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Our knowledge of the lower solar atmosphere is mainly obtained fromspectropolarimetric observations, which are often carried out in the red orinfrared spectral range and almost always cover only a single or a few spectrallines. Here we compare the quality of Stokes inversions of only a few spectrallines with many-line inversions. We investigate the feasibility ofspectropolarimetry in the short-wavelength range, 3000 \AA{} - 4300 \AA{},where the line density but also the photon noise are considerably higher thanin the red, so that many-line inversions could be particularly attractive inthat wavelength range. This is also timely because this wavelength range willbe the focus of a new spectropolarimeter in the third science flight of theballoon-borne solar observatory SUNRISE. For an ensemble of MHD atmospheres wesynthesize exemplarily spectral regions around 3140 \AA{}, 4080 \AA{}, and 6302\AA{}. The spectral coverage is chosen such that at a spectral resolving powerof 150000 the spectra can be recorded by a 2K detector. The synthetic Stokesprofiles are degraded with a typical photon noise and afterwards inverted. Theatmospheric parameters of the inversion of noisy profiles are compared with theinversion of noise-free spectra. We find that significantly more informationcan be obtained from many-line inversions than from a traditionally usedinversion of only a few spectral lines. We further find that information on theupper photosphere can be significantly more reliably obtained at shortwavelengths. In the mid and lower photosphere, the many-line approach at 4080\AA{} provides equally good results as the many-line approach at 6302 \AA{} forthe magnetic field strength and the LOS velocity, while the temperaturedetermination is even more precise by a factor of three. We conclude thatmany-line spectropolarimetry should be the preferred option in the future.

The potential of many-line inversions of photospheric spectropolarimetric data in the visible and near UV