All Figures

	Figure 1: Radial profile of all detected stellar objects with . The mean resolution is , broader than the telescope diffraction limit, as a consequence of the long integration time (3 h) and the large fields.
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In the text

	Figure 2: Objects classification using the MAG_AUTO-MU_MAX plane.
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In the text

	Figure 3: NAOS/CONICA -band image of the field centered at 0:00:16, 2:16:22. The total integration time is 10 350 s. The field size is with a pixel scale of 54 mas. Circles are detected galaxies and boxes are stars. The stellar FWHM is measured to be  . The bright star at the center of the image is used as the AO guide star.
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In the text

	Figure 4: Completeness for extended sources. Galaxies with parameters (,,B/T) uniformly distributed are simulated and placed at random positions in the fields.
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In the text

	Figure 5: Le Phare photometric redshift distribution for the 60 matched objects. The distribution is peaked around , in good agreement with the predictions of simple PLE models. Error bars show poissonnian errors.
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In the text

	Figure 6: Separation between regular and irregular objects. Left: simulated objects (empty squares), right: real objects (crosses).
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In the text

	Figure 7: Asymmetry versus magnitude: asymmetry begins to grow only at magnitudes greater then 22.2 which is greater than the limiting magnitude.
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In the text

	Figure 8: C-A calibration and classification. Boundaries are drawn using an automated classification method (SVM) that avoids the use of a nearby sample and subjective visual classifications. Left: simulated objects, open squares: objects with B/T<0.2, filled squares: objects with B/T>0.8. Right: real objects.
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In the text

	Figure 9: Example of PSF fitting in Fourier space. Squares: observations, dashed line: seeing-limited MTF, dotted line: diffraction-limited MTF. The AO MTF contains higher frequencies than the seeing-limited one. The telescope diffraction limit is not reached however in this example due to the undersampling of the instrumental setup.
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In the text

	Figure 10: Comparison of classification methods, show the probability that a galaxy classified with GIM2D is classified in the same morphological type by C-A. (see text for details).
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In the text

	Figure 11: Example of classification in the three main morphological types at different redshifts. The image size is .
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In the text

Figure 12: Comparison with ground-based observations. We performed a profile fitting on the same real galaxy observed with NACO ( left) and MegaCam (CFHTLS-i' band, right). The galaxy magnitude is KAB=20.5 and i'=21.3. Surface brightness profiles were computed within the isophotal areas enclosed by pixels  above the sky level. The corresponding limiting surface brightness is  mag arcsec-2 for the NACO image and  mag arcsec-2 for the MegaCam image. The fit was done with a pure de Vaucouleurs and exponential profile.

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In the text

	Figure 13: Galaxy distribution: comparison between K-band and I band C-A classifications. The figure shows the probability that a galaxy in the K-band is classified in the same morphological type in the I-band.
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In the text

	Figure 14: Comparison of classifications with different boundaries. We repeat the morphological classification with the boundaries used by Brinchmann et al. (1998). We conclude that the results do not change significantly which supports the validity of the employed method.
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In the text

Figure 15: Redshift distribution for the three morphological types. We plotted the Brinchmann et al. (1998) sample (circles) and our sample observed with ACS (squares) and with NACO (triangles). Brinchmann et al. (1998) and ACS data are corrected to the R rest-frame band. The NACO sample is observed from the K-band and no correction has been applied. The ACS and NACO samples have been separated into two redshift bins (z<0.8and z>0.8). The represented redshifts are the median redshifts of each bin.

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In the text

Figure 16: C-A cut for the ACS images. The same classification procedure has been repeated for the same sample observed with ACS in the I-band. Left: simulated objects. Right: real objects. Circles: B/T<0.2, Filled squares: B/T>0.8, crosses: real objects. Dotted line is the border used in Brinchmann et al. (1998) to separate bulge dominated from disk dominated, dashed line is the one computed in the paper.

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In the text

Figure A.1: Ks corrected number counts compared with other K-band surveys. The solid line is the best fitting power-law in the range , with a slope . Error bars show poissonian errors.


In the text