2025AJ....170..296C

We present integral field spectroscopy of ionized gas components in AGC 111629, an edge-on low surface brightness galaxy with a stellar mass of 5.7 × 10⁸M_⊙. AGC 111629 displays an irregular Hα morphology and an arch-like structure in the extraplanar region, which is absent in continuous stellar image. The irregular Hα morphology may be related to a past merger event with its satellite galaxy AGC 748815. A peanut-shaped structure at the center in the integrated [O III]λ5007 map, with a position angle that differs from that of the main stellar disk. This structure exhibits a higher [O III]λ5007/Hβ flux ratio, a larger equivalent width of [O III]λ5007, and a lower Hα/Hβ flux radio (<2.86). Some spaxels associated with the peanut-shaped structure fall within the composite region of the Baldwin-Phillips-Terlevich diagram based on [N II]λ6583. These features may be associated with the central active galactic nucleus (AGN). Additionally, a subpeak in the southern disk is clearly visible in the [O III]λ5007 map. An extended region (∼2 kpc) with an extremely low value of Hα/Hβ flux ratio is observed near this subpeak. We interpret the subpeak as a superbubble likely driven by supernova explosions in the southern disk. We derive the gas-phase metallicity, 12+log(O/H), using the [N II]λ6583/Hα diagnostic and find that AGC 111629 exhibits low central metallicity. This may result from feedback associated with AGN activity and supernova explosions.