Show simple item record

dc.contributor.authorGledhill, Timothy
dc.contributor.authorFroebrich, Dirk
dc.contributor.authorCampbell-White, J.
dc.contributor.authorJones, Alex
dc.date.accessioned2018-08-16T00:17:57Z
dc.date.available2018-08-16T00:17:57Z
dc.date.issued2018-09-21
dc.identifier.citationGledhill , T , Froebrich , D , Campbell-White , J & Jones , A 2018 , ' Planetary Nebulae in the UWISH2 survey ' , Monthly Notices of the Royal Astronomical Society , vol. 479 , no. 3 , sty1580 , pp. 3759-3777 . https://doi.org/10.1093/mnras/sty1580
dc.identifier.issn0035-8711
dc.identifier.otherORCID: /0000-0002-2859-4600/work/54896469
dc.identifier.urihttp://hdl.handle.net/2299/20456
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review.
dc.description.abstractNear-infrared imaging in the 1 - 0 S(1) emission line of molecular hydrogen is able to detect planetary nebulae (PNe) that are hidden from optical emission line surveys.We present images of 307 objects from the UWISH2 survey of the northern Galactic Plane, and with the aid of mid-infrared colour diagnostics draw up a list of 291 PN candidates. The majority, 183, are newdetections and 85 per cent of these are not present in Hα surveys of the region.We find that more than half (54 per cent) of the objects have a bipolar morphology and that some objects previously considered as elliptical or point-source in Hα imaging, appear bipolar in UWISH2 images. By considering a small subset of objects for which physical radii are available from the Hα surface brightness-radius relation, we find evidence that the H 2 surface brightness remains roughly constant over a factor 20 range of radii from 0.03 to 0.6 pc, encompassing most of the visible lifetime of a PN. This leads to the Hα surface brightness becoming comparable to that of H 2 at large radius (>0.5 pc). By combining the number of UWISH2 PNe without Hα detection with an estimate of the PN detection efficiency in H 2 emission, we estimate that PN numbers from Hα surveys may underestimate the true PN number by a factor between 1.5 and 2.5 within the UWISH2 survey area.en
dc.format.extent19
dc.format.extent1235154
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectInfrared: stars
dc.subjectPlanetary nebulae: general
dc.subjectStars: evolution
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titlePlanetary Nebulae in the UWISH2 surveyen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85051568487&partnerID=8YFLogxK
rioxxterms.versionofrecord10.1093/mnras/sty1580
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record