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We investigate the possibility of measuring intergalactic magnetic fieldsusing the dispersion measures and rotation measures of fast radio bursts. WithBayesian methods, we produce probability density functions for values of thesemeasures. We distinguish between contributions from the intergalactic medium,the host galaxy and the local environment of the progenitor. To this end, weuse constrained, magnetohydrodynamic simulations of the local Universe tocompute lines-of-sight integrals from the position of the Milky Way. Inparticular, we differentiate between predominantly astrophysical and primordialorigins of magnetic fields in the intergalactic medium. We test differentpossible types of host galaxies and probe different distribution functions offast radio burst progenitor locations inside the host galaxy. Under theassumption that fast radio bursts are produced by magnetars, we use analyticpredictions to account for the contribution of the local environment. We findthat less than 100 fast radio bursts from magnetars in stellar-windenvironments hosted by starburst dwarf galaxies at redshift $z \gtrsim 0.5$suffice to discriminate between predominantly primordial and astrophysicalorigins of intergalactic magnetic fields. However, this requires thecontribution of the Milky Way to be removed with a precision of $\approx 1\rm~rad~m^{-2}$. We show the potential existence of a subset of fast radiobursts whose rotation measure carry information on the strength of theintergalactic magnetic field and its origins.

Fast Radio Burst dispersion measures and rotation measures and the origin of intergalactic magnetic fields