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We examine the proposal that the dispersion measures (DMs) and Faradayrotation measures (RMs) of extragalactic linearly-polarized fast radio bursts(FRBs) can be used to probe the intergalactic magnetic field (IGMF) infilaments of galaxies. The DM through the cosmic web is dominated bycontributions from the warm-hot intergalactic medium (WHIM) in filaments andfrom the gas in voids. On the other hand, RM is induced mostly by the hotmedium in galaxy clusters, and only a fraction of it is produced in the WHIM.We show that if one excludes FRBs whose sightlines pass through galaxyclusters, the line-of-sight strength of the IGMF in filaments, $B_{||}$, isapproximately $C(\langle 1+z \rangle/f_{DM})(RM/DM)$, where $C$ is a knownconstant. Here, the redshift of the FRB is not required to be known; $f_{DM}$is the fraction of total DM due to the WHIM, while $\langle 1+z \rangle$ is theredshift of interevening gas weighted by the WHIM gas density, both of whichcan be evaluated for a given cosmology model solely from the DM of an FRB.Using data on structure formation simulations and a model IGMF, we show that$C(\langle 1+z \rangle/f_{DM})(RM/DM)$ closely reproduces the density-weightedline-of-sight strength of the IGMF in filaments of the large-scale structure.

Fast Radio Bursts as Probes of Magnetic Fields in the Intergalactic Medium