An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster
We present recent Chandra X-ray observations of the RX J0821.0+0752 galaxy cluster, in addition to ALMA observations of the CO(1-0) and CO(3-2) line emission tracing the molecular gas in its central galaxy. All of the CO line emission, originating from a molecular gas reservoir, is located several k...
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| Veröffentlicht in: | Astrophysical journal. Letters 2019-01, Vol.870 (2), p.57 |
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| creator | Vantyghem, A. N. McNamara, B. R. Russell, H. R. Edge, A. C. Nulsen, P. E. J. Combes, F. Fabian, A. C. McDonald, M. Salomé, P. |
| description | We present recent Chandra X-ray observations of the RX J0821.0+0752 galaxy cluster, in addition to ALMA observations of the CO(1-0) and CO(3-2) line emission tracing the molecular gas in its central galaxy. All of the CO line emission, originating from a molecular gas reservoir, is located several kiloparsecs away from the nucleus of the central galaxy. The cold gas is concentrated into two main clumps surrounded by a diffuse envelope. They form a wide filament coincident with a plume of bright X-ray emission emanating from the cluster core. This plume encompasses a putative X-ray cavity that is only large enough to have uplifted a small percent of the molecular gas. Unlike other brightest cluster galaxies, stimulated cooling, where X-ray cavities lift low-entropy cluster gas until it becomes thermally unstable, cannot have produced the observed gas reservoir. Instead, the molecular gas has likely formed as a result of sloshing motions in the intracluster medium induced by a nearby galaxy. Sloshing can emulate uplift by dislodging gas from the galactic center. This gas has the shortest cooling time, so it will condense if disrupted for long enough. |
| doi_str_mv | 10.3847/1538-4357/aaf1b4 |
| format | Article |
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N. ; McNamara, B. R. ; Russell, H. R. ; Edge, A. C. ; Nulsen, P. E. J. ; Combes, F. ; Fabian, A. C. ; McDonald, M. ; Salomé, P.</creator><creatorcontrib>Vantyghem, A. N. ; McNamara, B. R. ; Russell, H. R. ; Edge, A. C. ; Nulsen, P. E. J. ; Combes, F. ; Fabian, A. C. ; McDonald, M. ; Salomé, P.</creatorcontrib><description>We present recent Chandra X-ray observations of the RX J0821.0+0752 galaxy cluster, in addition to ALMA observations of the CO(1-0) and CO(3-2) line emission tracing the molecular gas in its central galaxy. All of the CO line emission, originating from a molecular gas reservoir, is located several kiloparsecs away from the nucleus of the central galaxy. The cold gas is concentrated into two main clumps surrounded by a diffuse envelope. They form a wide filament coincident with a plume of bright X-ray emission emanating from the cluster core. This plume encompasses a putative X-ray cavity that is only large enough to have uplifted a small percent of the molecular gas. Unlike other brightest cluster galaxies, stimulated cooling, where X-ray cavities lift low-entropy cluster gas until it becomes thermally unstable, cannot have produced the observed gas reservoir. Instead, the molecular gas has likely formed as a result of sloshing motions in the intracluster medium induced by a nearby galaxy. Sloshing can emulate uplift by dislodging gas from the galactic center. 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All rights reserved.</rights><rights>Copyright IOP Publishing Jan 10, 2019</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c413t-a95f0607dbd4cc44a7563ed1efebf88e7cf908cbba045eb554c984b4aae3f9dc3</citedby><cites>FETCH-LOGICAL-c413t-a95f0607dbd4cc44a7563ed1efebf88e7cf908cbba045eb554c984b4aae3f9dc3</cites><orcidid>0000-0002-3398-6916 ; 0000-0003-0297-4493 ; 0000-0002-2622-2627 ; 0000-0003-2658-7893 ; 0000-0002-9378-4072 ; 0000-0003-4227-4838 ; 0000-0001-5226-8349</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/aaf1b4/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,777,781,882,27905,27906,38871,53848</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aaf1b4$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://hal.sorbonne-universite.fr/hal-01998426$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Vantyghem, A. N.</creatorcontrib><creatorcontrib>McNamara, B. R.</creatorcontrib><creatorcontrib>Russell, H. R.</creatorcontrib><creatorcontrib>Edge, A. C.</creatorcontrib><creatorcontrib>Nulsen, P. E. J.</creatorcontrib><creatorcontrib>Combes, F.