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Mergers are suspected to be reliable triggers of both starformation and AGNactivity. However, the exact timing of this process remains poorly understood.Here, we present deep imaging and long slit spectroscopy data of a sample offour double-peaked [OIII] emitting AGN. These sources are often believed tohost binary AGN, or at least be currently undergoing major mergers. The samplepresented here either have previous IFU and high resolution imaging data thatshow double-nuclei in the IR as well as kinematicly and spatially distinct lineemitting regions. Two sources have detections of double point sources in eitherthe X-ray or radio. The sources studied are therefore likely binary AGN. TheAGN in this sample are luminous, radio-quiet and at low redshift. The $u/r/z$imaging data show host galaxies in a wide range of merger stages, with themajority (3/4) showing tidal tails or complex kinematics and morphologiesclearly indicating a recent merger. One source however -hosting a double X-raysource- shows quiescent morphologies with no clear signs of interaction fromimaging data. The spectroscopy in this case reveals a gas disk counter-rotatingwith respect to the stellar component. Spectroscopy of the other sources revealdisturbed kinematics further confirming their status as ongoing mergers. Ourdata show that AGN triggering in mergers may happen over a wide time span andthat sinking of black holes to the center of a merged system might takeconsiderable time in some cases. A detailed analysis will be published in anupcoming paper. Further studies of AGN in merging galaxies will show how thehosts of those AGN differ from normal mergers without AGN activity.

Host galaxies of double-peaked [OIII] emitting AGN: binary AGN or mergers?