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Françoise Combes February 13, 2014

Françoise Combes February 13, 2014. AGN-driven outflows. Perseus cooling flow. Mrk 231. Inefficient star formation Behroozi et al 2013. Gaibler et al 2011. MS0735.6+7421 cluster (McNamara et al. 2009). Outline. Very frequently, inflow and outflow occurs

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Françoise Combes February 13, 2014

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  1. Françoise Combes February 13, 2014 AGN-driven outflows Perseus cooling flow Mrk 231

  2. Inefficient star formation Behroozi et al 2013 Gaibler et al 2011

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

  4. Outline Very frequently, inflow and outflow occurs simultaneously -- more difficult to see the inflow 1- AGN feedback: cooling flows 2- SN+AGN inflow/outflow in galaxies 3- Mechanisms -- Energetics 4- ALMA and NOEMA perspectives

  5. 1- Gas flow in coolcore clusters Salomé et al 2006 Perseus A , Fabian et al 2003

  6. Cold CO in filaments 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 Velocity much lower than free-fall Salome et al 2008

  7. Numerical simulations(Revaz, Combes, Salome 2007) Buoyant bubbles, compression and cooling at the surfaces +Cold gas dragged upwards Log Temperature (150kpc) Log density (25x50kpc)

  8. Turbulence triggered by SF Perseus cluster simulated by Falceta-Goncalves et al 2010 MHD AGN heating reduces the cooling

  9. OI, CII with Herschel Same morphology + Same spectra between CO(2-1) and OI Same gas, cooling through different phases? No rotation, but inflows Edge et al 2010 Mittal et al 2010

  10. 2-Feedback in nuclei: H2 & CO 6 out of 300 systems searched show H2 outflows 4C12.50 SFR ~400-1000 Mo/yr Outflow ~130 Mo/yr Dasyra & Combes 2011, 2012

  11. AGN-driven molecular outflows Mrk 231 AGN and also nuclear Starburst, 107-108Mo Outflow 700Mo/yr Aalto et al 2012 high-density molecular tracers ( HCN, HCO+ HNC, HC3N CN, … IRAM Ferruglio et al 2010

  12. Molecular outflows: excitation In addition of several CO lines: More excited gas In the outflow Cicone et al 2012 Search in 7 ULIRGs and QSO: 100Mo/yr outflows found in 4 Cicone et al 2013

  13. Spatial extension in Mrk231 On kpc scales,  affects the galaxy Blue wing Red wing dM/dt = 3v MOF/ROF ~1000 Mo/yr, while SFR ~200 Mo/yr Kinetic power ~2 1044 erg/s  AGN Cicone et al 2012

  14. Dense gas in the base of the outflow Outflows in 4 out of 7 Mrk 231 Cicone et al 2013

  15. Relations outflow AGN, SFR For AGN-hosts, the outflow rate Correlates with the AGN power Starburst galaxies are on the line Mass loading factor ~1 For AGN-hosts, dM/dt is larger

  16. Comparison with AGN models Lower efficiency in Liners Higher in SB dM/dt v ~20 LAGN/c Can be explained by energy-driven outflows (Zubovas & King 2012)

  17. Molecular outflows are massive Aalto et al 2012 Some outflows are more massive then their dense nuclear disk, e.g. N1377 (S0) 200pc extent with modest 140km/s Mout= 1-5 107Mo, disk mass ~2 107 Mo N1377 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/yr OH, H2O abs Herschel, Sturm et al (2011), ULIRG+AGN Mrk231 (Feruglio et al 2010) 700 Mo/yr, depleted in 107 yrs N1266 (Alatalo et al 2011) Mout ~ 2 107Mo, depleted in ~108 yrs

  18. Ionized flows, more frequent • 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/s • Strong function of SFR (FeII, MgII, Keck) • Outflow and also inflow • Fraction of outflows • Independent of stellar mass, • color, or luminosity. • Collimated • Angle smaller with larger V

  19. Ionised or atomic gas (Na I D abs) Rupke et al 2005 All SB with SFR> 10Mo/yr Less frequent in AGN But Vel higher Differ only in Dvmax Mrk 231: both a high-velocity, small-scale and low-velocity, extended outflow

  20. Correlations with SFR, AGN Larger outflows at high z and at higher M But also higher SFR and M Martin et al 2012

  21. More frequent for SN than AGN Stacking by Chung et al 2011 Even in starburst, flows of 1000km/s Difficult 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, with HCN/HCO+ will give clues Stacked spectrum = 120h-antenna ALMA will get it in 2hours

  22. OH-119mabsorption by Herschel 43 mergers, ULIRGS & QSO, Veilleux et al 2013 OH wind detection rate As a function of Starburst Lum And AGN fraction Not significant..

  23. Molecular winds in mergers & QSO • Blue-shifted fast absorption is seen in 70% of objects • Wide angle geometry of outflow (145°) Veilleux et al 2013 • Only 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 driven • Spoon et al 2013 • OH emission decreases as the • silicate absorption increases • OH is located in the nuclear • cocoon, up to 2-4 108 Mo • of outflow

  24. Radio MOHEGs (MOlecular Hydrogen Emission Galaxies) A way to disentangle SN and AGN actions: outflows in non Star-forming objects 30% 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

  25. Guillard et al 2012

  26. High Spatial resolution Larger velocities close to the nuclear Starburst OH, H2O absorption lines -Herschel, V~1000km/s CO velocities: slow down to 100-400km/s N3079 M82

  27. Spatial resolution of ~300pc Molecular disk, concentrated R<200 pc of the nucleus SF rate ≈ 2 M ⊙ yr-1 Signs of quenching in the Hb lines, etc.. ETG (Sauron) Alatalo et al 2011 N1266

