The origin of the planetary nebula M 1-16. A morphokinematic and chemical analysis

Abstract

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 $-$40kms${}^{-1}$ to 20kms${}^{-1}$, with respect to the systemic velocity. The morpho-kinematic model indicates that the deprojected velocity of the lobe outflows are $\ge$100kms${}^{-1}$, and particularly the larger lobes and knots have a deprojected velocity of $\simeq$350kms${}^{-1}$; the inner ellipsoidal component has a deprojected velocity of $\simeq$29kms${}^{-1}$. A kinematical age of $\sim$8700yr has been obtained from the model assuming a homologous velocity expansion law and a distance of 6.2$\pm$1.9kpc. 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 $\simeq$0.618-0.713M${}_{\odot }$ and an initial mass for the progenitor star between 2.0 and 3.0M${}_{\odot }$ (depending on metallicity). An $T_{\mathrm{eff}}\simeq$140000K and log$(L/L_{\odot })$=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.

A&A in press. 11 pages, 9 figures

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