WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy Pairs
Galaxy interactions can significantly affect the star formation in galaxies, but it remains a challenge to achieve a consensus on the star formation rate (SFR) enhancement in galaxy pairs. Here, we investigate the SFR enhancement of gas-rich galaxy pairs detected by the Widefield ASKAP L -band Legac...
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IOP Publishing
2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ad9579 |
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| author | Qifeng Huang Jing Wang Xuchen Lin Se-Heon Oh Xinkai Chen B. Catinella N. Deg H. Dénes B. -Q. For B. S. Koribalski K. Lee-Waddell J. Rhee A. X. Shen Li Shao K. Spekkens L. Staveley-Smith T. Westmeier O. I. Wong A. Bosma |
| author_facet | Qifeng Huang Jing Wang Xuchen Lin Se-Heon Oh Xinkai Chen B. Catinella N. Deg H. Dénes B. -Q. For B. S. Koribalski K. Lee-Waddell J. Rhee A. X. Shen Li Shao K. Spekkens L. Staveley-Smith T. Westmeier O. I. Wong A. Bosma |
| author_sort | Qifeng Huang |
| collection | DOAJ |
| description | Galaxy interactions can significantly affect the star formation in galaxies, but it remains a challenge to achieve a consensus on the star formation rate (SFR) enhancement in galaxy pairs. Here, we investigate the SFR enhancement of gas-rich galaxy pairs detected by the Widefield ASKAP L -band Legacy All-sky Blind surveY. We construct a sample of 278 paired galaxies spanning a stellar mass ( M _* ) range from 10 ^7.6 to 10 ^11.2 M _⊙ . We obtain individual masses of atomic hydrogen (H i ) for these paired galaxies using a novel deblending algorithm for H i data cubes. Quantifying the interaction stages and strengths with parameters motivated by first-principles analysis, we find that, at fixed stellar and H i mass, the alteration in the SFR of galaxy pairs starts when their dark matter halos are encountered. For galaxies with a stellar mass lower than 10 ^9 M _⊙ , their SFRs show tentative suppression of 1.4 σ after the halo encounter, and then become enhanced when their H i disks overlap, regardless of mass ratios. In contrast, the SFRs of galaxies with M _* > 10 ^9 M _⊙ increase monotonically toward smaller projected distances and radial velocity offsets. When a close companion is present, a pronounced SFR enhancement is found for the most H i -poor high-mass galaxies in our sample. Collecting the observational evidence, we provide a coherent picture of the evolution of galaxy pairs and discuss how the tidal effects and hydrodynamic processes shape the SFR enhancement. Our results provide a coherent picture of gas-rich galaxy interactions and impose constraints on the underlying physical processes. |
| format | Article |
| id | doaj-art-540165f80f624b8493a64ce6b8a98695 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-540165f80f624b8493a64ce6b8a986952025-02-10T09:52:13ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01980115710.3847/1538-4357/ad9579WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy PairsQifeng Huang0https://orcid.org/0000-0003-2863-9837Jing Wang1https://orcid.org/0000-0002-6593-8820Xuchen Lin2https://orcid.org/0000-0002-4250-2709Se-Heon Oh3https://orcid.org/0000-0002-8379-0604Xinkai Chen4https://orcid.org/0000-0002-5016-6901B. Catinella5https://orcid.org/0000-0002-7625-562XN. Deg6https://orcid.org/0000-0003-3523-7633H. Dénes7https://orcid.org/0000-0002-9214-8613B. -Q. For8https://orcid.org/0000-0002-0196-5248B. S. Koribalski9https://orcid.org/0000-0003-4351-993XK. Lee-Waddell10https://orcid.org/0000-0003-4844-8659J. Rhee11https://orcid.org/0000-0001-8496-4306A. X. Shen12Li Shao13https://orcid.org/0000-0003-2015-777XK. Spekkens14https://orcid.org/0000-0002-0956-7949L. Staveley-Smith15https://orcid.org/0000-0002-8057-0294T. Westmeier16https://orcid.org/0000-0002-5300-2486O. I. Wong17https://orcid.org/0000-0003-4264-3509A. Bosma18https://orcid.org/0000-0002-1128-6089Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; [email protected]; Department of Astronomy, School of Physics, Peking University , Beijing 100871, People's Republic of ChinaKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; [email protected] Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; [email protected]; Department of Astronomy, School of Physics, Peking University , Beijing 100871, People's Republic of ChinaDepartment of Physics and Astronomy, Sejong University , 209 Neungdong-ro, Gwangjin-gu, Seoul, Republic of KoreaKavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China ; [email protected] Centre for Radio Astronomy Research (ICRAR), The University of Western Australia , 35 Stirling Highway, Crawley WA 6009, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaDepartment