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The X-ray telescope eROSITA onboard the newly launched SRG missionserendipitously observed the galaxy cluster A3408 ($z=0.0420$) during the PVobservation of the AGN 1H0707-495. Despite its brightness and large extent, ithas not been observed by any modern X-ray observatory. A neighbouring clusterin NW direction, A3407 ($z=0.0428$), appears to be close at least in projection($\sim 1.7$ Mpc). This cluster pair could be in a pre- or post-merger state.  We perform a detailed X-ray analysis of A3408. We construct particlebackground subtracted and exposure corrected images and surface brightnessprofiles in different sectors. The spectral analysis is performed out to$1.4r_{500}$. Additionally, a temperature map is presented depicting thedistribution of the ICM temperature. Furthermore, we make use of data from theRASS to estimate some bulk properties of A3408 and A3407, using the growthcurve analysis method and scaling relations.  The imaging analysis shows a complex morphology of A3408 with a strongelongation in SE-NW direction. This is quantified by comparing the surfacebrightness profiles of the NW, SW, SE and NE directions, where the NW and SEdirections show a significantly higher surface brightness compared to the otherdirections. We determine a gas temperature ${\rm k_B}T_{500}=(2.23\pm0.09)$keV. The T-profile reveals a hot core within $2'$ of the emission peak, ${\rmk_B}T=3.04^{+0.29}_{-0.25}$ keV. Employing a M-T relation, we obtain$M_{500}=(9.27\pm0.75)\times 10^{13}M_{\odot}$ iteratively. The $r_{200}$ ofA3407 and A3408 are found to overlap in projection which makes ongoinginteractions plausible. The 2d T-map reveals higher temperatures in W than in Edirection.  A3407 and A3408 are likely in a pre-merger state, affecting the ICMproperties, i.e., increased temperatures in the direction of A3407 indicateadiabatic compression or shocks due to the interaction.

EROSITA Spectro-Imaging Analysis of the Abell 3408 Galaxy Cluster