NGC7469 is a Seyfert 1 and NGC1068 is a Seyfert 2. Due to the adaptive optics system, the infrared camera field has a position fixed in regard to the centroid of the visible counterpart of the object observed. Any offset of the galaxy infrared peak relatively to the star infrared peak would correspond to a real offset between the galaxy infrared peak and its visible peak. In the case of NGC7469, we find no significant shift between the L band peak and the visible continuum peak.
North is up, east to the left.
In the case of NGC1068, our data show the presence of strong near-infrared emission within the central 100pc around the nucleus. For both K, L and M bands, the dominant emission peak is unresolved at resolutions down to 17 pc. From our first estimate of the near-infrared fluxes in K, L and M, we derive a dust temperature of 750 K. Dust properties Based on the flux measurements, we can deduce a blackbody temperature for the dust. In the former, we have derived the grain density as a function of distance from the central source. The dust can be heated up to T eff , the effective temperature of the nuclear radiation on the inner edge of the torus.