Fig. E.1.
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Solar power spectrum for observation between 1999 and 2002 after Gaussian smoothing over a kernel width s = 50nHz. Superimposed is the best MCMC fit. Top panel: Highlight of a l = 2, 0, 3, 1 mode group (left to right) and their fit (red). The power asymmetry due to non-symmetric m-components is visible in the data. Top panel, inset: Overall view of the modes. Bottom panel: Residual of the fit with two levels of Gaussian smoothing.
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