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Richard Davies, Eckhard Sturm Max Planck Institute for Extraterrestrial Physics, Germany

Black Hole Feeding & Feedback: what can we learn from nearby AGN?. Richard Davies, Eckhard Sturm Max Planck Institute for Extraterrestrial Physics, Germany. mm IRAM/PdBI. far-IR Herschel/PACS. near-IR VLT/SINFONI. near-IR VLTI/GRAVITY. Inflow Outflow. Imaging

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Richard Davies, Eckhard Sturm Max Planck Institute for Extraterrestrial Physics, Germany

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  1. Black Hole Feeding & Feedback: what can we learn from nearby AGN? Richard Davies, Eckhard Sturm Max Planck Institute for Extraterrestrial Physics, Germany mm IRAM/PdBI far-IR Herschel/PACS near-IR VLT/SINFONI near-IR VLTI/GRAVITY

  2. Inflow Outflow Imaging Martini+ 03, Simoes-Lopes+ 07: a variety of dust structures may be present, & are necessary but not sufficient to fuel AGN NGC1097 ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds BLR Integral field spectroscopy is revealing inflows: Fathi+ 06, Storchi-Bergmann+ 07, 09, 10, Riffel+ 08, 09, 11, Schnorr Műller+ 11, Davies+ 09, Hicks, RD, + in prep, MüllerSánchez, RD, + in prep ionisation cones BH mass star formation molecular outflows hot dust molecular gas CO Kinematics (PdBI) Haan+ 09, Garcia Burillo+ 11: gravity torques can drive inflow down to ~100pc, but only in 1/3 of 25 LLAGN studied by NUGA team 0.1pc 1pc 10pc 100pc 1kpc

  3. - photometric & kinematic evidence of young stellar populations • characteristic age from standard diagnostics (Brγ, SN rate, M/L) • delay of ~100Myr between star formation & AGN fuelling (Davies+ 07) • try to confirm presence of TP-AGB stars (CN at 1.1μm, C2 at 1.78μm) • (Melbourne & Davies) CO absorption Inflow Outflow K band non-stellar & stellar continuum NGC1097 ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds BLR ionisation cones stellar velocity stellar dispersion BH mass star formation molecular outflows hot dust molecular gas LAGN/LEdd 0.1pc 1pc 10pc 100pc 1kpc GC Starburst Age (Myr)

  4. Inflow Outflow Molecular Gas – high excitation CO lines (Hailey-Dunsheath+ 12) ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds BLR ionisation cones BH mass star formation molecular outflows hot dust molecular gas ME – H2 ringHE – infall clump PDR (stars) no recent starburst PDR (AGN) obscuration covering factor vs density shock if ring is shock heated jet/cloud interaction (but fine tuning) XDR if ring is X-ray heated if clump is X-ray heated 0.1pc 1pc 10pc 100pc 1kpc

  5. Inflow Outflow Ionisation Cones (Müller Sánchez+ 11 & in prep) - 6 targets, model ionisation cones + rotating disk in [SiVI] or Brg - in half, ionisation cones are bisected by the disk - relations between θout, Vmax, and MH2 ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds BLR ionisation cones NGC6814 residual (disk+cones) residual (disk) BH mass star formation molecular outflows hot dust molecular gas 0.1pc 1pc 10pc 100pc 1kpc Vmax vs θout MH2 vs θout

  6. Inflow Outflow Atomic & Ionised Outflow in M82 (Contursi+ ) Chandra (blue) Spitzer (red) HST + WIYN • disk/outflow kinematically separated • broad base to N outflow • model neutral gas as PDR, excited by central starburst • maps of G0, n, T, NHI • hole in τ[CII], matching HCO ring, with brighter Hα inside ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds BLR ionisation cones BH mass star formation molecular outflows hot dust molecular gas 0.1pc 1pc 10pc 100pc 1kpc [OIII] 88μm velocity [OIII] 88μm dispersion [OIII] 88μm / [OI] 63μm [CII] 158μm opacity

  7. Inflow Outflow Molecular Outflows OH absorption in ULIRGs & AGN (Fischer+10, Sturm+ 11 & in prep) Vmax vs SFR & LAGN ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds BLR ionisation cones BH mass star formation molecular outflows hot dust molecular gas 0.1pc 1pc 10pc 100pc 1kpc

  8. Inflow Outflow • Molecular Outflow in NGC3079 • - star formation 3Msun/yr in central 4kpc (Yamagishi+ 10) • 20-100keV: luminous compton thick AGN, 2-10keV > 1e42erg/s (Iyomoto+ 01) • no HII regions at base of outflow (Cecil+ 01) 5” 5” ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds Dodds-Eden+ in prep BLR HCN1-0 CO2-1 ionisation cones BH mass star formation molecular outflows hot dust molecular gas Cecil+ 01 PdBI: HCN, HCO+, SiO, HNC absorption 0.1pc 1pc 10pc 100pc 1kpc PACS: OH 119μm absorption

