Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with LBVN appearance

TL;DR

This study uses integral field spectroscopy and infrared data to analyze the morphology, kinematics, and chemical composition of the Wolf-Rayet nebula M1-67, revealing bipolar ejection features likely originating from a luminous blue variable eruption.

Contribution

It provides a detailed multi-wavelength analysis of M1-67, combining optical integral field spectroscopy with infrared data to uncover its bipolar structure and chemical enrichment, linking it to stellar evolution stages.

Findings

Bipolar structure with knots aligned NE-SW

Strong nitrogen enrichment and oxygen depletion

Ejection likely from a luminous blue variable eruption

Abstract

This work aims to disentangle the morphological, kinematic, and chemical components of the nebula M1-67 to shed light on its process of formation around the central Wolf-Rayet (WR) star WR124. We have carried out integral field spectroscopy observations over two regions of M1-67, covering most of the nebula in the optical range. Maps of electron density, line ratios, and radial velocity were created to perform a detailed analysis of the two-dimensional structure. We studied the physical and chemical properties by means of integrated spectra selected over the whole nebula. Photoionization models were performed to confirm the empirical chemical results theoretically. In addition, we analysed infrared spectroscopic data and the MIPS 24micron image of M1-67 from Spitzer. We find that the ionized gas of M1-67 is condensed in knots aligned in a preferred axis along the NE-SW direction, like a bipolar structure. Both electron density and radial velocity decrease in this direction when moving away from the central star. From the derived electron temperature, Te~8200 K, we have estimated chemical abundances, obtaining that nitrogen appears strongly enriched and oxygen depleted. From the last two results, we infer that this bipolarity is the consequence of an ejection of an evolved stage of WR124 with material processed in the CNO cycle. The infrared study has revealed that the bipolar axis is composed of ionized gas with a low ionization degree that is well mixed with warm dust and of a spherical bubble surrounding the ejection at 24micron. Taking the evolution of a 60 Mo star and the temporal scale of the bipolar ejection into account, we propose that the observed gas was ejected during an eruption in the luminous blue variable. The star has entered the WR phase recently without apparent signs of interaction between WR-winds and interstellar material.