The ALMA-CRISTAL survey: Resolved kinematic studies of main sequence star-forming galaxies at 4 < z < 6

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Volume 701 (September 2025)

A&A, 701 (2025) A260

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Table 2.

Kinematic classification and properties of CRISTAL galaxies.

ID	Classification a	PA_k b	V_obs/2 c	V_obs/2σ_int d	f_molgas e	K_asym f	Disk score g
		(°)	(km s⁻¹)				(Total: 8)
01a	Non-Disk	295.6	116.54 ± 26.56	0.41 ± 0.09	0.10 $_{- 0.06}^{+ 0.21}$ $_{-0.06}^{+0.21}$	0.29 ± 0.05	3
01b	Non-Disk	325.8	54.54 ± 5.64	0.46 ± 0.12	...	0.63 ± 0.78	3
02	Disk	126.9	65.19 ± 6.24	0.45 ± 0.04	0.43 $_{- 0.11}^{+ 0.21}$ $_{-0.11}^{+0.21}$	0.23 ± 0.03	5
03	Best Disk	126.6	50.0 ± 11.99	0.35 ± 0.09	0.13 $_{- 0.06}^{+ 0.14}$ $_{-0.06}^{+0.14}$	0.15 ± 0.03	7
04a	Non-Disk	171.5	47.16 ± 13.87	0.58 ± 0.17	0.39 $_{- 0.12}^{+ 0.25}$ $_{-0.12}^{+0.25}$	0.71 ± 0.12	1
04b	Non-Disk	207.9	27.6 ± 20.78	0.68 ± 0.51	...	0.54 ± 0.15	1
05a	Disk	...	...	...	$0 . 39_{- 0.13}^{+ 0.29}$ $0.39^{+0.29}_{-0.13}$	...	...h
05b	Non-Disk	...	...	...	...	...	...h
06a	Non-Disk	268.0	44.18 ± 2.09	0.57 ± 0.03	0.51 $_{- 0.13}^{+ 0.26}$ $_{-0.13}^{+0.26}$	2.10 ± 0.28	3
06b	Disk	79.0	48.11 ± 7.29	0.56 ± 0.09	...	0.35 ± 0.17	5
07a	Disk	359.0	83.3 ± 6.03	0.88 ± 0.08	0.43 $_{- 0.13}^{+ 0.28}$ $_{-0.13}^{+0.28}$	0.20 ± 0.03	5
07b	Non-Disk	66.8	63.37 ± 15.79	0.62 ± 0.16	...	0.84 ± 0.15	3
07c	Non-Disk	32.0	100.56 ± 19.01	0.91 ± 0.18	0.21 $_{- 0.09}^{+ 0.20}$ $_{-0.09}^{+0.20}$	0.81 ± 0.42	4
08	Best Disk	123.0	110.43 ± 28.70	0.94 ± 0.25	0.63 $_{- 0.13}^{+ 0.29}$ $_{-0.13}^{+0.29}$	0.18 ± 0.06	7
09a	Disk	170.0	84.27 ± 59.79	0.63 ± 0.45	0.74 $_{- 0.12}^{+ 0.32}$ $_{-0.12}^{+0.32}$	0.25 ± 0.27	6
10a	Non-Disk	226.0	127.79 ± 24.82	0.78 ± 0.16	0.73 $_{- 0.11}^{+ 0.23}$ $_{-0.11}^{+0.23}$	0.36 ± 0.06	3
10a-E	Disk	123.0	30.54 ± 15.88	0.32 ± 0.16	...	0.35 ± 0.03	6
11	Best Disk	335.0	63.19 ± 45.60	0.45 ± 0.32	0.73 $_{- 0.11}^{+ 0.23}$ $_{-0.11}^{+0.23}$	0.13 ± 0.05	8
12	Disk	34.3	25.72 ± 18.66	0.43 ± 0.31	0.67 $_{- 0.15}^{+ 0.43}$ $_{-0.15}^{+0.43}$	0.45 ± 0.08	7
