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We present a post-processing catalog of globular clusters (GCs) for the $39$most massive groups and clusters in the TNG50 simulation of the IlllustrisTNGproject (virial masses $M_{200} =[5\times 10^{12} \rm - 2 \times 10^{14}$]M$_{\odot}$). We tag GC particles to all galaxies with stellar mass $M_* \geq5\times10^6$ M$_{\odot}$, and we calibrate their masses to reproduce theobserved power-law relation between GC mass and halo mass for galaxies with$M_{200} \geq 10^{11}$ M$_{\odot}$ (corresponding to $M_* \sim 10^9$$M_{\odot}$). Here we explore whether an extrapolation of this $M_{\rmGC}$-$M_{200}$ relation to lower-mass dwarfs is consistent with currentobservations. We find a good agreement between our predicted number andspecific frequency of GCs in dwarfs with $\rm M_*=[5 \times 10^6 \rm - 10^9]$M$_{\odot}$ and observations. Moreover, we predict a steep decline in the GCoccupation fraction for dwarfs with $M_*<10^9$ M$_{\odot}$ which agrees wellwith current observational constraints. This declining occupation fraction isdue to a combination of tidal stripping in all dwarfs plus a stochasticsampling of the GC mass function for dwarfs with $M_* < 10^{7.5}$ M$_{\odot}$.Our simulations also reproduce available constraints on the abundance ofintra-cluster GCs in Virgo and Centaurus A. These successes provide support tothe hypothesis that the $M_{\rm GC}$-$M_{200}$ relation holds, albeit with morescatter, all the way down to the regime of classical dwarf spheroidals in theseenvironments. Our GC catalogs are publicly available as part of theIllustrisTNG data release.

Modeling globular clusters in the TNG50 simulation: predictions from dwarfs to giants