These are 3 subsets (300^3 cells each) derived from larger 1024^3 cosmological MHD simulations produced using ENZO on Piz-Daint (CSCS) by F.Vazza& collaborators. In these "astrophysical" models we impose a negligibly small initial seed field, and later seed magnetic fields from the feedback activity of star forming particles and/or supermassive BH particles in ENZO. In the "CSF3" run magnetic fields are only seeded by stellar feedback, assuming that 10% of the thermal feedback energy goes into magnetic field energy. In the "CSFBH2" run we also include seeding from BH (1% of energy goes into magnetic feedback). In the "CSFBH5" run the magnetic feedback efficiency from BH particles is increased to 10%. The star formation is implemented following Kravtsov+2003, while the BH particle are injected at z=4 (M=10^5 Msol) within halos and then evolve following the implementation by Kim+2011. The run are radiative and evolve also 7 chemical species. These dataset are extracted around a massive cluster at z=0, and give gas density, Dark Matter density, temperature and magnetic field components in cgs units [g/cm^3, K and Gauss]. Each cell has a comoving size of 83.3 kpc. The data are written in HDF5 format (https://support.hdfgroup.org/HDF5/). We additionally provide also .fits maps of the X and Z projection across the box, showing the volume weighted mean density, DM density, temperature, |B| and Bz. For more details on the simulations please refer to http://cosmosimfrazza.myfreesites.net/magnetic-models Vazza et al. 2017 CQG (http://iopscience.iop.org/article/10.1088/1361-6382/aa8e60) For parent models with primordial seeding models and non-radiative gas physics see https://b2share.eudat.eu/records/cf49996d869540b6aefc9a06ee5082f5