All Figures

	Figure 1: Compilation of the KMAC1: main steps of reduction and source catalogues.
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In the text

	Figure 2: Systematic dependence of the image size parameter  on the CCD x-coordinate. Different line types correspond to instrumental magnitudes v from 10 to 16.
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In the text

	Figure 3: Preliminary differences KMAC1-CMC13 in Dec plotted versus  for a few scans; stars are devided into three groups depending on v and shifted vertically by 0.5'' for clearness. Open circles refer to star images with the largest x>1050 px separation from the CCD reading register. Symbol size is proportional to v.
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In the text

	Figure 4: KMAC1-CMC13 differences versus for the stars of 12-14 mag: before and after calibration for instrumental errors.
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In the text

	Figure 5: Systematic differences KMAC1-CMC13 in Dec as a function of magnitude for 10 groups of star fields ordered by RA; before ( upper panel) and after ( bottom) calibration (3).
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In the text

	Figure 6: Systematic effect in measured V values: a) found from a comparison to photometric data by Sung et al. (2003) (crosses), Kuznetsov et al. (2003) (circles), Internet WEBDA database (inclined crosses) and Tycho2 (squares); b) the bias simulated with the model (5).
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In the text

	Figure 7: Two-color diagrams : a) for NGC 2264 stars, symbol size indicates star brightness (9 to 16 mag); b) for all stars, large dots show V<10.5 mag stars. Solid line (4) fits the bright star location, the dashed line refers to all stars, thick arrows show the direction of interstellar reddening. A geometry explaining the model (5) is also shown (see text).
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In the text

	Figure 8: Individual estimates (5) of bias in magnitudes for all stars, and its approximation (6) by the solid line.
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In the text

	Figure 9: color diagram for all stars, with V corrected. The solid line is the fitting function (7).
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In the text

	Figure 10: Magnitude residuals as a function of V: a) V-r' differences measured with reference to the fitting curve shown in Fig. 9; b) residuals between the KMAC1 and the Valinhos catalogue V values.
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In the text

	Figure 11: Correlation between Tycho2-CMC13 and Tycho2-KMAC1 preliminary differences: a) - in RA; b) - in Dec; correlation between Tycho2-UCAC2 and Tycho2-KMAC1 preliminary differences: c) - in RA; d) - in Dec; only differences exceeding 0.15'' are shown.
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In the text

	Figure 12: Distribution of KMAC1-CU fields across the sky.
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In the text

	Figure 13: Distribution of KMAC1 star number per field on rightascensions.
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In the text

	Figure 14: Distribution of the KMAC1-T (solid) and KMAC1-CU (dashed) star magnitudes.
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In the text

	Figure 15: Internal mean accuracy of one catalogue entry as a function of magnitude.
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In the text

	Figure 16: Rms residuals of the KMAC1 positions with the CMC13 and UCAC2; upper panel - for the version "T''; bottom - for the version "CU''.
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In the text

	Figure 17: External errors of the KMAC1 ("T'' and "CU'' versions) positions (curves) and photometry (open circles).
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In the text

	Figure 18: Systematic differences and of the KMAC1-T and KMAC1-CU positions to those in the CMC13 and UCAC2 as a function of magnitude.
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In the text

	Figure 19: Individual differences of declinations in the KMAC1-T and in CMC13 and UCAC2.
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In the text