On the crucial cluster Andrews-Lindsay 1 and a 4% distance solution for its planetary nebula

• Autor(a) principal: Majaess, Daniel J.
• Data de Publicação: 2014
• Outros Autores: Carraro, Giovanni, Moni Bidin, Christian, Bonatto, Charles Jose, Turner, D. G., Moyano, Maximiliano, Berdnikov, L., Giorgi, Edgard Ervar
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Institucional da UFRGS
• Texto Completo: http://hdl.handle.net/10183/126970
• topic: Aglomerados estelares; Nebulosas; Open clusters and associations: individual: Andrews-Lindsay 1 (ESO 96-SC04); Planetary nebulae: individual: PHR 1315-6555

Andrews-Lindsay 1 is a pertinent open cluster because it may host the planetary nebula (PN) PHR 1315-6555, yet ambiguities linger concerning its fundamental parameters (>50% scatter). New multiband BVJHW1−4 photometry for cluster and field stars, in concert with observations of recently discovered classical Cepheids, were used to constrain the reddening and velocity-distance profiles along the sightline. That analysis yielded the following parameters for the cluster: E(J − H) = 0.24 ± 0.03, d = 10.0 ± 0.4 kpc (dJH = 9.9 ± 0.6 kpc, dBV = 10.1 ± 0.5 kpc), and log τ = 8.90 ± 0.15. The steep velocity-distance gradient along ∼ 305◦ indicates that two remote objects sharing spatial and kinematic parameters (i.e., PHR 1315-6555 and Andrews-Lindsay 1) are associated, thus confirming claims that the PN is a cluster member. The new distance for PHR 1315-6555 is among the most precise established yet for a Galactic PN (σ/d = 4%).