Notes. The composite phenomenological model fitted to the data consists of an absorbed double blackbody plus power-law continuum, modified by a Gaussian absorption line, with [i, ii, iii] and without [1, 2] an edge component. The latter is introduced to take strong residuals at low energies, predominantly in eROSITA data (see the text for details), into account. Errors are 1σ confidence levels.^(†) We either performed a simple fit of TM8 [1, i, iii] or a simultaneous fit of the five data sets: TM8, XMM-Newton pn (2015, 2019), NuSTAR (both telescope units) [2, ii]. In [iii] we refit TM8 with a fixed power-law slope = 1.98, as found in the joint fit. The renormalization factors of the simultaneous fit [2] with respect to the TM8 dataset are 1.0267(27), 1.0058(29), , for pn (2015), pn (2019), and the two NuSTAR modules, respectively. The same factors are 0.951(4), 0.933(4), and for fit [ii]. ^(a)The column density is in units of 10²⁰ cm⁻². ^(b)The radiation radius at infinity for each blackbody component was computed assuming a distance of 288 pc. ^(c)The observed model flux is in units of 10⁻¹¹ erg s⁻¹ cm⁻² in energy band 0.2–12 keV. ^(*)Parameter kept frozen during the fitting.