OH and CO as tracers of molecular gas in MBM 53
ABSTRACT We observed the OH 18 cm lines in the northern portion of the high-latitude diffuse molecular cloud, MBM 53. The 1667 MHz line was detected in 11 of 44 lines of sight at rms levels of 7–10 mK. This region was previously observed in the CO(1–0) line at high sensitivity and spectral resolutio...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2019-07, Vol.486 (3), p.4414-4422 |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Donate, Emmanuel White, Josh Magnani, Loris |
| description | ABSTRACT
We observed the OH 18 cm lines in the northern portion of the high-latitude diffuse molecular cloud, MBM 53. The 1667 MHz line was detected in 11 of 44 lines of sight at rms levels of 7–10 mK. This region was previously observed in the CO(1–0) line at high sensitivity and spectral resolution. Donate & Magnani (2017) detected CO in 19 of the 44 lines of sight with an AV threshold of 0.25 mag, while the OH detection threshold in AV is 0.35 mag. We see more of the extent of the cloud with the CO(1–0) line when both transitions are observed with similar integration times. However, using standard assumptions for converting the OH and CO observations to the molecular mass in the region lead to three times greater value in the OH-derived mass. This somewhat puzzling result likely indicates that the OH/CO abundance varies significantly in the outer, low-extinction regions of MBM 53 and implies that a larger CO–H2 conversion factor may apply there. |
| doi_str_mv | 10.1093/mnras/stz1125 |
| format | Article |
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We observed the OH 18 cm lines in the northern portion of the high-latitude diffuse molecular cloud, MBM 53. The 1667 MHz line was detected in 11 of 44 lines of sight at rms levels of 7–10 mK. This region was previously observed in the CO(1–0) line at high sensitivity and spectral resolution. Donate & Magnani (2017) detected CO in 19 of the 44 lines of sight with an AV threshold of 0.25 mag, while the OH detection threshold in AV is 0.35 mag. We see more of the extent of the cloud with the CO(1–0) line when both transitions are observed with similar integration times. However, using standard assumptions for converting the OH and CO observations to the molecular mass in the region lead to three times greater value in the OH-derived mass. This somewhat puzzling result likely indicates that the OH/CO abundance varies significantly in the outer, low-extinction regions of MBM 53 and implies that a larger CO–H2 conversion factor may apply there.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stz1125</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2019-07, Vol.486 (3), p.4414-4422</ispartof><rights>2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2019</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c336t-5094df5b70dc09ccfddd525ac4fa2e3eecc2dd5709cf0c25eb8392bfc9d05cec3</citedby><cites>FETCH-LOGICAL-c336t-5094df5b70dc09ccfddd525ac4fa2e3eecc2dd5709cf0c25eb8392bfc9d05cec3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stz1125$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Donate, Emmanuel</creatorcontrib><creatorcontrib>White, Josh</creatorcontrib><creatorcontrib>Magnani, Loris</creatorcontrib><title>OH and CO as tracers of molecular gas in MBM 53</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
We observed the OH 18 cm lines in the northern portion of the high-latitude diffuse molecular cloud, MBM 53. The 1667 MHz line was detected in 11 of 44 lines of sight at rms levels of 7–10 mK. This region was previously observed in the CO(1–0) line at high sensitivity and spectral resolution. Donate & Magnani (2017) detected CO in 19 of the 44 lines of sight with an AV threshold of 0.25 mag, while the OH detection threshold in AV is 0.35 mag. We see more of the extent of the cloud with the CO(1–0) line when both transitions are observed with similar integration times. However, using standard assumptions for converting the OH and CO observations to the molecular mass in the region lead to three times greater value in the OH-derived mass. This somewhat puzzling result likely indicates that the OH/CO abundance varies significantly in the outer, low-extinction regions of MBM 53 and implies that a larger CO–H2 conversion factor may apply there.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNqFjz1PwzAURS0EEqFlZPfIYvJsx0k9QgQUqVUWOlvOs42K8lHZ6QC_nkC7M13p3qMrHULuODxw0DLvh2hTnqZvzoW6IBmXpWJCl-UlyQCkYquK82tyk9InABRSlBnJmzW1g6N1Q22iU7ToY6JjoP3YeTx2NtKPedgPdPu0pUouyVWwXfK351yQ3cvze71mm-b1rX7cMJSynJgCXbig2gocgkYMzjkllMUiWOGl94hibqp5C4BC-XYltWgDagcKPcoFYadfjGNK0QdziPvexi_Dwfzamj9bc7ad-fsTPx4P_6A_dCJXCw</recordid><startdate>20190701</startdate><enddate>20190701</enddate><creator>Donate, Emmanuel</creator><creator>White, Josh</creator><creator>Magnani, Loris</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope></search><sort><creationdate>20190701</creationdate><title>OH and CO as tracers of molecular gas in MBM 53</title><author>Donate, Emmanuel ; White, Josh ; Magnani, Loris</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c336t-5094df5b70dc09ccfddd525ac4fa2e3eecc2dd5709cf0c25eb8392bfc9d05cec3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Donate, Emmanuel</creatorcontrib><creatorcontrib>White, Josh</creatorcontrib><creatorcontrib>Magnani, Loris</creatorcontrib><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Donate, Emmanuel</au><au>White, Josh</au><au>Magnani, Loris</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>OH and CO as tracers of molecular gas in MBM 53</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2019-07-01</date><risdate>2019</risdate><volume>486</volume><issue>3</issue><spage>4414</spage><epage>4422</epage><pages>4414-4422</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
We observed the OH 18 cm lines in the northern portion of the high-latitude diffuse molecular cloud, MBM 53. The 1667 MHz line was detected in 11 of 44 lines of sight at rms levels of 7–10 mK. This region was previously observed in the CO(1–0) line at high sensitivity and spectral resolution. Donate & Magnani (2017) detected CO in 19 of the 44 lines of sight with an AV threshold of 0.25 mag, while the OH detection threshold in AV is 0.35 mag. We see more of the extent of the cloud with the CO(1–0) line when both transitions are observed with similar integration times. However, using standard assumptions for converting the OH and CO observations to the molecular mass in the region lead to three times greater value in the OH-derived mass. This somewhat puzzling result likely indicates that the OH/CO abundance varies significantly in the outer, low-extinction regions of MBM 53 and implies that a larger CO–H2 conversion factor may apply there.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stz1125</doi><tpages>9</tpages></addata></record> |
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| title | OH and CO as tracers of molecular gas in MBM 53 |
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