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How protoclusters evolved from sparse galaxy overdensities to mature galaxyclusters is still not well understood. In this context, detecting andcharacterizing the hot ICM at high redshifts (z~2) is key to understanding howthe continuous accretion from and mergers along the filamentary large-scalestructure impact the first phases of cluster formation. We study the dynamicalstate and morphology of the z=1.98 galaxy cluster XLSSC 122 withhigh-resolution observations (~5") of the ICM through the SZ effect. ViaBayesian forward modeling, we map the ICM on scales from the virial radius downto the core of the cluster. To constrain such a broad range of spatial scales,we employ a new technique that jointly forward-models parametric descriptionsof the pressure distribution to interferometric ACA and ALMA observations andmulti-band imaging data from the 6-m, single-dish Atacama Cosmology Telescope.We detect the SZ effect with $11\sigma$ in the ALMA+ACA observations and find aflattened inner pressure profile that is consistent with a non-cool coreclassification with a significance of $>3\sigma$. In contrast to the previousworks, we find better agreement between the SZ effect signal and the X-rayemission as well as the cluster member distribution. Further, XLSSC 122exhibits an excess of SZ flux in the south of the cluster where no X-rayemission is detected. By reconstructing the interferometric observations andmodeling in the uv-plane, we obtain a tentative detection of an infalling groupor filamentary-like structure that is believed to boost and heat up the ICMwhile the density of the gas is low. In addition, we provide an improved SZmass of $M_{500,\mathrm{c}} = 1.66^{+0.23}_{-0.20} \times 10^{14} \rm M_\odot$.Altogether, the observations indicate that we see XLSSC 122 in a dynamic phaseof cluster formation while a large reservoir of gas is already thermalized.

XLSSC 122 caught in the act of growing up: Spatially resolved SZ observations of a z=1.98 galaxy cluster