Low-density laboratory spectra near the He ii λ304 line

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Table A.1

Lines observed in EBIT within the wavelength band λ280 to λ320 when injecting CO₂.

Spectrum	Transition type	Line intensity	λ (Å)	Unc. (mÅ)	λ (Å)	λ (Å)
			This work		CHIANTI^a	NIST^b

Known carbon lines
C IV	2p−4d	blended	...	...	289.1409	289.141
C IV	2p−4d	0.7	289.21	100	289.2277	289.228
C IV	2p−4d	blended	...	...	289.2310	289.231
C IV	2p−4s	blended	...	...	296.8556	296.856
C IV	2p−4s	0.15	296.9	150	296.9506	296.951
C IV	2s−3p	3	312.4	100	312.4202	312.420
C IV	2s−3p	blended	...	...	312.4511	312.451

Known oxygen lines
O IV	2p−3d	0.4	285.7	150	285.7100	285.71
O IV	2p−3d	blended	...	...	285.8340	285.84
O V	2p²−2s3p	0.7	286.47	100	286.4485	286.448
O VIII	3s−4p	blended	...	...	292.4658	...
O VIII	3p−4s	0.45	292.6	100	292.5997	...
O VIII	3p−4s	...	...	...	292.9814	...
O IV	2p−3s	...	...	...	295.6580	295.658
O IV	2p−3s	blended	...	...	295.6670	295.667
O IV	2p−3s	1.25	295.82	100	295.8710	295.871
O IV	2p−3s	blended	...	...	295.8800	295.880
O III	2p−3s	...	...	...	...	295.942
O VI	2p−3s	10	300.2	100	150.0893 (II)	150.089 (II)
O VI	2p−3s	blended	...	...	150.1250 (II)	150.125 (II)
O III	2p−3d	1.9	303.6	100	303.4130−303.8000	303.41−303.80
O III	2p−3d	4	305.7	100	305.5960−305.8360	305.596−305.882
O IV	3p−3s	0.7	306.7	100	306.6210−306.8840	306.621−306.884
O III	2p−3d	...	...	...	308.3050	...
O IV	2p−3s	blended	...	...	311.4990	311.499
O IV	2p−3s	0.1	311.6	150	...	311.682
O IV	2p−3s	blended	...	...	311.7350	311.735

Unidentified lines
...	...	1.5	280.0	150	...	...
...	...	0.2	283.6	150	...	...
...	...	0.6	284.1	150	...	...
...	...	0.15	288.4	150	...	...
...	...	0.06	290.5	200	...	...
...	...	0.2	291.3	150	...	...
...	...	0.8	291.9	150	...	...
...	...	0.2	294.3	150	...	...
...	...	0.4	294.7	150	...	...
...	...	0.2	296.9	150	...	...
...	...	0.2	298.8	150	...	...
...	...	0.3	299.2	150	...	...
...	...	2.0	303.1	100	...	...
...	...	0.22	307.8	150	...	...
...	...	0.2	309.1	150	...	...
...	...	0.04	310.1	200	...	...
...	...	0.45	314.3	150	...	...
...	...	0.2	318.4	150	...	...

Notes. The unknown lines may technically originate in spectra up to C vi or O vii.

Reference. .

^(a)

From the CHIANTI database v. 7.1 and v.8 (Del Zanna et al. 2015);

^(b)

from the on-line database at NIST (Kramida et al. 2012)

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