FEASTS Combined with Interferometry. I. Overall Properties of Diffuse H i and Implications for Gas Accretion in Nearby Galaxies
We present a statistical study of the properties of diffuse H i in 10 nearby galaxies, comparing the H i detected by the single-dish telescope FAST (FEASTS program) and the interferometer Very Large Array (THINGS program), respectively. The THINGS observation missed H i with a median of 23% due to t...
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| Veröffentlicht in: | The Astrophysical journal 2024-06, Vol.968 (1), p.48 |
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| creator | Wang, Jing Lin, Xuchen Yang, Dong Staveley-Smith, Lister Walter, Fabian Wang, Q. Daniel Wang, Ran Battisti, A. J. Catinella, Barbara Chen, Hsiao-Wen Cortese, Luca Fisher, D. B. Ho, Luis C. Ji, Suoqing Jiang, Peng Kauffmann, Guinevere Kong, Xu Liu, Ziming Shao, Li Wang, Jie Wang, Lile Wang, Shun |
| description | We present a statistical study of the properties of diffuse H
i
in 10 nearby galaxies, comparing the H
i
detected by the single-dish telescope FAST (FEASTS program) and the interferometer Very Large Array (THINGS program), respectively. The THINGS observation missed H
i
with a median of 23% due to the short-spacing problem of interferometry and limited sensitivity. We extract the diffuse H
i
by subtracting the dense H
i
, which is obtained from the THINGS data with a uniform flux-density threshold, from the total H
i
detected by FAST. Among the sample, the median diffuse-H
i
fraction is 34%, and more diffuse H
i
is found in galaxies exhibiting more prominent tidal-interaction signatures. The diffuse H
i
we detected seems to be distributed in disk-like layers within a typical thickness of 1 kpc, different from the more halo-like diffuse H
i
detected around NGC 4631 in a previous study. Most of the diffuse H
i
is cospatial with the dense H
i
and has a typical column density of 10
17.7
–10
20.1
cm
−2
. The diffuse and dense H
i
exhibit a similar rotational motion, but the former lags by a median of 25% in at least the inner disks, and its velocity dispersions are typically twice as high. Based on a simplified estimation of circumgalactic medium properties and assuming pressure equilibrium, the volume density of diffuse H
i
appears to be constant within each individual galaxy, implying its role as a cooling interface. Comparing with existing models, these results are consistent with a possible link between tidal interactions, the formation of diffuse H
i
, and gas accretion. |
| doi_str_mv | 10.3847/1538-4357/ad3e61 |
| format | Article |
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i
in 10 nearby galaxies, comparing the H
i
detected by the single-dish telescope FAST (FEASTS program) and the interferometer Very Large Array (THINGS program), respectively. The THINGS observation missed H
i
with a median of 23% due to the short-spacing problem of interferometry and limited sensitivity. We extract the diffuse H
i
by subtracting the dense H
i
, which is obtained from the THINGS data with a uniform flux-density threshold, from the total H
i
detected by FAST. Among the sample, the median diffuse-H
i
fraction is 34%, and more diffuse H
i
is found in galaxies exhibiting more prominent tidal-interaction signatures. The diffuse H
i
we detected seems to be distributed in disk-like layers within a typical thickness of 1 kpc, different from the more halo-like diffuse H
i
detected around NGC 4631 in a previous study. Most of the diffuse H
i
is cospatial with the dense H
i
and has a typical column density of 10
17.7
–10
20.1
cm
−2
. The diffuse and dense H
i
exhibit a similar rotational motion, but the former lags by a median of 25% in at least the inner disks, and its velocity dispersions are typically twice as high. Based on a simplified estimation of circumgalactic medium properties and assuming pressure equilibrium, the volume density of diffuse H
i
appears to be constant within each individual galaxy, implying its role as a cooling interface. Comparing with existing models, these results are consistent with a possible link between tidal interactions, the formation of diffuse H
