Romano L.M. Corradi, Rebeca Galera Rosillo, David Jones
J. Drew (Univ. Hertfordshire) and IPHAS Collaboration (www.iphas.org); R. Greimel (Univ. Graz); M. Santander-García (OAN, Madrid); D.R. Gonçalves (Obs. Valongo, Brasil); U. Munari (INAF, Italia); L. Sabin (UNAM, México); T. Liimets (Tartu Observatory); B. Balick (Univ. Washington); L. Magrini (Univ. Florencia); R. Wesson, Henri Boffin (ESO); T. Hillwig (Valparaiso University, EEUU); B. Miszalski (SALT, Sudafrica)
This project has three major objectives: 1) To determine the physico-chemical characteristics of bipolar planetary nebulae and symbiotic nebulae, to help understanding the origin of bipolarity and to test theoretical models, mainly models with binary central stars, aimed at explaining the observed morphology and kinematics. 2) To study the low-ionization microstructures in planetary nebulae, their origin (in the context of the main shell formation), their physico-chemical characteristics, and their interaction with the nebular gas. 3) To discover and study galactic and extragalactic planetary nebulae, analyzing their physico-chemical properties and the metallicity gradients along the galactic discs.
Miszalski, B and collaborators (2016, MNRAS, 456, 633) re-discovered a dwarf nova system, an eruption of which was first observed by ancient Chinese astronomers in the year 483 CE.
Hillwig, T and collaborators (2016, ApJ, 832, 125) demonstrated that the symmetry axes of planetary nebulae with binary central stars always lie perpendicular to the orbital plane of the central binaries. The probability of encountering such a tight correlation by chance is less than a million to one.