Richard Davies, Reinhard Genzel, Linda Tacconi, Francisco Mueller S

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Richard Davies, Reinhard Genzel, Linda Tacconi,
Francisco Mueller Sánchez, Susanne Friedrich Max
Planck Institute for Extraterrestrial Physics and
Amiel Sternberg University of Tel Aviv, Israel

• extent, intensity, history of recent star
  formation and relation to AGN
• distribution kinematics of molecular gas, and
  relation to obscuring material
• black hole mass from stellar dynamics to test
  reverberation masses (BLR geometry) MBH-s
  relation

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Molecular Gas in NGC1068
CO 2-1 traces cold H2 (Schinnerer et al. 00) 1-0
S(1) traces hot H2
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Jet/cloud interaction in NGC1068
1 70pc
resolution
5GHz radio continuum sketch from Gallimore et
al. 96
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Molecular Gas the Torus in NGC1068
VLT interferometry warm 300K dust emission
with size scale 3pc FWHM (Jaffe et al.
04) static torus models Fritz et al. (06)
17pc radius Schartmann et al. (05) 5pc torus
radius (70pc outer) Granato et al. (97) 19pc
radius
5GHz radio continuum of S1 source (Gallimore et
al. 04) with maser spots (Greenhill et al. 96).
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Adaptive Optics Observations of AGN with Keck
VLT
ApJ, 613, 781 ApJ, 602, 148 ApJ, 646,
754 AA, 454, 481
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CO equivalent width measuring stellar continuum
STARS stellar cluster models WCO6-3 4.5Å
WCO2-0 12Å
adapted from Oliva et al. 1995
can correct for dilution estimate stellar
continuum
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Star Formation Diagnostics
NGC1068

• Br? equivalent width
• correct Br? for AGN contribution (e.g. NLR, jet)
  through morphology kinematics
• ratio to stellar continuum

• mass-to-light ratio
• use spatially resolved kinematics (Vrot s) to
  estimate dynamical mass
• correct LK for non-stellar continuum
• gives upper limit to M/LK for most recent star
  formation

Mkn 231

• radio continuum (supernova rate)
• resolved continuum with low TB probably star
  formation
• correct flux for unresolved point source
  associated with AGN, and also for any jet
  contribution
• estimate supernova rate

Carilli et al. (1998)
0.06 beam source size 0.440.31
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stars
molecular gas
Nuclear Disks NGC1097
velocity
dispersion
nuclear disk radius 40 pc mass 2.0108
Msun scale height 9 pc
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stars
molecular gas
Nuclear Disks NGC1068
velocity
dispersion
nuclear disk radius 70 pc mass 1.2108
Msun scale height 6 pc
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Star Formation Size Age
nuclear stellar continuum resolved in all cases
no distinct significant compact component on
scales smaller than this age is 5-300 Myr but
typically no longer active
Cid Fernandes 04 central 200pc of 79 nearby
Seyfert 2s 1/3-1/2 have experienced
significant star formation in last few hundred
Myr Kauffmann 03 central few kpc of 22600 AGN
in SDSS a significant fraction have
experienced star formation in the recent (Gyr)
past
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Stellar vs AGN Luminosity
starburst luminosity is a few percent of AGN on
scales lt10pc, but comparable to AGN on kpc scales
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Stellar Bolometric Luminosity
Eddington limited starbursts in central 10 pc
M51 star clusters or Arp 220 (Scoville
03) radiatively supported starburst models
(Thompson et al. 05)
note 500Lsun/Msun 1013Lsun/kpc2 for
S2104Msun/pc2
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stellar bolometric luminosity
Eddington limited starburst implies short star
formation timescale perhaps why we dont see
current activity
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Starburst AGN connection
Eddington ratio
roughly AGN luminosity
best estimate of time since most recent star
forming episode began
Delay of close to100 Myr between starburst AGN
activity
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Summary

• adaptive optics integral field spectroscopy of
  mostly type 1 AGN, with spatial resolution to
  better than 10pc
• detailed morphologies kinematics of molecular
  gas (e.g. NGC1068) and stars
• star formation
• recent star formation in nuclear disks
• on 10pc scales, starbursts are Eddington limited
  short lived
• suggestion of a delay between starburst activity
  AGN activity