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dc.contributor.authorBarker, Helen
dc.contributor.authorZijlstra, Albert
dc.contributor.authorMarco, Orsola De
dc.contributor.authorFrew, David J.
dc.contributor.authorDrew, J. E.
dc.contributor.authorCorradi, R. L. M.
dc.contributor.authorEislöffel, Jochen
dc.contributor.authorParker, Quentin A.
dc.date.accessioned2018-06-06T17:07:54Z
dc.date.available2018-06-06T17:07:54Z
dc.date.issued2018-04-21
dc.identifier.citationBarker , H , Zijlstra , A , Marco , O D , Frew , D J , Drew , J E , Corradi , R L M , Eislöffel , J & Parker , Q A 2018 , ' The binary fraction of planetary nebula central stars - III. the promise of VPHAS+ ' , Monthly Notices of the Royal Astronomical Society , vol. 475 , no. 4 , pp. 4504–4523 . https://doi.org/10.1093/mnras/stx3240
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 13078625
dc.identifier.otherPURE UUID: 81f1c2fc-0dc4-42e8-a622-d3b08256b3be
dc.identifier.otherArXiv: http://arxiv.org/abs/1712.03194v1
dc.identifier.otherScopus: 85042551510
dc.identifier.urihttp://hdl.handle.net/2299/20139
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. Content in the UH Research Archive is made available for personal research, educational, and non-commercial purposes only. Unless otherwise stated, all content is protected by copyright, and in the absence of an open license, permissions for further re-use should be sought from the publisher, the author, or other copyright holder.
dc.description.abstractThe majority of planetary nebulae (PNe) are not spherical, and current single-star models cannot adequately explain all the morphologies we observe. This has led to the Binary Hypothesis, which states that PNe are preferentially formed by binary systems. This hypothesis can be corroborated or disproved by comparing the estimated binary fraction of all PNe central stars (CS) to that of the supposed progenitor population. One way to quantify the rate of CS binarity is to detect near infra-red (IR) excess indicative of a low-mass main sequence companion. In this paper, a sample of known PNe within data release 2 of the ongoing VPHAS+ are investigated. We give details of the method used to calibrate VPHAS+ photometry, and present the expected colours of CS and main sequence stars within the survey. Objects were scrutinized to remove PN mimics from our sample and identify true CS. Within our final sample of 7 CS, 6 had previously either not been identified or confirmed. We detected an $i$ band excess indicative of a low-mass companion star in 3 CS, including one known binary, leading us to to conclude that VPHAS+ provides the precise photometry required for the IR excess method presented here, and will likely improve as the survey completes and the calibration process finalised. Given the promising results from this trial sample, the entire VPHAS+ catalogue should be used to study PNe and extend the IR excess-tested CS sample.en
dc.format.extent20
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectBinaries: general
dc.subjectPlanetary nebulae: general
dc.subjectStars: evolution
dc.subjectTechniques: photometric
dc.subjectWhite dwarfs
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe binary fraction of planetary nebula central stars - III. the promise of VPHAS+en
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85042551510&partnerID=8YFLogxK
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2018-04-21
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stx3240
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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