A morpho-kinematic and spectroscopic study of the bipolar nebulae: M 2−9, Mz 3, and Hen 2−104

Abstract

Context. Complex bipolar shapes can be generated either as a planetary nebula or a symbiotic system. The origin of the material ionised by the white dwarf is very different in these two scenarios, and it complicates the understanding of the morphologies of planetary nebulae. Aims. The physical properties, structure, and dynamics of the bipolar nebulae, M 2−9, Mz 3, and Hen 2−104, are investigated in detail with the aim of understanding their nature, shaping mechanisms, and evolutionary history. Both a morpho-kinematic study and a spectroscopic analysis, can be used to more accurately determine the kinematics and nature of each nebula. Methods. Long-slit optical echelle spectra are used to investigate the morpho-kinematics of M 2−9, Mz 3, and Hen 2−104. The morpho-kinematic modelling software SHAPE is used to constrain both the morphology and kinematics of each nebula by means of detailed 3D models. Near-infrared (NIR) data, as well as optical, spectra are used to separate Galactic symbiotic-type nebulae from genuine planetary nebulae by means of a 2MASS J−H/H−Ks diagram and a λ4363/Hγ vs. λ5007/Hβ diagnostic diagram, respectively. Results. The best-fitted 3D models for M 2−9, Mz 3, and Hen 2−104 provide invaluable kinematical information on the expansion velocity of its nebular components by means of synthetic spectra. The observed spectra match up very well with the synthetic spectra for each model, thus showing that each model is tightly constrained both morphologically and kinematically. Kinematical ages of the different structures of M 2−9 and Mz 3 have also been determined. Both diagnostic diagrams show M 2−9 and Hen 2−104 to fall well within the category of having a symbiotic source, whereas Mz 3 borders the region of symbiotic and young planetary nebulae in the optical diagram but is located firmly in the symbiotic region of the NIR colour−colour diagram. The optical diagnostic diagram is shown to successfully separate the two types of nebulae, however, the NIR colour−colour diagram is not as accurate in separating these objects. Conclusions. The morphology, kinematics, and evolutionary history of M 2−9, Mz 3, and Hen 2−104 are better understood using the interactive 3D modelling tool . The expansion velocities of the components for each nebula are better constrained and fitted with a vector field to reveal their direction of motion. The optical and NIR diagnostic diagrams used are important techniques for separating Galactic symbiotic-type nebulae from genuine planetary nebulae.

Dissecting a supernova impostor’s circumstellar medium: MUSEing about the SHAPE ofηCarinae’s outer ejecta

“…With SHAPE we derived that the emission of the outer shell can be matched with a bent cylinder geometry embedding the entire Homunculus nebula (Figure 4). This structure is reminiscent of the shape of the planetary nebula M 2-9 (Clyne et al 2015). The bending of the outer shell might have been caused by the interaction with a denser region of the ambient medium, slowing down the material.…”

The extended molecular envelope of the asymptotic giant branch star π1 Gruis as seen by ALMA

“…Expansion velocities of PNe are on average about a factor of two larger (∼20 km s −1 ; Gesicki & Zijlstra 2000;Huggins et al 2005) than typical AGB wind velocities, but more extreme velocities in excess of ∼100 km s −1 are also found in post-AGB stars and PNe (e.g., Vlemmings et al 2006;Clyne et al 2015). Bujarrabal et al (2001) studied the CO emission from 30 protoplanetary nebulae (P-PNe) and found that almost all of the sample sources have both a slowly expanding envelope (probably the remnant AGB wind) and fast (often bipolar) outflows.…”

A pilot search for mm-wavelength recombination lines from emerging ionized winds in pre-planetary nebulae candidates

“…Optical spectroscopic observations point to an expansive kinematics in the lobes, as for most pPNe and young PNe, with expansion velocities ranging from ∼23 km s −1 in the inner nebula up to ∼164 km s −1 in the outer lobe tips (Schwarz et al 1997;Torres-Peimbert et al 2010;Clyne et al 2015). The central core is dominated by Hα emission with ∼1600 km s −1 -wide wings.…”

“…M 2-9, also known as the "Butterfly" or the "Twin Jet" nebula, is a bright bipolar nebula discovered by Minkowski (1947) and considered by many authors to be in the earliest stages of becoming a PN. In the optical, it shows a bright compact core from which two bilobed nested structures emerge oriented nearly north-south (Schwarz et al 1997;Clyne et al 2015). The brightness and morphology of the optical nebula have been changing notably on a timescale of a few years or less since its discovery (e.g., Allen & Swings 1972;van den Bergh 1974;Kohoutek & Surdej 1980;Doyle et al 2000).…”