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 2.

Best-fit parameters from the model fit to P14 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]	$11 . 45_{- 0.13}^{+ 0.16}$ $11.45^{+0.16}_{-0.13}$	11.12 ± 0.19
$log (M_{\min}^{LT} / M_{⊙} h^{- 1})$ $\log(M_{{\rm{min}}}^{{\rm{LT}}}/{\mathrm{M}_\odot}\,h^{-1})$	[10.5,12.8]	$11 . 18_{- 0.27}^{+ 0.31}$ $11.18^{+0.31}_{-0.27}$	$11 . 56_{- 0.17}^{+ 0.21}$ $11.56^{+0.21}_{-0.17}$
$α_{LT}$ $\alpha_{{\rm{LT}}}$	[0.2,3.5]	$1 . 337_{- 0.072}^{+ 0.063}$ $1.337^{+0.063}_{-0.072}$	$1 . 436_{- 0.067}^{+ 0.075}$ $1.436^{+0.075}_{-0.067}$

SN₂₁₇	[0,50]	6.72 ± 0.76	22 ± 4
SN₃₅₃	[50,500]	273 ± 16	276 ± 20
SN₅₄₅	[400,4000]	1296 ± 120	1247 ± 100
SN₈₅₇	[200,8000]	1827 ± 300	$1899_{- 600}^{+ 400}$ $1899^{+400}_{-600}$
$f_{cal}^{353}$ $f^{353}_{{\rm{cal}}}$	1 ± 0.0156	0.999 ± 0.014	1.010 ± 0.015
$f_{cal}^{545}$ $f^{545}_{{\rm{cal}}}$	1 ± 0.122	1.096 ± 0.032	1.094 ± 0.032
$f_{cal}^{857}$ $f^{857}_{{\rm{cal}}}$	1 ± 0.128	1.289 ± 0.076	1.200 ± 0.072

𝒞_{217 × 353}	[−1, 1]	–	$0 . 648_{- 0.075}^{+ 0.068}$ $0.648^{+0.068}_{-0.075}$
𝒞_{217 × 545}	[−1, 1]	–	0.469 ± 0.054
𝒞_{217 × 857}	[−1, 1]	–	0.562 ± 0.070
𝒞_{353 × 545}	[−1, 1]	–	$0 . 946_{- 0.031}^{+ 0.035}$ $0.946^{+0.035}_{-0.031}$
𝒞_{353 × 857}	[−1, 1]	–	$0 . 937_{- 0.042}^{+ 0.056}$ $0.937^{+0.056}_{-0.042}$
𝒞_{545 × 857}	[−1, 1]	–	$0 . 934_{- 0.039}^{+ 0.046}$ $0.934^{+0.046}_{-0.039}$

Notes. First column; Model parameters sampled for the fit to P14 data. Second column; priors and ranges of variation imposed on the model parameters. We adopt uniform priors for all parameters (ranges are within square brackets), except for the calibration factors for the 353, 545 and 857 GHz frequency channels which are varied with a Gaussian priors centered on 1. Third and fourth columns; mean and standard deviation of the model parameters for the case in which the correlations for the shot noise are fixed to one and the case in which they are free to vary, respectively. In the former case, we obtain a χ² = 81 with 80 points and 10 free parameters. The latter case has the same number of points, 16 free parameters and χ² = 45.

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