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J/A+A/506/471     Frequency analysis of CoRoT B stars       (Degroote+, 2009)

CoRoT's view on newly discovered B-star pulsators: results for 358 candidate B pulsators from the initial run's exoplanet field data. Degroote P., Aerts C., Ollivier M., Miglio A., Debosscher J., Cuypers J., Briquet M., Montalban J., Thoul A, Noels A., De Cat P., Balaguer-Nunez L., Maceroni C., Ribas I., Auvergne M., Baglin A., Deleuil M., Weiss W., Jorda L., Baudin F., Samadi, R. <Astron. Astrophys. 506, 471 (2009)> =2009A&A...506..471D
ADC_Keywords: Stars, early-type ; Stars, B-type ; Stars, variable Keywords: methods: data analysis - stars: oscillations - stars: variable: general Abstract: We search for new variable B-type pulsators in the CoRoT data assembled primarily for planet detection, as part of CoRoT's Additional Programme. We aim to explore the properties of newly discovered B-type pulsators from the uninterrupted CoRoT spacebased photometry and to compare them with those of known members of the beta Cep and slowly pulsating B star (SPB) classes. We developed automated data analysis tools which include algorithms for jump correction, light curve detrending, frequency detection, frequency combination search and frequency and period spacing search. Besides numerous new classical slowly pulsating B stars, we find evidence for a new class of low-amplitude B-type pulsators between the SPB and delta Sct instability strips, with a very broad range of frequencies and low amplitudes, as well as several slowly pulsating B stars with residual excess power at frequencies typically a factor three above their expected g-mode frequencies. The frequency data we obtained for numerous new B-type pulsators represent an appropriate starting point for further theoretical analyses of these stars, once their effective temperature, gravity, rotation velocity and abundances will be derived spectroscopically in the framework of an ongoing FLAMES survey at VLT. Description: Results of frequency analyses for 352 candidate B pulsators (candidate Be stars are ommitted) from CoRoT's initial run. For each star, the following information is given: frequency number, amplitude + error, frequency value + error, phase + error. The error values for large amplitude frequencies can be slightly underestimated, as they are not corrected for correlation effects. Also given are comments about every frequency: if they are expected to be due to instrumental effects (e.g. orbit of the satellite), if they are harmonics or higher order combinations of previously identified frequencies. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file stars.dat 40 352 Star positions data/* 186 352 Frequency analysis for each star
See also: B/corot : CoRoT observation log (CoRoT, 2009) http://idoc-corot.ias.u-psud.fr/index.jsp : CoRoT Byte-by-byte Description of file: stars.dat
Bytes Format Units Label Explanations
1- 9 I9 --- CoRoT CoRoT star number 11- 17 F7.3 deg RAdeg Right ascension in decimal degrees (J2000) 19- 26 F8.5 deg DEdeg Declination in decimal degrees (J2000) 28- 40 A13 --- FileName Name of the file with frequency analysis in "data" subdirectory
Byte-by-byte Description of file: data/*
Bytes Format Units Label Explanations
1- 3 I3 --- nr Frequency number 8- 21 F14.10 mmag A Amplitude value 27- 39 F13.10 mmag e_A Mean error on the Amplitude value 44- 57 F14.10 1/d f Frequency value 63- 75 F13.10 1/d e_f Mean error on the frequency value 79- 87 F9.5 --- p ]-0.5,0.5] Phase value (in rad/2pi unit) 91- 99 F9.5 --- e_p Mean error on the phase value (in rad/2pi unit) 103-110 F8.3 --- S/N Signal-to-noise ratio, calculated over 6/d interval in the relevant periodogram (not the residual periodogram) 112-186 A75 --- Note Notes about the frequency (TeX format)
Acknowledgements: Pieter Degroote, pieter.degroote(at)ster.kuleuven.be
(End) Pieter Degroote [IvS Leuven, Belgium], Patricia Vannier [CDS] 02-Jun-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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