All Figures

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0346fig1.ps}\end{figure}$ Figure 1: Integrated K band spectrum of MRC0316-257 at z=3.13, extracted from all pixels in which the [OIII] $\lambda$ 5007 line emission exceeded 3 $\sigma$ , and covering the [OIII] $\lambda$ $\lambda$ 4959, 5007 doublet and H $\beta$ .
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In the text

$\begin{figure} \par\hspace*{2.5mm}\includegraphics[width=7.8cm,clip]{0346fig2a.ps}\vspace*{3mm} \includegraphics[width=7.6cm,clip]{0346fig2b.ps}\end{figure}$ Figure 2: Integrated H ( top) and K band spectrum ( bottom) of MRC0406-244 at z=2.42, extracted from all pixels in which the [OIII] $\lambda$ 5007 line emission exceeds 3 $\sigma$ . The inset in the upper panel shows the detected, relatively faint H $\beta$ , and [HeII] $\lambda$ 4685 lines, and the expected wavelength of [HeI] $\lambda$ 4471, which is not detected. The inset in the right panel shows ( from top to bottom): (1) the blended H $\alpha$ and [NII] $\lambda \lambda$ 6548, 6583 lines, and the [SII] $\lambda \lambda$ 6716, 6731 doublet (2) the best Gaussian fit to these lines (see text) (3) fit residuals. The fitted lines and residuals are shifted along the ordinate by arbitrary amouts.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0346fig3a.ps}\vspace*{3mm} \includegraphics[width=7.6cm,clip]{0346fig3b.ps}\end{figure}$ Figure 3: Integrated H ( top) and K band spectrum ( bottom) of TXS0828+193 at z= 2.57, extracted from all pixels in which the [OIII] $\lambda$ 5007 line emission exceeds 3 $\sigma$ . The inset in the upper panel shows the detected, relatively faint H $\beta$ , H $\gamma$ , and [HeII] $\lambda$ 4685 lines, and the expected wavelength of [HeI] $\lambda$ 4471, which is not detected. [OIII] $\lambda \lambda$ 4959, 5007 have complex profiles, where the different components arise from the blue and redshifted bubble, respectively. [OIII] $\lambda$ 6300 is faint, but detected with a significance of 5 $\sigma$ . In the K band, we detect H $\alpha$ and [NII] $\lambda \lambda$ 6548, 6583, and the fainter [OI] $\lambda$ 6300 line. The [SII] $\lambda \lambda$ 6716, 6731 doublet is at observed wavelengths >2.4 $\mu$ m, which are dominated by telluric absorption.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0346fig4a.ps}\vspace*{5mm} \includegraphics[width=7.7cm,clip]{0346fig4b.ps}\end{figure}$ Figure 4: A(H $\beta$ ) extinction maps for MRC0406-244 ( top) and TXS0828+193 ( bottom). Color bars show the extinctions (in magnitudes) estimated from the observed H $\beta$ /H $\alpha$ emission line ratios, assuming a galactic extinction law. Contours show the emission line morphology to ease orientation.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0346fig5.ps}\end{figure}$ Figure 5: Integrated spectra of the two bubbles in MRC0406-244, the redshifted southern bubble is shown on top, the blueshifted northern bubble is shown below. Upper panels show the spectra, Gaussian fits to the emission lines and fit residuals are shown in the mid and lower panels, respectively. Spectra are smoothed by 5 pixels spectrally, corresponding to $\sim$ 1/5 of the total line width. The measured [SII] $\lambda \lambda$ 6716, 6731 line ratios are consistent with electron densities of a few 100 cm^-3, with a best-fit value of 500 cm^-3 (see text). Redshifts and line widths were measured from the [OIII] $\lambda \lambda$ 4959, 5007 line doublet, so that the only free parameters to all other lines, including [SII], are the line fluxes.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0346fig6.ps} % \end{figure}$ Figure 6: Relationship between electron temperature and [OIII] line ratios for an electron density of 500 cm^-3. The green shaded area shows the temperature range for MRC0406-244 derived from a 3 $\sigma$ limit on [OIII] $\lambda$ 4363, the red area shows the range of temperatures from the ratio based on the measured [OIII] $\lambda$ 4363 flux in TXS0828+193, allowing for the 30% uncertainty. The inset shows a zoom on H $\gamma$ and [OIII] $\lambda$ 4363 in the H-band spectrum of TXS0828+193. Blue lines indicate the expected emission lines with the redshift and line width measured from [OIII] $\lambda$ 5007. The lower panel shows the fit rediduals.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{0346fig7.ps}\end{figure}$ Figure 7: [OIII] emission lines extracted from a small aperture (0.375 $^{\prime \prime }$ $\times$ 0.375 $^{\prime \prime }$ ) near the center of MRC0406-244. Line splitting is evident in both lines, with three narrow components and an underlying, broad component. The mid component in [OIII] $\lambda$ 4959 is affected by a night sky line residual. To guide the eye, we also show Gaussians for each component of the [OIII] $\lambda$ 4959 and [OII] $\lambda$ 5007 line respectively. Note that these are not strictly fits, but have the same line width and redshift for both [OIII] lines. The red component of this line appears fainter than the corresponding component of the [OIII] $\lambda$ 5007 line, because of an underlying broad component of the [OIII] $\lambda$ 5007 line superimposed, which we ignored.
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In the text

