Detection of non-linear resonances among gravity modes of slowly pulsating B stars: Results from five iterative pre-whitening strategies

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Volume 655 (November 2021)

A&A, 655 (2021) A59

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Table 1.

Five iterative pre-whitening strategies employed in this work.

Strategy	Hinting	Stop criterion	Final optimisation ^(a)
1	S/N	S/N < 4.0	Non-linear
2	A	p_A ^(b) > 0.05	Non-linear
3	A	p_LRT ^(c) > 0.05	Non-linear
4	S/N	p_LRT ^(c) > 0.05	Non-linear
5 ^(d)	A	p_LRT ^(c) > 0.05	Linear

Notes. Parameter hinting is performed by selecting either the highest-amplitude peak (A) in the residual LS periodogram (Lomb 1976; Scargle 1982) or the peak with the highest-amplitude S/N value using a 1 d⁻¹ window (S/N). The selected peak is not closer than 2.5/T to earlier extracted frequencies, where T is the total time span of the data (Loumos & Deeming 1978). Linear interpolation between the over-sampled frequency grid points of the LS periodogram is employed to determine the S/N value associated with the optimised frequency.

^(a)

Type of least-squares optimisation of the entire model at the end of each iterative pre-whitening step.

^(b)

The p-value for a Z-test based on extracted amplitude.

^(c)

The p-value for a LRT based on BIC values for the nested light curve regression models.

^(d)

The frequency extracted during the iterative pre-whitening step is optimised by selecting the largest-amplitude signal in an over-sampled LS periodogram in a 1 d⁻¹ region around the frequency hint.

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