  9. Inflow Outflow ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc circumnuclear torques, spirals, … coronal line clouds BLR ionisation cones BH mass star formation molecular outflows hot dust molecular gas 0.1pc 1pc 10pc 100pc 1kpc

  10. What next? [OIII] Coronal Line Clouds (GRAVITY) Outflow in NGC1068 Broad Line Region & Black Hole Masses (GRAVITY) • Exploiting GRAVITY • Binary AGN • Linking AO & VLTI scales using hydrodynamical simulations • Gas properties & impact of AGN on abundances – spatially resolved line ratios • Robust statistics – VLT large programme on BAT sample of AGN • Future outflow studies with IRAM/ALMA & HST/Gemini [SiVI] [FeII] Evidence that some BLRs are partially supported by rotation: e.g. - NLS1 maybe preferentially pole-on (Peterson+ 00, Boroson 11) - double-peaked BLRs (Eracleous+ 2003) - disk+wind structure in Mkn 110 (Kollatschny+ 03; see also Elitzur+ 08) - mass ratio distribution (Collin+ 06) - more velocity resolved reverberation mapping (Bentz+ 10) - emission line EW distribution (Risaliti+ 11) velocities up to 3200km/s (Cecil+ 02) Vmax = 1900km/s (Müller Sánchez+ 11) VLTI does not resolve BLR, but astrometry can measure velocity gradient - astrometry to <0.5% of FWHM easily achievable, simple phase measurement for VLTI - fraction of BLRs with rotation; their size, PA; & mass of central BH 3C273 Size-luminosity relation gives BLR size = 390 light-days, i.e. 0.13mas at z=0.158, much less than 4mas beam measurable from centroids of red & blue emission in BLR e.g. with 1.282μm Paβ shifted to 1.485μm in H-band How many? 1.875μm Paα shifted to K-band, 0.05<z<0.22, λL1500>1044erg/s -> several hundred sources 1000km/s @ NGC1068 (14.4Mpc) = 14μas/yr Circinus (4.2Mpc) = 49μas/yr Cen A (3.5Mpc) = 59μas/yr

  11. What next? • Exploiting GRAVITY • Binary AGN • Linking AO & VLTI scales using hydrodynamical simulations • Gas properties & impact of AGN on abundances – spatially resolved line ratios • Robust statistics – VLT large programme on BAT sample of AGN • Future outflow studies with IRAM/ALMA & HST/Gemini

  12. Dual & Binary AGN Dual AGN: are they really? Dual AGN, with 2 hard X-ray sources Koss+ 11 Komossa+ 03 AO imaging Fu+11 & Rosario+ 11: - 30-40% show 2 nuclei on kpc scales; - double peak due to outflow; - most QSOs are not mergers. McGurk+ 11: need AO + IFU to confirm AGN duality. Double-peaked [OIII] lines in 1% of SDSS QSOs Smith+ 10

  13. Dual & Binary AGN Binary AGN & BH recoil Boroson & Lauer 09, Lauer & Boroson 09 BLR+NLR BLR only absorption BLRs shifted by 2650km/s Best candidate for binary BH, ~0.1pc separation? 1” = 5.2kpc at z=0.38 -> 0.1pc = 19μas VLTI astrometry may be able to find spatial offsets between the BLRs

  14. Dual & Binary AGN Binary AGN & BH recoil Candidates for binary BHs, or extreme double-peaked BLRs (a la Eracleous)? Komossa+ 08: J0927+2943 @ z=0.713 Shields+ 09: J1050+3456 @ z=0.272 Hβ Hα BLR & NLR shifted by 2650km/s BLR & NLR shifted by 3500km/s Dotti+ 09: semi-major axis = 0.34pc 1” = 7.3kpc at z=0.71 -> 0.34pc = 47μas 1” = 4.2kpc at z=0.27 -> 0.2pc = 48μas

  15. What next? • Exploiting GRAVITY • Binary AGN • Linking AO & VLTI scales using hydrodynamical simulations • Gas properties & impact of AGN on abundances – spatially resolved line ratios • Robust statistics – VLT large programme on BAT sample of AGN • Future outflow studies with IRAM/ALMA & HST/Gemini Linking AO & VLTI scales (hydrodynamical simulations) VLTI 10μm image reconstruction Schartmann’s simulations AO observations stars Raban+ 09 If these are 2 components of the ‘torus’, they imply that it is a dynamical structure, whose properties are driven by star formation

