Notes. The table shows spectral type, distance d, interstellar extinction A_V, effective temperature T_eff, stellar luminosity L_⋆, stellar mass M_⋆, age, and UV and X-ray luminosities without extinction, i.e. as seen by the disk. Numbers written A(−B) mean A × 10^−B. The UV and X-ray luminosities are listed in units of (L_⊙). ⁽¹⁾Spectral types, ages and stellar masses are consistent with evolutionary tracks for solar-metallicity premain sequence stars by Siess et al. (2000), using T_eff & L_⋆ as input, ⁽²⁾FUV luminosity from 91.2 to 205 nm, as seen by the disk, ⁽³⁾hard FUV luminosity from 91.2 to 111 nm, as seen by the disk, ⁽⁴⁾X-ray luminosity for photon energies > 0.1 keV, as seen by the disk, ⁽⁵⁾hard X-ray luminosity from 1 keV to 10 keV, as seen by the disk, ⁽⁶⁾no matching track, values from closest point at T_eff = 9650 K and L_⋆ = 42 L_⊙, ⁽⁷⁾no matching track, values from closest point at T_eff = 10 000 K and L_⋆ = 42 L_⊙, ⁽⁸⁾no UV data, model uses an UV-powerlaw with f_UV = 0.025 and p_UV = 0.2 (see Woitke et al. 2016) ⁽⁹⁾no detailed X-ray data available, model uses a bremsstrahlungs-spectrum with L_X = 8.8 × 10²⁸ erg s⁻¹ and T_X = 20 MK, based on archival XMM survey data (M. Güdel, priv. comm.), ⁽¹⁰⁾“low-UV state” model, where a purely photospheric spectrum is assumed, ⁽¹¹⁾no X-ray data available, X-ray data taken from HD 97048, ⁽¹²⁾no matching track, values from closest point at T_eff = 7050 K and L_⋆ = 7 L_⊙, ⁽¹³⁾no X-ray data available, ⁽¹⁴⁾resolved binary, 2× spectral type M1, luminosities 0.69 L_⊙ and 0.56 L_⊙, separation 0.094″ ≈ 13 AU (Hillenbrand & White 2004), ⁽¹⁵⁾derived from fitting our UV, photometric optical and X-ray data ⁽¹⁶⁾no matching track, values taken from (Drabek-Maunder et al. 2016; Kraus et al. 2012), ⁽¹⁷⁾no UV data, model uses f_UV = 0.01 and p_UV = 2 (see Woitke et al. 2016, Appendix A for explanations), ⁽¹⁸⁾no X-ray data, model uses L_X = 10³⁰ erg s⁻¹ and T_X = 20 MK (see Woitke et al. 2016, Appendix A for explanations).