Post on 13-Jan-2016
description
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