Ionized Gas Components in Low Surface Brightness Galaxy AGC 111629

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 × 10 8 M ⊙ . AGC 111629 displays an irregular H α morphology and an arch-like structure in the extraplanar region, which is absent in continuous stellar image. The irregular H α 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 ] λ 5007 map, with a position angle that differs from that of the main stellar disk. This structure exhibits a higher [O iii ] λ 5007/H β flux ratio, a larger equivalent width of [O iii ] λ 5007, and a lower H α /H β 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 ] λ 6583. 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 ] λ 5007 map. An extended region (∼2 kpc) with an extremely low value of H α /H β 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 ] λ 6583/H α diagnostic and find that AGC 111629 exhibits low central metallicity. This may result from feedback associated with AGN activity and supernova explosions.