The AGN Team: R. Davies, R. Genzel, L. Tacconi, F. Müller Sánchez, E. Hicks, S. Friedrich

Huatulco, April 18th, 2007

Imaging Spectroscopy of the centers of nearby AGN: Direct observation of the Torus and the Stellar

Dynamical Black Hole Mass in NGC1068Francisco Müller Sánchez

Science Objectives

Object Classification D (Mpc) Resolution _ NGC 1097 LINER, Sy1 18 0.245” 21pc NGC 2992 Sy1 33 0.30” 48pc NGC 3227 Sy1 17 0.085” 7pc NGC 3783 Sy1 42 0.18” 37pc NGC 7469 Sy1 66 0.085” 27pcNGC 1068 Sy2 14 0.085” 6pc Circinus Sy2 4 0.22” 4pc Mkn 231 ULIRG, Sy1, QSO 170 0.176” 145pc IRAS 05189–2524 ULIRG, Sy1 170 0.12” 100pc

Using adaptive optics on VLT to reach scales down to 0.075” in the H- and K- bands, we can for the first time directly resolve the nuclear region of AGN and investigate:

- Star formation activity

- The properties of the molecular gas and its relation to the torus

- Black Hole mass from stellar dynamics

- The forbidden high-ionization lines

Using adaptive optics on VLT to reach scales down to 0.075” in the H- and K- bands, we can for the first time directly resolve the nuclear region of AGN and investigate:

- Star formation activity

- The properties of the molecular gas and its relation to the torus

- Black Hole mass from stellar dynamics

- The forbidden high-ionization lines

The instrument: SINFONI

SINFONI is an AO assisted near-infrared integral field spectrograph (SPIFFI) for the VLT:

- λ range from 1.1 - 2.45 µm

- Slicing into 32 slices

- 2048x2048 HAWAI 2RG detector

- slit width is selectable between 0.25", 0.1" and 0.025“

- Corresponding FOV sizes are 8"×8", 3.2"×3.2" and 0.8"×0.8“

- Four gratings provide spectral resolving powers of R=2000, 3000, 4000, 1500 in J, H, K, and H+K band, respectively

SINFONI is an AO assisted near-infrared integral field spectrograph (SPIFFI) for the VLT:

- λ range from 1.1 - 2.45 µm

- Slicing into 32 slices

- 2048x2048 HAWAI 2RG detector

- slit width is selectable between 0.25", 0.1" and 0.025“

- Corresponding FOV sizes are 8"×8", 3.2"×3.2" and 0.8"×0.8“

- Four gratings provide spectral resolving powers of R=2000, 3000, 4000, 1500 in J, H, K, and H+K band, respectively

R (pc)

SINFONI Data

• Recent star formation in nuclear disks of size ~50pc

• Starburst luminosity is a few percent of AGN on scales <10pc, but comparable to AGN on kpc scales

• On small scales, starbursts are very intense & short lived– Brγ equivalent width– Supernova rate– Mass-to-light ratios

• Suggestion of a delay between starburst activity & AGN activity

• Recent star formation in nuclear disks of size ~50pc

• Starburst luminosity is a few percent of AGN on scales <10pc, but comparable to AGN on kpc scales

• On small scales, starbursts are very intense & short lived– Brγ equivalent width– Supernova rate– Mass-to-light ratios

• Suggestion of a delay between starburst activity & AGN activity

Nuclear Star Formation in AGN

Dav

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• HWHMs generally less than 50 pc

• Sérsic fits suggest disk-like distributions

• Ordered velocity field suggests rotation

• Velocity dispersion is equal to or greater than the velocity speeds– Shocks can only account for a

dispersion up to 70 km s-1

– Remaining dispersion due to bulk motion of the gas, i.e. a thick disk

– Heating from a nuclear starburst and/or the AGN can maintain the vertical structure

• HWHMs generally less than 50 pc

• Sérsic fits suggest disk-like distributions

• Ordered velocity field suggests rotation

• Velocity dispersion is equal to or greater than the velocity speeds– Shocks can only account for a

dispersion up to 70 km s-1

– Remaining dispersion due to bulk motion of the gas, i.e. a thick disk

– Heating from a nuclear starburst and/or the AGN can maintain the vertical structure

