The Dispersion of Fast Radio Bursts from a Structured Intergalactic Medium at Redshifts z < 1.5

We analyze the sources of free electrons that produce the large dispersion measures, DM $\approx 300-1600$ (in units cm${}^{-3}$ pc), observed toward fast radio bursts (FRBs). Individual galaxies typically produce DM $\sim 25-60$ cm${}^{-3}$ pc from ionized gas in their disk, disk-halo interface, and circumgalactic medium. Toward an FRB source at redshift $z$, a homogeneous IGM containing a fraction $f_{\mathrm{I}\mathrm{G}\mathrm{M}}$ of cosmological baryons will produce DM $= (935~{\rm cm}^{-3}~{\rm pc}) f_{\rm IGM} , h_{70}^{-1} I(z)$,where$I(z) = (2/3 \Omega_m)[ { \Omega_m(1+z)^3 + \Omega_{\Lambda} }^{1/2} - 1 ]$. A structured IGM of photoionized Ly-alpha absorbers in the cosmic web produces similar dispersion, modeled from the observed distribution, $f_b(N,z)$, of H I (Lya-forest) absorbers in column density and redshift with ionization corrections and scaling relations from cosmological simulations. An analytic formula for DM($z$) applied to observed FRB dispersions suggests that $z_{\rm FRB} \approx 0.2-1.5$foranIGMcontainingasignificantbaryonfraction,$f_{\rm IGM} = 0.6\pm0.1$. Future surveys of the statistical distribution, DM($z)$, of FRBs identified with specific galaxies and redshifts, can be used to calibrate the IGM baryon fraction and distribution of Ly-alpha absorbers. Fluctuations in DM at the level $\pm 10$ cm${}^{-3}$ pc will arise from filaments and voids in the cosmic web.