richard davies, eckhard sturm max planck institute for extraterrestrial physics, germany

Richard Davies, Eckhard SturmMax Planck Institute for Extraterrestrial Physics, Germany

near-IR

VLT/SINFONI

far-IR

Herschel/PACS

mm

IRAM/PdBI

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

AGN? AGN?

near-IR

VLTI/GRAVITY

http://www.mpe.mpg.de/

1kpc 100pc 10pc 1pc 0.1pc 0.01pc

circumnuclear torques, spirals, …

star formation

molecular gas

hot dust

BLR

Inflow Inflow Outflow Outflow

0.1pc 1pc 10pc 100pc 1kpc

ionisation conescoronal 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 Műller+ 11, Davies+ 09, Hicks, RD, + in prep, Müller Sánchez, 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



star formation

molecular gas

hot dust

BLR





ionised outflows

L AGN/L

Edd

Starburst Age (Myr)GC

CO absorption

K band non-stellar & stellar continuumNGC1097

stellar velocity stellar dispersion



star formation

molecular gas

hot dust

BLR





ionised outflows

Molecular Gas – high excitation CO lines (Hailey-Dunsheath+ 12)

ME – H2 ring HE – infall clumpPDR (stars) no recent starburstPDR (AGN) obscuration covering factor vs densityshock if ring is shock heated jet/cloud interaction (but fine tuning)XDR if ring is X-ray heated if clump is X-ray heated



star formation

molecular gas

hot dust

BLR





ionised outflows

NGC6814

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

residual (disk) residual (disk+cones)

Vmax vs θout MH2 vs θout



star formation

molecular gas

hot dust

BLR





ionised outflows

Atomic & Ionised Outflow in M82(Contursi+ )

HST + WIYN Chandra (blue)Spitzer (red)

[OIII] 88μm velocity [OIII] 88μm dispersion [OIII] 88μm / [OI] 63μm [CII] 158μm opacity

• 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



star formation

molecular gas

hot dust

BLR





ionised outflows

Vmax vs SFR & LAGN

Molecular Outflows OH absorption in ULIRGs & AGN (Fischer+10, Sturm+ 11 & in prep)



star formation

molecular gas

hot dust

BLR





ionised outflows

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”

Cecil+ 01

HCN1-0 Dodds-Eden+ in prepCO2-1

5”

PACS: OH 119μm absorption

PdBI: HCN, HCO+, SiO, HNC absorption



star formation

molecular gas

hot dust

BLR





ionised outflows

What next?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 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 BLRe.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 sources1000km/s @ NGC1068 (14.4Mpc) = 14μas/yr

Circinus (4.2Mpc) = 49μas/yrCen A (3.5Mpc) = 59μas/yr

velocities up to 3200km/s (Cecil+ 02)

Vmax = 1900km/s (Müller Sánchez+ 11)

[FeII]Outflow in NGC1068

[SiVI]

[OIII] Coronal Line Clouds (GRAVITY)

Dual & Binary AGNDual & Binary AGNDual AGN: are they really?

Koss+ 11 Komossa+ 03Dual 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

Dual & Binary AGNDual & Binary AGNBinary AGN & BH recoil

Boroson & Lauer 09, Lauer & Boroson 09 BLR+NLR

BLR only

absorption

BLRs shifted by 2650km/sBest candidate for binary BH, ~0.1pc separation?

1” = 5.2kpc at z=0.38 -> 0.1pc = 19μasVLTI astrometry may be able to find spatial offsets between the BLRs

Dual & Binary AGNDual & Binary AGNBinary AGN & BH recoil

Candidates for binary BHs, or extreme double-peaked BLRs (a la Eracleous)?

1” = 4.2kpc at z=0.27 -> 0.2pc = 48μas

HαHβ

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 = 0.34pc1” = 7.3kpc at z=0.71 -> 0.34pc = 47μas



Raban+ 09

VLTI 10μm image reconstruction Schartmann’s simulations AO 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



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

Gas properties & impact of AGN on abundances



• 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

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 H2O in Mrk231 and NGC6240

-OT2 (with Spoon): 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 at 0.2 < z < 0.3 with highest SFR and L_AGN

-Other Herschel archival data (e.g. GOALS LIRGs?)

Step 1a and 1b: Detect and resolve broad CO wings spatial information

IRAS F08572 (recent observation)

Mrk 231 (Feruglio+2010)

1.2 kpc

Step 2: Measure several transitions excitation of the outflowing gas

Mrk 231 (Feruglio+2010, Cicone+ in prep)

Step 3: 13CO, HCN, HCO+ … (optical thickness, density…for the brightest targets)

5”

OH

~700 km/sNGC3079

Arp220 (Sakamoto+2009)

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

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) HSTWith 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) GEMINIRupke/Veilleux (NaID, etc.) spatially resolved atomic and ionized outflowing gasWith 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).

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)

NH3

H2OOI

NGC3079

Inflow in PACS spectra

richard davies, eckhard sturm max planck institute for extraterrestrial physics, germany

Documents

gravity binary agn

nearby agn

binary bhs

ao vlti scales

iramalma hstgeminiwhat

pc separation

lauer boroson

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