Abstract
Spectroscopic mapping of planetary nebulae (PNe) is particularly useful to capture the richness in terms of physical and chemical properties that exist in these objects. The advent of the multi-unit spectroscopic explorer (MUSE), a large integral field unit mounted on the ESO Very Large Telescope, allow us to obtain this information over the whole face of galactic PNe in a reasonable amount of time. This in turn reveals a wealth of information that can bring insight into this structural complexity. Here we discuss new results from commissioning data for the physical properties of IC 418 and succinctly review recently published results on two additional targets (NGC 3132 and NGC 7009). For the newly-analysed PN, electron densities are high with ne([S ii]) displaying a completely different structure than ne([Cl iii]). The electron temperature was relatively uniform, but somewhat higher at the rim as measured by two of the three used diagnostics ([S iii] 6312/9069, and [Ar iii] 5192/7136). The joint results for the three PNe amply illustrate the potential of MUSE for the study of galactic PNe.
Highlights
Planetary nebulae (PNe), extended ionised nebulae emerging from the evolution of low-mass (
These were not reflected in the header and were determined a posteriori by comparing continuum and emission line maps derived from the different data sets
It is worth noticing that with only .0.5 h of telescope time, several lines are clearly detected in the halo. This was one of the first set of data taken with this instrument and in that sense, the optimal observing protocols to observe with multi-unit spectroscopic explorer (MUSE) in general, and PNe in particular, were not at play
Summary
Planetary nebulae (PNe), extended ionised nebulae emerging from the evolution of low-mass (
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