  28. 3-Why molecular outflows? Outflowing gas is accelerated by a shock, and heated to 106-107K Molecules should be dissociated at such temperatures Even if cold clumps are carried out in the flow shock signature? Radiative cooling is quick enough to reform molecules in a large fraction of the outflowing material (Zubovas & King 2014) With V~1000km/s, and dM/dt ~1000 Mo/yr, efficient cooling produces multi-phase media, with triggered star formation

  29. AGN winds more than SF outflows? • Cooling efficient (free-free, metals) • Flow unstable, if R=Prad/Pgas<0.5 • (Krolik 1981), and • R~0.07 MBH/Mcrit fEDD ~0.07 • Multiphase, with RT instabilities • Time-scale for cooling << 1Myr • At kpc scales, SF induced • The SF results in a Luminosity • Comparable to LAGN 100Mo/yr! • This means that SB or AGN outflows • are difficult to disentangle • All could be due to AGN Zubovas & King 2014

  30. Energy-conserving outflows? • If the coolingisvery efficient,  momentum-conservingoutflow • But for veryfastwinds > 10 000km/s, radiative losses are slow • energy-conserving flow (Faucher-Giguère & Quataert 2012) • In some cases, even slow winds vin ~1000km/s driven by radiation • pressure on dust, couldbeenergy-conserving • Push by the hot post-shockgas, boost the momentum • Vs of the swept-up material • Boost of vin /2 Vs ~50! Explainswhymomentum flux >> LAGN/c • // Adiabatic phase, or Sedov-Taylor phase in SN remnant

  31. Slow cooling --High momentum fluxes T behind SW Full: protons Dash: electrons TComp= 2 107K Minimal e-heating Te=me/mpTp at the shock 2-temp plasma Faucher-Giguère & Quataert 2012

  32. Outflow solutions Momentum boost Represent the typical case of Mrk231, face-on, R~3kpc V~1000km/s Momentum flux =15 LAGN/c Faucher-Giguère & Quataert 2012

  33. Winds launch From accretion disks, as seen in UV absorption lines BAL quasars, or from X-rays coronae Thermal heating (Compton) makes the gas reach Vesc Radiation on electrons ( > Eddington) Or even radiation pressure on dust Or magnetic driving (Proga 2003, 2005) More realistically, all driving mechanisms together!

  34. Schematic view

  35. Need for AGN feedback Standard LCDM model: Toomany galaxies atbothends MBH-Mbulge relation N M/L = 80 N M/L Mass Mass Observations: lower number of dwarfs, and of giants Gultekin et al 2009

  36. AGN wind feedback Near the BH cooling is efficient (inv. Compton), and an outflow provides efficient feedback, if MBH > 3.67 108 (fg/0.16) (s/200km/s)4 Silk & Rees 1998, King (2003, 2010), Nayakshin & Power (2010) Since the outflow can reach kpc, where the radiation is much lower The critical value is slightly above the M-s relation, for fg=0.16, But the gas fraction could be lower. It might need sometimes after the critical mass is reached to clear up the bulge from gas  the BH has time to grow by a factor up to 10 Zubovas & King (2012

  37. The MBH-s relation Mass ratio between SMBH and bulge~1/700 Sometimeshigher, in galaxy clusters (cDgalaxy) McConnell et al 2011 Cannibal galaxies, fueled By cooling flow, without SF? There couldbeseveral M-s relations For spirals, ellipticals or clusters

  38. Different M-s relations Zubovas & King 2012

  39. Feedback loop? Torque limited growth Mostly gas accretion, sometimes Mergers (but not essential) Numerical evolution M-s relations for seeds Effects of initial conditions are Quickly erased dMBH/dt ~SFR with scatter No feedback loop required Angles-Alcazar et al 2013

  40. Positive AGN feedback SFR 3Myr 10Myr L* -Mgas 30Myr Zubovas et al 2013 Silk 2005, Dubois et al 2013

  41. Two-phase simulations Most of the outflow kinetic energy escapes through the voids Positive and negative feedback Cold gas is pushed by ram-pressure More feedback on low-density gas Nayakshin 2013

  42. Fractal structure 2pc-1kpc Efficient relativistic jets Wagner & Bicknell 2011

  43. Influence of the porosity Low filling factor Max cloud size 50pc Max cloud size 10pc Efficient relativistic jets, when Pjet/LEDD ~10-4- 10-2 Wagner et al 2012, 2013

  44. Radio jets triggered SF Young, restarted radio loud AGN 4C12.50 The outflow is located 100 pc from the nucleus where the radio jet interacts with the ISM Morganti et al 2013, Dasyra & Combes 2012

  45. Minkowski object HI: blue, Ha: light blue, Radio cont: purple Croft et al 2006

  46. 4- Perspectives with ALMA 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 Max Band 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

  47. Fueling in low-luminosity AGN 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 not follow the nuclear bar

  48. The Seyfert 2 NGC 1433 CO(3-2) map with ALMA, No HCN, HCO+(4-3) Beam = 0.5’’ = 24pc Discovery of an inner ILR at r=200pc + Molecular torus? 24pc size, dust cont. Combes et al 2013

  49. The smallest molecular outflow PV major axis Flow of 50pc size CO on HST PV minor axis CO on unsharp masked HST image

  50. Properties of the outflow 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-s relation, MBH = 4 106Mo (peculiar motions 5 108 Mo) SFR = 0.2 Mo/yr dM/dt ∼ (Mv/d) tanα= 7 tanα M⊙/yr,  ~40 SFR α = angle of outflow/line of sight Lkin=0.5 dM/dt v2 =2.3 tanα (1+ tan2α) 1040erg/s Lbol (AGN)= 1.3 1043 erg/s Flow momentum >> LAGN/c  Jet driven flow, Pjet = 2 1042 erg/s from radio

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