Phase-resolved XMM-Newton observations of the massive post-RLOF system HD 149404

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Table 2

Spectral fits of the EPIC and RGS spectra using 2-T plasma models with a 50–50 mix of primary and secondary winds.

Obs.	N_H	norm₁	norm₂	$χ_{v}^{2}$ $\[\chi_v^2\]$	d.o.f.	f_X (soft)	f_X (medium)	f_X (hard)

	(10²² cm⁻²)	(cm⁻⁵)	(cm⁻⁵)			(10⁻¹⁴ erg cm⁻² s⁻¹)
1	${0.48}_{- 0.03}^{+ 0.04}$ $\[0.48_{-0.03}^{+0.04}\]$	$({4.9}_{- 1.1}^{+ 1.4}) \times 10^{- 3}$ $\[\left(4.9_{-1.1}^{+1.4}\right) \times 10^{-3}\]$	$({1.24}_{- 0.04}^{+ 0.04}) \times 10^{- 3}$ $\[\left(1.24_{-0.04}^{+0.04}\right) \times 10^{-3}\]$	1.08	935	${29.2}_{- 0.5}^{+ 0.3}$ $\[29.2_{-0.5}^{+0.3}\]$	${31.5}_{- 0.4}^{+ 0.5}$ $\[31.5_{-0.4}^{+0.5}\]$	${6.5}_{- 0.1}^{+ 0.2}$ $\[6.5_{-0.1}^{+0.2}\]$
2	${0.41}_{- 0.04}^{+ 0.03}$ $\[0.41_{-0.04}^{+0.03}\]$	$({2.6}_{- 0.6}^{+ 0.7}) \times 10^{- 3}$ $\[\left(2.6_{-0.6}^{+0.7}\right) \times 10^{-3}\]$	$({0.84}_{- 0.03}^{+ 0.03}) \times 10^{- 3}$ $\[\left(0.84_{-0.03}^{+0.03}\right) \times 10^{-3}\]$	1.09	837	${22.5}_{- 0.4}^{+ 0.3}$ $\[22.5_{-0.4}^{+0.3}\]$	${22.2}_{- 0.4}^{+ 0.3}$ $\[22.2_{-0.4}^{+0.3}\]$	${4.5}_{- 0.1}^{+ 0.1}$ $\[4.5_{-0.1}^{+0.1}\]$
3	${0.51}_{- 0.04}^{+ 0.04}$ $\[0.51_{-0.04}^{+0.04}\]$	$({6.7}_{- 1.4}^{+ 1.8}) \times 10^{- 3}$ $\[\left(6.7_{-1.4}^{+1.8}\right) \times 10^{-3}\]$	$({1.29}_{- 0.04}^{+ 0.04}) \times 10^{- 3}$ $\[\left(1.29_{-0.04}^{+0.04}\right) \times 10^{-3}\]$	1.19	841	${31.3}_{- 0.5}^{+ 0.3}$ $\[31.3_{-0.5}^{+0.3}\]$	${33.4}_{- 0.4}^{+ 0.5}$ $\[33.4_{-0.4}^{+0.5}\]$	${6.8}_{- 0.1}^{+ 0.1}$ $\[6.8_{-0.1}^{+0.1}\]$

Notes. The model was defined as Eq. (1) with n = 2. The interstellar column was set to 3.72 × 10²¹ cm⁻² (Gudennavar et al. 2012), whereas the plasma temperatures were fixed to 0.20 and 0.65 keV. The abundances of C, N, and O were set respectively to 0.22, 6.26, and 0.83 times solar. All other abundances were fixed to solar following Asplund et al. (2009). The plasma normalisation parameters are equal to $\frac{10^{- 14}}{4 π d^{2}} \int n_{e} n_{H} d V$ $\[\frac{10^{-14}}{4 \pi \mathrm{d}^2} \int n_e ~n_{\mathrm{H}} \mathrm~{d} V\]$ in units cm⁻⁵ with d the distance to the source and ∫ n_e n_H dV the emission measure of the plasma. The last three columns yield the observed fluxes in the soft (0.5–1.0 keV), medium (1.0–2.0 keV), and hard (2.0–4.0 keV) energy bands.

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