Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]
We present the results of an unbiased 12 CO/ 13 CO/C 18 O ( J = 1–0) survey in a portion of the third Galactic quadrant (TGQ): 219.°75 ≤ l ≤ 229.°75 and −5.°25 ≤ b ≤ 5.°25. The high-resolution and high-sensitivity data sets help to unravel the distributions and physical properties of the molecular c...
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| Veröffentlicht in: | The Astrophysical journal. Supplement series 2023-09, Vol.268 (1), p.1 |
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| creator | Dong, Yiwei Sun, Yan Xu, Ye Lin, Zehao Bian, Shuaibo Hao, Chaojie Liu, Dejian Li, Yingjie Yang, Ji Su, Yang Zhou, Xin Zhang, Shaobo Yan, Qing-Zeng Chen, Zhiwei |
| description | We present the results of an unbiased
12
CO/
13
CO/C
18
O (
J
= 1–0) survey in a portion of the third Galactic quadrant (TGQ): 219.°75 ≤
l
≤ 229.°75 and −5.°25 ≤
b
≤ 5.°25. The high-resolution and high-sensitivity data sets help to unravel the distributions and physical properties of the molecular clouds (MCs) in the mapped area. In the LSR velocity range from ∼−1 to ∼85 km s
−1
, the molecular material successfully traces the Local, Perseus, and Outer arms. In the TGQ, the Outer arm appears to be more prominent than that in the second Galactic quadrant (SGQ), but the Perseus arm is not as conspicuous as that in the SGQ. A total of 1,502
12
CO, 570
13
CO, and 53 C
18
O molecular structures are identified, spanning over ∼2 and ∼6 orders of magnitude in size and mass, respectively. Tight mass–radius correlations and virial parameter–mass anticorrelations are observable. Yet, it seems that no clear correlations between velocity dispersion and effective radius can be found over the full dynamic range. The vertical distribution of the MCs renders evident pictures of the Galactic warp and flare. |
| doi_str_mv | 10.3847/1538-4365/acde81 |
| format | Article |
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12
CO/
13
CO/C
18
O (
J
= 1–0) survey in a portion of the third Galactic quadrant (TGQ): 219.°75 ≤
l
≤ 229.°75 and −5.°25 ≤
b
≤ 5.°25. The high-resolution and high-sensitivity data sets help to unravel the distributions and physical properties of the molecular clouds (MCs) in the mapped area. In the LSR velocity range from ∼−1 to ∼85 km s
−1
, the molecular material successfully traces the Local, Perseus, and Outer arms. In the TGQ, the Outer arm appears to be more prominent than that in the second Galactic quadrant (SGQ), but the Perseus arm is not as conspicuous as that in the SGQ. A total of 1,502
12
CO, 570
13
CO, and 53 C
18
O molecular structures are identified, spanning over ∼2 and ∼6 orders of magnitude in size and mass, respectively. Tight mass–radius correlations and virial parameter–mass anticorrelations are observable. Yet, it seems that no clear correlations between velocity dispersion and effective radius can be found over the full dynamic range. The vertical distribution of the MCs renders evident pictures of the Galactic warp and flare.</description><identifier>ISSN: 0067-0049</identifier><identifier>EISSN: 1538-4365</identifier><identifier>DOI: 10.3847/1538-4365/acde81</identifier><language>eng</language><publisher>Saskatoon: The American Astronomical Society</publisher><subject>CO line emission ; Correlation ; Galactic structure ; Interstellar molecules ; Milky Way ; Molecular clouds ; Molecular structure ; Physical properties ; Quadrants ; Spiral arms ; Velocity ; Vertical distribution</subject><ispartof>The Astrophysical journal. Supplement series, 2023-09, Vol.268 (1), p.1</ispartof><rights>2023. The Author(s). Published by the American Astronomical Society.</rights><rights>2023. 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-c369t-a1274b67102ce93cc0c07a9a9688c0dc4a128561e779740d24d6720da311304d3</cites><orcidid>0000-0002-7508-9615 ; 0000-0002-3904-1622 ; 0000-0003-4586-7751 ; 0000-0002-0197-470X ; 0000-0003-2549-7247 ; 0000-0001-7768-7320 ; 0000-0003-0849-0692 ; 0000-0003-2418-3350 ; 0000-0001-5602-3306 ; 