Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=6.04cm, height=14cm, angle=270,clip]{0912f3.eps}\end{figure}$ Figure 3: Redshift ( left) and absolute B magnitude ( right) distributions for the total M03 sample (unhatched), for the RL subsample of M03 (hatched), for the 17 sources of this study (cross-hatched) and for the sources with $2.0\protect\la z\protect\la 2.5$ studied by Mc99 (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=12cm, height=12cm, clip]{0912f4.eps}\end{figure}$ Figure 4: Distribution of Seyfert 1 and quasars in the optical plane of E1, FWHM(H $\beta _{\rm BC}$ ) (in units of km s^-1) vs. $R_{\rm FeII}$ . Open circles: M03, 215 AGN; filled circles: 17 VLT/ISAAC sources of the present study; open circles with dotted lines: 22 $z \approx 2.5$ sources studied by Mc99, with upper limits and uncertainties in $R_{\rm FeII}$ set according to M03.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,height=7.4cm,clip]{0912f5a.eps}\... ...graphics[width=7.3cm,height=7.2cm,clip]{0912f5e.eps}\hspace*{7.7cm} \end{figure}$ Figure 5: FWHM(H $\beta _{\rm BC}$ ), $R_{\rm FeII}$ , W(H $\beta _{\rm BC}$ ), W(Fe II $\lambda$ 4570), and W( [OIII] $\lambda$ 5007) vs. absolute blue magnitude M_B. Equivalent widths are in the rest frame, in units of Å; FWHM(H $\beta _{\rm BC}$ ) is in km s^-1. Open circles: M03 data; filled circles: VLT/ISAAC sources. Best fit according to a robust method is provided in the only case of a significant correlation.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm, height=8.8cm,clip]{0912f6.eps}\end{figure}$ Figure 6: FWHM(H $\beta _{\rm BC}$ ) vs. M_B for the M03+VLT/ISAAC 232 sources, with RQ (filled circles) and RL (open circles) identified. The thick lines are the predicted minimum FWHM(H $\beta _{\rm BC}$ ), as described in Sect. 5.3 (solid line), and the boundary between Populations A and B (dot-dashed line). The thin line refers to a slightly different fit to the $R_{\rm BLR}-L$ relationship, with $\alpha =0.7$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm, height=8.8cm,clip]{0912f7.eps}\end{figure}$ Figure 7: FWHM(Fe II $\lambda$ 4570) vs. FWHM(Fe II $\lambda$ 4570) for the 17 VLT/ISAAC sources. The dot-dashed line traces the locus of FWHM(H $\beta _{\rm BC}$ ) = FWHM(Fe II $\lambda$ 4570), while the continuous line is a least-squares best fit.
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In the text

$\begin{figure} \includegraphics[width=17cm, clip]{0912f1.eps}\end{figure}$ Figure 1: Calibrated spectra of the 17 intermediate-redshift quasars. Abscissae are rest-frame wavelength in Å, ordinates are specific flux in units of 10^-15 erg s^-1 cm^-1Å^-1. Note that, for HE 0353-3919, ${\sim } 100$ Å are missing in the blue side of the H $\beta _{\rm BC}$ profile, due to a gap between the ${\it sZ}$ and Z bands.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0912f2.eps}\end{figure}$ Figure 2: Spectral atlas of the 17 intermediate-redshift quasars. The left panels show the continuum-subtracted H $\beta$ spectral region. Abscissae are rest frame wavelength in Å, ordinates are specific flux in units 10^-15 erg s^-1 cm^-1 Å^-1. The best-fit FeII ${_{\rm opt}}$ emission (see text) is traced as a thin (green) line. The right panels show an expansion around H $\beta$ of the same spectrum after continuum and FeII ${_{\rm opt}}$ subtraction. Abscissae and ordinates are as above. The (blue and red) thick line shows a spline fitting of the pure H $\beta _{\rm BC}$ on the short and long wavelength side of the line respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.04cm, height=14cm, angle=270,clip]{0912f3.eps}\end{figure}$	Figure 3: Redshift ( left) and absolute B magnitude ( right) distributions for the total M03 sample (unhatched), for the RL subsample of M03 (hatched), for the 17 sources of this study (cross-hatched) and for the sources with $2.0\protect\la z\protect\la 2.5$ studied by Mc99 (dotted line).
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$\begin{figure} \par\includegraphics[width=12cm, height=12cm, clip]{0912f4.eps}\end{figure}$	Figure 4: Distribution of Seyfert 1 and quasars in the optical plane of E1, FWHM(H $\beta _{\rm BC}$ ) (in units of km s^-1) vs. $R_{\rm FeII}$ . Open circles: M03, 215 AGN; filled circles: 17 VLT/ISAAC sources of the present study; open circles with dotted lines: 22 $z \approx 2.5$ sources studied by Mc99, with upper limits and uncertainties in $R_{\rm FeII}$ set according to M03.
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$\begin{figure} \par\includegraphics[width=8.8cm, height=8.8cm,clip]{0912f7.eps}\end{figure}$	Figure 7: FWHM(Fe II $\lambda$ 4570) vs. FWHM(Fe II $\lambda$ 4570) for the 17 VLT/ISAAC sources. The dot-dashed line traces the locus of FWHM(H $\beta _{\rm BC}$ ) = FWHM(Fe II $\lambda$ 4570), while the continuous line is a least-squares best fit.
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$\begin{figure} \includegraphics[width=17cm, clip]{0912f1.eps}\end{figure}$	Figure 1: Calibrated spectra of the 17 intermediate-redshift quasars. Abscissae are rest-frame wavelength in Å, ordinates are specific flux in units of 10^-15 erg s^-1 cm^-1Å^-1. Note that, for HE 0353-3919, ${\sim } 100$ Å are missing in the blue side of the H $\beta _{\rm BC}$ profile, due to a gap between the ${\it sZ}$ and Z bands.
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