Stacking 3455 CHIME/FRB sightlines on 1288 SDSS voids shows a 3.2 sigma DM deficit toward centers, implying 60 percent baryon underdensity consistent with galaxy underdensity and hydrodynamical simulations.
S., Battaglia, N., Smith, K
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Kinetic Sunyaev-Zel'dovich reconstruction from WISExSuperCOSMOS and unWISE galaxies with Planck data yields tight upper limits on bulk velocities consistent with LambdaCDM out to 2000 h^{-1} Mpc while showing tension with a quasar dipole interpretation.
FRB DMs correlate at 2.6-5 sigma with galaxies, weak lensing, CIB, CMB lensing, tSZ, X-ray clusters, SXRB and radio continuum, consistent with moderate feedback models while ruling out weak feedback at 3.5 sigma via SXRB-DM.
FRB dispersion measures directly constrain suppression of the matter power spectrum due to feedback at k ~ 0.1-3 h/Mpc, reduce posterior variance by a factor of ~8 at k~1 h/Mpc, and exclude extreme large-scale feedback scenarios at ~2 sigma.
citing papers explorer
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Baryons in the Darkest Sites of the Universe
Stacking 3455 CHIME/FRB sightlines on 1288 SDSS voids shows a 3.2 sigma DM deficit toward centers, implying 60 percent baryon underdensity consistent with galaxy underdensity and hydrodynamical simulations.
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Measuring cosmic bulk flow with kinetic Sunyaev-Zel'dovich velocity reconstruction
Kinetic Sunyaev-Zel'dovich reconstruction from WISExSuperCOSMOS and unWISE galaxies with Planck data yields tight upper limits on bulk velocities consistent with LambdaCDM out to 2000 h^{-1} Mpc while showing tension with a quasar dipole interpretation.
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Backlighting the Cosmic Web with Fast Radio Bursts: An Anthology of Dispersion Measure Cross-Correlations with Large-Scale Structure and Baryon Tracers
FRB DMs correlate at 2.6-5 sigma with galaxies, weak lensing, CIB, CMB lensing, tSZ, X-ray clusters, SXRB and radio continuum, consistent with moderate feedback models while ruling out weak feedback at 3.5 sigma via SXRB-DM.
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Signatures of Suppressed Matter Clustering revealed by Fast Radio Bursts
FRB dispersion measures directly constrain suppression of the matter power spectrum due to feedback at k ~ 0.1-3 h/Mpc, reduce posterior variance by a factor of ~8 at k~1 h/Mpc, and exclude extreme large-scale feedback scenarios at ~2 sigma.