Slide 1

Richard Davies, Eckhard Sturm Max Planck Institute for Extraterrestrial Physics, Germany near-IR VLT/SINFONI far-IR Herschel/PACS mm IRAM/PdBI Black Hole Feeding & Feedback: what can we learn from nearby AGN? near-IR VLTI/GRAVITY Slide 2 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows Imaging Martini+ 03, Simoes-Lopes+ 07: a variety of dust structures may be present, & are necessary but not sufficient to fuel AGN Integral field spectroscopy is revealing inflows: Fathi+ 06, Storchi-Bergmann+ 07, 09, 10, Riffel+ 08, 09, 11, Schnorr Mller+ 11, Davies+ 09, Hicks, RD, + in prep, Mller Snchez, RD, + in prep NGC1097 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 Slide 3 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows L AGN /L Edd Starburst Age (Myr) GC CO absorption K band non-stellar & stellar continuum NGC1097 - photometric & kinematic evidence of young stellar populations - characteristic age from standard diagnostics (Br, SN rate, M/L) - delay of ~100Myr between star formation & AGN fuelling (Davies+ 07) - try to confirm presence of TP-AGB stars (CN at 1.1m, C 2 at 1.78m) (Melbourne & Davies) stellar velocity stellar dispersion Slide 4 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows Molecular Gas high excitation CO lines(Hailey-Dunsheath+ 12) ME H 2 ringHE infall clump PDR (stars) no recent starburst PDR (AGN) obscurationcovering factor vs density shock if ring is shock heatedjet/cloud interaction (but fine tuning) XDR if ring is X-ray heatedif clump is X-ray heated Slide 5 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows NGC6814 Ionisation Cones(Mller Snchez+ 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 out, V max, and M H2 residual (disk) residual (disk+cones) V max vs out M H2 vs out Slide 6 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows Atomic & Ionised Outflow in M82 (Contursi+ ) HST + WIYN Chandra (blue) Spitzer (red) [OIII] 88m velocity[OIII] 88m dispersion[OIII] 88m / [OI] 63m[CII] 158m opacity disk/outflow kinematically separated broad base to N outflow model neutral gas as PDR, excited by central starburst maps of G 0, n, T, N HI hole in [CII], matching HCO ring, with brighter H inside Slide 7 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows V max vs SFR & L AGN Molecular Outflows OH absorption in ULIRGs & AGN (Fischer+10, Sturm+ 11 & in prep) Slide 8 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows Molecular Outflow in NGC3079 - star formation 3M sun /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 Cecil+ 01 HCN1-0 Dodds-Eden+ in prep CO2-1 5 PACS: OH 119m absorption PdBI: HCN, HCO +, SiO, HNC absorption Slide 9 1kpc100pc10pc1pc0.1pc0.01pc circumnuclear torques, spirals, star formation molecular gas hot dust BLR Inflow Outflow 0.1pc1pc10pc100pc1kpc ionisation cones coronal line clouds BH mass molecular outflows ionised outflows Slide 10 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 Broad Line Region & Black Hole Masses(GRAVITY) 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) VLTI does not resolve BLR, but astrometry can measure velocity gradient - astrometry toseveral hundred sources 1000km/s @NGC1068(14.4Mpc)=14as/yr Circinus(4.2Mpc)=49as/yr Cen A(3.5Mpc)=59as/yr velocities up to 3200km/s (Cecil+ 02) V max = 1900km/s (Mller Snchez+ 11) [FeII] Outflow in NGC1068 [SiVI] [OIII] Coronal Line Clouds(GRAVITY) Slide 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 Slide 12 Dual & Binary AGN Dual AGN: are they really? Koss+ 11Komossa+ 03 Dual AGN, with 2 hard X-ray sources 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. Smith+ 10 Double-peaked [OIII] lines in 1% of SDSS QSOs Slide 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 = 19as VLTI astrometry may be able to find spatial offsets between the BLRs Slide 14 Dual & Binary AGN Binary AGN & BH recoil Candidates for binary BHs, or extreme double-peaked BLRs (a la Eracleous)? 1 = 4.2kpc at z=0.27 -> 0.2pc = 48as HHHH Shields+ 09: J1050+3456 @ z=0.272Komossa+ 08: J0927+2943 @ z=0.713 BLR & NLR shifted by 3500km/s BLR & NLR shifted by 2650km/s Dotti+ 09: semi-major axis = 0.34pc 1 = 7.3kpc at z=0.71 -> 0.34pc = 47as Slide 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 Raban+ 09 VLTI 10m image reconstructionSchartmanns simulationsAO observations Linking AO & VLTI scales(hydrodynamical simulations) If these are 2 components of the torus, they imply that it is a dynamical structure, whose properties are driven by star formation stars Slide 16 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 Molecular Gas abundances (e.g. NGC 3227: Davies, Dean & Sternberg 11) observational: line ratios -> LVG -> n, T, n/(dV/dr), [n i ] theoretical: X-ray excitation of gas -> [n i ] vs n/ NGC6951 Gas properties & impact of AGN on abundances Slide 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 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 Robust statistics - VLT large programme on BAT sample of AGN Slide 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 Slide 19 Outflow studies: potential Large Program at IRAM, and complementary programs IRAM PdBI LP? Based on confirmed molecular outflows from our Herschel-PACS GTO and OT archive: -SHINING: 23 RBGS ULIRGs -OT1 (with Veilleux): 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 H 2 O in Mrk231 and NGC6240 -OT2 (with Spoon): OH transitions in IRAS F00183 -OT2 (with Gonzlez-Alfonso): completing OH and H 2 O, NH 3, OH + in 9 (mostly) SHINING (U)LIRGs -OT2 (with Javier, prio2 mid1/3): OH119 in ULIRGs at 0.2 < z < 0.3 with highest SFR and L_AGN -Other Herschel archival data (e.g. GOALS LIRGs?) Slide 20 Step 1a and 1b: Detect and resolve broad CO wings spatial information IRAS F08572 (recent observation) Mrk 231 (Feruglio+2010) 1.2 kpc Slide 21 Step 2: Measure several transitions excitation of the outflowing gas Mrk 231 (Feruglio+2010, Cicone+ in prep) Slide 22 Step 3: 13 CO, HCN, HCO + (optical thickness, densityfor the brightest targets) 5 OH ~700 km/s NGC3079 Arp220 (Sakamoto+2009) Slide 23 V_max, outflow rates, depletion times, energetics, SB vs. AGN driven, dependency on characteristics of host galaxies (evolutionary stage, SFR, L_AGN, etc.) Slide 24 Complementary projects (ongoing and potential) 1) ALMA - OH at high z (e.g. Cloverleaf) (Javier) - [C II] broad wings at 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). Slide 25 Complementary projects (ongoing and potential) 5) SINFONI, XSHOOTER (et al.) - e.g. QSOs at z=2 in 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. nearby Seyferts (Ric) Slide 26 NH3 H2O OI NGC3079 Inflow in PACS spectra Slide 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