The phase curve of the ultra-hot Jupiter WASP-167b as seen by TESS

Open Access

Fig. 3

Best-fit A_g, I_p/I_★, ε, occultation depth, and R_p/R_★ as a function of the number of sinusoidal curves subtracted from the light curve. The dashed lines correspond to the 1σ uncertainty of the parameters obtained from the Φ₁₆(t) LC.

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