Repositório Digital

A- A A+

Investigating potential planetary nebula/cluster pairs

.

Investigating potential planetary nebula/cluster pairs

Mostrar registro completo

Estatísticas

Título Investigating potential planetary nebula/cluster pairs
Autor Moni Bidin, Christian
Majaess, Daniel J.
Bonatto, Charles Jose
Mauro, Francesco
Turner, D. G.
Geisler, Doug
Chené, André-Nicolas
Gormaz-Matamala, Alex C.
Borissova, Jura
Kurtev, Radostin Georgiev
Minniti, Dante
Carraro, Giovanni
Gieren, Wolfgang P.
Abstract Context. Fundamental parameters characterizing the end-state of intermediate-mass stars may be constrained by discovering planetary nebulae (PNe) in open clusters (OCs). Cluster membership may be exploited to establish the distance, luminosity, age, and physical size for PNe, and the intrinsic luminosity and mass of its central star. Aims. Four potential PN-OC associations were investigated to assess the cluster membership for the PNe. Methods. Radial velocities were measured from intermediate-resolution optical spectra, complemented with previous estimates in the literature.When the radial velocity study supported the PN/OC association, we analyzed whether other parameters (e.g., age, distance, reddening, central star brightness) were consistent with this conclusion. Results. Our measurements imply that the PNe VBe 3 and HeFa 1 are not members of the OCs NGC5999 and NGC6067, respectively, and that they very likely belong to the background bulge population. Conversely, consistent radial velocities indicate that NGC2452/NGC 2453 could be associated, but our results are not conclusive so additional observations are warranted. Finally, we demonstrate that all the available information point to He 2-86 being a young, highly internally obscured PN member of NGC4463. New near-infrared photometry acquired via the Vista Variables in the Via Lactea ESO public survey was used in tandem with existing UBV photometry to measure the distance, reddening, and age of NGC4463, finding d = 1.55 ± 0.10 kpc, E(B − V) = 0.41 ± 0.02, and τ = 65 ± 10 Myr, respectively. The same values should be adopted for the PN if the proposed cluster membership is confirmed.
Contido em Astronomy and astrophysics. Les Ulis. Vol. 561 (Jan. 2014), A119, 14 p.
Assunto Aglomerados estelares
Astronomia infravermelha
Dinamica estelar
Espectros astronômicos
Fotometria astronômica
Nebulosas planetarias
[en] Open clusters and associations: general
[en] Planetary nebulae: general
Origem Estrangeiro
Tipo Artigo de periódico
URI http://hdl.handle.net/10183/114538
Arquivos Descrição Formato
000954031.pdf (878.5Kb) Texto completo (inglês) Adobe PDF Visualizar/abrir

Este item está licenciado na Creative Commons License

Este item aparece na(s) seguinte(s) coleção(ões)


Mostrar registro completo

Percorrer



  • O autor é titular dos direitos autorais dos documentos disponíveis neste repositório e é vedada, nos termos da lei, a comercialização de qualquer espécie sem sua autorização prévia.
    Projeto gráfico elaborado pelo Caixola - Clube de Criação Fabico/UFRGS Powered by DSpace software, Version 1.8.1.