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Our knowledge of the low solar atmosphere, i.e., the photosphere andchromosphere, is based on the knowledge gained from the observations and thetheoretical and numerical modeling of these layers. In this sense, thethermodynamical and magnetic semi-empirical models of the solar atmosphere havesignificantly contributed to the advance in the understanding of the physics ofthe Sun. In the past, many of these models have been used as a reference thathelps us to, e.g., constrain the theoretical and numerical modeling, or toverify the goodness of physical parameters obtained from the inversion of thespectral lines. Nevertheless, semi-empirical models are quite limited by theassumptions that are inherent to the approach and do not necessarily provide anaccurate view of the instantaneous and local thermodynamic conditions in thesolar atmosphere. In this work, we provide an extensive collection ofthermodynamic model atmospheres for active regions (ARs) obtained from thesimultaneous inversion of 6 lines sensitive to changes in the thermodynamicalconditions in the chromosphere, and another 6 lines sensitive to changes in thethermodynamical conditions in the photospere. These inversions were made using320 representative profiles (RP) obtained by clustering the profiles in theumbra, penumbra, pore-like, plage, and surrounding quiet-sun in 126 activeregions. Due to the simultaneous inversion of the selected lines, the resultingrepresentative model atmosphere (RMA) samples the thermodynamics from thebottom of the photosphere to the top of the chromosphere. As a result, thisdatabase, named $IRIS^{2+}$ and formed by $40,320$ RP-RMA pairs, represents themost comprehensive collection of stratified-in-optical-depth thermodynamicmodels of the low solar atmosphere.

$IRIS^{2+}$: A comprehensive database of stratified thermodynamic models in the low solar atmosphere