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dc.contributor.authorVantyghem, ANen
dc.contributor.authorMcNamara, BRen
dc.contributor.authorRussell, Helenen
dc.contributor.authorHogan, MTen
dc.contributor.authorEdge, ACen
dc.contributor.authorNulsen, PEJen
dc.contributor.authorFabian, Andrewen
dc.contributor.authorCombes, Fen
dc.contributor.authorSalome, Pen
dc.contributor.authorBaum, SAen
dc.contributor.authorDonahue, Men
dc.contributor.authorMain, RAen
dc.contributor.authorMurray, NWen
dc.contributor.authorO'Connell, RWen
dc.contributor.authorO'Dea, CPen
dc.contributor.authorOonk, JBRen
dc.contributor.authorParrish, IJen
dc.contributor.authorSanders, JSen
dc.contributor.authorTremblay, Gen
dc.contributor.authorVoit, GMen
dc.date.accessioned2017-01-27T11:32:35Z
dc.date.available2017-01-27T11:32:35Z
dc.date.issued2016-12-01en
dc.identifier.issn0004-637X
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/262084
dc.description.abstractWe present ALMA CO(1–0) and CO(3–2) observations of the brightest cluster galaxy (BCG) in the 2A 0335+096 galaxy cluster ($z$ = 0.0346). The total molecular gas mass of 1.13 ± 0.15 × 10$^9$ $M_\odot$ is divided into two components: a nuclear region and a 7 kpc long dusty filament. The central molecular gas component accounts for 3.2 ± 0.4 × 10$^8$ $M_\odot$ of the total supply of cold gas. Instead of forming a rotationally supported ring or disk, it is composed of two distinct, blueshifted clumps south of the nucleus and a series of low-significance redshifted clumps extending toward a nearby companion galaxy. The velocity of the redshifted clouds increases with radius to a value consistent with the companion galaxy, suggesting that an interaction between these galaxies <20 Myr ago disrupted a pre-existing molecular gas reservoir within the BCG. Most of the molecular gas, 7.8 ± 0.9 × 10$^8$ $M_\odot$, is located in the filament. The CO emission is co-spatial with a 10$^4$ K emission-line nebula and soft X-rays from 0.5 keV gas, indicating that the molecular gas has cooled out of the intracluster medium over a period of 25–100 Myr. The filament trails an X-ray cavity, suggesting that the gas has cooled from low-entropy gas that has been lifted out of the cluster core and become thermally unstable. We are unable to distinguish between inflow and outflow along the filament with the present data. Cloud velocities along the filament are consistent with gravitational free-fall near the plane of the sky, although their increasing blueshifts with radius are consistent with outflow.
dc.description.sponsorshipSupport for this work was provided in part by the National Aeronautics and Space Administration through Chandra Award Number G05-16134X issued by the Smithsonian Astrophysical Observatory for an on behalf of the National Aeronautics and Space Administration under contract NAS8- 03060. A.N.V. and B.R.M. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. B.R.M. further acknowledges support from the Canadian Space Agency Space Science Enhancement Program.
dc.language.isoenen
dc.publisherIOP Publishing
dc.subjectgalaxies: activeen
dc.subjectgalaxies: clusters: individual (2A 0335+096)en
dc.subjectgalaxies: ISMen
dc.subjectgalaxies: kinematics and dynamicsen
dc.titleMolecular gas along a bright H$\alpha$ filament in 2A 0335+096 revealed by ALMAen
dc.typeArticle
prism.issueIdentifier2en
prism.number148en
prism.publicationDate2016en
prism.publicationNameAstrophysical Journalen
prism.volume832en
dc.identifier.doi10.17863/CAM.7332
dcterms.dateAccepted2016-10-01en
rioxxterms.versionofrecord10.3847/0004-637X/832/2/148en
rioxxterms.versionVoRen
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2016-12-01en
dc.contributor.orcidFabian, Andrew [0000-0002-9378-4072]
dc.identifier.eissn1538-4357
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idEuropean Research Council (340442)
cam.issuedOnline2016-11-29en
cam.orpheus.successThu Jan 30 12:56:43 GMT 2020 - The item has an open VoR version.*
rioxxterms.freetoread.startdate2100-01-01


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