  16. What next? Gas properties & impact of AGN on abundances • Exploiting GRAVITY • Binary AGN • Linking AO & VLTI scales using hydrodynamical simulations • Gas properties & impact of AGN on abundances – spatially resolved line ratios • Robust statistics – VLT large programme on BAT sample of AGN • Future outflow studies with IRAM/ALMA & HST/Gemini Molecular Gas – abundances (e.g. NGC 3227: Davies, Dean & Sternberg 11) observational: line ratios -> LVG -> n, T, n/(dV/dr), [ni] theoretical: X-ray excitation of gas -> [ni] vs n/ζ NGC6951

  17. What next? • Exploiting GRAVITY • Binary AGN • Linking AO & VLTI scales using hydrodynamical simulations • Gas properties & impact of AGN on abundances – spatially resolved line ratios • Robust statistics – VLT large programme on BAT sample of AGN • Future outflow studies with IRAM/ALMA & HST/Gemini Robust statistics - VLT large programme on BAT sample of AGN • Swift BAT, 6 years all-sky monitoring • 14-195keV measures direct emission from the AGN, low sensitivity to obscuration • widely accepted as least biased survey for AGN with respect to host galaxy properties • observe a complete volume limited sample of all AGN accessible to VLT

  18. What next? • Exploiting GRAVITY • Binary AGN • Linking AO & VLTI scales using hydrodynamical simulations • Gas properties & impact of AGN on abundances – spatially resolved line ratios • Robust statistics – VLT large programme on BAT sample of AGN • Future outflow studies with IRAM/ALMA & HST/Gemini

  19. Outflowstudies: potential Large Programat IRAM, andcomplementaryprograms • IRAM PdBI LP? • Based on confirmedmolecularoutflowsfromour Herschel-PACS GTO and OT archive: • SHINING: 23 RBGS ULIRGs • OT1 (withVeilleux): OH 119 spectra of 15 additional warm, quasar-dominated, late stage mergers • OT2 (with Veilleux): OH119 spectra of 5 IR-faint quasar-dominated late stage mergers • OH119 spectra of AGN winds (Swift-BAT AGN sample) • OT2 (with Fischer): Full OH ladder plus H2O in Mrk231 and NGC6240 • OT2 (withSpoon): OH transitions in IRAS F00183 • OT2 (with González-Alfonso): completing OH and H2O, NH3, OH+ in 9 (mostly) SHINING (U)LIRGs • OT2 (with Javier, prio2 mid1/3): OH119 in ULIRGs at0.2 < z < 0.3 withhighest SFR and L_AGN • Other Herschel archivaldata(e.g. GOALS LIRGs?)

  20. Step 1a and 1b: Detectandresolvebroad CO wings spatialinformation Mrk 231 (Feruglio+2010) IRAS F08572 (recent observation) 1.2 kpc

  21. Step 2: Measureseveraltransitions excitationoftheoutflowing gas Mrk 231 (Feruglio+2010, Cicone+ in prep)

  22. Step 3: 13CO, HCN, HCO+… (opticalthickness, density…forthebrightesttargets) ~700 km/s Arp220 (Sakamoto+2009) NGC3079 OH 5”

  23. V_max, outflow rates, depletion times, energetics, SB vs. AGN driven, dependency on characteristics of host galaxies (evolutionary stage, SFR, L_AGN, etc.)

  24. Complementaryprojects(ongoingand potential) 1) ALMA - OH at high z (e.g. Cloverleaf) (Javier) - [C II] broadwingsat high z (R. Maiolino) 2) HST With S. Veilleux: 30 FIR-bright and FIR-faint QSOs (QUEST/Herschel OT1) in UV (OVI, N V, Ly alpha…) absorbers. Outflows as function of host properties and age (merger  QSO). No spatial resolution (only low vs. high ionization as constraints for location) 3) GEMINI Rupke/Veilleux(NaID, etc.) spatially resolved atomic and ionized outflowing gas With J. Fischer: ro-vibrational CO lines at ~5 micron 4) Chandra With S. Veilleux(2D mapping of the temperature gradient and structure in the pronounced X-ray nebula in the Mrk231 wind).

  25. Complementaryprojects(ongoingand potential) 5) SINFONI, XSHOOTER (et al.) - e.g. QSOs at z=2in O III 5007 (in H band) and H(in K band) (R. Maiolino: Quasar 2QZ00) likely via blue shifted emission (red shifted part likely absorbed by dust in the galactic disk). Distinguish from rotation via enhanced dispersion. Hdepletion might indicate quenching. Follow up with AO-LGS, plus Xshooter. - e.g. nearbySeyferts(Ric)

  26. Inflow in PACS spectra NH3 NGC3079 H2O OI

  27. What next? • Exploiting GRAVITY • Binary AGN • Linking AO & VLTI scales using hydrodynamical simulations • Gas properties & impact of AGN on abundances – spatially resolved line ratios • Robust statistics – VLT large programme on BAT sample of AGN • Future outflow studies with IRAM/ALMA & HST/Gemini

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