Volume 619, November 2018
|Number of page(s)||8|
|Section||Stellar structure and evolution|
|Published online||08 November 2018|
When nature tries to trick us
An eclipsing eccentric close binary superposed on the central star of the planetary nebula M 3-2⋆,⋆⋆
European Southern Observatory, Karl-Schwarzschild-str. 2, 85748 Garching, Germany
2 Instituto de Astrofísica de Canarias, Vía Láctea s/n, 38200 La Laguna, Tenerife, Spain
3 Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
4 Department of Physics and Astronomy, University College London, Gower St, London, WC1E 6BT, UK
5 Las Campanas Observatory, Carnegie Institution of Washington, La Serena, Chile
6 South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa
7 Southern African Large Telescope Foundation, PO Box 9, Observatory 7935, South Africa
8 European Southern Observatory, Alonso de Córdova 3107, Casilla, 19001, Santiago Chile
9 Departamento de Ciencias Físicas, Universidad Andres Bello, Fernández Concha 700, Las Condes, Santiago
10 GRANTECAN, Cuesta de San José s/n, 38712 Breña Baja, La Palma, Spain
11 Observatorio Astronómico Nacional (OAN-IGN), C/Alfonso XII 3, 28014 Madrid, Spain
Accepted: 27 July 2018
Bipolar planetary nebulae (PNe) are thought to result from binary star interactions and, indeed, tens of binary central stars of PNe have been found, in particular using photometric time-series that allow for the detection of post-common envelope systems. Using photometry at the NTT in La Silla we have studied the bright object close to the centre of PN M 3-2 and found it to be an eclipsing binary with an orbital period of 1.88 days. However, the components of the binary appear to be two A or F stars, of almost equal mass, and are therefore too cold to be the source of ionisation of the nebula. Using deep images of the central star obtained in good seeing conditions, we confirm a previous result that the central star is more likely much fainter, located 2″ away from the bright star. The eclipsing binary is thus a chance alignment on top of the planetary nebula. We also studied the nebular abundance and confirm it to be a Type I PN.
Key words: methods: observational / binaries: eclipsing / stars: early-type / planetary nebulae: individual: PN G240.3-07.6 / stars: AGB and post-AGB
Based on ESO observations made under programmes 088.D-0573(A), 090.D-0435(A), 090.D-0693(A), 091.D-0475(A), 092.D-0449(A), 094.D-0031(A), 094.D-0031(A), and 096.D-0237(A).
Tables A.1 and A.2 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/619/A84
© ESO 2018
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.