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We use IllustrisTNG, a suite of gravity and MHD simulations, to study thedemographics and properties of jellyfish galaxies in the full cosmologicalcontext. By jellyfish galaxies, we mean satellites orbiting in massive groupsand clusters that exhibit highly asymmetric distributions of gas and gas tails.We use the TNG100 run and select galaxies at redshifts $z\le0.6$ with stellarmass exceeding $10^{9.5}{\rm M_\odot}$ and with host halo masses of$10^{13}-10^{14.6}\,{\rm M_\odot}$. Among more than about 6000 (2600) galaxieswith stars (and some gas), we identify 800 jellyfish galaxies by visuallyinspecting their gas and stellar mass maps in random projections. About $31\%$of cluster satellites are found with signatures of ram-pressure stripping andgaseous tails stemming from the main luminous bodies. This is a lower limit,since the random orientation entails a loss of about $30\%$ of galaxies that inan optimal projection would otherwise be identified as jellyfish. Theconnection with ram-pressure stripping is further confirmed by a series offindings: jellyfish galaxies are more frequent at intermediate and largecluster-centric distances ($r/R_{\rm 200c}\gtrsim 0.25$); they move through theICM with larger bulk velocities and Mach numbers than the general clusterpopulation, typically orbiting supersonically and experiencing larger rampressures. Furthermore, the gaseous tails usually extend in opposite directionsto the galaxy trajectory, with no relation between tail orientation and thehost's center. The frequency of jellyfish galaxies shows a very weak dependenceon redshift $(0\le z\le0.6)$ but larger fractions of disturbed gaseousmorphologies occur in more massive hosts and at smaller satellite masses.Finally, jellyfish galaxies are late infallers ($< 2.5-3$ Gyrs ago, at $z=0$)and the emergence of gaseous tails correlates well with the presence of bowshocks in the ICM.

Jellyfish galaxies with the IllustrisTNG simulations: I. Gas-stripping phenomena in the full cosmological context