All Figures

$\begin{figure} \par\includegraphics[width=8cm,height=11cm,clip]{fig01.eps} \end{figure}$ Figure 1: Photometric errors in V magnitude and U-B, B-V andV-I colours as a function of V.
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In the text

$\begin{figure} \par\includegraphics[width=16.2cm,clip]{fig02.eps} \end{figure}$ Figure 2: Finding chart of the NGC 1582 region ( $40^{\prime } \times 40^{\prime }$ and J filter). The black solid circle, $15^{\prime }$ in radius, indicates the adopted angular size for the cluster (see Sect. 3.1 and Fig. 3). The grey square indicates the area covered from Asiago. Adopted cluster members and probable cluster members are shown with small circles and triangles, respectively. For a coordinate reference, the center (X = 0; Y=0) corresponds to the cluster coordinates (see Table 1) and each X-Y unit is $0\hbox{$.\!\!^{\prime\prime}$ }465$ .
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{fig03.eps} \end{figure}$ Figure 3: Stellar surface density profile in the region of NGC 1582 as a function of the radius. Data have been taken from 2MASS catalog. Dotted lines indicate the adopted limits for the cluster and for the comparison field related with Fig. 8b.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{fig04.eps} \end{figure}$ Figure 4: a) Vector point plot for the stars $20^{\prime }$ around the center of NGC 1582 (data from HD Extension Charts and Tycho-2 catalogs). b) Radial velocities obtained from Echelle spectra. See captions of Figs. 6 and 8 for the meaning of the symbols. The crosses indicate the mean error values.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{fig05.eps} \end{figure}$ Figure 5: Spectra of a sample of bright stars in the field of NGC 1582. A few interesting lines are indicated. See Table 3 for details.
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In the text

$\begin{figure} \par\includegraphics[height=9cm]{fig06.eps} \end{figure}$ Figure 6: Color-color diagrams (CCDs) of stars in the region of NGC 1582. a) U-B vs. B-V diagram. The symbols have the following meaning: big circles are adopted member stars (m), triangles are probable member stars (pm), empty squares are non-member stars (nm), and small open circles are stars without any membership assignment. Black symbols indicate stars with CCD measurements whereas grey ones are for stars with data from the Tycho-2 catalog. The solid line is Schmidt-Kaler's (1982) ZAMS, whereas the dashed and dotted lines are the same ZAMS, but shifted by E_B-V = 0.35 and 1.2, respectively. The dashed arrow indicates the normal reddening path. b) B-V vs. V-I diagram. Symbols as in Fig. 5a. The solid lines represent the intrinsic positions for stars of luminosity classes V and III (Cousins 1978a,b). The dashed line gives the normal reddening path (R = 3.1).
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In the text

$\begin{figure} \par\includegraphics[height=9cm,clip]{fig07.eps} \end{figure}$ Figure 7: CMDs for all the stars covered in the field of NGC 1582. Symbols as in Fig. 5a. The solid line is the Schmidt-Kaler (1982) empirical MS fitted to the apparent distance modulus V-M_V = 11.4 ( V-M_V = V₀-M_V + 3.1 E_B-V, see Sect. 3.4).
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In the text

$\begin{figure} \par\includegraphics[height=9cm,clip]{fig08.eps} \end{figure}$ Figure 8: CMDs from 2MASS catalog. Symbols are as in Fig. 6a. a) Stars placed inside the cluster area. b) Stars placed in a ring around the cluster. The solid line in panel a) and the dotted one in panel b) are the intrinsic position for MS stars from the Schmidt-Kaler (1982) and Koornneef (1983) calibrations fitted to the apparent distance modulus J-M_J = 10.6 ( J-M_J = V₀-M_V + (3.1 - 2.3) E_B-V, see Sect. 3.4).
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm,clip]{fig09.eps} \end{figure}$ Figure 9: M_V vs. (B-V)₀ diagram of the members and probable members in the region of NGC 1582. Symbols as in Fig. 6a. Dashed curves are the isochrones from Girardi et al. (2000). The reported numbers give the $\log~(age)$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{fig10.eps} \end{figure}$ Figure 10: Finding chart of the NGC 1663 region ( $20^{\prime } \times 20^{\prime }$ and J filter). The black solid circle, $6^{\prime }$ radius, indicates the adopted angular size for the cluster (see Sect. 4.1 and Fig. 10). As in Fig. 2, grey square indicates the area covered from Asiago, and adopted members and probable members are enclosed in small circles and triangles, respectively. For a coordinate reference, the center (X = 0; Y=0) corresponds to the cluster coordinates (see Table 1), and each X-Y unit is $0\hbox{$.\!\!^{\prime\prime}$ }465$ . Field galaxies positions are indicated as grey circles.
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In the text

