A comprehensive catalogue of high-mass X-ray binaries in the Large Magellanic Cloud detected during the first eROSITA all-sky survey

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Volume 707 (March 2026)

A&A, 707 (2026) A225

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Table 10

Best-fit parameters for CXOU J053600.0−673507.

Parameter	Model	Value
N_H (cm⁻²)	tbvarabs	(3.5±0.4)×10²¹
Γ	powerlaw	1.23±0.29
T_plasma (eV)	vapec	$405_{- 13}^{+ 14}$ $Mathematical equation: $405_{ - 13}^{ + 14}$$
O	vapec	${0.43}_{- 0.07}^{+ 0.08}$ $Mathematical equation: $0.43_{ - 0.07}^{ + 0.08}$$
Ne	vapec	0.83±0.08
Fe	vapec	${0.070}_{- 0.013}^{+ 0.014}$ $Mathematical equation: $0.070_{ - 0.013}^{ + 0.014}$$
norm_on	vapec	$({8.1}_{- 1.0}^{+ 1.2}) \times 10^{- 4}$ $Mathematical equation: $\left( {8.1_{ - 1.0}^{ + 1.2}} \right) \times {10^{ - 4}}$$
norm_off	vapec	$({4.9}_{- 0.5}^{+ 0.6}) \times 10^{- 4}$ $Mathematical equation: $\left( {4.9_{ - 0.5}^{ + 0.6}} \right) \times {10^{ - 4}}$$

Notes. Best-fit parameters for CXOU J053600.0−673507 using the Xspec model tbabs*tbvarabs*(pow+vapec) in the on-region and tbabs*tbvarabs*vapec in the off-region. tbabs and tbvarabs account for the MW foreground absorption and the local absorption, respectively, as described in Sect. 4.3. The PB contribution is added separately, using only the RMF, not the ARF. The normalisation of the PB is frozen to a value scaled by the BACKSCAL parameter of the respective spectral files and the one used for modelling the PB in Yeung et al. (2023). All element abundances not specified for the vapec model did not improve the fit and were set to the LMC value of 0.49. The subscripts on and o f f indicate model parameters in the on- and off-regions, respectively.

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