low-density gas

Fractal structure 2pc-1kpc

42Efficient relativistic jets Wagner & Bicknell 2011

Influence of the porosity

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Efficient relativistic jets, when Pjet/LEDD ~10-4- 10-2

Wagner et al 2012, 2013

Low filling factor

Max cloud size 50pc

Max cloud size 10pc

Radio jets triggered SF

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Young, restarted radio loud AGN 4C12.50The outflow is located 100 pc from the nucleuswhere the radio jet interacts with the ISM

Morganti et al 2013, Dasyra & Combes 2012

Minkowski object

45Croft et al 2006

HI: blue, H: light blue, Radio cont: purple

4- Perspectives with ALMA

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In cycle 2, 4x more surface than PdB, will x 1.5 in cycle3

Cycle 2: 1mJy rms in 7min, 50km/s resolution, @345GHz, 2’’Between 2 105Mo to 108Mo z=0 to 1

10x more spatial resolution, mainly going to higher frequency

Resol FOV Freq Resol MaxBand 3 1.1" 44" 84-116 0.57 " 8.6 "Band 6 0.48" 19" 211-275 0.25 " 3.7 "Band 7 0.32" 13" 275-373 0.16 " 2.5 "Band 9 0.16" 6.5" 602-720 0.08 " 1.3 «  with ACA without

Fueling in low-luminosity AGN

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NGC 1433: barred spiral, the « Lord of the Rings » Buta et al 2001

Atomic gas only in the inner and outer ring (Ryder et al 1996)

CO in the nuclear ring and disk(Bajaja et al 1995)

CO(3-2) with ALMA(Cycle 0)

CO does notfollow the nuclearbar

The Seyfert 2 NGC 1433

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CO(3-2) map with ALMA, No HCN, HCO+(4-3)Beam = 0.5’’ = 24pc

Discovery of an innerILR at r=200pc

+ Molecular torus?24pc size, dust cont.

Combes et al 2013

The smallest molecular outflow

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PV major axis

PV minor axis

CO on HST

CO on unsharp masked HST image

Flow of 50pc size

Properties of the outflow

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MH2= 5.2 107 Mo in FOV=18’’ MH2= 1.8 108 Mo in beam 43’’ (Bajaja et al 1995)

Blue and red-shifted outflows, with 100km/s (200km/s if in the plane)2’’=50pc from the center, Total 7% of the mass= 3.6 106 Mo

From the M- relation, MBH = 4 106Mo (peculiar motions 5 108 Mo)SFR = 0.2 Mo/yrdM/dt (Mv/d) tan∼ α= 7 tanα M⊙/yr, ~40 SFR α = angle of outflow/line of sight

Lkin=0.5 dM/dt v2 =2.3 tanα (1+ tan2α) 1040 erg/sLbol (AGN)= 1.3 1043 erg/sFlow momentum >> LAGN/c Jet driven flow, Pjet = 2 1042 erg/s from radio

Other low-luminosity AGN flows

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Driven by both the starburst and the radio jets The LINER NGC 6764: 4.3106 M⊙ Vout~100 km/s (Leon et al. 2007) Larger than in NGC 1433, but outflow rate ~1 M⊙/yr

The LINER NGC 1266 highest flow rate of 13 M⊙/yr, with2.4 107 M⊙ of H2 and V=177 km/s (Alatalo et al. 2011)

LINER NGC1377, SFR of 1 M∼ ⊙/yr, outflow rate of 8 M⊙/yr, Mflow = 1.1 107 M⊙ at V=140 km/s (Aalto et al. 2012)

Future of IRAM PdBI

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Twice more surface (12antennae)EW baseline from 0.8 to 1.6km

Bandwidth from 8 GHz to 32 GHz

Sensitivity to continuum

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SUMMARY

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Gas outflows are very frequent in starburst, above an SFR~1Mo/yr

Outflows are also present around AGN, but much rarer, accordingto statistics, and stacking

Entrained molecular gas means a lot more mass (107-109 Mo)than ionised gas outflows

With ALMA and NOEMA, many more outflows could be studiedindividually, with more CO lines and dense tracers

The spatial resolution will allow to understand the detailedmechanisms (energy/momentum power, radiation pressure, kinetic impact)

Outflows at higher redshifts