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The most nearby clusters are the best places to study physical and enrichmenteffects in the faint cluster outskirts. A3158 located at z=0.059 is quiteextended with a characteristic radius r$_{200}$=23.95 arcmin. In 2019, A3158was observed as a calibration target in a pointed observation with the eROSITAtelescope onboard the SRG mission.  We determined 1d temperature, abundance and normalisation profiles fromeROSITA and XMM-Newton and Chandra data as well as 2d maps of temperaturedistribution from eROSITA data. The velocity dispersion was determined and thecluster mass was calculated.  The overall temperature was measured to be 4.725$\pm$ 0.035 keV. The profilesof eROSITA all agree on a ~10% level with those determined with XMM-Newton andChandra data. From the temperature map we see that the cluster lacks a coolcore, as noted before. The presence of a previously detected off-centre coolclump West of the central cluster region is observed. Furthermore there is abow shaped edge near the location of the cool gas clump West of the clustercentre. An extension of gas is detected for the first time further out in theWest. The velocity dispersion of the cluster was measured to be 1058$\pm$41 kms$^{-1}$. The total mass was determined as $M_{200}$=1.38$\pm$ 0.25x10$^{15}$$M_{\odot}$. The mass estimate from the M-T relation is significantly lower atM$_{200}$=5.09$\pm$ 0.59x10$^{14}M_{\odot}$. An extended X-ray source locatedSouth of the cluster also coincides with a galaxy overdensity with redshifts inthe range 0.05<z<0.07. These are indications that the cluster may be undergoingmerger activity. Another extended source located North of the cluster isdetected in X-rays and coincides with an overdensity of galaxies with redshiftsin the range of 0.070<z<0.077. This is likely a background cluster not relatedto A3158. Additionally a known SPT cluster at z=0.53 was detected.

X-Ray Studies of the Abell 3158 Galaxy Cluster with eROSITA