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 5.

Linear correlation between the fraction of rest-frame NIR flux in substructures or clumps and the sSFR and partial correlation between the flux fraction and (i) the stellar mass of the host galaxy at a fixed host’s SFR, and (ii) the SFR of the host galaxy at a fixed host’s stellar mass.

Redshift interval	Partial correlation with		Correlation with
Redshift interval	log₁₀ M_★	log₁₀ SFR	log₁₀ sSFR
Substructures
[1.0, 1.3)	$- 0 . 15_{- 0.05}^{+ 0.05}$ $-0.15^{+0.05}_{-0.05}$	$0 . 07_{- 0.06}^{+ 0.05}$ $0.07^{+0.05}_{-0.06}$	$0 . 15_{- 0.06}^{+ 0.05}$ $0.15^{+0.05}_{-0.06}$
[1.3, 1.75)	$- 0 . 07_{- 0.06}^{+ 0.04}$ $-0.07^{+0.04}_{-0.06}$	$0 . 15_{- 0.04}^{+ 0.03}$ $0.15^{+0.03}_{-0.04}$	$0 . 17_{- 0.04}^{+ 0.03}$ $0.17^{+0.03}_{-0.04}$
[1.75, 2.5)	$- 0 . 05_{- 0.03}^{+ 0.03}$ $-0.05^{+0.03}_{-0.03}$	$0 . 16_{- 0.03}^{+ 0.03}$ $0.16^{+0.03}_{-0.03}$	$0 . 17_{- 0.03}^{+ 0.03}$ $0.17^{+0.03}_{-0.03}$
[2.5, 4.0]	$- 0 . 13_{- 0.02}^{+ 0.04}$ $-0.13^{+0.04}_{-0.02}$	$0 . 14_{- 0.03}^{+ 0.03}$ $0.14^{+0.03}_{-0.03}$	$0 . 17_{- 0.03}^{+ 0.03}$ $0.17^{+0.03}_{-0.03}$

Clumps
[1.0, 1.3)	$- 0 . 54_{- 0.04}^{+ 0.05}$ $-0.54^{+0.05}_{-0.04}$	$- 0 . 08_{- 0.06}^{+ 0.06}$ $-0.08^{+0.06}_{-0.06}$	$0 . 23_{- 0.06}^{+ 0.05}$ $0.23^{+0.05}_{-0.06}$
[1.3, 1.75)	$- 0 . 49_{- 0.03}^{+ 0.03}$ $-0.49^{+0.03}_{-0.03}$	$- 0 . 08_{- 0.04}^{+ 0.04}$ $-0.08^{+0.04}_{-0.04}$	$0 . 23_{- 0.04}^{+ 0.04}$ $0.23^{+0.04}_{-0.04}$
[1.75, 2.5)	$- 0 . 51_{- 0.03}^{+ 0.03}$ $-0.51^{+0.03}_{-0.03}$	$- 0 . 11_{- 0.03}^{+ 0.04}$ $-0.11^{+0.04}_{-0.03}$	$0 . 24_{- 0.04}^{+ 0.03}$ $0.24^{+0.03}_{-0.04}$
[2.5, 4.0]	$- 0 . 47_{- 0.03}^{+ 0.03}$ $-0.47^{+0.03}_{-0.03}$	$- 0 . 10_{- 0.03}^{+ 0.04}$ $-0.10^{+0.04}_{-0.03}$	$0 . 23_{- 0.03}^{+ 0.04}$ $0.23^{+0.04}_{-0.03}$

Notes. Values are computed using the linear Pearson correlation and uncertainties correspond to the 95% confidence interval. Using the nonlinear Spearman correlation leads to similar trends but with stronger correlation coefficients, thus showing nonlinearity. A value close to +1 corresponds to positive correlation, while −1 corresponds to anticorrelation.

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