The extraordinary planetary nebula N66 in the LMC
M. Pena1, A. Peimbert1, W.-R. Hamann2, M. T. Ruiz3, M. Peimbert1
Morphology of the planetary nebula LMC-N66 (ionized by a [WN] star)
indicates that the nebula is a multipolar object with a very narrow
waist. It shows several jets, knots and filaments in opposite
directions from the central star. A couple of twisted long filaments
could be interpreted as due to point-symmetric type ejection. If such
is the case, the progenitor would be a binary precessing system. High
resolution spectroscopy shows that most of the material is approaching
or receding from the star. However the line profiles are very complex,
showing several components at different velocities. Our high resolution
spectroscopic data show that the different structures (knots, filaments,
...) present different radial velocities spreading from 240 to more
than 400 km/s. The system velocity is 300 km/s. There
are high velocity knots located to the north of the central star, moving
at more than 100 km/s relative to the system velocity.
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