The clumpy absorber in the high-mass X-ray binary Vela X-1

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Volume 608 (December 2017)

A&A, 608 (2017) A143

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Table 7

Neon lines in the low- and high-hardness spectra.

		Reference	Bayesian	v	Line	Equivalent	Value
		wavelength	Blocks α_sig		flux	width
		[Å]		[ km s^-1]	[ph s^-1 cm^-2 × 10^-5]	[Å]

High hardness	Ne x Lyα	12.1338^d	3.4	−220 ± 70		–	–
	Ne x Lyβ	10.23887^d	2	= v _{Ne x Lyα}		–	–
	Ne ix i	13.5520^e	2.5	= v _{Ne x Lyα}		–	–
	R ratio^c	–	–	–	–	–	^g
	G ratio^c	–	–	–	–	–	^g

Low hardness	Ne x Lyα	12.1338^d	4.6			–	–
	Ne x Lyβ	10.23887^d	no^a		–		–
	Ne ix r	13.4476^e	5^b	= v _{Ne x Lyα}		–	–
	Ne ix i	13.5520^e	5^b	= v _{Ne x Lyα}		–	–
	Ne ix f	13.6993^e	5^b	= v _{Ne x Lyα}		–	–
	Ne viii Kα	13.647^f	5^b	−220 ± 140	–		–

Notes.

^(a)

We run line searches for α ≥ 1.5.

^(b)

The He-like triplet emission lines and the Li-like absorption line are detected as one complex-shaped feature.

^(c)

All three triplet lines are assumed to have the same velocity.

^(d)

Erickson (1977).

^(e)

Drake (1988); for a discussion of errors on Drake (1988) values, see Notes to Table 4.

^(f)

Behar & Netzer (2002).

^(g)

These ratios formally correspond to fluxes of 2.4 × 10^-5 ph s^-1 cm^-2 for Ne ix f and 0.7 × 10^-5 ph s^-1 cm^-2 for Ne ix r.

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