$\begin{figure} \par\includegraphics[height=5.3cm,clip]{fig11.eps} \end{figure}$ Figure 11: Stellar densities in the region of NGC 1663 as a function of the radius from DSS-2 image. The dotted lines indicate the adopted limits for the cluster and for the comparison field related with Fig. 14b.
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In the text

$\begin{figure} \par\includegraphics[height=9cm,clip]{4345f12.eps} \end{figure}$ Figure 12: CCDs of the stars in the region of NGC 1663. a) U-B vs. B-V diagram. As for NGC 1582, symbols have the following meaning: circles are adopted member stars (m), triangles are probable member stars (pm), empty squares are non-members stars (nm) and small open circles are stars without any membership assignment. Field galaxies are indicated as white circles. The solid line is Schmidt-Kaler's (1982) ZAMS, whereas the dashed one indicates the same ZAMS, but shifted by E_B-V = 0.2. The dashed arrow indicates the normal reddening path. b) B-V vs. V-I diagram. Symbols as in Fig. 12a. The solid lines are the intrinsic positions for stars of luminosity classes V and III (Cousins 1978a,b), while the dashed one provides the normal reddening path (R = 3.1).
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In the text

$\begin{figure} \par\includegraphics[height=9cm,clip]{fig13.eps} \end{figure}$ Figure 13: Color-magnitude diagrams (CMDs) for all the stars covered in the field of NGC 1663. Symbols as in Fig. 12a. The solid line and dashed curves are the Schmidt-Kaler (1982) empirical ZAMS and isochrones from Girardi et al. (2002) respectively. They were fitted to the apparent distance modulus V-M_V = 9.8 ( V-M_V = V₀-M_V + 3.1 E_B-V, see Sect. 4.2). The numbers indicate $\log~(age)$ .
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In the text

$\begin{figure} \par\includegraphics[height=9.5cm,clip]{fig14.eps} \end{figure}$ Figure 14: CMDs from the 2MASS catalog. Symbols as in Fig. 12a. a) Stars placed inside the cluster area b) Stars placed in a ring around the cluster (see Fig. 10).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=11cm,clip]{fig01.eps} \end{figure}$	Figure 1: Photometric errors in V magnitude and U-B, B-V andV-I colours as a function of V.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{fig03.eps} \end{figure}$	Figure 3: Stellar surface density profile in the region of NGC 1582 as a function of the radius. Data have been taken from 2MASS catalog. Dotted lines indicate the adopted limits for the cluster and for the comparison field related with Fig. 8b.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{fig04.eps} \end{figure}$	Figure 4: a) Vector point plot for the stars $20^{\prime }$ around the center of NGC 1582 (data from HD Extension Charts and Tycho-2 catalogs). b) Radial velocities obtained from Echelle spectra. See captions of Figs. 6 and 8 for the meaning of the symbols. The crosses indicate the mean error values.
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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{fig05.eps} \end{figure}$	Figure 5: Spectra of a sample of bright stars in the field of NGC 1582. A few interesting lines are indicated. See Table 3 for details.
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$\begin{figure} \par\includegraphics[height=9cm,clip]{fig07.eps} \end{figure}$	Figure 7: CMDs for all the stars covered in the field of NGC 1582. Symbols as in Fig. 5a. The solid line is the Schmidt-Kaler (1982) empirical MS fitted to the apparent distance modulus V-M_V = 11.4 ( V-M_V = V₀-M_V + 3.1 E_B-V, see Sect. 3.4).
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$\begin{figure} \par\includegraphics[height=8.8cm,clip]{fig09.eps} \end{figure}$	Figure 9: M_V vs. (B-V)₀ diagram of the members and probable members in the region of NGC 1582. Symbols as in Fig. 6a. Dashed curves are the isochrones from Girardi et al. (2000). The reported numbers give the $\log~(age)$ .
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$\begin{figure} \par\includegraphics[height=5.3cm,clip]{fig11.eps} \end{figure}$	Figure 11: Stellar densities in the region of NGC 1663 as a function of the radius from DSS-2 image. The dotted lines indicate the adopted limits for the cluster and for the comparison field related with Fig. 14b.
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$\begin{figure} \par\includegraphics[height=9.5cm,clip]{fig14.eps} \end{figure}$	Figure 14: CMDs from the 2MASS catalog. Symbols as in Fig. 12a. a) Stars placed inside the cluster area b) Stars placed in a ring around the cluster (see Fig. 10).
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