Volume 519, September 2010
|Number of page(s)||8|
|Section||Interstellar and circumstellar matter|
|Published online||14 September 2010|
The kinematics of the quadrupolar nebula M 1–75 and the identification of its central star*
Isaac Newton Group of Telescopes, Ap. de Correos 321, 38700 Sta. Cruz de la Palma, Spain e-mail: email@example.com
2 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
3 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
4 LAE, Université de Montréal, CP 6128 Succ. Centre Ville, Montréal, 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 Científicas, Madrid, Spain
7 Stockholm Observatory, Department of Astronomy, Stockholm University, AlbaNova, 106 91 Stockholm, Sweden
8 Centro de Astrobiología, CSIC-INTA, Ctra de Torrejón a Ajalvir km 4, 28850 Torrejón de Ardoz, Spain
9 Instituto de Física de Cantabria (CSIC-Universidad de Cantabria), 39005 Santander, Cantabria, Spain
10 Dpto. de Física Moderna, Universidad de Cantabria, Avda de los Castros s/n, 39005 Santander, Cantabria, Spain
Accepted: 2 June 2010
Context. The link between how bipolar planetary nebulae are shaped and their central stars is still poorly understood.
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 GHαFAS 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 ~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 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.
Key words: planetary nebulae: general / planetary nebulae: individual: M 1–75 / planetary nebulae: individual: PN G068.8-00.0 / ISM: kinematics and dynamics
© ESO, 2010
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