A survey of extremely metal-poor gas at cosmic noon - Evidence of elevated [O/Fe]

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Volume 691 (November 2024)

A&A, 691 (2024) A285

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Table 1.

Journal of observations associated with our sample.

QSO	m_r	z_em	z_abs	Telescope/	Wavelength	Resolution	Integration	S/N ^(b)	Program
	(mag)			instrument	range ^(a) (Å)	(km s⁻¹)	time (s)		ID
J0140−0839	17.75	3.72	3.697	VLT/UVES	3050–10 430	8.3	12 000	30	080.A-0014(A)
				VLT/UVES	3760–10 430	7.3	60 000	51	105.20L3001
J0239−0649	18.66	2.49	2.416	VLT/UVES	3755–9465	7.3	18 000	11	108.222R.001
J0903+2628	18.98	3.22	3.078	Keck/HIRES	3840–6715	6.3	32 400	20	N162Hb, C230Hb
				Keck/HIRES	3245–7805	6.3	32 400	36	R351
J1001+0343	19.02	3.20	3.078	VLT/UVES	3282–6655	7.3	33 700	28	083.A-0042(A)
				VLT/UVES	3756–10 429	7.3	24 000	15	105.20L3.001
J1147+5034	19.45	2.52	2.519	Keck/HIRES	4070–8760	6.3	18 000	22	R304
J1358+0349	18.64	2.89	2.853	VLT/UVES	3285–9460	7.3	21 600	30	111.24LY.001
				VLT/UVES	3450–6645	6.4	24 000	30	093.A-0016(A)
				Keck/HIRES	3480–6345	6.2	24 000	–	H228Hb
J2150+0331	19.12	2.79	2.697	VLT/UVES	3760–9465	7.3	30 000	11	110.23R3.002
J2308+0854	19.40	2.77	2.768	VLT/UVES	3285–9465	7.3	36 000	19	108.222R.002

Notes.

^(a)

With some wavelength gaps.

^(b)

Near the bluest accessible Fe II line – typically λ1608 or λ2344. This is left empty if an Fe II feature is not covered. In the case of Fe IIλ1608, this is often the weakest line we cover and so it is a useful indicator of the quality of these data.

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