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We present a first attempt to model the narrow-line (NL) region of activegalactic nuclei (AGN) in hydrodynamic simulations of galaxy mergers, using anovel physical prescription. This model is used to determine the origin ofdouble-peaked NL (dNL) AGN in merging galaxies and their connection tosupermassive black hole (SMBH) pairs, motivated by recent observations of suchobjects. We find that dNL AGN induced by the relative motion of SMBH pairs area generic but short-lived feature of gaseous major mergers. dNL AGN shouldoften be observed in late-stage mergers, during the kpc-scale phase of SMBHinspiral or soon after the SMBH merger. However, even within the kpc-scalephase, only a minority of dNL AGN are directly induced by SMBH motion; theirlifetimes are typically a few Myr. Most double peaks arise from gas kinematicsnear the SMBH, although prior to the SMBH merger up to 80% of all dNL profilesmay be influenced by SMBH motion via altered peak ratios or velocity offsets.The total lifetimes of dNL AGN depend strongly on viewing angle and onproperties of the merging galaxies. Also, in a typical merger, at least 10-40%of the double peaks induced by SMBH motion have small projected separations,0.1-1 kpc, such that dual peaks of stellar surface brightness are not easilyresolved. Diffuse tidal features can indicate late-stage galaxy mergers,although they do not distinguish SMBH pairs from merged SMBHs. We show that dNLprofiles with peak velocity splittings > 500 km s^-1 or with measurable overallvelocity shifts are often associated with SMBH pairs. Our results support thenotion that selection of dNL AGN is a promising method for identifying dualSMBH candidates, but demonstrate the critical importance of high-resolution,multi-wavelength follow-up observations, and the use of multiple lines ofevidence, for confirming the dual nature of candidate SMBH pairs. (Abridged)

Double-peaked Narrow-Line Signatures of Dual Supermassive Black Holes in Galaxy Merger Simulations