Aims. This paper investigates the kinematics and shaping of the multipolar nebula M 1-75, and briefly discusses the location and nature of its central star.
Methods. Fabry-Perot data from GH alpha FAS on the WHT that samples the Doppler shift of the [NII] 658.3 nm line are used to study the dynamics of the nebula by means of a detailed 3D spatio-kinematical model. Multi-wavelength images and spectra from the WFC and IDS on the INT, as well as from ACAM on the WHT, allowed us to constrain the parameters of the central star.
Results. The two pairs of lobes, angularly separated by similar to 22 degrees, were ejected simultaneously approx. similar to 3500-5000 years ago, at the adopted distance range from 3.5 to 5.0 kpc. The larger lobes show a slight degree of point symmetry. The formation of the nebula could be explained by wind interaction in a system consisting of a post-AGB star surrounded by a disc warped by radiative instabilities. This requires the system to be a close binary or a single star that engulfed a planet as it died. On the other hand, we present broad- and narrow-band images and a low S/N optical spectrum of the highly-reddened, previously unnoticed star that is likely the nebular progenitor. Its estimated V-I colour allows us to derive a rough estimate of the parameters and nature of the central star.
2010. Vol. 519, A54- p.
planetary nebulae: general, planetary nebulae: individual: M 1-75, planetary nebulae: individual: PN G068.8-00.0, ISM: kinematics and dynamics