$\begin{figure} \par {\hspace*{2.85cm}\includegraphics[width=5.75cm,clip]{0346fig... ...space*{0.5cm} \includegraphics[width=5.75cm,clip]{0346fig8c.eps}\par\end{figure}$ Figure 8: Top: [OIII] $\lambda$ 5007 emission line morphology of MRC0316-257 at z=3.13 with contours showing the 1.4 GHz morphology. Bottom left: velocity map. Color bar shows the relative velocities in km s^-1, contours indicate the 1.4 GHz morphology. Bottom right: maps of the line widths, color bars show the FWHM in km s^-1, contours indicate the 1.4 GHz morphologies. North is up, east to the left in all images.
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In the text

$\begin{figure} \par\includegraphics[width=5.75cm,clip]{0346fig9a.eps}\hspace*{0.... ...s}\hspace*{0.5cm} \includegraphics[width=5.75cm,clip]{0346fig9d.eps}\end{figure}$ Figure 9: Top: [OIII] $\lambda$ 5007 emission line morphology of MRC0406-244 at z=2.42 with contours showing the 1.4 GHz morphology. Top right: [OIII] $\lambda$ 5007 emission line morphology with contours showing the line-free rest-frame optical continuum. Bottom left: velocity map. Color bar shows the relative velocities in km s^-1, contours indicate the 1.4 GHz morphology. Bottom right: maps of the line widths, color bars show the FWHM in km s^-1, contours indicate the 1.4 GHz morphologies. North is up, east to the left in all images.
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In the text

$\begin{figure} \par\includegraphics[width=5.75cm,clip]{0346fig9e.eps}\hspace*{0.... ...s}\hspace*{0.5cm} \includegraphics[width=5.75cm,clip]{0346fig9h.eps}\end{figure}$ Figure 10: Top: [OIII] $\lambda$ 5007 emission line morphology of TXS0828+193 at z=2.57 with contours showing the 1.4 GHz morphology. Top right: [OIII] $\lambda$ 5007 emission line morphology with contours showing the line-free rest-frame optical continuum. Bottom left: velocity map of TXS0828+193. Color bar shows the relative velocities in km s^-1, contours indicate the 1.4 GHz morphology. Bottom right: maps of the line widths, color bars show the FWHM in km s^-1, contours indicate the 1.4 GHz morphologies. North is up, east to the left in all images.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0346fig1.ps}\end{figure}$	Figure 1: Integrated K band spectrum of MRC0316-257 at z=3.13, extracted from all pixels in which the [OIII] $\lambda$ 5007 line emission exceeded 3 $\sigma$ , and covering the [OIII] $\lambda$ $\lambda$ 4959, 5007 doublet and H $\beta$ .
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0346fig4a.ps}\vspace*{5mm} \includegraphics[width=7.7cm,clip]{0346fig4b.ps}\end{figure}$	Figure 4: A(H $\beta$ ) extinction maps for MRC0406-244 ( top) and TXS0828+193 ( bottom). Color bars show the extinctions (in magnitudes) estimated from the observed H $\beta$ /H $\alpha$ emission line ratios, assuming a galactic extinction law. Contours show the emission line morphology to ease orientation.
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