The origin of the planetary nebula M 1–16: A morpho-kinematic and chemical analysis

• Published in: Astronomy and astrophysics (Berlin) 2023-08, Vol.676, p.A101
• Main Authors: Gómez-Muñoz, M. A., Vázquez, R., Sabin, L., Olguín, L., Guillén, P. F., Zavala, S., Michel, R.
• Format: Article
• Language: English
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/202346455

We investigated the origin of the Planetary Nebula (PN) M 1–16 using narrow-band optical imaging, and high- and low-resolution optical spectra to perform a detailed morpho-kinematic and chemical studies. M 1–16 is revealed to be a multipolar PN that predominantly emits in [O  III ] in the inner part of the nebula and [N  II ] in the lobes. A novel spectral unsharp masking technique was applied to the position-velocity (PV) maps to reveal a set of multiple structures at the centre of M 1–16 spanning radial velocities from −40 km s −1 to 20 km s −1 , with respect to the systemic velocity. The morpho-kinematic model indicates that the deprojected velocity of the lobe outflows are ≥100 km s −1 , and particularly the larger lobes and knots have a deprojected velocity of ≃350 km s −1 ; the inner ellipsoidal component has a deprojected velocity of ≃29 km s −1 . A kinematical age of ~8700 yr has been obtained from the model assuming a homologous velocity expansion law and a distance of 6.2 ± 1.9 kpc. The chemical analysis indicates that M 1–16 is a Type I PN with a central star of PN (CSPN) mass in the range of ≃0.618 – 0.713 M ⊙ and an initial mass for the progenitor star between 2.0 and 3.0 M ⊙ (depending on metallicity). An T eff ≃ 140 000 K and log( L / L ⊙ ) = 2.3 was estimated using the 3MdB photoionisation models to reproduce the ionisation. stage of the PN. All of these results have led us to suggest that M 1–16 is an evolved PN, contrary to the scenario of proto-PN suggested in previous studies. We propose that the mechanism responsible for the morphology of M 1–16 is related to the binary (or multiple star) evolution scenario.