To be or not to be: the case of the hot WHIM absorption in the blazar PKS 2155–304 sight line

J. Nevalainen; E. Tempel; J. Ahoranta; L. J. Liivamägi; M. Bonamente; E. Tilton; J. Kaastra; T. Fang; P. Heinämäki; E. Saar; A. Finoguenov

doi:10.1051/0004-6361/201833109

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Volume 621 (January 2019)

A&A, 621 (2019) A88

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Table 4.

Tests of LETG/ACIS data at λ ∼ 20 Å.

Sample	λ	EW
	Å	mÅ
W07±^a	20.03 ± 0.01	8.2 ± 2.3
W07+^b	20.03 ± 0.01	6.5 ± 2.7
W07−^c	20.02 ± 0.01	13.4 ± 5.0
3669^d	20.01^g	6.9 ± 3.2
Final^e	20.02 ± 0.01	6.0 ± 1.9
Final and 3669^f	20.02 ± 0.01	6.2 ± 1.7

Notes.

^(a)

Observations used in Williams et al. (2007), positive and negative first orders co-added.

^(b)

Observations used in Williams et al. (2007), but only positive first order.

^(c)

Observations used in Williams et al. (2007), but only negative first order.

^(d)

Large pointing offset observation 3669.

^(e)

Using all the public data in Oct 2017 obtained with Δy = +1.5 arcmin and SIM − Z = −8 mm.

^(f)

Combining the results of the final sample and of the observation 3669.

^(g)

After correcting the wavelength scale as indicated by the shift of the wavelength of the Galactic O I line.

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