We present the hypothesis that some of ring galaxies were formed by relicmagnetic torus - shaped wormholes. In the primordial plasma before therecombination magnetic fields of wormholes trap baryons whose energy is smallerthan a threshold energy. They work as the Maxwell's demons collecting baryonsfrom the nearest (horizon size) region and thus forming clumps of baryonicmatter which have the same torus-like shapes as wormhole throats. Such clumpsmay serve as seeds for the formation of ring galaxies and smaller objectshaving the ring form. Upon the recombination torus-like clumps may decay andmerge. Unlike galaxies, such objects may contain less or even no dark matter inhalos. However the most stringent feature of such objects is the presence of alarge - scale toroidal magnetic field. We show that there are threshold valuesof magnetic fields which give the upper and lower boundary values for thebaryon clumps in such protogalaxies.

Understanding how galaxies cease to form stars represents an outstandingchallenge for galaxy evolution theories. This process of "star formationquenching" has been related to various causes, including Active Galactic Nuclei(AGN) activity, the influence of large-scale dynamics, and the environment inwhich galaxies live. In this paper, we present the first results from afollow-up of CALIFA survey galaxies with observations of molecular gas obtainedwith the APEX telescope. Together with EDGE survey CARMA observations, wecollect $^{12}$CO observations that cover approximately one effective radius in472 CALIFA galaxies. We observe that the deficit of galaxy star formation withrespect to the star formation main sequence (SFMS) increases with the absenceof molecular gas and with a reduced efficiency of conversion of molecular gasinto stars, in line with results of other integrated studies. However, bydividing the sample into galaxies dominated by star formation and galaxiesquenched in their centres (as indicated by the average value of the H$\alpha$equivalent width), we find that this deficit increases sharply once a certainlevel of gas consumption is reached, indicating that different mechanisms driveseparation from the SFMS in star-forming and quenched galaxies. Our resultsindicate that differences in the amount of molecular gas at a fixed stellarmass are the primary driver for the dispersion in the SFMS, and the most likelyexplanation for the start of star-formation quenching. However, once a galaxyis quenched, changes in star formation efficiency drive how much a retiredgalaxy separates in star formation rate from star-forming ones of similarmasses. In other words, once a paucity of molecular gas has significantlyreduced star formation, changes in the star formation efficiency are whatdrives a galaxy deeper into the red cloud, retiring it.

Different processes have been proposed to explain the formation of S0s,including mergers, disc instabilities and quenched spirals. These processes areexpected to dominate in different environments, and thus leave characteristicfootprints in the kinematics and stellar populations of the individualcomponents within the galaxies. New techniques enable us to cleanly disentanglethe kinematics and stellar populations of these components in IFU observations.In this paper, we use buddi to spectroscopically extract the light from thebulge, disc and lens components within a sample of 8 S0 galaxies in extremeenvironments observed with MUSE. While the spectra of bulges and discs in S0galaxies have been separated before, this work is the first to isolate thespectra of lenses. Stellar populations analysis revealed that the bulges andlenses have generally similar or higher metallicities than the discs, and the$\alpha$-enhancement of the bulges and discs are correlated, while those of thelenses are completely unconnected to either component. We conclude that themajority of the mass in these galaxies was built up early in the lifetime ofthe galaxy, with the bulges and discs forming from the same material throughdissipational processes at high redshift. The lenses, on the other hand, formedover independent timescales at more random times within the lifetime of thegalaxy, possibly from evolved bars. The younger stellar populations andasymmetric features seen in the field S0s may indicate that these galaxies havebeen affected more by minor mergers than the cluster galaxies.