All Tables

Table 1: Top: V magnitude, parallax and absolute magnitude of HD 223460. Middle: spectral type, color indices and effective temperature. Bottom: estimated stellar parameters of HD 223460.
Table 2: HD 223460 observation log during XMM-Newton revolutions 107 and 200.
Table 3: X-ray luminosities (corrected for interstellar absorption) of HD 223460 in the 0.3-2 keV and 2-10 keV measured with the combined EPIC MOS and pn cameras. The percentage contribution in luminosity of hot plasmas (kT> 1 keV) is indicated between bracketts. The hardness ratio (hr) is defined as $hr = (L_{\rm >2~ ~keV}-L_{\rm 0.3-2~~keV})/(L_{\rm >2 ~keV}+L_{\rm 0.3- 2~keV})$ .
Table 4: Best fit parameters to EPIC data using a 2 components MEKAL model (Mewe et al. 1985) with variable abundance and a variable hydrogen column density.
Table 5: Best fit parameters to EPIC data using a 3 components MEKAL model (Mewe et al. 1985) with variable abundance and a variable hydrogen column density.
Table 6: Best fit parameters to RGS spectra in the 0.5-1.3 keV range recorded in revolutions 107 (upper table) and 200 (lower table) using a three components VMEKAL model. The temperature of each component were frozen to the value derived from the analysis of EPIC data (see Table 5). The metallicity was left free to vary. The oxygen and neon abundances were first tied to the abundance of the other elements (MODEL A). There were then left free to vary independently but with the same value for the different temperature components (MODEL B). In MODEL C, the hottest temperature component has been replaced by a VMEKAL component at $4 \times 10^{6}$ K where the Ne IX line is formed.
Table 7: Measured positions and flux estimate or upper limits of the strongest lines in the RGS spectra of HD 223460 obtained during revolutions 107 and 200. The columns give the predicted line positions, the measured line positions during revolution 107, the measured line positions during revolution 200, the ion and line identifications, the temperatures of maximum line formation, the line fluxes measured during revolution 107 and the line fluxes measured during revolution 200.
Table 8: Physical parameters of HD 223460 coronal loops derived from the XMM-Newton observations conducted during revolution 107 and 200. The electron density is derived from Eq. (1), i.e. $n_{\rm e} = 2 \times \sqrt { EM/(4 \pi \times GF \times R^{2} \times L)}$ .