All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{7608fig1.eps}\end{figure}$ Figure 1: Observed integrated spectra of the sample clusters. Spectra are in relative F $_{\lambda }$ units normalised at $\approx$ 5800 Å. Constants have been added to the spectra, except for the bottom one.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7608fig2.eps}\end{figure}$ Figure 2: Reddening histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 257 $\hbox {$^\circ $ }$ . The histogram corresponding to 365 known open clusters with E(B-V) < 2.5 is shown in solid lines. The dashed lines show the histogram for the 42 open clusters within E(B-V) intervals of 0.1 mag wide.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7608fig3.eps}\end{figure}$ Figure 3: Reddening histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 347 $\hbox {$^\circ $ }$ . Symbols as in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=7.75cm,clip]{7608fig4.eps}\end{figure}$ Figure 4: Age histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 257 $\hbox {$^\circ $ }$ . The histogram corresponding to the WEBDA open cluster younger than 4 Gyr is shown in solid lines. The histogram for the 42 open-cluster sample is shown in dashed lines.
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In the text

$\begin{figure} \par\includegraphics[width=7.75cm,clip]{7608fig5.eps}\end{figure}$ Figure 5: Age histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 347 $\hbox {$^\circ $ }$ . Symbols as in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig6.eps}\end{figure}$ Figure 6: Ya2 template spectrum of (2-4) Myr ( top), Yb2 template spectrum of (5-10) Myr ( bottom) and the new Yab template spectrum of (4-5) Myr ( middle) defined in the current study.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig7.eps}\end{figure}$ Figure 7: Yc template spectrum of 20 Myr ( top), Yd template spectrum of 40 Myr ( bottom) and the new redefined Ycd template spectrum of 30 Myr ( middle).
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig8.eps}\end{figure}$ Figure 8: Comparison of the Piatti et al. (2002) Yc template spectrum of 20 Myr ( top) with the new Yc template spectrum of 20 Myr ( bottom) redefined in the current study.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig9.eps}\end{figure}$ Figure 9: From top to bottom: the Yb2 template spectrum of (5-10) Myr, the redefined Yc template spectrum of 20 Myr and the new Ycd template spectrum of 30 Myr defined in the current study.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig10.eps}\end{figure}$ Figure 10: Comparison of the Piatti et al. (2002) Ib template spectrum of (3-4) Gyr ( top) with the redefined Ib template spectrum ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608figA1.eps}\end{figure}$ Figure A.1: Integrated spectrum of Markarian 38 corrected for the derived E(B-V) colour excess ( top), the template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608figA2.eps}\end{figure}$ Figure A.2: Individual spectrum of the bright star HD 167287 of Markarian 38 corrected for the derived E(B-V) colour excess ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig11.eps}\end{figure}$ Figure A.3: From top to bottom: observed integrated spectrum of NGC 6604, the cluster spectrum corrected for the derived E(B-V) colour excess, the Ya1 and Ya1_-WR template spectra of (2-4) Myr, and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig12.eps}\end{figure}$ Figure A.4: From top to bottom: observed integrated spectrum of NGC 6604, the cluster spectrum corrected for E(B-V) = 1.00, the Ya3 template spectrum of (2-4) Myr, and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig13.eps}\end{figure}$ Figure A.5: Integrated spectrum of Dolidze 34 corrected for the derived E(B-V) value ( top), the Yf (100-150 Myr) and Yh (500 Myr) template spectra ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig14.eps}\end{figure}$ Figure A.6: Observed individual spectrum of the bright star HD 172747 of Dolidze 34 ( top), the SC92 F6/5 V and A9/F0 V template spectra ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig15.eps}\end{figure}$ Figure A.7: From top to bottom: the observed integrated spectrum of Berkeley 80, the cluster spectrum corrected for the derived E(B-V) value, the template spectrum which best matches it, and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig16.eps}\end{figure}$ Figure A.8: Integrated spectrum of ESO 429-SC2 corrected for the derived E(B-V) value ( top), the template spectrum which best matches it ( middle),and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig17.eps}\end{figure}$ Figure A.9: From top to bottom: the observed integrated spectrum of ESO 445-SC74, the Ia (1 Gyr) and Ib (3-4 Gyr) template spectra, and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig18.eps}\end{figure}$ Figure A.10: From top to bottom: the integrated spectrum of Bochum 2 corrected for E(B-V) = 0.75, the Yb1 template of (5-10) Myr, the cluster spectrum corrected for E(B-V) = 0.87, the Ya3 template of (2.4) Myr, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig19.eps}\end{figure}$ Figure A.11: From top to bottom: the individual reddening-corrected spectra of stars 1, 2 and 3 (MV73) of Bochum 2, the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig20.eps}\end{figure}$ Figure A.12: Integrated spectrum of NGC 2311 corrected for the derived E(B-V) value ( top), the template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig21.eps}\end{figure}$ Figure A.13: From top to bottom: the integrated spectrum of NGC 2409 corrected for E(B-V) = 0.40, the Yd template spectrum of 40 Myr, the cluster spectrum corrected for E(B-V) = 0.10, the Ye template spectrum of 60 Myr, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig22.eps}\end{figure}$ Figure A.14: Integrated spectrum of Ruprecht 2 corrected for the derived E(B-V) value ( top), the template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig23.eps}\end{figure}$ Figure A.15: Individual spectrum of one of the dominant stars of Ruprecht 2 (CD-29 $\hbox {$^\circ $ }$ 3349) corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig24.eps}\end{figure}$ Figure A.16: Integrated spectrum of Pismis 7 corrected for the derived E(B-V) value ( top), the template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig25.eps}\end{figure}$ Figure A.17: Integrated spectrum of Hogg 9 corrected for the derived E(B-V) value ( top), the template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig26.eps}\end{figure}$ Figure A.18: Integrated spectrum of Hogg 10 corrected for the derived E(B-V) value ( top), the Yc (20 Myr) and Yd (40 Myr) template spectra ( middle), and the corresponding residuals between both comparisons ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig27.eps}\end{figure}$ Figure A.19: Individual spectrum of the dominant star HD 97253 of Hogg 10 corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig28.eps}\end{figure}$ Figure A.20: From top to bottom: the integrated spectrum of Basel 18 corrected for E(B-V) = 0.30, the Yd template spectrum of 40 Myr, the cluster spectrum corrected for E(B-V) = 0.05, the Ye template spectrum of (45-75) Myr, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig29.eps}\end{figure}$ Figure A.21: Individual spectrum of the dominant star HD 116841 of Basel 18 corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig30.eps}\end{figure}$ Figure A.22: Integrated spectrum of Trumpler 21 corrected for the derived E(B-V) value ( top), the Yd (40 Myr) and Yc (20 Myr) template spectra ( middle), and the corresponding flux residuals between both comparisons ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig31.eps}\end{figure}$ Figure A.23: From top to bottom: the observed integrated spectrum of BH 151, the cluster spectrum corrected for E(B-V) = 1.70, the Ya3 template spectrum of (2-4) Myr, the cluster spectrum corrected for E(B-V) = 2.00, the Ya1 template spectrum of (2-4) Myr, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig32.eps}\end{figure}$ Figure A.24: From top to bottom: the integrated spectrum of NGC 5281 corrected for E(B-V) = 0.30, the Yc template spectrum of 20 Myr, the cluster spectrum corrected for E(B-V) = 0.20, the Yd template spectrum of 40 Myr, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig33.eps}\end{figure}$ Figure A.25: Individual spectrum of the bright star HD 119699 of NGC 5281 corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig34.eps}\end{figure}$ Figure A.26: Individual spectrum of the bright star CPD-62 $\hbox {$^\circ $ }$ 3568 of NGC 5281 corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig35.eps}\end{figure}$ Figure A.27: Individual spectrum of the star HD 119682 of NGC 5281 corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig36.eps}\end{figure}$ Figure A.28: Individual spectrum of the star CPD-62 $\hbox {$^\circ $ }$ 3559 of NGC 5281 corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig37.eps}\end{figure}$ Figure A.29: From top to bottom: the integrated spectrum of Lyngå 1 corrected for E(B-V) = 0.35, the Yf template spectrum of (100-150) Myr, the cluster spectrum corrected for E(B-V) = 0.38, the Ye template spectrum of (45-75) Myr, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig38.eps}\end{figure}$ Figure A.30: Individual spectrum of the star No. 1 from Vázquez et al. (2003) of Lyngå 1 corrected for reddening ( top), the SC92 template spectrum which best matches it ( middle), and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ ( bottom). Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig39.eps}\end{figure}$ Figure A.31: From top to bottom: the observed integrated spectrum of Pismis 20, the cluster spectrum corrected for the derived E(B-V) value, the Ya3 (2-4 Myr) and Yb3 (5-10 Myr) template spectra, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig40.eps}\end{figure}$ Figure A.32: From top to bottom: the observed individual spectrum of the star HD 134959 of Pismis 20, the star spectrum corrected for reddening, the SC92 B1 I and B3/5 I template spectra, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig41.eps}\end{figure}$ Figure A.33: From top to bottom: the observed integrated spectrum of Hogg 22 (without the contribution of the brightest star HD 150958), the cluster spectrum corrected for E(B-V) = 0.55, the Yb1 template spectrum of (5-10) Myr, the cluster spectrum corrected for E(B-V) = 0.75, the Ya3 template spectrum of (2-4) Myr, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig42.eps}\end{figure}$ Figure A.34: From top to bottom: the observed individual spectrum of the star HD 150958 of Hogg 22, the spectrum corrected for reddening, the SC92 template spectrum which best matches it, and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{7608fig43.eps}\end{figure}$ Figure A.35: From top to bottom: the integrated spectrum of NGC 6204 corrected for the derived E(B-V) value, the Yd (40 Myr) and Ye (45-75) Myr template spectra, and the corresponding flux residuals between both comparisons. Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig44.eps}\end{figure}$ Figure A.36: From top to bottom: the observed integrated spectrum of Pismis 24, the cluster spectrum corrected for E(B-V) = 1.20, the Ya3 template spectrum of (2-4) Myr and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig45.eps}\end{figure}$ Figure A.37: From top to bottom: the observed spectrum of Pismis 24, the cluster spectrum corrected for E(B-V) = 1.70, the Yb3 template spectrum of (5-10) Myr, and the flux residuals according to ( $F_{\rm cluster}-F_{\rm template}$ )/ $F_{\rm cluster}$ . Units as in Fig. 1.

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{7608fig1.eps}\end{figure}$	Figure 1: Observed integrated spectra of the sample clusters. Spectra are in relative F $_{\lambda }$ units normalised at $\approx$ 5800 Å. Constants have been added to the spectra, except for the bottom one.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7608fig2.eps}\end{figure}$	Figure 2: Reddening histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 257 $\hbox {$^\circ $ }$ . The histogram corresponding to 365 known open clusters with E(B-V) < 2.5 is shown in solid lines. The dashed lines show the histogram for the 42 open clusters within E(B-V) intervals of 0.1 mag wide.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7608fig3.eps}\end{figure}$	Figure 3: Reddening histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 347 $\hbox {$^\circ $ }$ . Symbols as in Fig. 2.
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$\begin{figure} \par\includegraphics[width=7.75cm,clip]{7608fig4.eps}\end{figure}$	Figure 4: Age histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 257 $\hbox {$^\circ $ }$ . The histogram corresponding to the WEBDA open cluster younger than 4 Gyr is shown in solid lines. The histogram for the 42 open-cluster sample is shown in dashed lines.
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$\begin{figure} \par\includegraphics[width=7.75cm,clip]{7608fig5.eps}\end{figure}$	Figure 5: Age histograms in the 90 $\hbox {$^\circ $ }$ Galactic sector centred at l = 347 $\hbox {$^\circ $ }$ . Symbols as in Fig. 3.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig6.eps}\end{figure}$	Figure 6: Ya2 template spectrum of (2-4) Myr ( top), Yb2 template spectrum of (5-10) Myr ( bottom) and the new Yab template spectrum of (4-5) Myr ( middle) defined in the current study.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig7.eps}\end{figure}$	Figure 7: Yc template spectrum of 20 Myr ( top), Yd template spectrum of 40 Myr ( bottom) and the new redefined Ycd template spectrum of 30 Myr ( middle).
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig8.eps}\end{figure}$	Figure 8: Comparison of the Piatti et al. (2002) Yc template spectrum of 20 Myr ( top) with the new Yc template spectrum of 20 Myr ( bottom) redefined in the current study.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig9.eps}\end{figure}$	Figure 9: From top to bottom: the Yb2 template spectrum of (5-10) Myr, the redefined Yc template spectrum of 20 Myr and the new Ycd template spectrum of 30 Myr defined in the current study.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7608fig10.eps}\end{figure}$	Figure 10: Comparison of the Piatti et al. (2002) Ib template spectrum of (3-4) Gyr ( top) with the redefined Ib template spectrum ( bottom).
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