Spatially resolved star formation relations in local luminous infrared galaxies along the complete merger sequence

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Volume 707 (March 2026)

A&A, 707 (2026) A144

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Table 4.

Statistical parameters of the SFE vs b relation across the merger sequence for clumps and beam-sized regions.

Merger	Clumps				Beam-sized regions

stages	ρ_s	${log}_{10} \frac{b}{M_{⊙} {pc}^{- 2} {(km s^{- 1})}^{- 2}}$ $Mathematical equation: $ \log_{10}\frac{b}{M_\odot\,\mathrm{pc}^{-2}\,(\mathrm{km\,s^{-1}})^{-2}} $$	${log}_{10} \frac{SFE}{{Myr}^{- 1}}$ $Mathematical equation: $ \log_{10}\frac{\mathrm{SFE}}{\mathrm{Myr}^{-1}} $$	slope	ρ_s	${log}_{10} \frac{b}{M_{⊙} {pc}^{- 2} {(km s^{- 1})}^{- 2}}$ $Mathematical equation: $ \log_{10}\frac{b}{M_\odot\,\mathrm{pc}^{-2}\,(\mathrm{km\,s^{-1}})^{-2}} $$	${log}_{10} \frac{SFE}{{Myr}^{- 1}}$ $Mathematical equation: $ \log_{10}\frac{\mathrm{SFE}}{\mathrm{Myr}^{-1}} $$	slope
Isolated galaxies	0.06	−0.24 ± 0.58	−2.64 ± 0.25	0.01 ± 0.01	0.20	0.46 ± 0.32	−2.93 ± 0.32	0.21 ± 0.01
Galaxy pairs	−0.35	−0.57 ± 0.40	−2.67 ± 0.21	−0.18 ± 0.01	−0.02	−0.07 ± 0.20	−2.81 ± 0.22	−0.02 ± 0.01
Early-stage	−0.12	−1.22 ± 0.46	−2.61 ± 0.41	−0.24 ± 0.03 / 0.87 ± 0.01	0.20	0.33 ± 0.30	−2.97 ± 0.41	0.33 ± 0.05
Mid-stage	0.44	−0.72 ± 0.61	−2.72 ± 0.46	0.67 ± 0.11	0.27	0.05 ± 0.26	−3.21 ± 0.35	0.41 ± 0.03
Late-stage	0.61	0.47 ± 0.36	−2.57 ± 0.41	0.66 ± 0.05	−0.10	0.59 ± 0.44	−3.09 ± 0.30	−0.09 ± 0.01

Notes. For each merger stage (isolated galaxies, galaxy pairs, early-stage mergers, mid-stage mergers, and late-stage mergers), the table lists the Spearman’s rank correlation coefficient ρ_sp (two-sided p-values), the mean and error bars (from the mean absolute deviation) of log₁₀b [M_⊙pc⁻²(km s⁻¹)⁻²] and log₁₀SFE [Myr⁻¹], and the best-fit power-law indices (slopes). For early-stage mergers we use MARS fit.

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