Radial Distribution of Star Formation and Gas-phase Metallicity in Spiral-Elliptical Galaxy Pairs
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| Main Authors: | , , , , , |
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| Format: | Preprint |
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2026
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| _version_ | 1866915938939437056 |
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| author | Shi, Cailu Feng, Shuai Shen, Shiyin Li, Linlin Cui, Wenyuan Hu, Guozhen |
| author_facet | Shi, Cailu Feng, Shuai Shen, Shiyin Li, Linlin Cui, Wenyuan Hu, Guozhen |
| contents | Using integral field spectroscopy from SDSS-IV MaNGA, we investigate the radial distributions of star formation rate (SFR) and gas-phase metallicity in spiral galaxies that reside in spiral-elliptical (S+E) pairs. Spirals in S+E pairs show suppressed central star formation and elevated metallicities, whereas spirals in spiral-spiral pairs exhibit centrally enhanced star formation and reduced metallicities. The degree of SFR suppression and metallicity enhancement in S+E pairs depends on the masses of the pair members. Spirals with more massive elliptical companions experience stronger star-formation suppression and larger increases in metallicity, while lower-mass spirals show more pronounced metallicity enhancement. In addition, within S+E systems, galaxies with asymmetric gas velocity fields display enhanced SFR and higher metallicities, whereas those with symmetric velocity fields exhibit clear central suppression. Based on these results, we infer that in S+E pairs, the spiral galaxy experiences suppressed gas accretion once it enters the hot circumgalactic medium of its early-type companion, which leads to the observed decline in star-formation activity. When a close encounter takes place, tidal perturbations can compress the remaining cold gas and trigger enhanced star formation, producing rapid chemical enrichment and the associated increase in metallicity. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2604_14092 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Radial Distribution of Star Formation and Gas-phase Metallicity in Spiral-Elliptical Galaxy Pairs Shi, Cailu Feng, Shuai Shen, Shiyin Li, Linlin Cui, Wenyuan Hu, Guozhen Astrophysics of Galaxies Using integral field spectroscopy from SDSS-IV MaNGA, we investigate the radial distributions of star formation rate (SFR) and gas-phase metallicity in spiral galaxies that reside in spiral-elliptical (S+E) pairs. Spirals in S+E pairs show suppressed central star formation and elevated metallicities, whereas spirals in spiral-spiral pairs exhibit centrally enhanced star formation and reduced metallicities. The degree of SFR suppression and metallicity enhancement in S+E pairs depends on the masses of the pair members. Spirals with more massive elliptical companions experience stronger star-formation suppression and larger increases in metallicity, while lower-mass spirals show more pronounced metallicity enhancement. In addition, within S+E systems, galaxies with asymmetric gas velocity fields display enhanced SFR and higher metallicities, whereas those with symmetric velocity fields exhibit clear central suppression. Based on these results, we infer that in S+E pairs, the spiral galaxy experiences suppressed gas accretion once it enters the hot circumgalactic medium of its early-type companion, which leads to the observed decline in star-formation activity. When a close encounter takes place, tidal perturbations can compress the remaining cold gas and trigger enhanced star formation, producing rapid chemical enrichment and the associated increase in metallicity. |
| title | Radial Distribution of Star Formation and Gas-phase Metallicity in Spiral-Elliptical Galaxy Pairs |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2604.14092 |