Morphology and ionization characteristics of planetary nebulae PB 1 and PC 19

Abstract

We present results of our study of two planetary nebulae (PNe), PB1 and PC 19. We use the optical spectra of these two PNe observed at 2 m Himalayan Chandra Telescope and also archival and literature data for the study. We use the morphokinematic code shape to construct 3D morphologies of the PNe and the photoionization code cloudy to model the observed spectra. The 3D model of PB 1 consists of an elongated shell surrounded by a bipolar halo and that of PC 19 consists of an open lobed bipolar structure and a spiral filamentary pair. We analyse the ionization structure of the PNe by deriving several plasma parameters and by photoionization modelling. We estimate the elemental abundances of the elements, He, C, N, O, Ne, S, Ar, and Cl, from our analysis. We find He, C, and N abundances to be significantly higher in case of PB 1. We estimate different physical parameters of the central stars, namely effective temperature, luminosity, and gravity, and of the nebula, namely hydrogen density profiles, radii, etc., from photoionization modelling. We estimate distances to the PNe as ∼4.3 kpc for PB 1 and as ∼5.6 kpc for PC 19 by fitting the photoionization models to absolute observed fluxes. Progenitor masses are estimated from theoretical evolutionary trajectories and are found to be ∼1.67 and ∼2.38 M⊙ for PB 1 and PC 19, respectively.

A New View of Observed Galaxies through 3D Modelling and Visualisation

“…The software tool Shape [50] builds upon this modelling approach to provide an interactive construction and analysis tool for planetary nebulae, used in several related works focusing on reconstruction of planetary nebulae (e.g. [17,1]). The SlicerAstro [45] extension to scientific visualisation software 3DSlicer [14] allows users to visualise (H i) data in 3D, two spatial dimensions and a third velocity dimension.…”

“…optical, radio, infrared and ultraviolet) allow the measurement and derivation of many different properties, together enabling us to study galaxy morphology, kinematics, composition, mass, age, and formation history. Conversely, simulation of astronomical objects has been an active research topic in astronomy for many years [40,54] with an aim to gain a better understanding of physical processes occurring over timescales so long, and 1 Corresponding author: tim.dykes@hpe.com across spatial scales so massive, that we cannot hope to observe them in real-time. In both cases, visualisation has been used extensively to help understand, analyse, and disseminate the results of such efforts, as discussed in Section 2.…”

Photo-ionization structures of Planetary Nebula IC 2003 with [WR] central star

“…This helps to constrain accurately the chemical and physical parameters of PNe as well as to derive the central star parameters (Maciel et al, 2010;Garcı ´a-Rojas et al, 2016). Photo-ionization models were derived for some PNe involving gas and dust components earlier by different authors (van Hoof and van de Steene, 1999;Bohigas, 2008;Otsuka et al, 2017;Bandyopadhyay et al, 2020) The central stars of PNe (CSPNe) are broadly classified into two groups based on their hydrogen content, viz. the hydrogen-rich and the hydrogen-poor CSPNe (Acker and Neiner, 2003;Weidmann and Gamen, 2011), and also by Muthumariappan and Parthasarathy (2020) (hereafter, MP20).…”