We present the coronal imaging of two active eclipsing binaries, ER Vul and XY UMa based on the X-ray data obtained from the XMM-Newton satellite. The results indicate that these systems are very soft X-ray sources, with a majority of the X-rays coming below 2 keV energy. The X-ray light curves show orbital modulation with an apparent primary eclipse, and modelling of the X-ray light curves reveals that both components of these systems are active, with the primary component being more X-ray bright than the secondary. Furthermore, results from the coronal imaging indicate that the coronae of both components are connected for the detached and semidetached binaries ER Vul and XY UMa, respectively. In the case of XY UMa, a highly active region near the coronal connection region is found, which is twice as bright as the second component in the system. Three flaring events are detected in the binary system XY UMa, which originated in the same active region that lies somewhere in between the two binary components.