Issue |
A&A
Volume 446, Number 3, February II 2006
|
|
---|---|---|
Page(s) | 813 - 825 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361:20042191 | |
Published online | 20 January 2006 |
Near-infrared adaptive optics dissection of the core of NGC 1068 with NAOS-CONICA
1
LESIA, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France e-mail: dgratadour@gemini.edu
2
DOTA-ONERA, Av. de la division Leclerc, Châtillon, France
Received:
15
October
2004
Accepted:
1
September
2005
We present an update analysis of recent near-infrared adaptive optics observations of
NGC 1068 obtained with NAOS-CONICA at VLT/UT4. Ks, and
bands images were deconvolved using MISTRAL, a regularized
algorithm based on a maximum a posteriori estimation of the object. Two
regularization methods, one including a new maximum likelihood estimation of
the object Power Spectral Density, and an edge preserving one, have
been tested and converge to consistent results. The deconvolved images show
a coherent evolution of the IR emission from 2.2 to 4.8
.
Deconvolution brings new elements: a) it strengthens the very peculiar
nature of the four parallel elongated nodules previously discovered along
the jet, which appear unresolved perpendicular to their long axis; b) it
underlines the strong correlation between UV clouds and IR features, and c)
it provides a more accurate multi-wavelength registration of the actual
active nucleus. The overall aspect of the central
IR
emission seems to point to the jet as a major mechanism to shape the NLR.
For each identified structure, we derive a color temperature now based on
three bands (M, L and K), before and after deconvolution, confirming the
need for clumps of dust at unexpectedly high and almost constant temperature
(about 500 K) up to 70 pc north of the nucleus. We explore several
mechanisms to explain the color temperature and show that shocks, induced
for instance by the interaction of the jet with a giant cloud, is unlikely
to be the dominating mechanism to heat the dust. We detail our model
of transient heating of Very Small Grains and show that it can
provide a consistent explanation of the K, L, M colors and their lack of
variation with distance when 0.6 nm diamond-like grains are heated by 4 to
8 eV UV photons. However, we do not exclude the possibility that part of the
excitation could come from shocks. At Ks, deconvolution reinforces the
previous claim that the central core is partially resolved along the N-S
direction: the best fit to our data is an elliptical Gaussian extended
along
with a 2.1 pc FWHM along this direction. This result agrees
with the predictions of the radiative transfer model we previously
developed to interpret the spectroscopic behavior at K, and is consistent with
VLTI/VINCI measurements. Several questions are raised by this study: a)
is the jet dominant in shaping the NLR of this AGN? b) what is the real
state of the dust in the environment of the core; c) is the simple
doughnut torus model able to explain IR emission of the central
source with a morphology that appears increasingly complex at small scale?
Key words: galaxies: Seyfert / galaxies: individual: NGC 1068 / infrared: galaxies / techniques: image processing / radiative transfer / galaxies: jets
© ESO, 2006
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