The X-Ray Luminosity--Mass Relation for Local Clusters of Galaxies

Details The X-Ray Luminosity--Mass Relation for Local Clusters of Galaxies The X-Ray Luminosity--Mass Relation for Local Clusters of Galaxies

2006-02-15

arxiv.org/abs/astro-ph/0602324v2

Astrophys.J.648:956-968,2006

Astronomy and Astrophysics

Astrophysics

18 pages, 13 figures, accepted to ApJ. We have incorporated the WMAP cosmology constraints in our analysis

Scientific paper

10.1086/506248

We investigate the relationship between soft \xray luminosity and mass for low redshift clusters of galaxies by comparing observed number counts to expectations of $\Lambda$CDM cosmologies. We use a three-parameter model for the conditional probability of luminosity given mass and epoch, described as a log-normal distribution of fixed width centered on a power-law scaling relation, $L \spropto M^p\rhoc^s(z)$. We use an ensemble of simulated clusters to argue that the observed, intrinsic variance in the temperature--luminosity relation is directly indicative of mass--luminosity variance, and derive $\sigm \se 0.43 \pm 0.06$ from HIFLUGCS data. Adding this to the likelihood analysis results in best-fit estimates $p \se 1.59 \pm 0.05$, $\lnlf \se 1.34 \pm 0.09$, and $\sigm \se 0.37 \pm 0.05$ for self-similar redshift evolution in a concordance ($\Omega_m \se 0.3$, $\Omega_\Lambda \se 0.7$, $\sigma_8 \se0.9$) universe. We show that the present-epoch intercept is very sensitive to power spectrum normalization, $\lnlf \spropto \sigate^{-4}$, and the slope is weakly sensitive to the matter density, $p \spropto \Omega_m^{1/2}$. The intercept derived here is dimmer by a factor 2, and slope slightly steeper, than the L-M relation published using hydrostatic mass estimates of the HIFLUGCS sample. We show that this discrepancy is largely due to Malmquist bias of the \xray\ flux-limited sample. In light of new WMAP constraints, we discuss the interplay between parameters and sources of systematic error, and offer a compromise model with $\Omega_m \se 0.24$, $\sigma_8 \se 0.85$, and somewhat lower scatter $\sigm \se 0.25$, in which hydrostatic mass estimates remain accurate to $\ssim 15%$. We stress the need for independent calibration of the L-M relation via weak gravitational lensing.

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