Notes. - The valuesprovided in the column “Posterior" were derived in this work, except when specified otherwise in the column “Source". The references for these external sources are APASS DR9 (Henden et al. 2016), 2MASS (Skrutskie et al. 2006), GAIA-DR2 (Gaia Collaboration et al. 2018), K19 (Kostov et al. 2019), and BJ18 (Bailer-Jones et al. 2018). - The justifications of the choices of prior s can be found in Appendix D. These priors were used for all the analyses performed in Sects. 4.1.1, 4.1.2, and 4.2 with only one exception (see ^(‡) below).

- and stand for uniform and Jeffreys probability distributions, respectively, with vmin and vmax as the minimum and maximum values. JP stands for joint prior (see Appendix D for more details).

^(•) indicates that the parameter is a main or jumping parameter for the MCMC explorations performed in Sects. 4.1 to 4.2.2.

^(*) For the nontransiting planets, a is computed from a∕R_*.

^(†) For the prior of τ_decay, " + τ_decay, τ_decay > P_rot∕2" indicates an additional condition imposed on the prior of this parameter.

^(‡) The only exception to the fact that the prior s used are those provided in the column “Prior" of this table is for the ephemerides parameters P and t_ic of the three transiting planets in Sect. 4.1.2. In these cases, the prior s used are the posterior s obtained for these parameters during the analysis of the TESS LC alone (see Sect. 4.1.1). The prior s are , , , , , and .

^(§) The parameters reported for planetary candidate 5 are obtained from the analysis presented in Sect. 4.1.2. In contrast to the parameters of the other planets, which were obtained through the analysis described in Sect. 4.2.2, they do not include any condition related to dynamical stability.

^(¶) M_ref is the mean anomaly computed at the reference time 1354 BTJD, the time of the first TESS measurement.

^(||) As described inSect. 3.3, the abundance ratios [Mg/H] and [Si/H] are not directly measured on the observed spectra. They are statistical estimates obtained from a population of stars to which we believe L 98-59 belongs.