Black Hole Feeding & Feedback: what can we learn from nearby AGN?

Transcription

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

2 Inflow Outflow circumnuclear torques, spirals, 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: 1kpc 100pc 10pc 1pc 0.1pc 0.01pc star formation BH mass Davies+ 09, Hicks, RD, hot + dust in prep, Müller molecular gas BLR Fathi+ 06, Storchi-Bergmann+ 07, 09, 10, Riffel+ 08, 09, 11, Schnorr Műller+ 11, Sánchez, RD, + in prep 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 NGC1097 coronal line clouds ionisation cones ionised outflows 0.1pc 1pc 10pc 100pc 1kpc molecular outflows

3 Inflow CO absorption K band non-stellar & stellar continuum NGC1097 circumnuclear torques, spirals, BLR Outflow - 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, C 2 at 1.78μm) coronal line clouds (Melbourne & Davies) ionisation cones ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc 0.1pc 1pc 10pc 100pc 1kpc star formation stellar velocity molecular gas BH mass hot dust stellar dispersion L AGN /L Edd molecular outflows GC Starburst Age (Myr)

4 Inflow Outflow Molecular Gas high excitation CO lines (Hailey-Dunsheath+ 12) circumnuclear torques, spirals, BLR coronal line clouds ionisation cones ionised outflows 1kpc 100pc 10pc 1pc 0.1pc 0.01pc 0.1pc 1pc 10pc 100pc 1kpc star formation hot dust BH mass molecular outflows molecular gas ME H 2 ring HE 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

5 Inflow circumnuclear torques, spirals, BLR 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 θ out, V max, and M H2 coronal line clouds ionisation cones ionised outflows 1kpc 100pc 10pc 1pc residual 0.1pc (disk) 0.01pc residual 0.1pc (disk+cones) 1pc 10pc 100pc 1kpc NGC6814 star formation hot dust BH mass molecular outflows molecular gas V max vs θ out M H2 vs θ out

6 Inflow Outflow Atomic & Ionised Outflow in M82 (Contursi+ ) disk/outflow kinematically separated broad base to N outflow circumnuclear torques, spirals, 1kpc 100pc 10pc 1pc 0.1pc 0.01pc HST + WIYN coronal line clouds model neutral gas as PDR, excited BLR by central starburst maps of G 0, n, T, N HI hole in τ[cii], matching HCO ring, with brighter Hα inside Chandra (blue) Spitzer (red) ionisation cones ionised outflows 0.1pc 1pc 10pc 100pc 1kpc star formation hot dust BH mass molecular outflows molecular gas [OIII] 88μm velocity [OIII] 88μm dispersion [OIII] 88μm / [OI] 63μm [CII] 158μm opacity

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

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

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

10 What next? Exploiting Broad GRAVITY Line Region & Black Hole Masses (GRAVITY) Binary Evidence AGN that some BLRs are partially supported by rotation: Coronal Line Clouds (GRAVITY) [OIII] e.g. - NLS1 maybe preferentially pole-on (Peterson+ 00, Boroson 11) Linking AO & VLTI scales Outflow using in hydrodynamical NGC1068 simulations - double-peaked BLRs (Eracleous+ 2003) Gas properties & impact of [FeII] AGN on abundances [SiVI] - disk+wind structure in Mkn 110 (Kollatschny+ spatially 03; resolved see also line Elitzur+ ratios Robust 08) statistics VLT large programme on BAT sample of AGN Future outflow - mass studies ratio distribution with IRAM/ALMA (Collin+& 06) HST/Gemini - more velocity resolved reverberation mapping (Bentz+ 10) VLTI does - not emission resolve line BLR, EW but distribution astrometry (Risaliti+ can measure 11) velocity gradient velocities up to - astrometry to <0.5% of FWHM easily achievable, simple phase 3200km/s (Cecil+ 02) measurement for VLTI - fraction of BLRs with rotation; their V max size, = PA; 1900km/s & mass (Müller of central Sánchez+ BH 11) 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, λl 1500 >10 44 erg/s -> several hundred 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 Double-peaked [OIII] lines in 1% of SDSS QSOs AO imaging Fu+11 & Rosario+ 11: % 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

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: z=0.713 Shields+ 09: z=0.272 BLR & NLR shifted by 2650km/s Hβ Hα 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 Linking AO & VLTI scales (hydrodynamical simulations) Binary AGN VLTI Linking 10μm AO image & VLTI reconstruction scales using hydrodynamical Schartmann s simulations simulations AO observations Gas properties & impact of AGN on abundances spatially resolved line ratios stars Robust statistics VLT large programme on BAT sample of AGN Future outflow studies with IRAM/ALMA & HST/Gemini 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? Exploiting GRAVITY Gas properties & impact of AGN on abundances Binary AGN Molecular Gas abundances Linking AO & VLTI scales NGC6951 using hydrodynamical (e.g. NGC 3227: simulations Davies, Dean & Sternberg 11) Gas properties & impact of AGN on observational: abundances spatially resolved line ratios Robust statistics VLT large programme line on BAT ratios sample -> LVG of -> AGN n, T, n/(dv/dr), [n i ] theoretical: Future outflow studies with IRAM/ALMA & HST/Gemini X-ray excitation of gas -> [n i ] vs n/ζ

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

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 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 NGC OT2 (with Spoon): OH transitions in IRAS F OT2 (with González-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?)

20 Step 1a and 1b: Detect and resolve broad CO wings spatial information Mrk 231 (Feruglio+2010) 1.2 kpc IRAS F08572 (recent observation)

21 Step 2: Measure several transitions excitation of the outflowing gas Mrk 231 (Feruglio+2010, Cicone+ in prep)

22 Step 3: 13 CO, HCN, HCO + (optical thickness, density for the brightest targets) Arp220 (Sakamoto+2009) NGC3079 ~700 km/s 5 OH

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 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).

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)

26 Inflow in PACS spectra NH3 OI H2O NGC3079

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