Molecular gas in AGN

Morphologies of the coronal lines

NGC1068

- Seyfert 2

- D = 14 Mpc: 1” = 70 pc

- Spiral galaxy (Sb)

- Two datasets (25 and 100 mas H+K)

- Seyfert 2

- D = 14 Mpc: 1” = 70 pc

- Spiral galaxy (Sb)

- Two datasets (25 and 100 mas H+K)

CO 2-1 traces cold H2 at 0.7” resolution(Schinnerer et al. 00)

1-0 S(1) traces hot H2 at 85 mas resolution(Mueller Sanchez et al. 07)

CO 2-1 traces cold H2 at 0.7” resolution(Schinnerer et al. 00)

1-0 S(1) traces hot H2 at 85 mas resolution(Mueller Sanchez et al. 07)

Molecular gas in NGC1068

5GHz radio continuum & sketch from Gallimore et al. 96

5GHz radio continuum & sketch from Gallimore et al. 96

1” = 70pc resolution

Jet/Cloud interaction in NGC1068

Molecular Gas and the Torus in NGC1068

5GHz radio continuum of S1 source (Gallimoreet al. 04) with maser spots (Greenhill et al. 96).

VLT interferometrywarm 300K dust emission with size scale ~3pc FWHM (Jaffe et al. 04)

Torus models- Fritz et al. (06): 17pc radius- Schartmann et al. (05): 5pc ‘torus radius’ (70pc outer)- Hoenig et al. (06): 17pc radius

VLT interferometrywarm 300K dust emission with size scale ~3pc FWHM (Jaffe et al. 04)

Torus models- Fritz et al. (06): 17pc radius- Schartmann et al. (05): 5pc ‘torus radius’ (70pc outer)- Hoenig et al. (06): 17pc radius

Evidence for inflow:northern part moving towards us & southern part away with a difference of ~100km/s

Evidence for inflow:northern part moving towards us & southern part away with a difference of ~100km/s

Fuelling the AGN

Mdyn from gas dispersion: Mdyn = 5.2x10^7 Msun

Mdyn from stars: Mdyn = 2.3x10^7 Msun

Mdisk = 3.2x10^7 Msun

Mgas = 4.5x10^7 Msun

Mbh = 1x10^7 Msun

Mdust = 4.5x10^5 Msun

nuclear disk:radius ~70 pcmass ~1.8×108 Msunscale height ~6 pc

nuclear disk:radius ~70 pcmass ~1.8×108 Msunscale height ~6 pc

stars

disp

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loci

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molecular gas

Nuclear disk in NGC1068

Star formation in NGC1068

Dispersion at 0.5” = 100 km/s

Mstars = 1.8 x 108 Msun

LK = 4.5 x 107 Lsun

M/LK = 4 Age = 200-400 Myrs

Dispersion at 0.5” = 100 km/s

Mstars = 1.8 x 108 Msun

LK = 4.5 x 107 Lsun

M/LK = 4 Age = 200-400 Myrs

M

N

O

P

Q

RS

L

M

N

O

P

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Ionized gas

Z = 2 Zsun

Z = 1 ZsunZ = 1 Zsun

Z = 2 Zsun

-1.2-1.4-1.7-2.0

L

MN P

Q

RS

Photoionization models

Molecular hydrogen nuclear disk on size of ~50pcRecent star formation in nuclear disks of size ~50pcDistribution and Kinematics of both the nuclear stars and molecular hydrogen are consistent with clumpy torus modelsTorus is a mixture of stars and gasSuggestion of a delay between starburst activity & AGN activityFantastic amount of detail to study in individual galaxies.

Increase sample size with LGSFSpatially resolve nuclear disks

Sigma dropsFueling of AGN

Measure MBH in reverberation mapped AGNCalibration of indirect methodConstrain BLR geometry

Summary and Future studies

nuclear disk:radius ~40 pcmass ~2.0×108 Msunscale height ~9 pc

nuclear disk:radius ~40 pcmass ~2.0×108 Msunscale height ~9 pc

stars molecular gas

velo

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disp

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Nuclear Disks: NGC1097