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We investigate the cool gas absorption in galaxy clusters bycross-correlating MgII absorbers detected in quasar spectra from Data Release16 of the Sloan Digital Sky Survey (SDSS) with galaxy clusters identified inthe Dark Energy Spectroscopic Instrument (DESI) survey. We find significantcovering fractions ($1-5\, \%$ within $r_{500}$, depending on the chosenredshift interval), $\sim 4-5$ times higher than around random sightlines.While the covering fraction of cool gas in clusters decreases with increasingmass of the central galaxy, the total MgII mass within $r_{\rm 500}$ isnonetheless $\sim 10$ times higher than for SDSS luminous red galaxies (LRGs).The MgII covering fraction versus impact parameter is well described by a powerlaw in the inner regions and a exponential function at larger distances. Thecharacteristic scale of the transition between these two regimes is smaller forlarge equivalent width absorbers. Cross-correlating MgII absorption withphoto-z selected cluster member galaxies from DESI reveals a statisticallysignificant connection. The median projected distance between MgII absorbersand the nearest cluster member is $\sim200$ kpc, compared to $\sim500$ kpc inrandom mocks with the same galaxy density profiles. We do not find acorrelation between MgII strength and the star formation rate of the closestcluster neighbour. This suggests that cool gas in clusters, as traced by MgIIabsorption, is: (i) associated with satellite galaxies, (ii) dominated by coldgas clouds in the intracluster medium, rather than by the interstellar mediumof galaxies, and (iii) may originate in part from gas stripped from thesecluster satellites in the past.

Cool circumgalactic gas in galaxy clusters: connecting the DESI legacy imaging survey and SDSS DR16 MgII absorbers