Dynamical resonances in PHANGS galaxies | Astronomy & Astrophysics (A&A)

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Volume 691 (November 2024)

A&A, 691 (2024) A351

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Table 2.

Comparison of the methods of the literature.

Method	$\frac{\| CR - {CR}_{Method} \|}{CR}$ $\cfrac{\|\rm CR - \rm CR_{\mathrm{Method}}\|}\mathrm{CR}$	$\frac{CR}{{CR}_{Method}}$ $\cfrac\mathrm{CR}\mathrm{CR_{\mathrm{Method}}}$	ρ	p-value	N
(1)	(2)	(3)	(4)	(5)	(6)
All methods	0.46 ± 0.44	0.90 ± 0.50	0.64	< 0.001	63
Tremaine-Weinberg (general)	0.23 ± 0.21	0.87 ± 0.16	0.79	< 0.001	16
Tremaine-Weinberg (gas = CO+Hα)	0.23 ± 0.23	0.89 ± 0.17	0.77	0.005	11
Tremaine-Weinberg (CO)	0.18 ± 0.09	0.89 ± 0.12	0.89	0.037	5
Tremaine-Weinberg (Hα)	0.27 ± 0.29	0.89 ± 0.21	0.77	0.072	6
Tremaine-Weinberg (MUSE-M_⋆)	0.25 ± 0.16	0.81 ± 0.10	0.89	0.037	5
Offset method	0.53 ± 0.23	2.58 ± 0.94	0.50	0.667	3
Phase-reversal method	0.52 ± 0.38	0.77 ± 0.28	0.69	0.085	7
Potential-density phase-shift	0.31 ± 0.25	0.97 ± 0.34	0.83	0.007	12
Hydrodynamical simulations	0.86 ± 0.63	0.60 ± 0.20	0.67	0.034	10
Kinematics	0.24 ± 0.16	0.95 ± 0.23	0.79	0.059	6
Morphology	0.96 ± 0.41	0.54 ± 0.15	−0.07	0.899	6
Torques	0.44 ± 0.34	1.02 ± 0.37	−0.87	0.333	3^⋆

Notes. Column (1) states the method used to calculate the corotation. Column (2) reports the quotient |CR_This paper − CR_Method|/CR_{This paper} while Col. (3) contains the relative quotient CR_{This paper}/CR_Method. Column (4) contains the Spearman correlation coefficient (ρ), Col. (5) contains its associated p-value, and Col. (6) contains the number of galaxies in each method (only taking into account galaxies with QF = 1, 2). N^⋆ means the number of galaxies is higher (as seen in Fig. 7) but we chose not to include some of them for the reasons explained in Sect. 5.1 for each particular case. References on each method can be found in Table D.1.

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