Clumpiness of galaxies revealed in the near-infrared with COSMOS-Web - Substructures at 1 < z < 4 and their link to stellar mass and star formation

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Volume 706 (February 2026)

A&A, 706 (2026) A136

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Table 1.

Differences in stellar mass and star formation rate between CIGALE and LEPHARE for galaxies in the sample.

Redshift range	Δlog₁₀ M_★	Δlog₁₀ SFR
	[dex]	[dex]
1.0 ≤ z < 1.3	0.12 $_{- 0.20}^{+ 0.11}$ $^{+0.11}_{-0.20}$	$- 0 . 02_{- 0.30}^{+ 0.39}$ $-0.02^{+0.39}_{-0.30}$
1.3 ≤ z < 1.75	0.12 $_{- 0.24}^{+ 0.13}$ $^{+0.13}_{-0.24}$	$- 0 . 04_{- 0.30}^{+ 0.34}$ $-0.04^{+0.34}_{-0.30}$
1.75 ≤ z < 2.5	0.12 $_{- 0.22}^{+ 0.13}$ $^{+0.13}_{-0.22}$	$- 0 . 05_{- 0.29}^{+ 0.26}$ $-0.05^{+0.26}_{-0.29}$
2.5 ≤ z ≤ 4.0	0.16 $_{- 0.12}^{+ 0.15}$ $^{+0.15}_{-0.12}$	$- 0 . 11_{- 0.28}^{+ 0.22}$ $-0.11^{+0.22}_{-0.28}$

Notes. We compute the difference galaxy per galaxy evaluating the parameters from CIGALE with respect to LEPHARE. For each redshift bin, we provide the median difference and uncertainties correspond to the 16th and 84th quantiles. Positive values indicate that the parameters from CIGALE are higher than those from LEPHARE.

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