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We use a cluster sample selected independently of the intracluster mediumcontent with reliable masses to measure the mean gas mass fraction and itsscatter, the biases of the X-ray selection on gas mass fraction, and thecovariance between the X-ray luminosity and gas mass. The sample is formed by34 galaxy clusters in the nearby ($0.050<z<0.135$) Universe, mostly with$14<\log M_{500}/M_\odot \lesssim 14.5$, and with masses calculated with thecaustic technique. First, we found that integrated gas density profiles havesimilar shapes, extending earlier results based on subpopulations of clusterssuch as those that are relaxed or X-ray bright for their mass. Second, theX-ray unbiased selection of our sample allows us to unveil a variegatepopulation of clusters; the gas mass fraction shows a scatter of $0.17\pm0.04$dex, possibly indicating a quite variable amount of feedback from cluster tocluster, which is larger than is found in previous samples targetingsubpopulations of galaxy clusters, such as relaxed or X-ray bright clusters.The similarity of the gas density profiles induces an almost scatterlessrelation between X-ray luminosity, gas mass, and halo mass, and modulatesselection effects in the halo gas mass fraction: gas-rich clusters arepreferentially included in X-ray selected samples. The almost scatterlessrelation also fixes the relative scatters and slopes of the $L_X-M$ and$M_{gas}-M$ relations and makes core-excised X-ray luminosities and gas massesfully covariant. Therefore, cosmological or astrophysical studies involvingX-ray or SZ selected samples need to account for both selection effects andcovariance of the studied quantities with X-ray luminosity/SZ strength.

Variegate galaxy cluster gas content: Mean fraction, scatter, selection effects and covariance with X-ray luminosity