Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{3079f1_1.eps}\end{figure}$ Figure 1: U-B vs. B-V for the stars in STELIB corrected for interstellar extinction. The different symbols represent different stellar spectral classes: full circles are dwarf main sequence stars (class V), open circles, giants (class III) and plus sign, super-giants of classes I and II. Small circles are used for stars with no spectral class determination.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{3079f2_1.eps} \in... ...2_2.eps}\par\includegraphics[angle=270,width=7cm,clip]{3079f2_3.eps}\end{figure}$ Figure 2: $T_{{\rm eff}}$ vs. B-V, U-B and R-I. The colors are corrected for interstellar extinction. Symbols are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{3079f3_1.eps} \... ...9f3_2.eps} \includegraphics[angle=270,width=7cm,clip]{3079f3_3.eps}\end{figure}$ Figure 3: Log(g) vs. log( $T_{{\rm eff}}$ ) and HR diagrams. Symbols are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{3079f4_1.eps}\end{figure}$ Figure 4: Metallicity distribution. Symbols are the same as in Fig. 1. Horizontal lines show the limits of the subsets described in Table 11.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{3079f5_1.eps}\end{figure}$ Figure 5: Comparison of Vega spectrum in the UV with published SED (filled circles).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{3079f6_1.eps}\end{figure}$ Figure 6: Comparison of calibrated standard stars spectra observed at JKT with published SED (bold curve).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{3079f7_1.eps}\end{figure}$ Figure 7: Comparison of calibrated standard stars spectra observed at SSO 2.3 m with published SED (bold curve).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3079f8_1.eps}\end{figure}$ Figure 8: Synthetic spectra built with STELIB compared to synthetic spectra obtained with Kurucz spectra using GISSEL02. SSP, wavelength range 3300 Å to 5000 Å, Z= 0.02 (solar metallicity) and Z= 0.004, from 1 Gyr to 12 Gyr. The Kurucz spectra are shifted downward by 10% of the scale for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3079f9_1.eps}\end{figure}$ Figure 9: Synthetic spectra built with STELIB compared to synthetic spectra obtained with Kurucz spectra using GISSEL02. SSP, wavelength range 4800 Å to 7000 Å, Z= 0.02 (solar metallicity) and Z= 0.004, from 1 Gyr to 12 Gyr. The Kurucz spectra are shifted downward by 10% of the scale for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=16.cm,clip]{3079f10.eps}\end{figure}$ Figure 10: Comparison of galaxy spectra, in and foreground of the cluster of galaxies AC 114, with solar metallicity SSP synthetic spectra. See Table 12 for identification. The observed spectra are not corrected for atmospheric molecular bands (the main one appears at about 5800 Å for $z\sim$ 0.3 galaxies). The observed spectra appear as a black line, and the model as a grey line. The model spectra are shifted downward by 20% of the scale for clarity. The legends in the figure give the observed redshift of the galaxies and the age of the models. The contribution of emission lines in the Balmer series is visible on observed spectra b, c and h.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3079f11.eps}\end{figure}$ Figure 11: Residuals of the comparison between synthetic photometry and published photoelectric photometry: UBVRI magnitude residuals versus Johnson magnitudes in the Lausanne database. Dashed lines correspond to 1 $\sigma$ rms.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3079f12.eps}\end{figure}$ Figure 12: Residuals of the comparison between synthetic photometry and published photoelectric photometry: UBVRI magnitude residuals versus Johnson colors in the Lausanne database. Dashed lines correspond to 1 $\sigma$ rms.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3079f13.eps}\end{figure}$ Figure 13: Residuals of the comparison between synthetic photometry and published photoelectric photometry: color residuals versus Johnson colors in the Lausanne database. Dashed lines correspond to 1 $\sigma$ rms.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{3079f1_1.eps}\end{figure}$	Figure 1: U-B vs. B-V for the stars in STELIB corrected for interstellar extinction. The different symbols represent different stellar spectral classes: full circles are dwarf main sequence stars (class V), open circles, giants (class III) and plus sign, super-giants of classes I and II. Small circles are used for stars with no spectral class determination.
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$\begin{figure} \par\includegraphics[angle=270,width=7cm,clip]{3079f2_1.eps} \in... ...2_2.eps}\par\includegraphics[angle=270,width=7cm,clip]{3079f2_3.eps}\end{figure}$	Figure 2: $T_{{\rm eff}}$ vs. B-V, U-B and R-I. The colors are corrected for interstellar extinction. Symbols are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{3079f3_1.eps} \... ...9f3_2.eps} \includegraphics[angle=270,width=7cm,clip]{3079f3_3.eps}\end{figure}$	Figure 3: Log(g) vs. log( $T_{{\rm eff}}$ ) and HR diagrams. Symbols are the same as in Fig. 1.
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$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{3079f4_1.eps}\end{figure}$	Figure 4: Metallicity distribution. Symbols are the same as in Fig. 1. Horizontal lines show the limits of the subsets described in Table 11.
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$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{3079f5_1.eps}\end{figure}$	Figure 5: Comparison of Vega spectrum in the UV with published SED (filled circles).
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{3079f6_1.eps}\end{figure}$	Figure 6: Comparison of calibrated standard stars spectra observed at JKT with published SED (bold curve).
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{3079f7_1.eps}\end{figure}$	Figure 7: Comparison of calibrated standard stars spectra observed at SSO 2.3 m with published SED (bold curve).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3079f8_1.eps}\end{figure}$	Figure 8: Synthetic spectra built with STELIB compared to synthetic spectra obtained with Kurucz spectra using GISSEL02. SSP, wavelength range 3300 Å to 5000 Å, Z= 0.02 (solar metallicity) and Z= 0.004, from 1 Gyr to 12 Gyr. The Kurucz spectra are shifted downward by 10% of the scale for clarity.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3079f9_1.eps}\end{figure}$	Figure 9: Synthetic spectra built with STELIB compared to synthetic spectra obtained with Kurucz spectra using GISSEL02. SSP, wavelength range 4800 Å to 7000 Å, Z= 0.02 (solar metallicity) and Z= 0.004, from 1 Gyr to 12 Gyr. The Kurucz spectra are shifted downward by 10% of the scale for clarity.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3079f11.eps}\end{figure}$	Figure 11: Residuals of the comparison between synthetic photometry and published photoelectric photometry: UBVRI magnitude residuals versus Johnson magnitudes in the Lausanne database. Dashed lines correspond to 1 $\sigma$ rms.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3079f12.eps}\end{figure}$	Figure 12: Residuals of the comparison between synthetic photometry and published photoelectric photometry: UBVRI magnitude residuals versus Johnson colors in the Lausanne database. Dashed lines correspond to 1 $\sigma$ rms.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3079f13.eps}\end{figure}$	Figure 13: Residuals of the comparison between synthetic photometry and published photoelectric photometry: color residuals versus Johnson colors in the Lausanne database. Dashed lines correspond to 1 $\sigma$ rms.
Open with DEXTER