EDP Sciences
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Volume 488, Number 3, September IV 2008
Page(s) L79 - L82
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200810529
Published online 08 August 2008

A&A 488, L79-L82 (2008)
DOI: 10.1051/0004-6361:200810529


Discovery of eclipsing binary central stars in the planetary nebulae M 3-16, H 2-29, and M 2-19

B. Miszalski1, 2, A. Acker1, A. F. J. Moffat3, Q. A. Parker2, 4, and A. Udalski5

1  Observatoire Astronomique, Université Louis Pasteur, 67000 Strasbourg, France
    e-mail: brent@newb6.u-strasbg.fr, acker@newb6.u-strasbg.fr
2  Department of Physics, Macquarie University, Sydney NSW 2109, Australia
    e-mail: qap@ics.mq.edu.au
3  Dépt. de physique, Univ. de Montréal CP 6128, Succ. Centre-Ville, Montréal, QC H3C 3J7, Canada
    e-mail: moffat@astro.umontreal.ca
4  Anglo-Australian Observatory, Epping, NSW 1710, Australia
5  Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warsaw, Poland
    e-mail: udalski@astrouw.edu.pl

Received 5 July 2008 / Accepted 4 August 2008

Progress in understanding the formation and evolution of planetary nebulae (PN) has been restricted by a paucity of well-determined central star masses. To address this deficiency we aim to (i) increase significantly the number of known eclipsing binary central stars of PN (CSPN); and subsequently (ii) measure directly their masses and absolute dimensions by combining their light curve parameters with planned radial velocity data. Using photometric data from the third phase of the Optical Gravitational Lensing Experiment (OGLE), we searched for periodic variability in a large sample of PN towards the Galactic Bulge using Fourier and phase-dispersion minimisation techniques. Among some dozen periodically variable CSPN found, we report on three new eclipsing binaries: M 3-16, H 2-29 and M 2-19. We present images, confirmatory spectroscopy and light curves of the systems.

Key words: stars: binaries: eclipsing -- ISM: planetary nebulae: general

© ESO 2008