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We present the first near-infrared K-band long-baseline interferometricmeasurement of the prototype Seyfert 2 galaxy NGC 1068 with resolution lambda/B\~ 10 mas obtained with the Very Large Telescope Interferometer (VLTI) and thetwo 8.2m Unit Telescopes UT2 and UT3. The adaptive optics system MACAO wasemployed to deliver wavefront-corrected beams to the K-band commissioninginstrument VINCI. A squared visibility amplitude of 16.3 +/- 4.3 % was measuredfor NGC 1068 at a sky-projected baseline length of 45.8 m and azimuth angle44.9 deg. This value corresponds to a FWHM of the K-band intensity distributionof 5.0 +/- 0.5 mas (0.4 +/- 0.04 pc) at the distance of NGC 1068) if itconsists of a single Gaussian component. Taking into account K-band speckleinterferometry observations (Wittkowski et al. 1998; Weinberger et al. 1999;Weigelt et al. 2004), we favor a multi-component model for the intensitydistribution where a part of the flux originates from scales clearly smallerthan about 5 mas (<0.4 pc), and another part of the flux from larger scales.The K-band emission from the small (< 5 mas) scales might arise fromsubstructure of the dusty nuclear torus, or directly from the central accretionflow viewed through only moderate extinction.Comment: Accepted for publication in Astronomy and Astrophysics Letter

VLTI/VINCI observations of the nucleus of NGC 1068 using the adaptive optics system MACAO