Study of binary central stars of planetary nebulae with GALEX and corollary optical surveys.
type: CreativeWork
description: Planetary Nebulae (PNe) are the descendants of low- and intermediate-mass stars (0.8--8.0 M☉). The shape of the PN takes place at some point between the asymptotic giant branch (AGB) and the white dwarf (WD) stellar phases. Among the astrophysical phenomena, the PNe shows an impressive variety of complex morphologies. In fact, most of the PNe known are not spherical (more than 80%) and present shapes from slightly elliptical to bipolar (or multipolar), as well as knots and/or collimated outflows at high velocities, reaching 600 km s-1 in the most extreme cases. The aim of this thesis is to explore how binarity affects the evolution of low- and intermediate-mass stars during the PN phase. We started by looking for photometric data of the known central stars of PNe (CSPNe) in different databases (from the ultraviolet to the near-infrared) in order to search for a double spectral energy distribution (SED) composed by a hot-star (the ionizing star) and a cool companion star. We compiled a catalog of PNe by combining the coordinates PNe catalogs found in the literature, and matched them with the Galaxy Evolution Explorer (GALEX) database (GPNcat). The FUV and NUV photometry, included in GALEX, allow us to extract the hottest stellar objects, which are elusive in optical wavelengths due to its Teff and luminosity. We matched the GPNcat with Sloan Digital Sky Survey (SDSS) and the Panoramic Survey and Rapid Response System (PanSTARRS) databases (GPNcatxSDSSDR14xPS1DR2), both providing five magnitudes in the optical range (SDSS ugriz and PS1 grizy). We separated the resolved PNe, with sizes (diameters) at least twice the resolution of GALEX, from unresolved PNe. For resolved PNe, the flux of the CS were isolated by using aperture photometry techniques. The final catalog, GPNcatxSDSSDR14xPS1DR2, contains 326 PNe with both UV and optical photometry of which 222 are resolved. Most of the PNe are not spherical, and current single-star models cannot explain the morphologies we o…
abstract: Planetary Nebulae (PNe) are the descendants of low- and intermediate-mass stars (0.8--8.0 M☉). The shape of the PN takes place at some point between the asymptotic giant branch (AGB) and the white dwarf (WD) stellar phases. Among the astrophysical phenomena, the PNe shows an impressive variety of complex morphologies. In fact, most of the PNe known are not spherical (more than 80%) and present shapes from slightly elliptical to bipolar (or multipolar), as well as knots and/or collimated outflows at high velocities, reaching 600 km s-1 in the most extreme cases. The aim of this thesis is to explore how binarity affects the evolution of low- and intermediate-mass stars during the PN phase. We started by looking for photometric data of the known central stars of PNe (CSPNe) in different databases (from the ultraviolet to the near-infrared) in order to search for a double spectral energy distribution (SED) composed by a hot-star (the ionizing star) and a cool companion star. We compiled a catalog of PNe by combining the coordinates PNe catalogs found in the literature, and matched them with the Galaxy Evolution Explorer (GALEX) database (GPNcat). The FUV and NUV photometry, included in GALEX, allow us to extract the hottest stellar objects, which are elusive in optical wavelengths due to its Teff and luminosity. We matched the GPNcat with Sloan Digital Sky Survey (SDSS) and the Panoramic Survey and Rapid Response System (PanSTARRS) databases (GPNcatxSDSSDR14xPS1DR2), both providing five magnitudes in the optical range (SDSS ugriz and PS1 grizy). We separated the resolved PNe, with sizes (diameters) at least twice the resolution of GALEX, from unresolved PNe. For resolved PNe, the flux of the CS were isolated by using aperture photometry techniques. The final catalog, GPNcatxSDSSDR14xPS1DR2, contains 326 PNe with both UV and optical photometry of which 222 are resolved. Most of the PNe are not spherical, and current single-star models cannot explain the morphologies we o…
author: G´omez Mu˜noz, Marco Antonio
date published: 2020
date modified: 2026-07-24T05:12:21Z
provider: Universidad de la Laguna
publisher: Networked Digital Library of Theses and Dissertations
type: WebPage
source organization: Universidad de la Laguna