0000-0001-7526-0120</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4365/acde81/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,2096,27901,27902,38845,38867,53815,53842</link.rule.ids></links><search><creatorcontrib>Dong, Yiwei</creatorcontrib><creatorcontrib>Sun, Yan</creatorcontrib><creatorcontrib>Xu, Ye</creatorcontrib><creatorcontrib>Lin, Zehao</creatorcontrib><creatorcontrib>Bian, Shuaibo</creatorcontrib><creatorcontrib>Hao, Chaojie</creatorcontrib><creatorcontrib>Liu, Dejian</creatorcontrib><creatorcontrib>Li, Yingjie</creatorcontrib><creatorcontrib>Yang, Ji</creatorcontrib><creatorcontrib>Su, Yang</creatorcontrib><creatorcontrib>Zhou, Xin</creatorcontrib><creatorcontrib>Zhang, Shaobo</creatorcontrib><creatorcontrib>Yan, Qing-Zeng</creatorcontrib><creatorcontrib>Chen, Zhiwei</creatorcontrib><title>Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]</title><title>The Astrophysical journal. Supplement series</title><addtitle>APJS</addtitle><addtitle>Astrophys. J. Suppl</addtitle><description>We present the results of an unbiased
12
CO/
13
CO/C
18
O (
J
= 1–0) survey in a portion of the third Galactic quadrant (TGQ): 219.°75 ≤
l
≤ 229.°75 and −5.°25 ≤
b
≤ 5.°25. The high-resolution and high-sensitivity data sets help to unravel the distributions and physical properties of the molecular clouds (MCs) in the mapped area. In the LSR velocity range from ∼−1 to ∼85 km s
−1
, the molecular material successfully traces the Local, Perseus, and Outer arms. In the TGQ, the Outer arm appears to be more prominent than that in the second Galactic quadrant (SGQ), but the Perseus arm is not as conspicuous as that in the SGQ. A total of 1,502
12
CO, 570
13
CO, and 53 C
18
O molecular structures are identified, spanning over ∼2 and ∼6 orders of magnitude in size and mass, respectively. Tight mass–radius correlations and virial parameter–mass anticorrelations are observable. Yet, it seems that no clear correlations between velocity dispersion and effective radius can be found over the full dynamic range. The vertical distribution of the MCs renders evident pictures of the Galactic warp and flare.</description><subject>CO line emission</subject><subject>Correlation</subject><subject>Galactic structure</subject><subject>Interstellar molecules</subject><subject>Milky Way</subject><subject>Molecular clouds</subject><subject>Molecular structure</subject><subject>Physical properties</subject><subject>Quadrants</subject><subject>Spiral arms</subject><subject>Velocity</subject><subject>Vertical distribution</subject><issn>0067-0049</issn><issn>1538-4365</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp1UctuFDEQHCGQWAJ3jpa4ZpL2Y6Y9SBzQAiFSEEEKJxRZPbaX9WoYL_bMIX_AiQNfwjfwKXwJ3gwKJ07dqq6u6lZV1VMOJ1IrPOWN1LWSbXNK1nnN71WrO-h-tQJosQZQ3cPqUc47AMBGdqvq-6uQpxT6eQpxzIxGxy63NzlYGthlinufpuAzixv2Lg7ezgMlth7i7DILI5u2nl1tQ3LsjAayU7Dsw0wu0Tg9ZwN7wT4J3p38-onNMRNi6a5vTfrD8Pe3H03BRJku9fpx9WBDQ_ZP_taj6uOb11frt_XF-7Pz9cuL2sq2m2riAlXfIgdhfSetBQtIHXWt1hacVYWgm5Z7xA4VOKFciwIcSc4lKCePqvNF10XamX0KXyjdmEjB3AIxfTZUPreDN8SVbrRXPWKvNqi05MiFI6UaR4hQtJ4tWvsUv84-T2YX5zSW8005QiBvtcTCgoVlU8w5-c2dKwdzSNAc4jKHuMySYFk5XlZC3P_T_C_9DwyFmqc</recordid><startdate>20230901</startdate><enddate>20230901</enddate><creator>Dong, Yiwei</creator><creator>Sun, Yan</creator><creator>Xu, Ye</creator><creator>Lin, Zehao</creator><creator>Bian, Shuaibo</creator><creator>Hao, Chaojie</creator><creator>Liu, Dejian</creator><creator>Li, Yingjie</creator><creator>Yang, Ji</creator><creator>Su, Yang</creator><creator>Zhou, Xin</creator><creator>Zhang, Shaobo</creator><creator>Yan, Qing-Zeng</creator><creator>Chen, Zhiwei</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/0000-0002-7508-9615</orcidid><orcidid>https://orcid.org/0000-0002-3904-1622</orcidid><orcidid>https://orcid.org/0000-0003-4586-7751</orcidid><orcidid>https://orcid.org/0000-0002-0197-470X</orcidid><orcidid>https://orcid.org/0000-0003-2549-7247</orcidid><orcidid>https://orcid.org/0000-0001-7768-7320</orcidid><orcidid>https://orcid.org/0000-0003-0849-0692</orcidid><orcidid>https://orcid.org/0000-0003-2418-3350</orcidid><orcidid>https://orcid.org/0000-0001-5602-3306</orcidid><orcidid>https://orcid.org/0000-0001-7526-0120</orcidid></search><sort><creationdate>20230901</creationdate><title>Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]</title><author>Dong, Yiwei ; Sun, Yan ; Xu, Ye ; Lin, Zehao ; Bian, Shuaibo ; Hao, Chaojie ; Liu, Dejian ; Li, Yingjie ; Yang, Ji ; Su, Yang ; Zhou, Xin ; Zhang, Shaobo ; Yan, Qing-Zeng ; Chen, Zhiwei</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c369t-a1274b67102ce93cc0c07a9a9688c0dc4a128561e779740d24d6720da311304d3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>CO