Redshift drift reconstruction for some cosmological models from observations

Abstract

Redshift drift is a tool to directly probe the expansion history of the universe. Based on the Friedmann-Robertson-Walker framework, we reconstruct the velocity drift and deceleration factor for several cosmological models using observational H(z) data from the differential ages of galaxies and baryon acoustic oscillation peaks, luminosity distance of Type Ia supernovae, cosmic microwave background shift parameter, and baryon acoustic oscillation distance parameter. They can, for the first time, provide an objective and quantifiable measure of the redshift drift. We find that reconstructed velocity drift with different peak values and corresponding redshifts can potentially provide a method to distinguish the quality of competing dark energy models at low redshifts. Better fitting between models and observational data indicate that current data are insufficient to distinguish the quality of these models. However, by comparing with the simulated velocity drift from Liske et al, we find that the Dvali-Gabadadze-Porrati model is inconsistent with the data at high redshift, which originally piqued the interest of researchers in the topic of redshift drift. Considering the deceleration factor, we are able to give a stable instantaneous estimation of a transition redshift of z t ∼ 0.7 from joint constraints, which incorporates a more complete set of values than the previous study that used a single data set.

Forecast and analysis of the cosmological redshift drift

“…Due to the near future possibilities to measure the cosmological redshift drift, this type of observations has recently drawn some attention. The reconstruction of the theoretical SL signal that different cosmological models would produce has been explored quite extensively [30,31]. It comes out that the range and variety of the different cosmological redshift drift signals created by various models is remarkable: from those created by different proposals for dark energy's equation of state or modified gravity [32,33], to the ones created by backreaction in an inhomogeneous universe without the presence of dark energy [34]; from the peculiar signals for Lemaître-Tolman-Bondi models [35,36], to even a null signal [37] for the R h = ct Universe, or other several exotic scenarios [38][39][40][41][42][43].…”