Sharpening quasar absorption lines with ESPRESSO - Temperature of warm gas at z ∼ 2, constraints on the Mg isotopic ratio, and structure of cold gas at z ∼ 0.5

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Volume 651 (July 2021)

A&A, 651 (2021) A78

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Table 2.

Absorption lines identified in the ESPRESSO spectrum of HE 0001−2340.

z_abs^(a)	v_range^(b)	Species	Line IDs
	(km s⁻¹)		(Å)
0.00001		Na I	5891, 5897
0.27052		Ca II	3934, 3969
0.45206	[0, +150]	Fe I	2719, 2967, 3021, 3441
			3720, 3825, 3861
		Mg II	2796, 2083
		Mg I	2852
		Ca II	3934, 3969
		Ca I	4227
0.94902	[−60, +130]	Mg II	2796, 2803
		Mg I	2852
		Fe II	2586, 2600, 2344, 2382
1.58643	[−200, +150]	C IV	1548, 1550
		Mg II	2796, 2803
		Mg I	2852
		Si II	1526
		Fe II	1608, 2344, 2374, 2382
			2586, 2600
1.65147	[−40, +40]	C IV	1548, 1550
		Si II	1526
		Al III	1854, 1862
		Mg II	2796, 2803
		Mg I	2852
1.66602	[−100, +120]	C IV	1548, 1550
1.72721		C IV	1548, 1550
1.82737	[−40, +50]	C IV	1548, 1550
		Si IV	1393, 1402
2.03228	[−50, +50]	C IV	1548, 1550
2.18716	[−450, +30]	H I	1215
		DI	1215
		C IV	1548, 1550
		Si II	1260, 1304, 1526
		Fe II	1260, 1608, 2344, 2374
			2382
		O I	1302
		C II	1334
		Si IV	1392, 1402
		Al II	1670
		Al III	1854, 1682
2.25710		C IV	1548, 1550

Notes.

^(a)

Redshifts marked in bold face correspond to systems considered in this work.

^(b)

In case of an absorption complex spread over more than a few tens of km s⁻¹, we provide in this column the velocity range over which components are detected (with respect to the main absorption redshift given in the first column).

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