All Figures

	Figure 1: CCD image of NGC 2336 in the V passband.
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In the text

Figure 2: NGC 2336 photometric profiles (in mag arcsec-2) along the major axis of the galaxy ( ) ( a), b)), and along the major axis of the bar ( ) ( c), d)), in the U (dotted line), B (dashed line), V (solid line) ( a), c)), and V (solid line), R (dashed line), and I (dotted line) ( b), d)) passbands. Negative angular distances correspond to the southern ( a), b)) and the eastern ( c), d)) parts of NGC 2336. These profiles cut across the galactic components at the following locations: ( a),  b)) nucleus ( ), bulge ( ), ring ( ), external disk ( ), spiral arms ( ); ( c), d)) nucleus ( ), bulge ( ), bar ( ), ring ( ), spiral arms ( ). The two sharp-peaked maxima in ( a), b)) at radii of and are field stars. The coordinate accuracy is .

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In the text

	Figure 3: Isophotal map of NGC 2336 in the a) B and b) I passbands. The isophotal contour levels a) 20.0, 21.0, 21.5, 22.0, 22.5, 23.5, 24.5 B mag arcsec-2, and b) 19.5, 20.0, 20.5, 21.0, 21.5, 22.0, 22.5 I mag arcsec-2, are shown.
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In the text

	Figure 4: The dependence of a) position angle and b) ellipticity ( ) of the smoothed isophotes of NGC 2336, on the angular distance r from the galaxy center, in the U (thick solid line), B (long dashed line), V (dotted line), R (short dashed line) and I (thin solid line) passbands.
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In the text

	Figure 5: NGC 2336 color index maps in a) U-B, b) B-V, c) V-R, and d) R-I. Contours of constant color index are shown, with levels set at: a) U-B = 0.2, 0.4, 0.6 mag, b) B-V = 0.45, 0.6, 0.75 mag, c) V-R = 0.35, 0.42, 0.5 mag, and d) R-I = 0.4, 0.5 mag. Redder regions are shaded darker than bluer ones. Regions with SNR < 5 are indicated by the white areas.
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In the text

Figure 6: NGC 2336 color profiles along the major axis of the galaxy ( ) ( a), b)), and along the major axis of the bar ( ) ( c), d)), in the ( a), c)) U-B (solid line), B-V (dashed line), V-R (solid line), and R-I (dashed line) ( b), d)) color indices. Only profiles for regions having are shown. Negative angular distances correspond to the southern ( a), b)) and eastern parts ( c), d)) of NGC 2336. These profiles cut across the galactic components at the following locations: ( a), b)) nucleus ( ), bulge ( ), ring ( ), external disk ( ), spiral arms ( ); ( c), d)) nucleus ( ), bulge ( ), bar ( ), ring ( ), spiral arms ( ). The coordinate accuracy is .

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In the text

Figure 7: a) The radial light distribution dependence on the angular distance r from the center of NGC 2336, in the U (thick solid line), B (long dashed line), V (dotted line), R (short dashed line) and I (thin solid line) passbands. b) Comparison of our data (solid lines) with results from Boroson (1981) for the B passband (diagonal crosses), and with those from Heraudeau & Simien (1996) for the V passband (vertical crosses).

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In the text

Figure 8: Two-color diagrams: a) (U-B)0i vs. (B-V)0i, b) (B-V)0i vs. (V-R)0i, and c) (B-V)0i vs. (V-I)0i for different regions in NGC 2336. The boxes enclose the observed positions of the integrated color indices for galaxies which follow the normal color sequence (NCS), as calculated in Buta & Williams (1995). The dashed curves in a) represent evolutionary tracks for stellar systems with: constant star formation rate (long dashed curve), and an instantaneous starburst (short dashed curve), with the objects ageing (and reddening) from 1 Myr to 15 Gyr during their approach to the NCS (the small vertical crosses indicate ages of: 10 Myr, 100 Myr, 1 Gyr and 10 Gyr). These tracks were calculated using the PEGASE2 code (see Fioc & Rocca-Volmerange 1997). The dotted curve towards the top right of a) shows the color change resulting from a starburst in an old stellar system (age 15 Gyr), from Fioc & Rocca-Volmerange (1997), with the young (age 1 Myr) population mass fraction changing from (bottom) to (top). The short dashed arrows in the bottom left of each plot show the direction of the correction for internal absorption due to dust in the galaxy. The vertical and horizontal bars show the color index measurement errors for each region of the galaxy. The numbers denoting these regions are explained in the text (see Sect. 3.4).

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In the text

Figure 9: Graphical description of the method used to estimate the ages and intrinsic reddenings for star formation regions, by their positions in the two-color diagram. Evolutionary tracks of synthetically aged stellar systems with Z = 0.008 (dotted curve), 0.02 (solid curve), and 0.05 (long dashed curve), are shown. The numbers (106 and 107) are the ages of the synthetic systems in years. The arrow gives the direction of the correction for dust absorption, and its length corresponds to an extinction of A(V) = 0.5 mag. Color index error bars are shown for a typical star formation region.

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In the text

Figure 10: Two-color diagrams: a) (U-B)0i vs. (B-V)0i, b) (B-V)0i vs. (V-R)0i, and c) (B-V)0i vs. (V-I)0i, for the NGC 2336 star formation regions. Evolutionary tracks of synthetically aged stellar systems, with Z = 0.008 (short dashed curves), 0.02 (solid curves), and 0.05 (long dashed curves), are shown. Small vertical crosses indicate system ages of: 1, 10, 100 Myr and 1 Gyr. The numbers are the base 10 logarithms of the system ages in years. The color index error bars are shown. Short dashed arrows give the direction of the correction for internal dust absorption in the galaxy.

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In the text

	Figure 11: Number distribution histograms of the star formation regions in NGC 2336, by: a) diameter, b) age, and c) deprojected distance from the galaxy center.
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In the text