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Past observations and simulations predict an increasingly inhomogeneous gasdistribution towards the outskirts of galaxy clusters, but the exact propertiesof such gas clumping are not yet well known. The outskirts of Abell 133 benefitfrom deep X-ray observations, with a 2.4 Ms ultra-deep Chandra exposure as wellas eight archival Suzaku pointings, making it a unique laboratory to study theclumping of the intracluster medium. We searched for significant clumpcandidates, in particular aiming to identify those that could represent genuineICM inhomogeneity. To further understand how clumping biases the thermodynamicprofiles, we compared the measurements including and excluding the clumpcandidates. We jointly analyzed Chandra and Suzaku observations of Abell 133.We selected clump candidates with at least 2$\sigma$ significance based on theChandra image and further discussed their origins using information from theDESI Legacy Imaging Surveys cluster catalogue, as well as the CFHT r-bandimage. We performed multiple rounds of Suzaku spectral analysis with differentcorrections for the underlying point sources and clump distribution, andcompared the resulting thermodynamic profiles. We detected 16 clump candidatesusing Chandra, most of which are identified as background clusters or galaxiesas opposed to intrinsic inhomogeneity. Even after the correction of theresolved clumps, the entropy profile approaching the outskirts still flattens,deviating from the power law model expected from self-similar evolution, whichimplies that unresolved clumping and other complex physics should contribute tothe entropy flattening in the outskirts.

Investigating the outskirts of Abell 133 with Suzaku and Chandra observations