All Figures

$\begin{figure} \par\includegraphics*[angle=-90,width=8.8cm,clip]{aa3164-f1.ps} \end{figure}$ Figure 1: Synthetic equivalent width $W^{\rm syn}$ against observed equivalent width $W^{\rm obs}$ for all $W_j^{\rm obs} \ge 1.0$ Å absorption features used to constrain the star-formation and chemical-enrichment histories of 73 BCGs (see Tables 3 and 4). The dash line is the identity line. Different symbols denote different absorption features, as indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{aa3164-f2.ps} \end{figure}$ Figure 2: Star formation histories of 73 BCGs. In each panel, the numbers on the horizontal axis represent the stellar age groups, as indicated in the bottom right of the figure. The vertical axis shows the percentage contributions of stars in the various age groups to the integrated flux at 5870 Å.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{aa3164-f3.ps}\end{figure}$ Figure 3: Comparison of synthetic spectra (red-solid lines) to the observed spectra of four BCGs (corrected for galactic reddening; black-solid lines): Haro 35, I Zw 117, I Zw 53, and I Zw 56. The contributions to the synthetic spectra by old stars (OLD, $10^{10}~{\rm yr}$ ), intermediate-age stars (INT, 10⁹, $5\times10^{9}~{\rm yr}$ ), young stars (YS, 10⁷- $5\times10^{9}~{\rm yr}$ ), and newly-born stars (H II) are also shown. The emission line spectrum appears in the OBS-SYN difference, at the bottom of each panel. (This figure is available in color in electronic form.)
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In the text

$\begin{figure} \par\includegraphics*[angle=-90,width=17.2cm,clip]{aa3164-f4.ps} \end{figure}$ Figure 4: Results of the empirical population synthesis analysis for the galaxies with asymptotic (young-star) metallicities [ $Z/Z_\odot ]=-0.5$ (stars) and 0.0 (squares), condensed on an evolutionary diagram. The horizontal axis ${X}_{\rm H+Y}$ = ${X}_{\rm HII}$ + ${X}_{\rm YS}$ is the fraction of light at $\lambda$ 5870 Å due to star clusters between the 10⁷ and $5\times10^8~{\rm yr}$ age bins and H II regions, while the fraction ${X}_{\rm INT}$ due to stars in the 10⁹ and $5\times10^{9}~{\rm yr}$ age bins is plotted along the vertical axis. Dotted lines indicate lines of constant ${X}_{\rm OLD}$ ( $10^{10}~{\rm yr}$ ), as labeled.
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In the text

$\begin{figure} \par\includegraphics*[angle=-90,width=8.8cm,clip]{aa3164-f5.ps} \end{figure}$ Figure 5: Distribution of the equivalent widths (in units of Å) for the underlying Balmer absorption features, which were measured from the synthetic stellar population spectrum.
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In the text

$\begin{figure} \par\includegraphics*[angle=-90,width=8.8cm,clip]{aa3164-f1.ps} \end{figure}$	Figure 1: Synthetic equivalent width $W^{\rm syn}$ against observed equivalent width $W^{\rm obs}$ for all $W_j^{\rm obs} \ge 1.0$ Å absorption features used to constrain the star-formation and chemical-enrichment histories of 73 BCGs (see Tables 3 and 4). The dash line is the identity line. Different symbols denote different absorption features, as indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=17.2cm,clip]{aa3164-f2.ps} \end{figure}$	Figure 2: Star formation histories of 73 BCGs. In each panel, the numbers on the horizontal axis represent the stellar age groups, as indicated in the bottom right of the figure. The vertical axis shows the percentage contributions of stars in the various age groups to the integrated flux at 5870 Å.
Open with DEXTER

$\begin{figure} \par\includegraphics*[angle=-90,width=8.8cm,clip]{aa3164-f5.ps} \end{figure}$	Figure 5: Distribution of the equivalent widths (in units of Å) for the underlying Balmer absorption features, which were measured from the synthetic stellar population spectrum.
Open with DEXTER