The FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass Function
Using the Five-hundred-meter Aperture Spherical radio Telescope, we have performed an Ursa Major supergroup H i survey covering the entire UMa region centered at R.A. = 11 ^h 59 ^m 28 $\mathop{.}\limits^{{\rm{s}}}$ 3, decl. = 49°05′18″ with a radius of 7 $\mathop{.}\limits^{\unicode{x000B0}}$ 5. We...
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2025-01-01
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| author | Haiyang Yu Ming Zhu Chuan-Peng Zhang Peng Jiang Jin-Long Xu |
| author_facet | Haiyang Yu Ming Zhu Chuan-Peng Zhang Peng Jiang Jin-Long Xu |
| author_sort | Haiyang Yu |
| collection | DOAJ |
| description | Using the Five-hundred-meter Aperture Spherical radio Telescope, we have performed an Ursa Major supergroup H i survey covering the entire UMa region centered at R.A. = 11 ^h 59 ^m 28 $\mathop{.}\limits^{{\rm{s}}}$ 3, decl. = 49°05′18″ with a radius of 7 $\mathop{.}\limits^{\unicode{x000B0}}$ 5. We have obtained the most complete catalog of H i sources in the UMa supergroup, containing 178 H i sources with velocities in the range 625–1213.4 km s ^−1 and masses in the range 10 ^6.0 –10 ^10.1 M _⊙ assuming a distance of 17.4 Mpc. Among them, 55 H i sources were detected for the first time, of which 32 do not have known optical redshifts. For these 32 sources, we have searched the DESI Legacy Surveys and found optical counterparts for 25 of them (with optical images, but no redshifts), with the remaining seven sources being pure H i clouds without an optical counterpart. We detected H i distributions in some interacting systems and discussed four small groups in detail. We computed the neutral hydrogen mass function (H i MF) of the UMa supergroup using the 1/ ${V}_{\max }$ method and fitting it with the nonlinear least-squares (NLLS) and modified maximum likelihood (MML) methods. We obtained the following H i MF parameters: log _10 ( ϕ _* /Mpc ^−3 ) = −0.78 ± 0.15, α = −1.05 ± 0.07, and log _10 ( M _* / M _⊙ ) = 9.87 ± 0.19 for the NLLS method, and log _10 ( ϕ _* /Mpc ^−3 ) = −0.70 ± 0.11, α = −1.05 ± 0.05, and log _10 ( M _* / M _⊙ ) = 9.77 ± 0.13 for the MML method. This result is similar to that derived from the Very Large Array blind survey, but the slope is steeper because we detected more low-mass galaxies. The slope is flatter than that of the global H i MF, which agrees with the theoretical prediction that galaxies in high-density regions are stripped of gas due to interactions. |
| format | Article |
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| institution | DOAJ |
| issn | 0067-0049 |
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| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Supplement Series |
| spelling | doaj-art-87b09e8ba2924f2086fd73fca295b2a62025-08-20T03:07:58ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0127823710.3847/1538-4365/adcc1aThe FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass FunctionHaiyang Yu0https://orcid.org/0000-0001-9838-7159Ming Zhu1https://orcid.org/0000-0001-6083-956XChuan-Peng Zhang2https://orcid.org/0000-0002-4428-3183Peng Jiang3https://orcid.org/0009-0003-3527-8520Jin-Long Xu4https://orcid.org/0000-0002-7384-797XNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Beijing 100101, People’s Republic of China ; hyyu@nao.cas.cn, mz@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China; CAS Key Laboratory of FAST, National FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Beijing 100101, People’s Republic of China ; hyyu@nao.cas.cn, mz@nao.cas.cn; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China; CAS Key Laboratory of FAST, National FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; Guizhou Radio Astronomical Observatory, Guizhou University , Guiyang 550000, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Beijing 100101, People’s Republic of China ; hyyu@nao.cas.cn, mz@nao.cas.cn; CAS Key Laboratory of FAST, National FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; Guizhou Radio Astronomical Observatory, Guizhou University , Guiyang 550000, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Beijing 100101, People’s Republic of China ; hyyu@nao.cas.cn, mz@nao.cas.cn; CAS Key Laboratory of FAST, National FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; Guizhou Radio Astronomical Observatory, Guizhou University , Guiyang 550000, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Beijing 100101, People’s Republic of China ; hyyu@nao.cas.cn, mz@nao.cas.cn; CAS Key Laboratory of FAST, National FAST, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; Guizhou Radio Astronomical Observatory, Guizhou University , Guiyang 550000, People’s Republic of ChinaUsing the Five-hundred-meter Aperture Spherical radio Telescope, we have performed an Ursa Major supergroup H i survey covering the entire UMa region centered at R.A. = 11 ^h 59 ^m 28 $\mathop{.}\limits^{{\rm{s}}}$ 3, decl. = 49°05′18″ with a radius of 7 $\mathop{.}\limits^{\unicode{x000B0}}$ 5. We have obtained the most complete catalog of H i sources in the UMa supergroup, containing 178 H i sources with velocities in the range 625–1213.4 km s ^−1 and masses in the range 10 ^6.0 –10 ^10.1 M _⊙ assuming a distance of 17.4 Mpc. Among them, 55 H i sources were detected for the first time, of which 32 do not have known optical redshifts. For these 32 sources, we have searched the DESI Legacy Surveys and found optical counterparts for 25 of them (with optical images, but no redshifts), with the remaining seven sources being pure H i clouds without an optical counterpart. We detected H i distributions in some interacting systems and discussed four small groups in detail. We computed the neutral hydrogen mass function (H i MF) of the UMa supergroup using the 1/ ${V}_{\max }$ method and fitting it with the nonlinear least-squares (NLLS) and modified maximum likelihood (MML) methods. We obtained the following H i MF parameters: log _10 ( ϕ _* /Mpc ^−3 ) = −0.78 ± 0.15, α = −1.05 ± 0.07, and log _10 ( M _* / M _⊙ ) = 9.87 ± 0.19 for the NLLS method, and log _10 ( ϕ _* /Mpc ^−3 ) = −0.70 ± 0.11, α = −1.05 ± 0.05, and log _10 ( M _* / M _⊙ ) = 9.77 ± 0.13 for the MML method. This result is similar to that derived from the Very Large Array blind survey, but the slope is steeper because we detected more low-mass galaxies. The slope is flatter than that of the global H i MF, which agrees with the theoretical prediction that galaxies in high-density regions are stripped of gas due to interactions.https://doi.org/10.3847/1538-4365/adcc1aCatalogsSurveysGalaxy clustersH I line emissionExtragalactic radio sources |
| spellingShingle | Haiyang Yu Ming Zhu Chuan-Peng Zhang Peng Jiang Jin-Long Xu The FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass Function The Astrophysical Journal Supplement Series Catalogs Surveys Galaxy clusters H I line emission Extragalactic radio sources |
| title | The FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass Function |
| title_full | The FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass Function |
| title_fullStr | The FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass Function |
| title_full_unstemmed | The FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass Function |
| title_short | The FAST Ursa Major Supergroup H i Survey (FUMaS): Catalog and H i Mass Function |
| title_sort | fast ursa major supergroup h i survey fumas catalog and h i mass function |
| topic | Catalogs Surveys Galaxy clusters H I line emission Extragalactic radio sources |
| url | https://doi.org/10.3847/1538-4365/adcc1a |
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