All Figures

Figure 1: FeH Stokes I and Stokes V line profiles ( upper and lower panel, respectively). Solid lines represent synthetic Stokes profiles; observed Stokes I and V profiles are shown with dotted lines. The top Stokes I spectrum shows a sunspot observation from Wallace et al. (1998), while the bottom Stokes I spectrum (shifted for the sake of clarity) as well as the Stokes V spectrum correspond to our own sunspot observations at IRSOL. Synthetic profiles are based on the theory by Dulick et al. (2003) and were calculated with a field strength of 3 kG, umbral models with effective temperatures of 4300 K and 4800 K (Hauschildt et al. 1999), and filling factors of 0.95 and 0.8 to fit the Wallace and IRSOL data, respectively.

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In the text

	Figure 2: The same as Fig. 1 but for a different wavelength region. Synthetic profiles (solid) are based on the theory by Dulick et al. (2003) and were calculated with a field strength of 3 kG, umbral models with of 4000 K and 4500 K (Hauschildt et al. 1999), and filling factors of 0.97 and 0.8 to fit the Wallace and IRSOL data, respectively.
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In the text

Figure 3: The same as Fig. 1 for a different spectral window containing FeH lines that suffer from unknown perturbations. Observations (dotted) are compared with two different models, the first being based on our empirically determined spin-orbit constants (solid), and the second one (dashed) assuming the theory by Dulick et al. (2003). Both synthetic spectra were calculated with a field strength of 3 kG, umbral models with of 4300 K and 4800 K (Hauschildt et al. 1999), and filling factors of 0.98 and 0.9 to fit the Wallace and IRSOL data, respectively.

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In the text