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dc.contributor.authorKopytova, Taisiya G.
dc.contributor.authorCrossfield, Ian J M
dc.contributor.authorDeacon, Niall R.
dc.contributor.authorBrandner, Wolfgang
dc.contributor.authorBuenzli, Esther
dc.contributor.authorBayo, Amelia
dc.contributor.authorSchlieder, Joshua E.
dc.contributor.authorManjavacas, Elena
dc.contributor.authorBiller, Beth A.
dc.contributor.authorKopon, Derek
dc.date.accessioned2017-07-19T16:37:10Z
dc.date.available2017-07-19T16:37:10Z
dc.date.issued2014-11-17
dc.identifier.citationKopytova , T G , Crossfield , I J M , Deacon , N R , Brandner , W , Buenzli , E , Bayo , A , Schlieder , J E , Manjavacas , E , Biller , B A & Kopon , D 2014 , ' Deep z-band observations of the coolest y dwarf ' , The Astrophysical Journal , vol. 797 , no. 1 , 3 . https://doi.org/10.1088/0004-637X/797/1/3
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 10013114
dc.identifier.otherPURE UUID: 507e2de3-93d0-4cf0-a293-a822bece72be
dc.identifier.otherScopus: 84914671688
dc.identifier.urihttp://hdl.handle.net/2299/18995
dc.descriptionTaisiya G. Kopytova, et al., “Deep z-band observations of the coolest y dwarf”, The Astrophysical Journal, Vol. 797(1), November 2014. © 2014. The American Astronomical Society.
dc.description.abstractWISE J085510.83-071442.5 (hereafter, WISE 0855-07) is the coolest Y dwarf known to date and is located at a distance of 2.31 ± 0.08 pc, giving it the fourth largest parallax of any known star or brown dwarf system. We report deep z-band observations of WISE 0855-07 using FORS2 on UT1/Very Large Telescope. We do not detect any counterpart to WISE 0855-07 in our z-band images and estimate a brightness upper limit of AB mag > 24.8 (F ν <0.45 μJy) at 910 ± 65 nm with 3σ confidence. We combine our z-band upper limit with previous near- and mid-infrared photometry to place constraints on the atmospheric properties of WISE 0855-07 via comparison to models which implement water clouds in the atmospheres of T eff <300 K substellar objects. We find that none of the available models that implement water clouds can completely reproduce the observed spectral energy distribution of WISE 0855-07. Every model significantly disagrees with the (3.6 μm/4.5 μm) flux ratio and at least one other bandpass. Since methane is predicted to be the dominant absorber at 3-4 μm, these mismatches might point to an incorrect or incomplete treatment of methane in current models. We conclude that (a) WISE0855-07 has T eff 200-250 K, (b)en
dc.format.extent4
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.subjectbrown dwarfs
dc.subjectstars: individual (WISE J085510.83-071442.5)
dc.subjectstars: low-mass
dc.subjectNuclear and High Energy Physics
dc.titleDeep z-band observations of the coolest y dwarfen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionUniversity of Hertfordshire
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=84914671688&partnerID=8YFLogxK
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2014-11-17
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/797/1/3
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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