  We have analyzed the properties of a sample of 33 groups and clusters of
galaxies and examine the baryon content to check for trends over a decade in
temperature down to 1 keV. We examine the relative contribution of galaxies and
ICM to baryons in clusters through the gas-to-stellar mass ratio and find that
the typical stellar contribution to the baryonic mass is between 5 and 20%.
This ratio is found to be roughly independent of temperature. Therefore, we do
not confirm the trend of increasing gas-to-stellar mass ratio with increasing
temperature as previously claimed. We also determine distribution of the baryon
fraction with the density contrast. Virial masses are estimated from two
different mass estimators: one based on the isothermal hydrostatic equation
(IHE), the other based on scaling law models (SLM). Comparing the two methods,
we find that SLM lead to less dispersed baryon fractions over all density
contrasts and that the derived mean absolute valuesare significantly lower than
IHE mean values. We show that this is not due to the uncertainties on the outer
slope $\beta$ of the gas density profile but is rather indicating that IHE
masses are less reliable. Examining the shape of the baryon fraction profiles
we find that cluster baryon fractions estimated from SLM follow a scaling law.
Moreover, we do not find any strong evidence of increasing baryon (gas)
fraction with temperature, neither do we find the slope $\beta$ to increase
with temperature. The absence of clear trends between $f_{b}$ and
$M_{gas}/M_{*}$ with temperature is consistent with the similarity of baryon
fraction profiles and suggests that non-gravitational processes such as galaxy
feedback, do not play a dominant r\^ole in heating the intra-cluster gas on the
virial scale.
