Compact planetary nebulae MaC 2-1 and Sp 4-1: Photoionization models and dust characteristics

TL;DR

This study combines optical, infrared, and imaging data to model planetary nebulae MaC 2-1 and Sp 4-1, revealing their dust compositions, physical properties, and progenitor characteristics in a comprehensive manner.

Contribution

It provides the first detailed photoionization models and dust analysis for these two planetary nebulae, integrating multi-wavelength data for a self-consistent understanding.

Findings

MaC 2-1 contains SiC and MgS dust.

Sp 4-1 hosts PAH molecules.

Progenitors had masses of 1.2 and 1.55 solar masses, respectively.

Abstract

We study the characteristics of planetary nebulae (PNe), MaC 2-1 and Sp 4-1. We use our optical spectra taken at 2 m Himalayan Chandra Telescope, Spitzer mid-infrared (mid-IR) spectra, HST images, and IR photometric data. These PNe have not been individually studied in details earlier. Both the PNe are in the low- to moderate-excitation class. MaC 2-1 shows the presence of silicon carbide (SiC) and magnesium sulphide (MgS) dust. Sp 4-1 hosts polycyclic aromatic hydrocarbon (PAH) molecules. We obtain plasma properties of the PNe from the optical and mid-IR emission line fluxes. We compute photoionization models of the PNe for self-consistent estimation of physical parameters associated with the central star and the nebula, including nebular abundances. From the modelling of the IR data, we obtain the characteristics of dust and molecules formed in the nebulae. From our study, we estimate that the progenitors of MaC 2-1 and Sp 4-1 had masses of 1.2 and 1.55 $M_{\sun}$, respectively, and both of them seem to have born in metal poor environment. Both are distant PNe, with the estimated distances of 16 and 18 kpc for MaC 2-1 and Sp 4-1, respectively.