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Astron. Astrophys. 337, 198-206 (1998)
New multi-site observations of the ![[FORMULA]](../../../entities/ldelta.gif)
Scuti stars BS and BT Cancri
Results of the STEPHI VII campaign on the Praesepe cluster
M.M. Hernández 1,
E. Michel 2,
J.A. Belmonte 1,
S.Y. Jiang 3,
M. Álvarez 4,
M. Chevreton 5,
M. Paparó 6,
H. Kjeldsen 7,
D. Bauduin 2,
J. Fromage 2,
M.J. Goupil 2,
Z.P. Li 3,
Y.Y. Liu 3,
A. Mangeney 8,
G. Massacrier 9,
O. Ringot 2,
T. Roca Cortés 1,
B. Servan 2 and
I. Vidal 1
1 Instituto de Astrofísica de Canarias, E-38200 La
Laguna, Tenerife, Spain
2 Observatoire de Paris-Meudon, DASGAL, URA CNRS 335,
F-92195 Meudon, France
3 Beijing Observatory, Chinese Academy of Sciences,
Beijing, P.R. China
4 Instituto de Astronomía de la UNAM, Ap.P. 877,
Ensenada, BC, Mexico
5 Observatoire de Paris-Meudon, DAEC, F-92195 Meudon,
France
6 Konkoly Observatory, Hungarian Academy of Sciences, P.O.
Box 67, H-1525 Budapest, Hungary
7 Institute of Physics and Astronomy, Aarhus University,
Bygn. 520, DK-8000 Aarhus C, Denmark
8 Observatoire de Paris-Meudon, DESPA, F-92195 Meudon,
France
9 Centre de Recherche Astronomique de Lyon, CNRS-UMR 5574,
ENS Lyon, F-69364 Lyon, France
Received 22 April 1998 / Accepted 4 June 1998
Abstract
New observations of BS and BT Cnc were performed during the STEPHI
VII campaign in 1996 February. An overall run of 115 hours of data was
collected. Different methods have been used to analyse the time
series, bringing the detection of 2 frequencies for BT Cnc and 3
frequencies for BS Cnc above the 99% confidence level. A comparison
with the literature reveals that the dominant mode of BT Cnc
(![[FORMULA]](img2.gif)
9.8 c/d) has kept excited over tens of years,
while the secondary modes have not been the same all the time.
However, during the very last years the two frequencies detected by us
have been the only ones noticeably excited in the spectrum.
Key words: stars:
oscillations 
Scu
open clusters and associations: individual :
Praesepe
stars: individual: BS Cnc; BT Cnc
Send offprint requests to: M.M. Hernández, (mmanuel@iac.es)
Contents
- 1. Introduction
- 2. The target stars: BS and BT Cnc
- 3. The observations
- 4. Frequency analysis of the time series
- 4.1. Comparative analysis of different methods
- 4.1.1. ISWF
- 4.1.2. ISWF with statistical weights
- 4.1.3. MUFRAN
- 4.2. Effect of using different filters in the same time series
- 4.1. Comparative analysis of different methods
- 5. Discussion of results
- 6. Conclusions
- Acknowledgements
- References
© European Southern Observatory (ESO) 1998
Online publication: August 6, 1998
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