Abstract
We used the PCA (Principal Component Analysis) tomography technique to analyze J and K band datacubes for the inner ≈ 350 pc radius of the Seyfert 2 galaxy Mrk 1066, obtained with the Gemini/NIFS (Near-Infrared Integral-Field Spectrograph) at a spatial resolution of ≈ 35 pc. The first eigenvector is dominated by emission from the AGN and host galaxy and corresponds to 95% of the variance of the data. The second eigenvector for the K band presents an anti-correlation between the blue and red wavelengths. In corresponding tomogram, it is observed that the nuclear emission is dominated by red part, and thus we interpret this eigenvector as being due the emission of the dusty torus. A rotating disk is observed in eigenspectrum 2 (in J band) and eigenspectrum 3 (in K band) and their respective tomograms. Correlations among line and radio emission are observed for the next eigenspectrum. Double line profiles are seen in the eigenvector 3 (for the J band) and 4 (K band), probably originated by the interaction of the radio jet with the line-emitting gas. The analysis of the fifth eigenspectrum for the K band and its tomogram shows that the H_{2} emission concentrated in two spiral arms originated from a nuclear ring of molecular hydrogen (with radius of ∼ 0.2") surrounding the nucleus of the galaxy ring and extend to up to 1.5" from the nucleus to northeast and to southwest. This structure was hot seen in the "traditional" analysis of the cube.
