EDP Sciences
Free access
Issue
A&A
Volume 405, Number 1, July I 2003
Page(s) 207 - 221
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20030531


A&A 405, 207-221 (2003)
DOI: 10.1051/0004-6361:20030531

A search for planets in the metal-enriched binary HD 219542

S. Desidera1, R. G. Gratton1, M. Endl2, M. Barbieri3, R. U. Claudi1, R. Cosentino4, 5, S. Lucatello1, 6, F. Marzari7 and S. Scuderi3

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

(Received 3 Febraury 2003 / Accepted 21 March 2003 )

Abstract
The components of the wide binary HD 219542 were recently found to differ in metallicity by about 0.1 dex (Gratton et al. 2001b). 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 ~ 96-97%. 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

Offprint request: S. Desidera, desidera@pd.astro.it

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