FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies
We present the H i surface density (Σ _H _i ) radial distributions based on total-power H i images obtained by FAST in the FEASTS program, for 35 galaxies with inclinations lower than 72°. We derive the H i radius R _001 , which is the radius for the 0.01 M _⊙ pc ^−2 (~10 ^18.1 cm ^−2 ) isodensity l...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada95a |
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| author | Jing Wang Dong Yang Xuchen Lin Qifeng Huang Zhijie Qu Hsiao-wen Chen Hong Guo Luis C. Ho Peng Jiang Zezhong Liang Céline Péroux Lister Staveley-Smith Simon Weng |
| author_facet | Jing Wang Dong Yang Xuchen Lin Qifeng Huang Zhijie Qu Hsiao-wen Chen Hong Guo Luis C. Ho Peng Jiang Zezhong Liang Céline Péroux Lister Staveley-Smith Simon Weng |
| author_sort | Jing Wang |
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| description | We present the H i surface density (Σ _H _i ) radial distributions based on total-power H i images obtained by FAST in the FEASTS program, for 35 galaxies with inclinations lower than 72°. We derive the H i radius R _001 , which is the radius for the 0.01 M _⊙ pc ^−2 (~10 ^18.1 cm ^−2 ) isodensity level, 100 times deeper than the 1 M _⊙ pc ^−2 level previously commonly used to measure R _1 . The profile shapes show a large diversity at a given radius in units of kpc, group virial radius, and R _1 , but they align more tightly with the radius normalized by R _001 . The universal H i profile has a scatter of ~0.2 dex and a scale length of ~0.11 R _001 in the outer region. We derive a new R _001 – M _H _i relation, which has a scatter of 0.03 dex and a similar slope of ~0.5 to the previously known R _1 – M _H _i relation. Excluding strongly tidal-interacting galaxies, the ratio R _001 / R _1 (anti)correlates strongly and significantly with the H i -to-stellar mass ratio and specific star formation rate, but not with the stellar mass, M _H _i , dark matter mass, or star formation rate. The strongly tidal-interacting galaxies tend to show deviations from these trends and have the most flattened profiles. These results imply that, in the absence of major tidal interactions, physical processes must cooperate so that Σ _H _i distributes in a self-similar way in the outer region down to the 0.01 M _⊙ pc ^−2 level. Moreover, they may drive gas flows in such a way that H i -richer galaxies have H i disks that not only extend further but also transport H i inward more efficiently from R _001 to R _1 . |
| format | Article |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| series | The Astrophysical Journal |
| spelling | doaj-art-5d4e30158f1f4060852a4302021acc002025-02-03T07:01:24ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198012510.3847/1538-4357/ada95aFEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby GalaxiesJing Wang0https://orcid.org/0000-0002-6593-8820Dong Yang1https://orcid.org/0000-0002-5679-3447Xuchen Lin2https://orcid.org/0000-0002-4250-2709Qifeng Huang3https://orcid.org/0000-0003-2863-9837Zhijie Qu4https://orcid.org/0000-0002-2941-646XHsiao-wen Chen5https://orcid.org/0000-0001-8813-4182Hong Guo6https://orcid.org/0000-0003-4936-8247Luis C. Ho7https://orcid.org/0000-0001-6947-5846Peng Jiang8https://orcid.org/0009-0003-3527-8520Zezhong Liang9Céline Péroux10https://orcid.org/0000-0002-4288-599XLister Staveley-Smith11https://orcid.org/0000-0002-8057-0294Simon Weng12Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; jwang_astro@pku.edu.cnKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; jwang_astro@pku.edu.cnKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; jwang_astro@pku.edu.cnKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; jwang_astro@pku.edu.cnDepartment of Astronomy and Astrophysics, The University of Chicago , 5640 S. Ellis Avenue, Chicago, IL 60637, USADepartment of Astronomy and Astrophysics, The University of Chicago , 5640 S. Ellis Avenue, Chicago, IL 60637, USAShanghai Astronomical Observatory, Chinese Academy of Sciences , Shanghai 200030, People's Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; jwang_astro@pku.edu.cnNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, People's Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; jwang_astro@pku.edu.cnEuropean Southern Observatory , Karl-Schwarzschildstrasse 2, D-85748 Garching bei München, Germany; Aix Marseille Université , CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388 Marseille, FranceInternational Centre for Radio Astronomy Research, University of Western Australia , 35 Stirling Highway, Crawley, WA 6009, Australia; ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia; Sydney Institute for Astronomy, School of Physics A28, University of Sydney , NSW 2006, Australia; ATNF , CSIRO Space and Astronomy, PO Box 76, Epping, NSW 1710, AustraliaWe present the H i surface density (Σ _H _i ) radial distributions based on total-power H i images obtained by FAST in the FEASTS program, for 35 galaxies with inclinations lower than 72°. We derive the H i radius R _001 , which is the radius for the 0.01 M _⊙ pc ^−2 (~10 ^18.1 cm ^−2 ) isodensity level, 100 times deeper than the 1 M _⊙ pc ^−2 level previously commonly used to measure R _1 . The profile shapes show a large diversity at a given radius in units of kpc, group virial radius, and R _1 , but they align more tightly with the radius normalized by R _001 . The universal H i profile has a scatter of ~0.2 dex and a scale length of ~0.11 R _001 in the outer region. We derive a new R _001 – M _H _i relation, which has a scatter of 0.03 dex and a similar slope of ~0.5 to the previously known R _1 – M _H _i relation. Excluding strongly tidal-interacting galaxies, the ratio R _001 / R _1 (anti)correlates strongly and significantly with the H i -to-stellar mass ratio and specific star formation rate, but not with the stellar mass, M _H _i , dark matter mass, or star formation rate. The strongly tidal-interacting galaxies tend to show deviations from these trends and have the most flattened profiles. These results imply that, in the absence of major tidal interactions, physical processes must cooperate so that Σ _H _i distributes in a self-similar way in the outer region down to the 0.01 M _⊙ pc ^−2 level. Moreover, they may drive gas flows in such a way that H i -richer galaxies have H i disks that not only extend further but also transport H i inward more efficiently from R _001 to R _1 .https://doi.org/10.3847/1538-4357/ada95aInterstellar mediumDisk galaxiesGalaxy evolutionCircumgalactic medium |
| spellingShingle | Jing Wang Dong Yang Xuchen Lin Qifeng Huang Zhijie Qu Hsiao-wen Chen Hong Guo Luis C. Ho Peng Jiang Zezhong Liang Céline Péroux Lister Staveley-Smith Simon Weng FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies The Astrophysical Journal Interstellar medium Disk galaxies Galaxy evolution Circumgalactic medium |
| title | FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies |
| title_full | FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies |
| title_fullStr | FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies |
| title_full_unstemmed | FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies |
| title_short | FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies |
| title_sort | feasts radial distribution of h i surface densities down to 0 01 m⊙ pc 2 of 35 nearby galaxies |
| topic | Interstellar medium Disk galaxies Galaxy evolution Circumgalactic medium |
| url | https://doi.org/10.3847/1538-4357/ada95a |
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