All Figures

$\begin{figure} \par {\includegraphics[width=16.8cm,clip]{7017fig1.ps} } \end{figure}$ Figure 1: From left to right: a) the Fe I 630 nm continuum intensity, b) the calcium wing intensity at 396.490 nm which was calibrated to FTS data (Stenflo et al. 1984), c) the outer calcium wing intensity (W1), d) the inner calcium wing intensity (W3), e) the H-index, f) the masks which separate network (white) from the inter-network (gray), and g) the magnetic flux density obtained from the inversion. We did not use the black region between the network and inter-network. Each small tickmark is 1 arcsec. Note that sampling in x and y directions are different.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{7017fig2.ps} } \end{figure}$ Figure 2: Sample averaged calcium profile of one of the maps (the average profile is similar for all other maps). The bands are explained in Table 1.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{7017fig3.ps} } \end{figure}$ Figure 3: Scatter plot of the $H_{2{\rm v}}$ band vs. peak definition. In the band definition, a fixed spectral range was used. Gray and black show the network and inter-network, respectively.
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In the text

$\begin{figure} \par {\includegraphics[width=16.5cm,clip]{7017fig4.ps} } \end{figure}$ Figure 4: Histograms of the intensity parameters for the network (thick) and inter-network (thin), using the band sample: a) the H-index, b) $H_{2{\rm v}}$ , c) $H_{2{\rm r}}$ , d) W3 (the inner wing intensity), e) W2 (the middle wing intensity), f) W1 (the outer wing intensity), g) the calcium wing intensity at 396.490 nm which was used for normalization (see Fig. 2), and h) Fe I 630.2 nm normalized continuum intensity (see Table 1 for definitions).
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In the text

$\begin{figure} \par {\includegraphics[width=15cm,clip]{7017fig5.ps} } \end{figure}$ Figure 5: Histograms of the magnetic field parameters for the network (thick) and inter-network (thin), using the peak sample: a) the absolute magnetic flux density, b) the field strength, c) Stokes-V amplitude, d) Fe I 630.25 nm V velocity, e) the amplitude asymmetry, and f) the area asymmetry.
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In the text

$\begin{figure} \par {\includegraphics[width=8.1cm,clip]{7017fig6.ps} } \end{figure}$ Figure 6: Upper panels: correlation between the $H_{2{\rm v}}$ and $H_{2{\rm r}}$ based on the peak sample and the H-index. Lower left: correlation between W₁ and the H-index. Lower right: correlation of the ( V/R) ratio with the calcium core position. Gray and black show the network and inter-network, respectively (for abbreviations, see Table 1).
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In the text

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{7017fig7.ps} } \end{figure}$ Figure 7: Top left: scatter plot of the amplitude vs. area asymmetries. Bottom left: scatter plot of the area asymmetry vs. the V velocity. Right panels: scatter plots of the amplitude and area asymmetries vs. the Fe I 630.25 nm V amplitude. Gray and black show the network and inter-network, respectively.
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In the text

$\begin{figure} \par {\includegraphics[width=7.2cm,clip]{7017fig8.ps} } \end{figure}$ Figure 8: Upper panel: correlation between the H-index and the absolute magnetic flux density. Gray is the original data and black is the binned data: each point is average of 25 points. The middle curve shows a fit of a power law to the original data (Eq. (1)), the other two curves give the 1 $-\sigma$ error range of the fit. Lower panel: there is no correlation between the H-index and the magnetic flux density in inter-network.
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In the text

$\begin{figure} \par {\includegraphics[width=16.9cm,clip]{7017fig9.ps} } \end{figure}$ Figure 9: Correlation between the H-index and amplitude/area asymmetry and V velocity. Plusses and squares show network and inter-network, respectively. The binning method is similar to Fig. 8.
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In the text

$\begin{figure} \par {\includegraphics[width=7.2cm,clip]{7017fig10.ps} } \end{figure}$ Figure 10: In the left column diagrams, only the points with a negative V velocity are plotted. In the right panels, only points with a negative area asymmetry are plotted. Pluses and squares show network and inter-network, respectively.
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In the text

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{7017fgA1.ps} } \end{figure}$ Figure A.1: Close up view of the flux density distribution for the inter-network. At a value of $\sim$ 4.0 Mx cm^-2, the histogram shows a peak.

In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{7017fgA2.ps} } \end{figure}$ Figure A.2: The upper four plots show an example of the original Stokes profiles and the inversion fits. The lower four figures show the same profile with a rms noise value two times larger and corresponding fits. The magnetic field strength, magnetic filling factor, and macro turbulence velocity for the original and noisy profiles are (842, 1543) G, (7.6, 5.3)%, and (2.95, 2.77) km s^-1 respectively. The x-axis shows the spectral coordinate in mÅ.

