Chandra high-resolution spectra of Apep Plume: Exploring the colliding-wind picture in X-rays

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Volume 693 (January 2025)

A&A, 693 (2025) A266

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Table 1.

Line parameters.

Line	λ_lab^(a)	FWHM ^(b)	Line shift ^(c)	Flux ^(d)	Ratio
	(Å)	(km s⁻¹)	(km s⁻¹)		(ATOMDB)
Fe XXV K_α	1.850	< 1000 ^(e)	669 ^(e)	27.20 $_{- 4.44}^{+ 4.81}$ $^{+4.81}_{-4.44}$
(i/r)				0.59 $_{- 0.31}^{+ 0.51}$ $^{+0.51}_{-0.31}$	0.38
(f/r)				0.52 $_{- 0.21}^{+ 0.32}$ $^{+0.32}_{-0.21}$	0.31
S XVI L_α	4.727	2447 $_{- 775}^{+ 885}$ $^{+885}_{-775}$	−139 $_{- 330}^{+ 332}$ $^{+332}_{-330}$	10.36 $_{- 2.97}^{+ 3.30}$ $^{+3.30}_{-2.97}$
Si XIV L_α	6.180	2830 $_{- 543}^{+ 678}$ $^{+678}_{-543}\phantom{0}$	−173 $_{- 227}^{+ 228}$ $^{+228}_{-227}$	10.64 $_{- 2.37}^{+ 2.80}$ $^{+2.80}_{-2.37}$

Notes. Results from the fits to the line profiles of emission lines in Apep Plume with the associated 1σ errors. The first-order MEG and HEG spectra were fitted simultaneously. For the He-like triplet (Fe XXV), the flux ratios of the intercombination to the resonance line (i/r) and of the forbidden to the resonance line (f/r) are given as well. The Cash statistic (Cash 1979) was adopted in the fits.

^(a)

The laboratory wavelength of the main component.

^(b)

The line width (full width at half-maximum, FWHM).

^(c)

The shift of the spectral line centroid.

^(d)

The observed total multiplet flux in units of 10⁻⁶ photons cm⁻² s⁻¹.

^(e)

Because of the poor photon statistics, these line parameters are not constrained.

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