Constraining the [C II] luminosity function from the power spectrum of line-intensity maps at redshift 3.6

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Table 2.

Properties of simulated central (C) and satellite (S) [C II] emitters in different mass bins of their host DM haloes at z = 5 (see also Fig. 3).

Halo mass [M_⊙]	C/S	${\bar{N}}_{i}$ $\bar{N}_i$	$\frac{L_{i}}{L_{tot}}$ $\frac{L_i}{L_{\mathrm{tot}}}$	log₁₀L₅₀ [L_⊙]	${log}_{10} \frac{L_{80}}{L_{20}}$ $\log_{10}\frac{L_{80}}{L_{20}}$
10⁹ − 10¹⁰	C	1	0.87	4.58	0.83
	S	0.68	0.13	3.57	1.27

10¹⁰ − 10¹¹	C	1	0.70	6.56	1.09
	S	5.58	0.30	4.64	2.08

10¹¹ − 10¹²	C	1	0.72	7.84	0.51
	S	5.58	0.28	5.93	1.61

Notes. From left to right, we list the mean number of objects per halo, the collective fractional contribution to the total halo luminosity, the median luminosity of one emitter, and the ratio between the 80^th and the 20^th percentile of the individual emitters. Consistently with Fig. 3, the top two and the bottom entries refer to the high- and low-resolution MARIGOLD simulations, respectively.

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