Notes. ⁽¹⁾3σ upper limit on the pulsed fraction of a signal in the 1 mHz–0.18 Hz range. ⁽²⁾3σ upper limit on the rms fractional variation in the 10 μHz–3 mHz range. ⁽³⁾Given the presence of the eclipse, for this observation we did not derive the rms fractional variation. ⁽⁴⁾For the light curves of this source we considered a bin time of 2000 s, given the lower count statistics. Correspondingly, the rms fractional variation is computed in the 10 μHz–0.5 mHz range.