A halo model approach to describe clustering and emission of the two main star-forming galaxy populations for cosmic infrared background studies

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Volume 692 (December 2024)

A&A, 692 (2024) A190

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Table 5.

Best-fit parameters from the model fit to V19 data.

Parameter	Prior	Results	Results
		𝒞_{ν₁ × ν₂} = 1	𝒞_{ν₁ × ν₂} Open
$log (M_{\min}^{ET} / M_{⊙} h^{- 1})$ $\log(M_{{\rm{min}}}^{{\rm{ET}}}/{\mathrm{M}_\odot} \, h^{-1})$	[10.7,12.8]	12.40 ± 0.11	$12 . 38_{- 0.18}^{+ 0.22}$ $12.38^{+0.22}_{-0.18}$
$α_{ET}$ $\alpha_{{\rm{ET}}}$	[0.2,3.5]	0.67 ± 0.23	1.12 ± 0.31
$log (M_{\min}^{LT} / M_{⊙} h^{- 1})$ $\log(M_{{\rm{min}}}^{{\rm{LT}}}/{\mathrm{M}_\odot} \, h^{-1})$	[10.5,12.8]	$11 . 79_{- 0.19}^{+ 0.25}$ $11.79^{+0.25}_{-0.19}$	$11 . 91_{- 0.25}^{+ 0.34}$ $11.91^{+0.34}_{-0.25}$
$α_{LT}$ $\alpha_{{\rm{LT}}}$	[0.2,3.5]	1.253 ± 0.044	1.311 ± 0.071

SN₆₀₀	[300,3000]	$1117_{- 140}^{+ 120}$ $1117^{+120}_{-140}$	1788 ± 300
SN₈₅₇	[2000,7000]	3739 ± 340	5153 ± 530
SN₁₂₀₀	[5000,13 000]	8506 ± 710	9688 ± 900
$f_{cal}^{600}$ $f^{600}_{{\rm{cal}}}$	1 ± 0.11	1.055 ± 0.071	1.046 ± 0.084
$f_{cal}^{857}$ $f^{857}_{{\rm{cal}}}$	1 ± 0.11	1.072 ± 0.064	0.973 ± 0.066
$f_{cal}^{1200}$ $f^{1200}_{{\rm{cal}}}$	1 ± 0.11	0.962 ± 0.066	0.907 ± 0.069

𝒞_{600 × 857}	[−1, 1]	–	$0 . 983_{- 0.012}^{+ 0.014}$ $0.983^{+0.014}_{-0.012}$
𝒞_{600 × 1200}	[−1, 1]	–	0.885 ± 0.032
𝒞_{857 × 1200}	[−1, 1]	–	0.9558 ± 0.0092

Notes. Same as Table 2 but for the V19 dataset. When the correlation coefficients are fixed to unity, we obtain χ² = 101 with 132 points and 10 free parameters. In the case where the correlation coefficients are free to vary, we have 13 free parameters and obtain χ² = 80.

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