Extended ionised and clumpy gas in a normal galaxy at z = 7.1 revealed by ALMA

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Table 3

Properties of the [O iii] clumps observed in the field of view of BDF-3299.

Clump	S/N_integrated ^a	S/N_peak ^b	FWHM	v_{[ O III ]}−v_Lyα	F([O iii])	L([O iii])	Distance
			[km s^-1]	[km s^-1]	[mJy km s^-1]	[10⁸L_⊙]	[′′]

clump-I	7.2	5.0	40 ± 10	440 ± 5	85 ± 12	1.8 ± 0.2	0.7
clump-II	6.9	5.3	40 ± 10	32 ± 5	100 ± 14	2.2 ± 0.3	2.5
clump-III	6.7	5.6	80 ± 10	110 ± 10	260 ± 40	5.8 ± 0.6	6.5

Notes.

^(a)

The integrated significance is the ratio between the integrated flux of the line and the relative error calculated in the extracted spectrum.

^(b)

Significance of the line emission “peak” in the collapsed image. The peak emission significance is slightly lower than the line integrated significance because the emission is spatially slightly extended.

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