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Table 1.

FUV WHIM absorbers in the sight line to blazar PKS 2155–304.

IDa zFUVb Line
zX-rayc λ(O VII Heα)d λ(O VIII Lyα)d
Metal
BLA
Ion EWe logN(cm−2)f EWg bh logN(cm−2)i
(mÅ) (mÅ) (km s−1) (Å) (Å)
A1 0.00878 49 ± 8 59 ± 8 13.0 ± 0.1 0.00878 21.79 19.14
A2 0.01892 59 ± 4 38 ± 4 13.0 ± 0.1 0.01892 22.01 19.33
A3aj 0.05405 O VI 32 ± 5k, 30 ± 9k 13.6 ± 0.1 315 ± 4 44 ± 0 14.1 ± 0.1 0.05425 22.77 20.00
A3bj 0.05445 60 ± 31 54 ± 7 13.0 ± 0.1
A4aj 0.05659 477 ± 10 48 ± 1 14.5 ± 0.3 0.05683 22.83 20.05
A4bj 0.05707 O VI 44 ± 11l 13.6 ± 0.1 424 ± 11 68 ± 1 14.0 ± 0.0
A5 0.08062 Si IV 12 ± 4m 12.1±0.1 29 ± 5 40 ± 5 12.7 ± 0.1 0.08062 (23.34)n 20.50
A6aj 0.10552 360 ± 7 54 ± 1 14.1 ± 0.2 0.10569 23.83 20.97
A6bj 0.10586 156 ± 22 66 ± 4 13.5 ± 0.0

Notes.

(a)

Name of absorber.

(b)

Redshift of FUV absorber.

(c)

Our adopted redshift for the X-ray follow-up.

(d)

Redshifted wavelength of O VII Heα and O VIII Lyα.

(e)

Equivalent width of the metal line.

(f)

Column density of the metal line.

(g)

Equivalent width of the BLA.

(h)

Doppler parameter of the BLA.

(i)

Column density of the BLA.

(j)

Two FUV absorbers at the same WHIM structure candidate are shown separately.

(k)

Equivalent width of the O VI 1031.9 Å and 1037.6 Å transitions, respectively.

(l)

Equivalent width of the only significantly detected O VI 1031.9 Å transition.

(m)

Equivalent width of the only significantly detected Si IV 1393.8 Å transition.

(n)

The possible A5 O VIII line would land at problematic wavelengths due to astrophysical and instrumental oxygen edges which prevents an accurate modelling; we therefore excluded this line from further analyses.

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