All Figures

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[width=12cm]{5433fig1.eps}} \end{figure}$ Figure 1: High-contrast display of the continuum-subtracted H $\alpha$ image. The light contours delineate continuum-subtracted [S II] emission while the dark contours represent the I-band image. The HHOs are labeled. HH 892A is located at the reference position [0 $^{\prime \prime }$ , 0 $^{\prime \prime }$ ]. HH 892B is situated at [-8 $^{\prime \prime }$ , -87 $^{\prime \prime }$ ]. The northern part of the new nebula at [0 $^{\prime \prime }$ , -30 $^{\prime \prime }$ ] is visible in H $\alpha$ too.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[]{5433fig2.eps}} \end{figure}$ Figure 2: Spectrum of HH 892A. The identified lines are labeled. The horizontal line marks the 3 $\sigma$ detection limit.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[]{5433fig3.eps}} %\end{figure}$ Figure 3: Kiso I-band ( top) and TLS RGB ( bottom) images of the central region of LDN 1415 (FOV 3 $^\prime$ $\times$ 3 $^\prime$ ). The contours represent the 2MASS Ks image at [4, 8, 16] $\sigma$ . The TLS image is based on the stacked I, H $\alpha$ , and R frames. The new arcuate nebula is accompanied by extended faint emission to the north. The printed version of the paper shows the summed-up images.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{5433fig4.eps} \end{figure}$ Figure 4: H $\alpha$ spectrum of the nebula. The light grey line shows the spectrum of LMZ 12 (Reipurth & Aspin 2004) for comparison, scaled to match the emission component.
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In the text

$\begin{figure} \includegraphics[width=12cm]{5433fig5.eps} %\end{figure}$ Figure 5: 2MASS J, H, and Ks images ( left to right) of the IR source (FOV 1 $.\mkern -4mu^\prime$ 5 $\times$ 1 $.\mkern -4mu^\prime$ 5). The intensity range is [-1, 15] $\sigma$ . North is up and east to the left.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[]{5433fig6.eps}} \end{figure}$ Figure 6: Spectral energy distribution of the embedded object based on the values given in Table 1. Asterisks mark the low-state fluxes while diamonds represent refer to the high-state values. The line represents the SED of L1014-IRS (Young et al.), scaled to the distance of LDN 1415.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[]{5433fig2.eps}} \end{figure}$	Figure 2: Spectrum of HH 892A. The identified lines are labeled. The horizontal line marks the 3 $\sigma$ detection limit.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{5433fig4.eps} \end{figure}$	Figure 4: H $\alpha$ spectrum of the nebula. The light grey line shows the spectrum of LMZ 12 (Reipurth & Aspin 2004) for comparison, scaled to match the emission component.
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$\begin{figure} \includegraphics[width=12cm]{5433fig5.eps} %\end{figure}$	Figure 5: 2MASS J, H, and Ks images ( left to right) of the IR source (FOV 1 $.\mkern -4mu^\prime$ 5 $\times$ 1 $.\mkern -4mu^\prime$ 5). The intensity range is [-1, 15] $\sigma$ . North is up and east to the left.
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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics[]{5433fig6.eps}} \end{figure}$	Figure 6: Spectral energy distribution of the embedded object based on the values given in Table 1. Asterisks mark the low-state fluxes while diamonds represent refer to the high-state values. The line represents the SED of L1014-IRS (Young et al.), scaled to the distance of LDN 1415.
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