All Figures

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{4657fig1.ps}\end{figure}$ Figure 1: Magnetogram of the scanned region. The gray scale indicates the amplitude of the Stokes V profile of the strongest Fe line present in the observed spectral domain.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4657fig2.ps}\end{figure}$ Figure 2: Example of the spectral domain observed with the target Mn I line at 5537 Å on the left showing the line asymmetries attributed to the hyperfine coupling, and the two Fe I lines used for reference.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4657fig3.ps}\end{figure}$ Figure 3: Examples of Stokes V ( left) and Q ( right) profiles normalized to the continuum intensity for the Mn 1 line at 5537.7 Å. Three cases of the same spectral line are displaced horizontally by 1 Å for clarity purposes. They are computed using Milne-Eddington atmospheres with constant magnetic field strengths of, from left to right, 100, 600 and 900 G. The dotted horizontal lines are placed at $\pm$ 10^-3 of the continuum intensity as a reference to a typical noise level in solar spectropolarimetry. Figure reproduced from López Ariste et al. (2002).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4657fig4.ps}\end{figure}$ Figure 4: Ratio between the main lobe of Stokes V and the HFS feature for synthetic profiles of increasing field strength.
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In the text

$\begin{figure} \par\includegraphics[width=3.5cm,clip]{4657f5a.ps}\hspace*{1.5mm} \includegraphics[width=3.5cm,clip]{4657f5b.ps}\end{figure}$ Figure 5: Stokes V profiles from network points ( from left to right) 5 (445-764 $\rm Mx/cm^2$ ) and 9 (335-574 $\rm Mx/cm^2$ ).
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In the text

$\begin{figure} \par\includegraphics[width=3.5cm,clip]{4657f6a.ps}\hspace*{1.5mm} \includegraphics[width=3.5cm,clip]{4657f6b.ps}\end{figure}$ Figure 6: Stokes V profiles from network points 4 (142-243 $\rm Mx/cm^2$ ) and 7 (214-367 $\rm Mx/cm^2$ ).
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{4657fig7.ps}\end{figure}$ Figure 7: Filling factors for the kG (diamonds) and the hG (crosses) components as a function of the longitudinal flux density in profiles of the network.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{4657fig8.ps}\end{figure}$ Figure 8: Average Stokes V profile of the full observed region.
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In the text

$\begin{figure} \par\includegraphics[width=3.5cm,clip]{4657f9a.ps}\hspace*{1.5mm} \includegraphics[width=3.5cm,clip]{4657f9b.ps}\end{figure}$ Figure 9: Average Stokes V profiles for two different internetwork regions.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{4657f10.ps}\end{figure}$ Figure 10: Synthetic profiles of the specified field strengths (300, 600, 1000 and 1500 G respectively) are polluted with several realizations of a Gaussian noise of amplitude slightly bigger than the signal itself. The sum of all the realizations simulates the addition procedure performed on the observations. The experiment results in that the HFS spectral features survive the addition of noise and, conversely, noise cannot reproduce those features on its own.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4657f11.ps}\end{figure}$ Figure 11: Filling factors for the kilogauss (diamonds) and the hG (crosses) components of the magnetic atmosphere in internetwork regions.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{4657fig1.ps}\end{figure}$	Figure 1: Magnetogram of the scanned region. The gray scale indicates the amplitude of the Stokes V profile of the strongest Fe line present in the observed spectral domain.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4657fig2.ps}\end{figure}$	Figure 2: Example of the spectral domain observed with the target Mn I line at 5537 Å on the left showing the line asymmetries attributed to the hyperfine coupling, and the two Fe I lines used for reference.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4657fig4.ps}\end{figure}$	Figure 4: Ratio between the main lobe of Stokes V and the HFS feature for synthetic profiles of increasing field strength.
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$\begin{figure} \par\includegraphics[width=3.5cm,clip]{4657f5a.ps}\hspace*{1.5mm} \includegraphics[width=3.5cm,clip]{4657f5b.ps}\end{figure}$	Figure 5: Stokes V profiles from network points ( from left to right) 5 (445-764 $\rm Mx/cm^2$ ) and 9 (335-574 $\rm Mx/cm^2$ ).
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$\begin{figure} \par\includegraphics[width=3.5cm,clip]{4657f6a.ps}\hspace*{1.5mm} \includegraphics[width=3.5cm,clip]{4657f6b.ps}\end{figure}$	Figure 6: Stokes V profiles from network points 4 (142-243 $\rm Mx/cm^2$ ) and 7 (214-367 $\rm Mx/cm^2$ ).
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{4657fig7.ps}\end{figure}$	Figure 7: Filling factors for the kG (diamonds) and the hG (crosses) components as a function of the longitudinal flux density in profiles of the network.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{4657fig8.ps}\end{figure}$	Figure 8: Average Stokes V profile of the full observed region.
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$\begin{figure} \par\includegraphics[width=3.5cm,clip]{4657f9a.ps}\hspace*{1.5mm} \includegraphics[width=3.5cm,clip]{4657f9b.ps}\end{figure}$	Figure 9: Average Stokes V profiles for two different internetwork regions.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4657f11.ps}\end{figure}$	Figure 11: Filling factors for the kilogauss (diamonds) and the hG (crosses) components of the magnetic atmosphere in internetwork regions.
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