Abstract
Spatially resolved observations of the planetary nebula M2-42 (PN G008.2-04.8) obtained with the Wide Field Spectrograph on the Australian National University 2.3 m telescope have revealed the remarkable features of bipolar collimated jets emerging from its main structure. Velocity-resolved channel maps derived from the [N II] $\lambda$6584 emission line disentangle different morphological components of the nebula. This information is used to develop a three-dimensional morpho-kinematic model, which consists of an equatorial dense torus and a pair of asymmetric bipolar outflows. The expansion velocity of about 20 km s$^{-1}$ is measured from the spectrum integrated over the main shell. However, the deprojected velocities of the jets are found to be in the range of 80-160 km s$^{-1}$ with respect to the nebular center. It is found that the mean density of the collimated outflows, 595 $\pm$ 125 cm$^{-3}$, is five times lower than that of the main shell, 3150 cm$^{-3}$, whereas their singly ionized nitrogen and sulfur abundances are about three times higher than those determined from the dense shell. The results indicate that the features of the collimated jets are typical of fast, low-ionization emission regions.
Highlights
M2-42 ( = PN G008.2−04.8 = Hen 2-393 = VV 177 = Sa 2-331) was discovered as a planetary nebula (PN) by Minkowski (1947)
We present the spatially resolved observations of M2-42 obtained with the Wide Field Spectrograph (WiFeS) on the Australian National University (ANU) 2.3 m telescope
Using the velocity-resolved channel maps derived from the [N ii] λ6584 emission line, a morpho-kinematic model has been developed which includes different morphological components of the nebula: a dense torus and a pair of asymmetric bipolar outflows in opposite directions
Summary
We estimate a distance of 7400+−557500 from the Hα surface brightness-radius relation for a sample of 332 PNe (Frew et al 2016), total flux value of log F (Hα) = −11.39 erg cm−2 s−1 (Frew et al 2013), c(Hβ)= 0.99 (Wang & Liu 2007), and angular radius of 2 arcsec (Stanghellini et al 2008). It could be a Galactic Bulge PN (GBPN).
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