MUSE-DARK - II. 3D morpho-kinematic modelling of lensed galaxies: Tully-Fisher relation of z ∼ 1 star-forming galaxies

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Table 3.

TFR best-fit parameters.

M	v	v/σ₀	Local reference	a	b_ref	b	σ_{⊥, int}	N
M_★	v_1.8	> 1	Free slope	$3 . 73_{- 0.26}^{+ 0.29}$ $Mathematical equation: $ 3.73^{+0.29}_{-0.26} $$	–	$1 . 75_{- 0.59}^{+ 0.51}$ $Mathematical equation: $ 1.75^{+0.51}_{-0.59} $$	0.12	95
M_★	v_1.8	> 1	Reyes et al. (2011)	3.70	2.22	$1 . 81_{- 0.05}^{+ 0.05}$ $Mathematical equation: $ 1.81^{+0.05}_{-0.05} $$	0.12	95
M_★	v_1.8	> 2	Reyes et al. (2011)	3.70	2.22	$1 . 74_{- 0.05}^{+ 0.05}$ $Mathematical equation: $ 1.74^{+0.05}_{-0.05} $$	0.10	79
M_★	v_2.0	> 1	Ristea et al. (2024)	3.85	1.84	$1 . 47_{- 0.05}^{+ 0.05}$ $Mathematical equation: $ 1.47^{+0.05}_{-0.05} $$	0.12	95
M_bar	v_2.0	> 1	Free slope	$3 . 11_{- 0.36}^{+ 0.45}$ $Mathematical equation: $ 3.11^{+0.45}_{-0.36} $$	-	$3 . 61_{- 0.91}^{+ 0.72}$ $Mathematical equation: $ 3.61^{+0.72}_{-0.91} $$	0.16	95
M_bar	v_2.0	> 1	Lelli et al. (2019)	3.14	3.54	$3 . 54_{- 0.06}^{+ 0.06}$ $Mathematical equation: $ 3.54^{+0.06}_{-0.06} $$	0.16	95

Notes. We tested the robustness of the fits by varying the velocity definition (at 1.8 or 2R_e), the criterion to define rotationally supported galaxies (v/σ₀ > 1 or v/σ₀ > 2), and the adopted local reference slopes (a). For each configuration, we report the local reference zero point (b_ref), the best-fit zero point (b), the orthogonal intrinsic scatter (σ_{⊥, int}), and the number of galaxies entering the fit (N).

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