Probing cosmology and gastrophysics with fast radio bursts: Cross-correlations of dark matter haloes and cosmic dispersion measures

Abstract

For future surveys of fast radio bursts (FRBs), we clarify information available from cosmic dispersion measures (DMs) through cross-correlation analyses of foreground dark matter haloes (hosting galaxies and galaxy clusters) with their known redshifts. With a halo-model approach, we predict that the cross-correlation with cluster-sized haloes is less affected by the details of gastrophysics, providing robust cosmological information. For less massive haloes, the cross-correlation at angular scales of $<10\mathrm{arcmin}$ is sensitive to gas expelled from the halo centre due to galactic feedback. Assuming $20000$ FRBs over $20000{\mathrm{deg}}^2$ with a localisation error being 3 arcmin, we expect that the cross-correlation signal at halo masses of $10^{12}-10^{14}{M}_{\odot }$ can be measured with a level of $\sim 1\%$ precision in a redshift range of $0<z<1$. Such precise measurements enable one to put a 1.5\% level constraint on ${\sigma }_8({\Omega }_{\mathrm{M}}/0.3{)}^{0.5}$ and a 3\% level constraint on $({\Omega }_{\mathrm{b}}/0.049)(h/0.67)(f_{\mathrm{e}}/0.95)$ (${\sigma }_8$, ${\Omega }_{\mathrm{M}}$, ${\Omega }_{\mathrm{b}}$, $h$ and $f_{\mathrm{e}}$ are the linear mass variance smoothed at $8h^{-1}\mathrm{Mpc}$, mean mass density, mean baryon density, the present-day Hubble parameter and fraction of free electrons in cosmic baryons today), whereas the gas-to-halo mass relation in galaxies and clusters can be constrained with a level of $10\%-20\%$. Furthermore the cross-correlation analyses can break the degeneracy among ${\Omega }_{\mathrm{b}}$, $h$ and $f_{\mathrm{e}}$, inherent in the DM-redshift relation. Our proposal opens new possibilities for FRB cosmology, while it requires extensive galaxy redshift catalogues and further improvement of the halo model.

21 pages, 9 figures, 4 tables. Accepted for publication in MNRAS

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• The Physics of Fast Radio Bursts
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