Notes. Since all but one of the stars have an HD number, and these stars are known in the literature by their HD numbers, we have chosen to order the table by those in Col. 1. Column 2 gives the TESS Input Catalogue (TIC) number. Column 3 gives spectral classifications; all of those are some type of Ap star, since that was a selection criterion. Columns 4–6 give V, T_eff, and log g where there are estimates of those available. The uncertainties of T_eff and log g are likely to be 100s K and up to 0.3 dex, respectively; we have not rounded the values taken from the compilations to reflect these uncertainties. The data in Cols. 3–6 were taken from the TIC (version 8.0) or SIMBAD compilations. Column 7 indicates whether a star is a known roAp star. Column 8 gives information about the measured magnetic field strengths. All three values correspond to the mean over a rotation period (if known) or over the existing observations (otherwise) of the range spanned by each of the following magnetic field moments: ⟨B_z⟩_rms is the root-mean-square longitudinal field, as defined by Bohlender et al. (1993). It is essentially the quadratic mean of the mean longitudinal magnetic field. Since the latter is a signed quantity, and may reverse its sign over a rotation cycle, taking the quadratic mean is the way to avoid cancellation and to define a parameter that characterises the actual strength of the longitudinal field. We denote by B₀ the average value over a rotation cycle of the mean magnetic field modulus ⟨B⟩; this is the same quantity as listed in Col. 3 of Table 13 of Mathys (2017). The notation Q₀ refers to the average value over a rotation cycle of the mean quadratic magnetic field ⟨B_q⟩; this is the same quantity as listed in Col. 10 of Table 13 of Mathys (2017). Column 10 gives measurements for the stellar rotation periods, with the following column giving the references for those; the references are for compilations, where the original source reference can be found. Column 12 gives a comment on the width and the magnetic resolution of the spectral lines, from the source identified in Col. 13 (see text). Column 14, the penultimate column, gives various notes, including variable star names, primarily for the roAp stars, since the stars studied here, by definition, do not show rotational variation and hence are not α² CVn stars; that column also notes that some of these stars show δ Sct variations. The final column indicates in which TESS 27 d sectors the star was observed.

References. (1) Mathys (2017); (2) Mathys et al. (2019a); (3) Bagnulo et al. (2015); (4) Mathys & Hubrig (1997); (5) Medupe et al. (2015); (6) Hubrig et al. (2002); (7) Mathys (2019); (8) this paper (8/C: based on ESO-CES spectra; 8/F: based on ESO-FEROS spectra; 8/H: based on SALT-HRS spectrum).