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Article: A high-mass planetary nebula in a Galactic open cluster

TitleA high-mass planetary nebula in a Galactic open cluster
Authors
Issue Date2019
PublisherNature Publishing Group. The Journal's web site is located at https://www.nature.com/natastron/
Citation
Nature Astronomy, 2019, v. 3 n. 9, p. 851-857 How to Cite?
AbstractPlanetary nebulae are the ionized ejected envelopes surrounding the remnant cores of dying stars. Theory predicts that main-sequence stars of one to about eight solar masses may eventually form planetary nebulae. Until now, this has not been confirmed at the higher end of the mass range. Here we report that the planetary nebula BMP J1613-5406 is associated with the Galactic star cluster NGC 6067. Stars evolving off the main sequence of this cluster have a mass of around five solar masses. Our confidence in the association between the planetary nebula and the cluster comes from their tightly consistent radial velocities in a sightline with a steep velocity–distance gradient, common distances, and reddening and location of the planetary nebula within the cluster boundary. This is an unprecedented example of a planetary nebula whose progenitor star mass approaches the theoretical lower limit of core-collapse supernova formation. This finding provides observational evidence supporting theoretical predictions that stars of five solar masses and more can form planetary nebulae.
Persistent Identifierhttp://hdl.handle.net/10722/272299
ISSN
2023 Impact Factor: 12.9
2023 SCImago Journal Rankings: 3.311
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorFragkou, V-
dc.contributor.authorParker, QA-
dc.contributor.authorZijlstra, AA-
dc.contributor.authorCrause, L-
dc.contributor.authorBarker, H-
dc.date.accessioned2019-07-20T10:39:33Z-
dc.date.available2019-07-20T10:39:33Z-
dc.date.issued2019-
dc.identifier.citationNature Astronomy, 2019, v. 3 n. 9, p. 851-857-
dc.identifier.issn2397-3366-
dc.identifier.urihttp://hdl.handle.net/10722/272299-
dc.description.abstractPlanetary nebulae are the ionized ejected envelopes surrounding the remnant cores of dying stars. Theory predicts that main-sequence stars of one to about eight solar masses may eventually form planetary nebulae. Until now, this has not been confirmed at the higher end of the mass range. Here we report that the planetary nebula BMP J1613-5406 is associated with the Galactic star cluster NGC 6067. Stars evolving off the main sequence of this cluster have a mass of around five solar masses. Our confidence in the association between the planetary nebula and the cluster comes from their tightly consistent radial velocities in a sightline with a steep velocity–distance gradient, common distances, and reddening and location of the planetary nebula within the cluster boundary. This is an unprecedented example of a planetary nebula whose progenitor star mass approaches the theoretical lower limit of core-collapse supernova formation. This finding provides observational evidence supporting theoretical predictions that stars of five solar masses and more can form planetary nebulae.-
dc.languageeng-
dc.publisherNature Publishing Group. The Journal's web site is located at https://www.nature.com/natastron/-
dc.relation.ispartofNature Astronomy-
dc.rightsThis is a post-peer-review, pre-copyedit version of an article published in Nature Astronomy. The final authenticated version is available online at: https://doi.org/10.1038/s41550-019-0796-x-
dc.titleA high-mass planetary nebula in a Galactic open cluster-
dc.typeArticle-
dc.identifier.emailFragkou, V: vfragkou@hku.hk-
dc.identifier.emailParker, QA: quentinp@hku.hk-
dc.identifier.emailZijlstra, AA: zijlstra@hku.hk-
dc.identifier.authorityParker, QA=rp02017-
dc.description.naturepostprint-
dc.identifier.doi10.1038/s41550-019-0796-x-
dc.identifier.scopuseid_2-s2.0-85068105634-
dc.identifier.hkuros298514-
dc.identifier.volume3-
dc.identifier.issue9-
dc.identifier.spage851-
dc.identifier.epage857-
dc.identifier.isiWOS:000485096800017-
dc.publisher.placeUnited Kingdom-
dc.identifier.issnl2397-3366-

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