</creatorcontrib><creatorcontrib>Fabian, A. C.</creatorcontrib><creatorcontrib>McDonald, M.</creatorcontrib><creatorcontrib>Salomé, P.</creatorcontrib><title>An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster</title><title>Astrophysical journal. Letters</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We present recent Chandra X-ray observations of the RX J0821.0+0752 galaxy cluster, in addition to ALMA observations of the CO(1-0) and CO(3-2) line emission tracing the molecular gas in its central galaxy. All of the CO line emission, originating from a molecular gas reservoir, is located several kiloparsecs away from the nucleus of the central galaxy. The cold gas is concentrated into two main clumps surrounded by a diffuse envelope. They form a wide filament coincident with a plume of bright X-ray emission emanating from the cluster core. This plume encompasses a putative X-ray cavity that is only large enough to have uplifted a small percent of the molecular gas. Unlike other brightest cluster galaxies, stimulated cooling, where X-ray cavities lift low-entropy cluster gas until it becomes thermally unstable, cannot have produced the observed gas reservoir. Instead, the molecular gas has likely formed as a result of sloshing motions in the intracluster medium induced by a nearby galaxy. Sloshing can emulate uplift by dislodging gas from the galactic center. This gas has the shortest cooling time, so it will condense if disrupted for long enough.</description><subject>Astrophysics</subject><subject>Clumps</subject><subject>Cold gas</subject><subject>Cooling</subject><subject>Emission</subject><subject>Entropy</subject><subject>Galactic Astrophysics</subject><subject>Galactic clusters</subject><subject>Galaxies</subject><subject>galaxies: active</subject><subject>galaxies: clusters: individual (RX J0821+0752)</subject><subject>galaxies: ISM</subject><subject>galaxies: kinematics and dynamics</subject><subject>Gas flow</subject><subject>Holes</subject><subject>Molecular gases</subject><subject>Physics</subject><subject>Reservoirs</subject><subject>Stars & galaxies</subject><subject>Uplift</subject><subject>X-ray emissions</subject><issn>0004-637X</issn><issn>2041-8205</issn><issn>1538-4357</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNp1kN1LwzAUxYMoOKfvPgb0RbQuaZKmfZxjH8pEEIW9hTRN2EZtatKq--9NqcwXfbrcc3_ncDkAnGN0S1LKR5iRNKKE8ZGUBuf0AAz20iEYIIRolBC-OgYn3m-7Nc6yAbgbV3BaWfdmWw8fbalVW0oH59LDWWk_4aaCzVrD5xV8QGmMrxFncbiW8msHJ2XrG-1OwZGRpddnP3MIXmfTl8kiWj7N7yfjZaQoJk0kM2ZQgniRF1QpSiVnCdEF1kbnJk01VyZDqcpziSjTOWNUZSnNqZSamKxQZAiu-ty1LEXtNm_S7YSVG7EYL0WnIZwFR5x84MBe9Gzt7HurfSO2tnVVeE_EJGE8kIgFCvWUctZ7p80-FiPRtSq6CkVXoehbDZbL3rKx9W-mrLci5UjEIpB1YQJ28wf2b-o3uOWCkw</recordid><startdate>20190110</startdate><enddate>20190110</enddate><creator>Vantyghem, A. 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C.</creator><creator>McDonald, M.</creator><creator>Salomé, P.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><general>Bristol : IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0002-3398-6916</orcidid><orcidid>https://orcid.org/0000-0003-0297-4493</orcidid><orcidid>https://orcid.org/0000-0002-2622-2627</orcidid><orcidid>https://orcid.org/0000-0003-2658-7893</orcidid><orcidid>https://orcid.org/0000-0002-9378-4072</orcidid><orcidid>https://orcid.org/0000-0003-4227-4838</orcidid><orcidid>https://orcid.org/0000-0001-5226-8349</orcidid></search><sort><creationdate>20190110</creationdate><title>An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster</title><author>Vantyghem, A. N. ; McNamara, B. R. ; Russell, H. R. ; Edge, A. C. ; Nulsen, P. E. 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Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Vantyghem, A. N.</au><au>McNamara, B. R.</au><au>Russell, H. R.</au><au>Edge, A. C.</au><au>Nulsen, P. E. J.</au><au>Combes, F.</au><au>Fabian, A. C.</au><au>McDonald, M.</au><au>Salomé, P.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJ</stitle><addtitle>Astrophys. 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| subjects | Astrophysics Clumps Cold gas Cooling Emission Entropy Galactic Astrophysics Galactic clusters Galaxies galaxies: active galaxies: clusters: individual (RX J0821+0752) galaxies: ISM galaxies: kinematics and dynamics Gas flow Holes Molecular gases Physics Reservoirs Stars & galaxies Uplift X-ray emissions |
| title | An Enormous Molecular Gas Flow in the RX J0821+0752 Galaxy Cluster |
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