In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{7017fgA3.ps} } \end{figure}$ Figure A.3: Histograms of the inter-network field strengths of one of the maps based on the inversion of original data (black) and noisy data (red).

In the text

$\begin{figure} \par {\includegraphics[width=8.1cm,clip]{7017fgB1.ps} } \end{figure}$ Figure B.1: Comparison between two different slit widths and the same modulation speed. The black and blue profiles correspond to slit widths of 0.48 and 0.18 arcsec, respectively. The red profile is the blue profile multiplied by a constant factor of 2.6 for all pixels. The green profiles show the 1- $\sigma$ rms value ( $\sim$ 1%) from the mean curve (red).

In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{7017fgB2.ps} } \end{figure}$ Figure B.2: Dark subtracted spectrum of the umbra in a sunspot.

In the text

$\begin{figure} \par {\includegraphics[width=16.9cm,clip]{7017fgB3.ps} } \end{figure}$ Figure B.3: Left: a single Ca II H spectrum of the umbra and quiet sun profiles in a sunspot. Asterisks show spectral bands that were used to estimate the true signal (see Sect. B.3.2). Right: close up view of the quiet sun and umbral profiles near the calcium line core. The true signal (about 5% in the wing close to the Ca core according to Wallace et al. (2000) was subtracted from the umbral profile. The red curve shows 12% of the quiet sun profile. The two cyan curves show an uncertainty interval of one sigma (1%).

In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{7017fgB4.ps} } \end{figure}$ Figure B.4: Ratio of the umbral profile to a quiet sun profile. If one considers all the spectrum, the ratio will be 10 $\pm$ 3% while considering only parts of the wing close to the Ca II H core, the ratio will be 12 $\pm$ 1%. Note to the mismatch between the quiet sun and umbral profiles at spectral line positions due to different broadenings.

In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{7017fgB5.ps} } \end{figure}$ Figure B.5: Distribution of the readout error in a set of 50 dark currents with 8 accumulations.

In the text

$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{7017fgB6.ps} } \end{figure}$ Figure B.6: Upper panel: a row in a dark frame with 6 accumulation. The red curve is a polynomial fit to subtract systematic shift from the random noise. Lower panel: the residual signal after subtraction of the polynomial, which is the real noise. Note to the large difference between the rms of the map (excluding its borders) and the rms of the residuals.

In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{7017fgB7.ps} } \end{figure}$ Figure B.7: A sample calcium profile. We use the calcium core minimum counts to estimate the photon noise. In this case, the signal-to-noise ratio at the calcium core is more than 10.

In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{7017fig2.ps} } \end{figure}$	Figure 2: Sample averaged calcium profile of one of the maps (the average profile is similar for all other maps). The bands are explained in Table 1.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{7017fig3.ps} } \end{figure}$	Figure 3: Scatter plot of the $H_{2{\rm v}}$ band vs. peak definition. In the band definition, a fixed spectral range was used. Gray and black show the network and inter-network, respectively.
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$\begin{figure} \par {\includegraphics[width=15cm,clip]{7017fig5.ps} } \end{figure}$	Figure 5: Histograms of the magnetic field parameters for the network (thick) and inter-network (thin), using the peak sample: a) the absolute magnetic flux density, b) the field strength, c) Stokes-V amplitude, d) Fe I 630.25 nm V velocity, e) the amplitude asymmetry, and f) the area asymmetry.
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$\begin{figure} \par {\includegraphics[width=8.1cm,clip]{7017fig6.ps} } \end{figure}$	Figure 6: Upper panels: correlation between the $H_{2{\rm v}}$ and $H_{2{\rm r}}$ based on the peak sample and the H-index. Lower left: correlation between W₁ and the H-index. Lower right: correlation of the ( V/R) ratio with the calcium core position. Gray and black show the network and inter-network, respectively (for abbreviations, see Table 1).
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$\begin{figure} \par {\includegraphics[width=8.3cm,clip]{7017fig7.ps} } \end{figure}$	Figure 7: Top left: scatter plot of the amplitude vs. area asymmetries. Bottom left: scatter plot of the area asymmetry vs. the V velocity. Right panels: scatter plots of the amplitude and area asymmetries vs. the Fe I 630.25 nm V amplitude. Gray and black show the network and inter-network, respectively.
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$\begin{figure} \par {\includegraphics[width=16.9cm,clip]{7017fig9.ps} } \end{figure}$	Figure 9: Correlation between the H-index and amplitude/area asymmetry and V velocity. Plusses and squares show network and inter-network, respectively. The binning method is similar to Fig. 8.
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$\begin{figure} \par {\includegraphics[width=7.2cm,clip]{7017fig10.ps} } \end{figure}$	Figure 10: In the left column diagrams, only the points with a negative V velocity are plotted. In the right panels, only points with a negative area asymmetry are plotted. Pluses and squares show network and inter-network, respectively.
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