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We use the IllustrisTNG simulations to show how the fractions of quenchedgalaxies vary across different environments and cosmic time, and to quantifythe role AGN feedback and preprocessing play in quenching group and clustersatellites. At $z=0$, we select galaxies with $M_* = 10^{9-12} M_{\odot}$residing within ($\leq R_{200c}$) groups and clusters of total host mass$M_{200c}=10^{13-15.2} M_{\odot}$. TNG predicts a quenched fraction of$\sim70-90\%$ (on average) for centrals and satellites $\gtrsim 10^{10.5}M_{\odot}$, regardless of host mass, cosmic time ($0\leq z\leq0.5$),clustercentric distance and time since infall in the $z=0$ host. Low-masscentrals ($\lesssim 10^{10} M_{\odot}$), instead, are rarely quenched unlessthey become members of groups ($10^{13-14} M_{\odot}$) or clusters($\geq10^{14} M_{\odot}$), where the quenched fraction rises to $\sim80\%$. Thefraction of low-mass passive galaxies is higher closer to the host center andfor more massive hosts. The population of low-mass satellites accreted$\gtrsim$4-6 Gyr ago in massive hosts is almost entirely passive, thussuggesting an upper limit for the time needed for environmental quenching tooccur. In fact, $\sim30\%$ of group and cluster satellites that are quenched at$z=0$ were already quenched before falling into their current host, and thebulk of them quenched as early as 4 to 10 billion years ago. For low-massgalaxies ($\lesssim10^{10-10.5}M_{\odot}$), this is due to preprocessing,whereby current satellites may have been members of other hosts, and hence haveundergone environmental processes, before falling into their final host, thismechanism being more common and more effective for the purposes of quenchingfor satellites found today in more massive hosts. On the other hand, massivegalaxies quench on their own and because of AGN feedback, regardless of whetherthey are centrals or satellites.

Quenched fractions in the IllustrisTNG simulations: the roles of AGN feedback, environment, and pre-processing