13	Non-Disk	17.0	145.26 ± 13.16	0.96 ± 0.11	0.63 $_{- 0.13}^{+ 0.27}$ $_{-0.13}^{+0.27}$	0.37 ± 0.03	4
14	Non-Disk	61.9	73.79 ± 27.03	0.55 ± 0.20	0.78 $_{- 0.10}^{+ 0.23}$ $_{-0.10}^{+0.23}$	0.49 ± 0.33	3
15	Best Disk	308.2	37.27 ± 3.89	0.28 ± 0.03	0.41 $_{- 0.13}^{+ 0.27}$ $_{-0.13}^{+0.27}$	0.51 ± 0.22	7
16	Non-Disk	14.0	52.58 ± 9.06	0.44 ± 0.08	0.69 $_{- 0.14}^{+ 0.35}$ $_{-0.14}^{+0.35}$	2.78 ± 0.70	1
19	Best Disk	313.0	110.58 ± 37.79	0.89 ± 0.31	0.70 $_{- 0.12}^{+ 0.27}$ $_{-0.12}^{+0.27}$	0.17 ± 0.32	8
20	Best Disk	17.0	68.31 ± 13.26	0.73 ± 0.14	0.47 $_{- 0.15}^{+ 0.35}$ $_{-0.15}^{+0.35}$	0.14 ± 0.08	8
21	Non-Disk	41.0	27.82 ± 18.31	0.19 ± 0.12	0.59 $_{- 0.13}^{+ 0.28}$ $_{-0.13}^{+0.28}$	2.17 ± 1.43	4
22a	Disk	...	...	...	$0 . 71_{- 0.12}^{+ 0.28}$ $0.71^{+0.28}_{-0.12}$	...	...i
22b	Non-Disk	...	...	...	...	...	...i
23a	Non-Disk	354.0	45.79 ± 1.27	0.40 ± 0.02	0.40 $_{- 0.12}^{+ 0.23}$ $_{-0.12}^{+0.23}$	1.12 ± 0.29	3
23b	Disk	260.0	51.31 ± 2.32	0.34 ± 0.02	0.25 $_{- 0.09}^{+ 0.18}$ $_{-0.09}^{+0.18}$	0.21 ± 0.02	6
23c	Best Disk	45.0	92.78 ± 4.82	0.83 ± 0.06	0.17 $_{- 0.07}^{+ 0.13}$ $_{-0.07}^{+0.13}$	0.17 ± 0.04	8
24	Non-Disk	60.0	140.69 ± 22.69	0.43 ± 0.07	0.51 $_{- 0.05}^{+ 0.06}$ $_{-0.05}^{+0.06}$	0.38 ± 0.11	4
25a	Non-Disk	309.0	60.03 ± 30.54	0.61 ± 0.31	...	0.45 ± 0.10	4
25b	Non-Disk	335.0	98.95 ± 26.06	0.86 ± 0.23	...	0.32 ± 0.08	4

Notes.

^(a)

Classification of the sample based on the disk score.

^(b)

Position angle along the kinematic major axis pointing to the blue side.

^(c)

Half-difference between the observed maximum and minimum velocities: V_obs/2 = (V_max − V_min)/2.

^(d)

Ratios between (c) and the [C II] integrated line widths σ_int.

^(e)

Molecular gas fraction inferred in Appendix C for systems with dust continuum detection

^(f)

Asymmetry measure of the velocity and velocity dispersion fields following Shapiro et al. (2008) demarcation.

^(g)

The sum of points from the metrics outlined in Sects. 3.1–3.5, with the following scheme: Best Disk when disk score ⩾7; Disk if 5–6; and Non-Disk when ⩽4.

^(h)

See Posses et al. (2025).

⁽ⁱ⁾

See Telikova et al. (2025).

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