i
, and gas accretion.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ad3e61</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Accretion ; Astronomical models ; Circumgalactic medium ; Density ; Disks ; Galaxies ; Galaxy evolution ; Galaxy formation ; Interferometry ; Interstellar atomic gas</subject><ispartof>The Astrophysical journal, 2024-06, Vol.968 (1), p.48</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c398t-931421b4baea5ee86114d03a37fb0f9d3ea2d217daed8e2c95ff1211c5f8b7d3</cites><orcidid>0000-0002-9663-3384 ; 0000-0002-4250-2709 ; 0000-0002-8057-0294 ; 0000-0002-5387-7952 ; 0000-0002-9279-4041 ; 0000-0001-8813-4182 ; 0000-0003-4793-7880 ; 0000-0002-7660-2273 ; 0000-0003-4956-5742 ; 0000-0002-7625-562X ; 0000-0003-0645-5260 ; 0000-0001-6947-5846 ; 0000-0002-7422-9823 ; 0000-0001-9658-0588 ; 0000-0003-2015-777X ; 0000-0002-6593-8820 ; 0000-0003-4569-2285 ; 0000-0002-9937-2351 ; 0000-0002-6540-7042</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ad3e61/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,2096,27901,27902,38867,53842</link.rule.ids></links><search><creatorcontrib>Wang, Jing</creatorcontrib><creatorcontrib>Lin, Xuchen</creatorcontrib><creatorcontrib>Yang, Dong</creatorcontrib><creatorcontrib>Staveley-Smith, Lister</creatorcontrib><creatorcontrib>Walter, Fabian</creatorcontrib><creatorcontrib>Wang, Q. Daniel</creatorcontrib><creatorcontrib>Wang, Ran</creatorcontrib><creatorcontrib>Battisti, A. J.</creatorcontrib><creatorcontrib>Catinella, Barbara</creatorcontrib><creatorcontrib>Chen, Hsiao-Wen</creatorcontrib><creatorcontrib>Cortese, Luca</creatorcontrib><creatorcontrib>Fisher, D. B.</creatorcontrib><creatorcontrib>Ho, Luis C.</creatorcontrib><creatorcontrib>Ji, Suoqing</creatorcontrib><creatorcontrib>Jiang, Peng</creatorcontrib><creatorcontrib>Kauffmann, Guinevere</creatorcontrib><creatorcontrib>Kong, Xu</creatorcontrib><creatorcontrib>Liu, Ziming</creatorcontrib><creatorcontrib>Shao, Li</creatorcontrib><creatorcontrib>Wang, Jie</creatorcontrib><creatorcontrib>Wang, Lile</creatorcontrib><creatorcontrib>Wang, Shun</creatorcontrib><title>FEASTS Combined with Interferometry. I. Overall Properties of Diffuse H i and Implications for Gas Accretion in Nearby Galaxies</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We present a statistical study of the properties of diffuse H
i
in 10 nearby galaxies, comparing the H
i
detected by the single-dish telescope FAST (FEASTS program) and the interferometer Very Large Array (THINGS program), respectively. The THINGS observation missed H
i
with a median of 23% due to the short-spacing problem of interferometry and limited sensitivity. We extract the diffuse H
i
by subtracting the dense H
i
, which is obtained from the THINGS data with a uniform flux-density threshold, from the total H
i
detected by FAST. Among the sample, the median diffuse-H
i
fraction is 34%, and more diffuse H
i
is found in galaxies exhibiting more prominent tidal-interaction signatures. The diffuse H
i
we detected seems to be distributed in disk-like layers within a typical thickness of 1 kpc, different from the more halo-like diffuse H
i
detected around NGC 4631 in a previous study. Most of the diffuse H
i
is cospatial with the dense H
i
and has a typical column density of 10
17.7
–10
20.1
cm
−2
. The diffuse and dense H
i
exhibit a similar rotational motion, but the former lags by a median of 25% in at least the inner disks, and its velocity dispersions are typically twice as high. Based on a simplified estimation of circumgalactic medium properties and assuming pressure equilibrium, the volume density of diffuse H
i
appears to be constant within each individual galaxy, implying its role as a cooling interface. Comparing with existing models, these results are consistent with a possible link between tidal interactions, the formation of diffuse H
i
