Detalles de publicación
PP 010040
The kinematics of the quadrupolar nebula M 1–75 and the identification of its central star
1 Isaac Newton Group of Telescopes, Ap. de Correos 321, E-38700 Sta. Cruz de la Palma, Spaine-mail: msantander@ing.iac.es
2 Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain
3 Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain
4 LAE, Universit´e de Montr´eal, C.P. 6128 Succ. Centre Ville, Montr´eal, QC H3C 3J7, Canada
5 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester, M13 9PL, UK
6 Consejo Superior de Investigaciones Cient´ıficas, Madrid, Spain
7 Stockholm Observatory, Department of Astronomy, Stockholm University, AlbaNova, 106 91 Stockholm, Sweden
8 Centro de Astrobiolog´ıa, CSIC-INTA, Ctra de Torrej´on a Ajalvir km 4, E-28850 Torrej´on de Ardoz, Spain
9 Instituto de F´ısica de Cantabria (CSIC-Universidad de Cantabria), E-39005 Santander, Cantabria, Spain
10 Dpto. de F´ısica Moderna, Universidad de Cantabria, Avda de los Castros s/n, E-39005 Santander, Cantabria, Spain
Context. The link between the shaping of bipolar planetary nebulae and their central stars is still poorly understood.
Aims. The kinematics and shaping of the multipolar nebula M 1–75 are hereby investigated, and the location and nature of its central
star are briefly discussed.
Methods. Fabry-Perot data from GH FAS on the WHT sampling the Doppler shift of the [Nii] 658.3 nm line are used to study the
dynamics of the nebula, by means of a detailed 3-D spatio-kinematical model. Multi-wavelength images and spectra from the WFC
and IDS on the INT, and from ACAM on the WHT, allowed us to constrain the parameters of the central star.
Results. The two pairs of lobes, angularly separated by 22, were ejected simultaneously approx. 3500-5000 years ago, at the
adopted distance range from 3.5 to 5.0 kpc. The larger lobes show evidence of a slight degree of point symmetry. The shaping 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 which 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 which 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
Aims. The kinematics and shaping of the multipolar nebula M 1–75 are hereby investigated, and the location and nature of its central
star are briefly discussed.
Methods. Fabry-Perot data from GH FAS on the WHT sampling the Doppler shift of the [Nii] 658.3 nm line are used to study the
dynamics of the nebula, by means of a detailed 3-D spatio-kinematical model. Multi-wavelength images and spectra from the WFC
and IDS on the INT, and from ACAM on the WHT, allowed us to constrain the parameters of the central star.
Results. The two pairs of lobes, angularly separated by 22, were ejected simultaneously approx. 3500-5000 years ago, at the
adopted distance range from 3.5 to 5.0 kpc. The larger lobes show evidence of a slight degree of point symmetry. The shaping 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 which 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 which 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