X-ray flux -- mass relation for $z\gtrsim 0.7$ galaxy clusters

We use a subsample of co-detections of the ACT and MaDCoWS cluster catalogs to verify the predicted relation between the observed X-ray flux $F_X$ in the 0.5-2~keV band and the cluster mass $M_{500\mathrm{c}}$ for halos at $z>0.6-0.7$. We modify this relation by introducing a correction coefficient $\eta$, which is supposed to encapsulate factors associated with a particular method of flux estimation, the sample selection function, the definition of the cluster mass, etc. We show that the X-ray flux, being the most basic X-ray observable, serves as a convenient and low-cost mass indicator for distant galaxy clusters with photometric or even missing redshifts (by setting $z=1$) as long as it is known that $z\gtrsim 0.6-0.7$. The correction coefficient $\eta$ is $\approx 0.8$ if $M_{500\mathrm{c}}^{\mathrm{U}\mathrm{P}\mathrm{P}}$ from the ACT-DR5 catalog are used as cluster masses and $\eta \approx 1.1$ if weak-lensing-calibrated masses $M_{500\mathrm{c}}^{\mathrm{C}\mathrm{a}\mathrm{l}}$ are used instead.