of Physics, Engineering Physics and Astronomy, Queen’s University , Kingston, ON K7L 3N6, CanadaSchool of Physical Sciences and Nanotechnology, Yachay Tech University , Hacienda San José S/N, 100119, Urcuquí, EcuadorInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia , 35 Stirling Highway, Crawley WA 6009, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaAustralia Telescope National Facility , CSIRO, Space and Astronomy, P.O. Box 76, Epping, NSW 1710, Australia; School of Science, Western Sydney University , Locked Bag 1797, Penrith, NSW 2751, AustraliaInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia , 35 Stirling Highway, Crawley WA 6009, Australia; CSIRO Space and Astronomy , PO Box 1130, Bentley WA 6102, Australia; International Centre for Radio Astronomy Research (ICRAR), Curtin University , Bentley, WA 6102, AustraliaInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia , 35 Stirling Highway, Crawley WA 6009, AustraliaCSIRO Space and Astronomy , PO Box 1130, Bentley WA 6102, AustraliaNational Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaDepartment of Physics, Engineering Physics and Astronomy, Queen’s University , Kingston, ON K7L 3N6, CanadaInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia , 35 Stirling Highway, Crawley WA 6009, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , AustraliaInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia , 35 Stirling Highway, Crawley WA 6009, AustraliaInternational Centre for Radio Astronomy Research (ICRAR), The University of Western Australia , 35 Stirling Highway, Crawley WA 6009, Australia; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) , Australia; CSIRO Space and Astronomy , PO Box 1130, Bentley WA 6102, AustraliaAix Marseille Université , CNRS, CNES, LAM, F-13388 Marseille Cedex 13, FranceGalaxy interactions can significantly affect the star formation in galaxies, but it remains a challenge to achieve a consensus on the star formation rate (SFR) enhancement in galaxy pairs. Here, we investigate the SFR enhancement of gas-rich galaxy pairs detected by the Widefield ASKAP L -band Legacy All-sky Blind surveY. We construct a sample of 278 paired galaxies spanning a stellar mass ( M _* ) range from 10 ^7.6 to 10 ^11.2 M _⊙ . We obtain individual masses of atomic hydrogen (H i ) for these paired galaxies using a novel deblending algorithm for H i data cubes. Quantifying the interaction stages and strengths with parameters motivated by first-principles analysis, we find that, at fixed stellar and H i mass, the alteration in the SFR of galaxy pairs starts when their dark matter halos are encountered. For galaxies with a stellar mass lower than 10 ^9 M _⊙ , their SFRs show tentative suppression of 1.4 σ after the halo encounter, and then become enhanced when their H i disks overlap, regardless of mass ratios. In contrast, the SFRs of galaxies with M _* > 10 ^9 M _⊙ increase monotonically toward smaller projected distances and radial velocity offsets. When a close companion is present, a pronounced SFR enhancement is found for the most H i -poor high-mass galaxies in our sample. Collecting the observational evidence, we provide a coherent picture of the evolution of galaxy pairs and discuss how the tidal effects and hydrodynamic processes shape the SFR enhancement. Our results provide a coherent picture of gas-rich galaxy interactions and impose constraints on the underlying physical processes.https://doi.org/10.3847/1538-4357/ad9579GalaxiesGalaxy evolutionGalaxy interactionsInterstellar atomic gas |
| spellingShingle | Qifeng Huang Jing Wang Xuchen Lin Se-Heon Oh Xinkai Chen B. Catinella N. Deg H. Dénes B. -Q. For B. S. Koribalski K. Lee-Waddell J. Rhee A. X. Shen Li Shao K. Spekkens L. Staveley-Smith T. Westmeier O. I. Wong A. Bosma WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy Pairs The Astrophysical Journal Galaxies Galaxy evolution Galaxy interactions Interstellar atomic gas |
| title | WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy Pairs |
| title_full | WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy Pairs |
| title_fullStr | WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy Pairs |
| title_full_unstemmed | WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy Pairs |
| title_short | WALLABY Pilot Survey: Star Formation Enhancement and Suppression in Gas-rich Galaxy Pairs |
| title_sort | wallaby pilot survey star formation enhancement and suppression in gas rich galaxy pairs |
| topic | Galaxies Galaxy evolution Galaxy interactions Interstellar atomic gas |
| url | https://doi.org/10.3847/1538-4357/ad9579 |
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