| Issue |
A&A
Volume 405, Number 1, July I 2003
|
|
|---|---|---|
| Page(s) | 207 - 221 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20030531 | |
| Published online | 16 June 2003 | |
A search for planets in the metal-enriched binary HD 219542*
1
INAF – Osservatorio Astronomico di Padova, Vicolo dell' Osservatorio 5, 35122 Padova, Italy e-mail: gratton,claudi,lucatello@pd.astro.it
2
McDonald Observatory, The University of Texas at Austin, Austin, TX 78712, USA e-mail: mike@astro.as.utexas.edu
3
CISAS, c/o Dipartimento di Fisica, Università di Padova, via Marzolo 8, 35131 Padova, Italy e-mail: mauro.barbieri@pd.infn.it
4
INAF – Oss. Astrofisico di Catania, via S. Sofia 78, Catania, Italy e-mail: scuderi@ct.astro.it
5
INAF – Centro Galileo Galilei, calle Alvarez de Abreu 70, 38700 Santa Cruz de La Palma (TF), Spain e-mail: cosentino@tng.iac.es
6
Dipartimento di Astronomia, Universitá di Padova, Vicolo dell'Osservatorio 2, Padova, Italy
7
Dipartimento di Fisica, Universitá di Padova, via Marzolo 8, 35131 Padova, Italy e-mail: francesco.marzari@pd.infn.it
Corresponding author: S. Desidera, desidera@pd.astro.it
Received:
January
1900
Accepted:
21
March
2003
The components of the wide binary HD 219542 were recently
found to differ in metallicity by about 0.1 dex (Gratton
et al. [CITE]). In this paper, we present the
results of 2 years of high precision radial velocity
monitoring of these stars performed at the Telecopio Nazionale
Galileo (TNG) using the high resolution spectrograph SARG.
No indication for radial velocity variations above
the measurement errors (~5 m s-1) was found for the
metal richer component A. This allows us to place upper
mass-limits for planets around this star.
HD 219542 B instead shows a low amplitude
variation with a 112 day period at a confidence level
of ~
%.
This might suggest the presence of a Saturn-mass planet, although
it is still possible that these variations are due
to moderate activity of the star.
Tests based on variations of bisectors, stellar magnitude
and line equivalent widths were inconclusive so far.
Key words: stars: planetary systems / stars: binaries: visual / stars: individual: HD 219542 / stars: activity / techniques: radial velocities / techniques: spectroscopic
Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Centro Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, and observations collected at the European Southern Observatory, Chile, using FEROS spectrograph at 1.5 m telescope (proposal ID: 69.D-0338).
© ESO, 2003
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