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The spectral window, containing Fraunhofer lines formed in the solarphotosphere, around the magnetically sensitive Cr I lines at 5780.9, 5781.1,5781.7, 5783.0, and 5783.8 \r{A}, with Land\'e g-factors between 1.6 and 2.5,is explored. The goal is to analyze simultaneously 15 spectral lines, whichcomprise Cr I, Cu I, Fe I, Mn I, and Si I lines, without polarimetry to inferthe thermodynamic and magnetic properties in strongly magnetized plasmas usingan inversion code. The study is based on a new setup at the Vacuum TowerTelescope (VTT, Tenerife) which includes fast spectroscopic scans in thewavelength range around the Cr I 5781.75 \r{A} line. The snapshot 385 of theEnhanced Network simulation from the Bifrost code serves to synthesize all thelines, which are in turn inverted simultaneously with SIR to establish the bestinversion strategy. This strategy is then applied to VTT observations of asunspot belonging to NOAA 12723 on 2018 September 30 and the results arecompared to full-disk vector-field data obtained with the Helioseismic andMagnetic Imager (HMI). The 15 simultaneously inverted intensity profiles(Stokes I) delivered accurate temperatures and Doppler velocities when comparedagainst the simulations. The derived magnetic fields and inclinations are mostaccurate when the fields are oriented along the line-of-sight (LOS) and lessaccurate when the fields are transverse to the LOS. In general, the resultsappear similar to the HMI vector-field data, although some discrepancies exist.The analyzed spectral range has the potential to deliver thermal, dynamic, andmagnetic information in strongly magnetized features on the Sun, such as poresand sunspots, even without polarimetry. The highest sensitivity of the lines isfound in the lower photosphere, on average around $\log \tau = -1$. Themultiple-line inversions provide smooth results across the whole field-of-view.

Multiple Stokes I inversions to infer magnetic fields in the spectral range around Cr I 5782 \r{A}