Constancy of the Cluster Gas Mass Fraction in the R_h=ct Universe

TL;DR

This study compares the R_h=ct universe model with LCDM using galaxy cluster gas mass fraction data, finding R_h=ct consistent with observations and statistically favored over LCDM without free parameter tuning.

Contribution

It provides the first direct comparison of R_h=ct and LCDM models using gas mass fraction data, showing R_h=ct's consistency and statistical preference.

Findings

R_h=ct model fits the data well up to z<2

Model selection favors R_h=ct with ~95% likelihood

LCDM also consistent but less favored statistically

Abstract

The ratio of baryonic to dark matter densities is assumed to have remained constant throughout the formation of structure. With this, simulations show that the fraction f_gas(z) of baryonic mass to total mass in galaxy clusters should be nearly constant with redshift z. However, the measurement of these quantities depends on the angular distance to the source, which evolves with z according to the assumed background cosmology. An accurate determination of f_gas(z) for a large sample of hot (kT_e > 5 keV), dynamically relaxed clusters could therefore be used as a probe of the cosmological expansion up to z < 2. The fraction f_gas(z) would remain constant only when the "correct" cosmology is used to fit the data. In this paper, we compare the predicted gas mass fractions for both LCDM and the R_h=ct Universe and test them against the 3 largest cluster samples. We show that R_h=ct is consistent with a constant f_gas in the redshift range z < 2, as was previously shown for the reference LCDM model (with parameter values H_0=70 km/s/Mpc, Omega_m=0.3 and w_de=-1). Unlike LCDM, however, the R_h=ct Universe has no free parameters to optimize in fitting the data. Model selection tools, such as the Akaike Information Criterion (AIC) and the Bayes Information Criterion (BIC), therefore tend to favour R_h=ct over LCDM. For example, the BIC favours R_h=ct with a likelihood of ~95% versus ~5% for LCDM.