Multiwavelength campaign on Mrk 509 - VIII. Location of the X-ray absorber

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Table 3

Strongest contributions to the dominant absorption troughs for components C, D, and E.

Comp	Ion and dominant	λ ^a	E ^b	W ₁ ^c	W ₂ ^d	ΔW^e
	transition/blend	(Å)	(keV)	(eV)	(eV)	(eV)

C	O vii 1s–3p...7p	18.63	0.663	0.99	0.75	−0.24
C	Fe ix	16.54	0.721	0.17	0.06	−0.11
C	Fe x	16.36	0.729	0.52	0.23	−0.29
C	Fe xi	16.18	0.738	0.84	0.43	−0.41
C	Fe xii	16.03	0.745	0.69	0.53	−0.16
C	Fe xiii	15.89	0.756	0.60	0.55	−0.05
C	Fe xiv	15.63	0.767	0.27	0.32	+0.05
C	O viii 1s–3p,4p,5p	16.01	0.768	1.58	1.50	−0.06
C	Fe xv	15.36	0.777	0.16	0.23	+0.07
C	Fe xvi	15.26	0.786	0.13	0.22	+0.09
C	Fe xvii 2p–3s,3d	15.01	0.789	0.57	1.07	+0.50

D	O viii 1s–3p,4p,5p	16.01	0.766	0.41	0.26	−0.15
D	Fe xvii	15.01	0.794	0.47	0.25	−0.22
D	Fe xviii	14.20	0.836	1.27	0.89	−0.38
D	Fe xix	13.52	0.881	1.54	1.41	−0.13
D	Ne ix 1s–2p	13.45	0.891	0.20	0.11	−0.09
D	Fe xx 2p-3d	12.84	0.929	0.65	0.86	+0.21

E	Fe xx 2p–3d	12.84	0.935	0.07	0.00	−0.07
E	Ne x 1s–2p	12.13	0.987	0.66	0.46	−0.16
E	Fe xxi 2p–3d	12.29	0.987	0.40	0.07	−0.33
E	Fe xxii 2s–3p	11.71	1.038	0.84	0.19	−0.65
E	Fe xxiii 2s–3p	10.98	1.092	1.01	0.47	−0.54
E	Fe xxiv 2s–3p	10.62	1.127	1.06	0.76	−0.30

Notes.

^(a)

Laboratory wavelength of the strongest individual spectral line of the ion that contributes to the blend.

^(b)

Predicted energy of the line centroid of all lines from the given ion that contribute to the blend, in the observer’s frame (thus accounting for cosmological redshift).

^(c)

Total equivalent width of all the lines of the ion contributing to the blend, for the parameters of the time-averaged spectrum (see Table 1).

^(d)

As above, but for log ξ higher by 0.1 dex.

^(e)

Difference in equivalent width for the case with a higher ionisation parameter compared with the time-averaged spectrum.

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