line emission</topic><topic>Correlation</topic><topic>Galactic structure</topic><topic>Interstellar molecules</topic><topic>Milky Way</topic><topic>Molecular clouds</topic><topic>Molecular structure</topic><topic>Physical properties</topic><topic>Quadrants</topic><topic>Spiral arms</topic><topic>Velocity</topic><topic>Vertical distribution</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Dong, Yiwei</creatorcontrib><creatorcontrib>Sun, Yan</creatorcontrib><creatorcontrib>Xu, Ye</creatorcontrib><creatorcontrib>Lin, Zehao</creatorcontrib><creatorcontrib>Bian, Shuaibo</creatorcontrib><creatorcontrib>Hao, Chaojie</creatorcontrib><creatorcontrib>Liu, Dejian</creatorcontrib><creatorcontrib>Li, Yingjie</creatorcontrib><creatorcontrib>Yang, Ji</creatorcontrib><creatorcontrib>Su, Yang</creatorcontrib><creatorcontrib>Zhou, Xin</creatorcontrib><creatorcontrib>Zhang, Shaobo</creatorcontrib><creatorcontrib>Yan, Qing-Zeng</creatorcontrib><creatorcontrib>Chen, Zhiwei</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>DOAJ Directory of Open Access Journals</collection><jtitle>The Astrophysical journal. Supplement series</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Dong, Yiwei</au><au>Sun, Yan</au><au>Xu, Ye</au><au>Lin, Zehao</au><au>Bian, Shuaibo</au><au>Hao, Chaojie</au><au>Liu, Dejian</au><au>Li, Yingjie</au><au>Yang, Ji</au><au>Su, Yang</au><au>Zhou, Xin</au><au>Zhang, Shaobo</au><au>Yan, Qing-Zeng</au><au>Chen, Zhiwei</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25]</atitle><jtitle>The Astrophysical journal. Supplement series</jtitle><stitle>APJS</stitle><addtitle>Astrophys. J. Suppl</addtitle><date>2023-09-01</date><risdate>2023</risdate><volume>268</volume><issue>1</issue><spage>1</spage><pages>1-</pages><issn>0067-0049</issn><eissn>1538-4365</eissn><abstract>We present the results of an unbiased
12
CO/
13
CO/C
18
O (
J
= 1–0) survey in a portion of the third Galactic quadrant (TGQ): 219.°75 ≤
l
≤ 229.°75 and −5.°25 ≤
b
≤ 5.°25. The high-resolution and high-sensitivity data sets help to unravel the distributions and physical properties of the molecular clouds (MCs) in the mapped area. In the LSR velocity range from ∼−1 to ∼85 km s
−1
, the molecular material successfully traces the Local, Perseus, and Outer arms. In the TGQ, the Outer arm appears to be more prominent than that in the second Galactic quadrant (SGQ), but the Perseus arm is not as conspicuous as that in the SGQ. A total of 1,502
12
CO, 570
13
CO, and 53 C
18
O molecular structures are identified, spanning over ∼2 and ∼6 orders of magnitude in size and mass, respectively. Tight mass–radius correlations and virial parameter–mass anticorrelations are observable. Yet, it seems that no clear correlations between velocity dispersion and effective radius can be found over the full dynamic range. The vertical distribution of the MCs renders evident pictures of the Galactic warp and flare.</abstract><cop>Saskatoon</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4365/acde81</doi><tpages>18</tpages><orcidid>https://orcid.org/0000-0002-7508-9615</orcidid><orcidid>https://orcid.org/0000-0002-3904-1622</orcidid><orcidid>https://orcid.org/0000-0003-4586-7751</orcidid><orcidid>https://orcid.org/0000-0002-0197-470X</orcidid><orcidid>https://orcid.org/0000-0003-2549-7247</orcidid><orcidid>https://orcid.org/0000-0001-7768-7320</orcidid><orcidid>https://orcid.org/0000-0003-0849-0692</orcidid><orcidid>https://orcid.org/0000-0003-2418-3350</orcidid><orcidid>https://orcid.org/0000-0001-5602-3306</orcidid><orcidid>https://orcid.org/0000-0001-7526-0120</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | The Astrophysical journal. Supplement series, 2023-09, Vol.268 (1), p.1 |
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| source | IOP Publishing Free Content; DOAJ Directory of Open Access Journals; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; IOPscience extra; Alma/SFX Local Collection |
| subjects | CO line emission Correlation Galactic structure Interstellar molecules Milky Way Molecular clouds Molecular structure Physical properties Quadrants Spiral arms Velocity Vertical distribution |
| title | Distributions and Physical Properties of Molecular Clouds in the Third Galactic Quadrant: l = [219.°75, 229.°75] and b = [−5.°25, 5.°25] |
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