The Link between Galaxy Structure Properties and Star Formation in Local Galaxies
To investigate the role of morphology in galaxy evolution, we analyze the relationships between galaxy structure, star formation, and H i gas content. Using multiband images from the DESI Legacy Imaging Surveys, we perform detailed structural decompositions on a representative local galaxy sample fr...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/adceed |
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| author | Zhimin Zhou Wenwen Wang |
| author_facet | Zhimin Zhou Wenwen Wang |
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| description | To investigate the role of morphology in galaxy evolution, we analyze the relationships between galaxy structure, star formation, and H i gas content. Using multiband images from the DESI Legacy Imaging Surveys, we perform detailed structural decompositions on a representative local galaxy sample from xGASS. Structural components and color properties are examined as functions of deviations from the star formation main sequence (ΔSFR _MS ) and H i gas deficiency (Δ f _H I ). We find that bulge fractions decrease with higher ΔSFR _MS and lower stellar mass, indicating that star-forming galaxies are predominantly disk dominated while quiescent galaxies are bulge dominated. The slope of the color ( g − r ) versus ΔSFR _MS relationship decreases from low to high stellar masses and from outer to inner regions, with greater color variation in massive galaxies. Color gradients are predominantly negative, becoming shallower in lower-mass galaxies and in the outer disk regions. We also identify inflection points in the color gradient and bulge fraction relations with ΔSFR _MS , with main-sequence galaxies having the lowest bulge fractions and steepest color gradients. At fixed stellar mass, we observe only a slight correlation between bulge fraction and H i deficiency. However, outer disk colors show a stronger dependence on H i content than inner regions, and color gradients flatten as Δ f _H I increases. These results suggest that H i gas is more closely linked to star-forming, disk-dominated systems, supporting the idea that gas accretion fuels star formation primarily in galaxy disks. |
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| id | doaj-art-b76ef5b3b60d4cdabe305ed5bbf4d195 |
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| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| spelling | doaj-art-b76ef5b3b60d4cdabe305ed5bbf4d1952025-08-20T01:56:46ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01985220610.3847/1538-4357/adceedThe Link between Galaxy Structure Properties and Star Formation in Local GalaxiesZhimin Zhou0https://orcid.org/0000-0002-4135-0977Wenwen Wang1National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; College of Astronomy and Space Sciences, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaTo investigate the role of morphology in galaxy evolution, we analyze the relationships between galaxy structure, star formation, and H i gas content. Using multiband images from the DESI Legacy Imaging Surveys, we perform detailed structural decompositions on a representative local galaxy sample from xGASS. Structural components and color properties are examined as functions of deviations from the star formation main sequence (ΔSFR _MS ) and H i gas deficiency (Δ f _H I ). We find that bulge fractions decrease with higher ΔSFR _MS and lower stellar mass, indicating that star-forming galaxies are predominantly disk dominated while quiescent galaxies are bulge dominated. The slope of the color ( g − r ) versus ΔSFR _MS relationship decreases from low to high stellar masses and from outer to inner regions, with greater color variation in massive galaxies. Color gradients are predominantly negative, becoming shallower in lower-mass galaxies and in the outer disk regions. We also identify inflection points in the color gradient and bulge fraction relations with ΔSFR _MS , with main-sequence galaxies having the lowest bulge fractions and steepest color gradients. At fixed stellar mass, we observe only a slight correlation between bulge fraction and H i deficiency. However, outer disk colors show a stronger dependence on H i content than inner regions, and color gradients flatten as Δ f _H I increases. These results suggest that H i gas is more closely linked to star-forming, disk-dominated systems, supporting the idea that gas accretion fuels star formation primarily in galaxy disks.https://doi.org/10.3847/1538-4357/adceedGalaxy bulgesGalaxy evolutionGalaxy structureStar formation |
| spellingShingle | Zhimin Zhou Wenwen Wang The Link between Galaxy Structure Properties and Star Formation in Local Galaxies The Astrophysical Journal Galaxy bulges Galaxy evolution Galaxy structure Star formation |
| title | The Link between Galaxy Structure Properties and Star Formation in Local Galaxies |
| title_full | The Link between Galaxy Structure Properties and Star Formation in Local Galaxies |
| title_fullStr | The Link between Galaxy Structure Properties and Star Formation in Local Galaxies |
| title_full_unstemmed | The Link between Galaxy Structure Properties and Star Formation in Local Galaxies |
| title_short | The Link between Galaxy Structure Properties and Star Formation in Local Galaxies |
| title_sort | link between galaxy structure properties and star formation in local galaxies |
| topic | Galaxy bulges Galaxy evolution Galaxy structure Star formation |
| url | https://doi.org/10.3847/1538-4357/adceed |
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