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Observational searches for dual active galactic nuclei (dAGNs) at kiloparsecseparations are crucial for understanding the role of galaxy mergers in theevolution of galaxies. In addition, kpc-scale dAGNs may serve as the parentpopulation of merging massive black hole (MBH) binaries, an important source ofgravitational waves. We use a semi-analytical model to describe the orbitalevolution of unequal mass MBH pairs under the influence of stellar and gaseousdynamical friction in post-merger galaxies. We quantify how the detectabilityof approximately 40,000 kpc-scale dAGNs depends on the structure of their hostgalaxies and the orbital properties of the MBH pair. Our models indicate thatkpc-scale dAGNs are most likely to be detected in gas-rich post-merger galaxieswith smaller stellar bulges and relatively massive, rapidly rotating gas disks.The detectability is also increased in systems with MBHs of comparable massesfollowing low eccentricity prograde orbits. In contrast, dAGNs with retrograde,low eccentricity orbits are some of the least detectable systems among ourmodels. The dAGNs in models in which the accreting MBHs are allowed to exhibitradiative feedback are characterized by a significantly lower overalldetectability. The suppression in detectability is most pronounced in gas-richmerger remnant galaxies, where radiation feedback is more likely to arise. Ifso, then large, relatively gas poor galaxies may be the best candidates fordetecting dAGNs.

The Detectability of Kiloparsec Scale Dual AGNs: The Impact of Galactic Structure and Black Hole Orbital Properties