, and gas accretion.</description><subject>Accretion</subject><subject>Astronomical models</subject><subject>Circumgalactic medium</subject><subject>Density</subject><subject>Disks</subject><subject>Galaxies</subject><subject>Galaxy evolution</subject><subject>Galaxy formation</subject><subject>Interferometry</subject><subject>Interstellar atomic gas</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp9kc2P0zAQxSMEEmXhztESHGk3_ogTH6uyH5FWLNL2wM2a2GNwlcbBToGe-NdxCFouiJPlp_d-M6NXFK9pueGNqC9pxZu14FV9CZajpE-K1aP0tFiVZSnWktefnhcvUjrMX6bUqvh5fbV92D-QXTh2fkBLvvvpC2mHCaPDGI44xfOGtBty_w0j9D35GMOIcfKYSHDkvXfulJDcEk9gsKQ9jr03MPkwJOJCJDeQyNaYiLNE_EA-IMTunPUefmTIy-KZgz7hqz_vRbG_vtrvbtd39zftbnu3Nlw101pxKhjtRAcIFWIjKRW25MBr15VO5YuBWUZrC2gbZEZVzlFGqalc09WWXxTtgrUBDnqM_gjxrAN4_VsI8bOGfJTpUcsOBJVKqJwTkMdjpSpVV6YDxpQ0mfVmYY0xfD1hmvQhnOKQt9e8lFLUrJQsu8rFZWJIKaJ7nEpLPTem53r0XI9eGsuRd0vEh_Ev8z_2t_-ww3jQSjaaatHo0Tr-CwHIo8A</recordid><startdate>20240601</startdate><enddate>20240601</enddate><creator>Wang, Jing</creator><creator>Lin, Xuchen</creator><creator>Yang, Dong</creator><creator>Staveley-Smith, Lister</creator><creator>Walter, Fabian</creator><creator>Wang, Q. Daniel</creator><creator>Wang, Ran</creator><creator>Battisti, A. J.</creator><creator>Catinella, Barbara</creator><creator>Chen, Hsiao-Wen</creator><creator>Cortese, Luca</creator><creator>Fisher, D. B.</creator><creator>Ho, Luis C.</creator><creator>Ji, Suoqing</creator><creator>Jiang, Peng</creator><creator>Kauffmann, Guinevere</creator><creator>Kong, Xu</creator><creator>Liu, Ziming</creator><creator>Shao, Li</creator><creator>Wang, Jie</creator><creator>Wang, Lile</creator><creator>Wang, Shun</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0002-9663-3384</orcidid><orcidid>https://orcid.org/0000-0002-4250-2709</orcidid><orcidid>https://orcid.org/0000-0002-8057-0294</orcidid><orcidid>https://orcid.org/0000-0002-5387-7952</orcidid><orcidid>https://orcid.org/0000-0002-9279-4041</orcidid><orcidid>https://orcid.org/0000-0001-8813-4182</orcidid><orcidid>https://orcid.org/0000-0003-4793-7880</orcidid><orcidid>https://orcid.org/0000-0002-7660-2273</orcidid><orcidid>https://orcid.org/0000-0003-4956-5742</orcidid><orcidid>https://orcid.org/0000-0002-7625-562X</orcidid><orcidid>https://orcid.org/0000-0003-0645-5260</orcidid><orcidid>https://orcid.org/0000-0001-6947-5846</orcidid><orcidid>https://orcid.org/0000-0002-7422-9823</orcidid><orcidid>https://orcid.org/0000-0001-9658-0588</orcidid><orcidid>https://orcid.org/0000-0003-2015-777X</orcidid><orcidid>https://orcid.org/0000-0002-6593-8820</orcidid><orcidid>https://orcid.org/0000-0003-4569-2285</orcidid><orcidid>https://orcid.org/0000-0002-9937-2351</orcidid><orcidid>https://orcid.org/0000-0002-6540-7042</orcidid></search><sort><creationdate>20240601</creationdate><title>FEASTS Combined with Interferometry. I. Overall Properties of Diffuse H i and Implications for Gas Accretion in Nearby Galaxies</title><author>Wang, Jing ; Lin, Xuchen ; Yang, Dong ; Staveley-Smith, Lister ; Walter, Fabian ; Wang, Q. Daniel ; Wang, Ran ; Battisti, A. J. ; Catinella, Barbara ; Chen, Hsiao-Wen ; Cortese, Luca ; Fisher, D. B. ; Ho, Luis C. ; Ji, Suoqing ; Jiang, Peng ; Kauffmann, Guinevere ; Kong, Xu ; Liu, Ziming ; Shao, Li ; Wang, Jie ; Wang, Lile ; Wang, Shun</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c398t-931421b4baea5ee86114d03a37fb0f9d3ea2d217daed8e2c95ff1211c5f8b7d3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Accretion</topic><topic>Astronomical models</topic><topic>Circumgalactic medium</topic><topic>Density</topic><topic>Disks</topic><topic>Galaxies</topic><topic>Galaxy evolution</topic><topic>Galaxy formation</topic><topic>Interferometry</topic><topic>Interstellar atomic gas</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Wang, Jing</creatorcontrib><creatorcontrib>Lin, Xuchen</creatorcontrib><creatorcontrib>Yang, Dong</creatorcontrib><creatorcontrib>Staveley-Smith, Lister</creatorcontrib><creatorcontrib>Walter, Fabian</creatorcontrib><creatorcontrib>Wang, Q. 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Daniel</au><au>Wang, Ran</au><au>Battisti, A. J.</au><au>Catinella, Barbara</au><au>Chen, Hsiao-Wen</au><au>Cortese, Luca</au><au>Fisher, D. B.