The observability of galaxy merger signatures in nearby gas-rich spirals

Galaxy mergers are crucial to understanding galaxy evolution, therefore we must determine their observational signatures select them from large IFU samples such as MUSE and SAMI. We employ 24 high-resolution idealised hydrodynamical merger simulations based on the "Feedback In Realistic Environment" (FIRE-2) model observability of various configurations stages using synthetic images velocity maps. Our cover a range orbital at fixed 1:2.5 stellar mass ratio for two gas rich spirals low redshift. Morphological kinematic asymmetries computed maps spanning each interaction. divide interaction sequence into three: (1) pair phase; (2) merging (3) post-coalescence phase. correctly identify between first pericentre passage 500 Myr after coalescence asymmetry with 66% completeness, depending upon phase field-of-view observation. detect fewer in (40%) many more phases (97%). find that detectability decreases field-of-view, except retrograde mergers, where centrally concentrated asymmetric features enhances detectability. Using cut-off derived combination photometric asymmetry, increase these detections 89% overall, 79% pairs, close 100% post-coalescent phases. By this combined mitigate some effects caused by smaller fields-of-view subtended massively multiplexed integral field spectroscopy programmes.