Issue |
A&A
Volume 549, January 2013
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|
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Article Number | A30 | |
Number of page(s) | 14 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/201219601 | |
Published online | 11 December 2012 |
Online material
Summary of the light curves of WASP-3b analyzed in this work.
Central instants of WASP-3b transits estimated from all individual light curves.
Appendix A: A new eclipsing variable
A star in the WASP-3 field (UCAC3 ,
, epoch 2000.0; Zacharias et al. 2010), initially chosen as reference star, was found to be variable and was excluded from the reference list. A complete light curve of this variable was assembled by registering the magnitudes on the N1-2 and N4-N6 frames on a common zero point (Fig. A.1, upper panel). When folded on the P ≃ 0.3524 day peak detected in the Lomb-Scargle periodogram, the binned curve shows a periodical pattern with equal maxima and slightly different minima, typical of contact eclipsing binaries (W UMa-type; Fig. A.1, lower panel). We derived the following ephemeris, setting Φ = 0 at the phase of primary minimum and estimating uncertainties through a bootstrapping algorithm:
(A.1)This variable star appears to be unpublished, and we submitted it to the International Variable Star Index (identifier: VSX J183407.3+353859). Colors from catalog magnitudes: V = 15.63, R = 14.99 (NOMAD; Zacharias et al. 2004), J = 14.64, H = 14.34, Ks = 14.21 (2MASS; Skrutskie et al. 2006), and proper motions μαcosδ = −32 mas/yr, μδ = 19 mas/yr (UCAC3) suggest that this object could be a binary with both components of late-G spectral type.
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Fig. A.1
Light curve of a previously unreported R ~ 15 variable star in the WASP-3 field, classified as a contact eclipsing binary (see text for details). Top panel: unbinned data points folded on the best-fit period P = 0.353626 days. Different nights are coded in different colors. Bottom panel: same as above, binned on 0.02 intervals in phase. |
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© ESO, 2012
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