</au><au>Ho, Luis C.</au><au>Ji, Suoqing</au><au>Jiang, Peng</au><au>Kauffmann, Guinevere</au><au>Kong, Xu</au><au>Liu, Ziming</au><au>Shao, Li</au><au>Wang, Jie</au><au>Wang, Lile</au><au>Wang, Shun</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>FEASTS Combined with Interferometry. I. Overall Properties of Diffuse H i and Implications for Gas Accretion in Nearby Galaxies</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2024-06-01</date><risdate>2024</risdate><volume>968</volume><issue>1</issue><spage>48</spage><pages>48-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We present a statistical study of the properties of diffuse H
i
in 10 nearby galaxies, comparing the H
i
detected by the single-dish telescope FAST (FEASTS program) and the interferometer Very Large Array (THINGS program), respectively. The THINGS observation missed H
i
with a median of 23% due to the short-spacing problem of interferometry and limited sensitivity. We extract the diffuse H
i
by subtracting the dense H
i
, which is obtained from the THINGS data with a uniform flux-density threshold, from the total H
i
detected by FAST. Among the sample, the median diffuse-H
i
fraction is 34%, and more diffuse H
i
is found in galaxies exhibiting more prominent tidal-interaction signatures. The diffuse H
i
we detected seems to be distributed in disk-like layers within a typical thickness of 1 kpc, different from the more halo-like diffuse H
i
detected around NGC 4631 in a previous study. Most of the diffuse H
i
is cospatial with the dense H
i
and has a typical column density of 10
17.7
–10
20.1
cm
−2
. The diffuse and dense H
i
exhibit a similar rotational motion, but the former lags by a median of 25% in at least the inner disks, and its velocity dispersions are typically twice as high. Based on a simplified estimation of circumgalactic medium properties and assuming pressure equilibrium, the volume density of diffuse H
i
appears to be constant within each individual galaxy, implying its role as a cooling interface. Comparing with existing models, these results are consistent with a possible link between tidal interactions, the formation of diffuse H
i
, and gas accretion.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ad3e61</doi><tpages>39</tpages><orcidid>https://orcid.org/0000-0002-9663-3384</orcidid><orcidid>https://orcid.org/0000-0002-4250-2709</orcidid><orcidid>https://orcid.org/0000-0002-8057-0294</orcidid><orcidid>https://orcid.org/0000-0002-5387-7952</orcidid><orcidid>https://orcid.org/0000-0002-9279-4041</orcidid><orcidid>https://orcid.org/0000-0001-8813-4182</orcidid><orcidid>https://orcid.org/0000-0003-4793-7880</orcidid><orcidid>https://orcid.org/0000-0002-7660-2273</orcidid><orcidid>https://orcid.org/0000-0003-4956-5742</orcidid><orcidid>https://orcid.org/0000-0002-7625-562X</orcidid><orcidid>https://orcid.org/0000-0003-0645-5260</orcidid><orcidid>https://orcid.org/0000-0001-6947-5846</orcidid><orcidid>https://orcid.org/0000-0002-7422-9823</orcidid><orcidid>https://orcid.org/0000-0001-9658-0588</orcidid><orcidid>https://orcid.org/0000-0003-2015-777X</orcidid><orcidid>https://orcid.org/0000-0002-6593-8820</orcidid><orcidid>https://orcid.org/0000-0003-4569-2285</orcidid><orcidid>https://orcid.org/0000-0002-9937-2351</orcidid><orcidid>https://orcid.org/0000-0002-6540-7042</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
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| ispartof | The Astrophysical journal, 2024-06, Vol.968 (1), p.48 |
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| language | eng |
| recordid | cdi_proquest_journals_3066472062 |
| source | IOP Publishing Free Content; DOAJ Directory of Open Access Journals; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Accretion Astronomical models Circumgalactic medium Density Disks Galaxies Galaxy evolution Galaxy formation Interferometry Interstellar atomic gas |
| title | FEASTS Combined with Interferometry. I. Overall Properties of Diffuse H i and Implications for Gas Accretion in Nearby Galaxies |
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