The interaction of the cosmic microwave background ( CMB ) with the hot gas in clusters of galaxies , the so-called Sunyaev–Zel ’ dovich ( SZ ) effect , is a very useful tool that allows us to determine the physical conditions in such clusters and fundamental parameters of the cosmological models .
In this work , we determine the dependence of the the SZ surface brightness amplitude with redshift and mass of the clusters .
We have used PLANCK+IRAS data in the microwave-far infrared and a catalog with \gtrsim 10 ^ { 5 } clusters of galaxies extracted from the SDSS by Wen et al .
( 2012 ) .
We estimate and subtract the dust emission from those clusters .
From the residual flux , we extract its SZ flux densities .

The absolute value of the SZ amplitude indicates that the gas mass is around 10 % of the total mass for cluster masses of M \sim 10 ^ { 14 } M _ { \odot } .
This amplitude is compatible with no evolution with redshift and proportional to M ^ { 2.70 \pm 0.37 } ( using X-ray derived masses ) or M ^ { 2.51 \pm 0.38 } ( using weak-lensing derived masses ) , with some tension regarding the expectations of the self-similar dependence ( amplitude proportional to M ^ { 5 / 3 } ) .

Other secondary products of our analysis include that clusters have a dust emission with emissivity index \beta \sim 2 and temperature T \sim 25 K ; we confirm that the CMB temperature agrees with a dependence of T _ { 0 } ( 1 + z ) with clusters of much lower mass than those explored previously ; and we find that the cluster masses derived by Wen et al .
( 2012 ) from a richness-mass relationship are biased by a factor of ( 1 + z ) ^ { -1.8 } with respect to the X-ray and weak–lensing measurements .