Extreme mass ratio inspirals (EMRIs) are expected to host large accretion disks around the central supermassive black hole within the system. Thus the orbiting smaller mass compact objects (NS, WD, or stellar mass black holes) interact and experience hydrodynamic drag as it swim through the accretion disk of the central black hole. The interaction between the disk and the companion alters the orbital behavior, thereby affecting the profiles of the emitted gravitational waves (GWs). Therefore observing such GW signals one could in principle identify the existence of an accretion disk in such systems. In this chapter we studied such EMRIs with accretion disks. We computed the dynamics of the companion and the resulting GW incorporating the effect of disk interaction, i.e., accretion drag and dynamical friction. We have chosen the transonic disks as the fluid dynamical model to describe accretion flow. We found that the disk’s presence is detectable with the present sensitivity of LISA. Detectability increases with the central black hole’s accretion rate. For our disk model the disk is detectable for accretion rate as low as \(0.1\dot {M}_E\) for 1 year observation by LISA.