Ionized gas components in low surface brightness galaxy AGC 111629
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arXiv
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| Natura: | Preprint |
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2025
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| author | Cao, Tian-Wen Chen, Pei-Bin Li, Zi-Jian Cheng, Cheng Kalari, Venu M. Shen, Meng-Ting Zhang, Chun-Yi Wang, Junfeng Galaz, Gaspar Wu, Hong Chen, Zi-Qi |
| author_facet | Cao, Tian-Wen Chen, Pei-Bin Li, Zi-Jian Cheng, Cheng Kalari, Venu M. Shen, Meng-Ting Zhang, Chun-Yi Wang, Junfeng Galaz, Gaspar Wu, Hong Chen, Zi-Qi |
| contents | We present integral field spectroscopy of ionized gas components in AGC 111629, an edge-on low surface brightness galaxy (LSBG) with a stellar mass of 5.7$\times$10$^{8}$ M$_{\odot}$. 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 [OIII]$λ$5007 map, with a position angle that differs from that of the main stellar disk. This structure exhibits a higher [OIII]$λ$5007/H$β$ flux ratio, a larger equivalent width (EW) of [OIII]$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 BPT diagram based on [NII]$λ$6583. These features may be associated with the central AGN. Additionally, a sub-peak in the southern disk is clearly visible in the [OIII]$λ$5007 map. An extended region ($\sim$ 2 kpc) with an extremely low value of H$α$/H$β$ flux ratio is observed near this sub-peak. We interpret the sub-peak as a superbubble likely driven by supernova explosions in the southern disk. We derive the gas-phase metallicity, 12+log(O/H), using the [NII]$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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_06667 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Ionized gas components in low surface brightness galaxy AGC 111629 Cao, Tian-Wen Chen, Pei-Bin Li, Zi-Jian Cheng, Cheng Kalari, Venu M. Shen, Meng-Ting Zhang, Chun-Yi Wang, Junfeng Galaz, Gaspar Wu, Hong Chen, Zi-Qi Astrophysics of Galaxies We present integral field spectroscopy of ionized gas components in AGC 111629, an edge-on low surface brightness galaxy (LSBG) with a stellar mass of 5.7$\times$10$^{8}$ M$_{\odot}$. 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 [OIII]$λ$5007 map, with a position angle that differs from that of the main stellar disk. This structure exhibits a higher [OIII]$λ$5007/H$β$ flux ratio, a larger equivalent width (EW) of [OIII]$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 BPT diagram based on [NII]$λ$6583. These features may be associated with the central AGN. Additionally, a sub-peak in the southern disk is clearly visible in the [OIII]$λ$5007 map. An extended region ($\sim$ 2 kpc) with an extremely low value of H$α$/H$β$ flux ratio is observed near this sub-peak. We interpret the sub-peak as a superbubble likely driven by supernova explosions in the southern disk. We derive the gas-phase metallicity, 12+log(O/H), using the [NII]$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. |
| title | Ionized gas components in low surface brightness galaxy AGC 111629 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2510.06667 |