Notes. The stars are ordered by increasing TIC number, as given in Col. 1. The HD numbers are listed in Col. 2, as alternative identifications. The spectral types appearing in Col. 3 are from the Renson catalogue; the V magnitudes in Col. 4 were extracted from SIMBAD; the effective temperatures T_eff and surface gravities log g in Cols. 5 and 6 were taken from the TIC. The roAp stars (see Sect. 3) are identified in Col. 7. Column 8 presents the magnetic data available in the literature, with the relevant references in Col. 9. The values of up to three magnetic moments are given; all of them correspond to the mean of the respective moment over a rotation period (if known and adequately sampled by the existing measurements) or over the observations that have been obtained (otherwise). The first one is the root-mean square longitudinal magnetic field, ⟨B_z⟩_rms, as defined by Bohlender et al. (1993). In essence, this is the quadratic mean of the mean longitudinal magnetic field (the line-intensity weighted average over the stellar disc of the component of the magnetic vector along the line of sight). The second one is the average value B₀ over a rotation cycle of the mean magnetic field modulus ⟨B⟩ (that is, the same quantity as listed in Col. 3 of Table 13 of Mathys 2017). The third field moment, Q₀, is the average value over a rotation period of the mean quadratic magnetic field ⟨B_q⟩; this is the same quantity as appearing in Col. 10 of Table 13 of Mathys (2017). The period values from the literature appear in Col. 10. They come from the references specified in Col. 11. Column 12 contains the v sin i values (as numbers), when they could be found, or indications about the resolution or width of the spectral lines (as letters). The references from which this information originates appear in Col. 13. For some stars, a note was added in Col. 14. The last column indicates in which TESS 27-d sectors the data analysed in this study were obtained.

References. (1) Romanyuk et al. (2017); (2) Giarrusso et al. (2022); (3) Mathys (2017); (4) Mathys et al. (1997); (5) Ryabchikova & Romanovskaya (2017); (6) Abt & Morrell (1995); (7) Elkin et al. (2012); (8) Levato et al. (1996); (9) Sikora et al. (2019); (10) Ryabchikova et al. (2000); (11) Kochukhov et al. (2002); (12) Leone et al. (2003); (13) Bychkov et al. (2016); (14) Scholz (1979); (15) Wraight et al. (2012); (16) Freyhammer et al. (2008); (17) Zorec & Royer (2012); (18) Bagnulo et al. (2003); (19) Bagnulo et al. (2006).