Issue |
A&A
Volume 577, May 2015
|
|
---|---|---|
Article Number | A107 | |
Number of page(s) | 9 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361/201525875 | |
Published online | 12 May 2015 |
Online material
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Fig. 3
Same as Fig. 2 for BI 57 (a best-fitting double sinusoid, with the two periods of 787 d and 400 d is added in red in the left panel; these periods are indicated by tickmarks in the middle panel; prewhitening in the right panel was performed for P = 400 d). The potentially problematic OGLE-IV dataset (LMC532.08) is shown in green. |
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Fig. 5
Period search results for 2dFS 936. Left: comparison of the different period search methods. The presence of a signal is marked by a maximum for Fourier and AOV methods, but a minimum for conditional entropy, Renson and Lafler & Kinman methods. Middle: Fourier periodogram for the raw (top) and prewhitened (middle, for the best-fit Fourier period) data of 2dFS 936, along with the spectral window (bottom). Right: photometric variations of 2dFS 936, phased using the best-fit ephemeris (see Table 2). The thick red line corresponds to the best-fit Fourier sinusoid, while the symbols for data are as in Fig. 1. |
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Fig. 7
Same as Fig. 5 for LMC164-2 (see Table 2 for ephemeris). We note in the left panel the presence of peaks at frequencies corresponding to multiples of the fundamental period for all methods except Fourier, and in the middle panel the best-fit signal at 0.126 d-1, its second harmonic at 0.25 d-1, and their daily aliases at 0.87 d-1 and 0.75 d-1, respectively. |
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© ESO, 2015
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