The physics and kinematics of the evolved, interacting planetary nebula PN G342.0-01.7

Abstract

Integral field spectroscopy has been obtained for very few evolved planetary nebulae (PNe). Here we aim to study the physical and kinematical characteristics of the unstudied old planetary nebula PN G342.0-01.7, which shows evidence of interaction with its surrounding interstellar medium. We used integral field spectra from the Wide Field Spectrograph on the ANU 2.3 m telescope to provide spectroscopy across the whole object covering the spectral range 3400−7000 Å. We formed narrow-band images to investigate the excitation structure. The spectral analysis shows that the object is a distant Peimbert Type I planetary nebula (PN) of low excitation, formally of excitation class of 0.5. The low electron density, high dynamical age, and low surface brightness of the object confirm that it is observed fairly late in its evolution. It shows clear evidence for dredge-up of CN-processed material characteristic of its class. In addition, the low peculiar velocity of 7 km s −1 shows it to be a member of the young disk component of our Galaxy. We further determined an average expansion velocity of V exp = 20.2 ± 1.3 km s −1 , a local standard of rest radial velocity RV LSR = −27.7 ± 1.7 km s −1 , and a distance of 2.06±0.6 kpc for the object. We built a self-consistent photoionisation model for the PN matching the observed spectrum, the Hβ luminosity, and the diameter. On the basis of this we derive an effective temperature log T eff ∼ 5.05 and luminosity 1.85 < log L < 2.25. The temperature is much higher than might have been expected using the excitation class, proving that this can be misleading in classifying evolved PNe. PN G342.0-01.7 is in interaction with its surrounding interstellar medium through which the object is moving in the south-west direction. This interaction drives a slow shock into the outer PN ejecta. A shock model suggests that it only accounts for about 10% of the total luminosity, but has an important effect on the global spectrum of the PN.

Exploring the differences of integrated and spatially resolved analysis using integral field unit data: the case of Abell 14

“…However, only a few PNe had been observed and studied with IFS, the majority of them during the last 5-6 yr (e.g. Tsamis et al 2008;Danehkar et al 2013;Monteiro et al 2013;Danehkar et al 2014;Ali et al 2015Ali et al , 2016Danehkar 2015;Danehkar & Parker 2015;Basurah et al 2016;Danehkar et al 2016;Walsh et al 2016;Dopita et al 2017Dopita et al , 2018Walsh et al 2018;Ali & Dopita 2019) and imaging fourier transform spectroscopy (Lagrois et al 2015).…”

Deciphering the bipolar planetary nebula Abell 14 with 3D ionization and morphological studies

“…However, both studies agree that Abell 14 is an extremely nitrogenrich nebula with log(N/O) = 0.48 (B03) and 0.62 (H10). A similarly high N/O abundance ratio has been found in highly evolved bipolar PNe such as PN G321.6+02.2 (Corradi et al 1997), HaTr 10 (Tajitsu et al 1999, RCW 24 and RCW 69 (Frew et al 2006), and PN G342.0-01.7 (Ali et al 2015). Each of these PNe exhibits very low electron density (Ne) and very hot, optically faint central star, like that of Abell 14.…”

Physical and chemical properties of Wolf-Rayet planetary nebulae

“…WiFeS has recently been used for a number of southern Galactic PNe (e.g. Ali et al 2015Ali et al , 2016Basurah et al 2016;Dopita et al 2017).…”