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Positioning the near-infrared versus optical emission peaks in NGC 1068 with adaptive optics.
The nuclear region of the Seyfert galaxy NGC 1068 has been mapped in thenear-infrared, from 1.25 to 2.23μm, with the ESO adaptive opticsystem COME-ON+, at a spatial resolution of about 0.5". Imaging wascarried out in the standard J, H, K spectral bands. In addition,simultaneous imaging in the near-infrared (K band) and in the visible (Iband) was performed to accurately locate the emission peaks in these twobands. These data show the presence of strong near-infrared emission,within the central 100pc around the nucleus. The dominant emission peakis unresolved at a resolution of about 30pc. The infrared (K band)emission peak is found to be offset by 0.28" south and 0.08" west of theoptical (I band) continuum peak, and so corresponds to the location ofthe hidden nucleus, as defined from maser and molecular emission. Thecompact infrared source, which radiates more than 66% of thenear-infrared flux, appears to be associated with dust heated directlyby the central active nucleus, while the extended near-infrared emissionregion may be related to additional local emitting processes. Wesummarize in this paper the up-to-date existing tentative astrometry forNGC 1068, from UV to radio.
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