The Galaxy Activity, Torus, and Outflow Survey (GATOS) - X. Molecular gas clumpiness under the influence of AGN

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Table A.1.

Properties of the sample.

Name	D_L	$log L_{X}^{2 - 10 keV}$ $\log L_{\mathrm{X}}^{2-10 \text{ keV}}$	log λ_Edd	i	PA

	Mpc	erg s⁻¹		°	°
NGC 613	17.2	41.20	-3.48	36	122
NGC 1068	14.0	42.82	-0.70	41	289
NGC 1326	14.9	39.90	-4.02	53	71
NGC 1365	18.3	42.09	-2.15	41	40
NGC 1433	9.7	39.20	–	33	199
NGC 1566	7.2	40.50	-2.89	49	44
NGC 1672	11.4	39.10	-6.41	29	155
NGC 3227	23.0	42.37	-1.20	52	152
NGC 4941	20.5	41.40	-2.10	41	212
NGC 5643	16.9	42.41	-1.23	30	301
NGC 6300	14.0	41.73	-1.72	57	95
NGC 6814	22.8	42.24	-1.62	57	84
NGC 7213	22.0	41.85	-3.01	35	133
NGC 7314	17.4	42.18	-2.07	55	191
NGC 7465	27.2	41.93	-2.10	54	66
NGC 7582	22.5	43.49	-1.70	59	344

Notes. Distances (D_L) correspond to median values of redshift-independent distances taken from the NASA Extragalactic Database (NED). X-ray luminosities ( $L_{X}^{2 - 10 keV}$ $L_{\mathrm{X}}^{2-10 \text{ keV}}$ ) are taken from Ricci et al. (2017), Combes et al. (2019), García-Burillo et al. (2024). Eddington ratios (λ_Edd) are taken from Koss et al. (2017), García-Burillo et al. (2024). Inclinations (i) and position angles (PA) were derived with the kinemetry software (Krajnović et al. 2006) presented in García-Burillo et al. (2021).

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