CO(1–0) imaging reveals 10-kiloparsec molecular gas reservoirs around star-forming galaxies at high redshift

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Volume 700 (August 2025)

A&A, 700 (2025) A278

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Table 1.

Spectroscopic redshifts and CO(1–0) and [C I](1–0) half-light radii for individual galaxies.

Source ID	z_spec	CO(1–0)		[C I](1–0)
		[arcsec]	[kpc]	[arcsec]	[kpc]
AS2COS1.1	4.625	≤2.62	≤17	≤1.36	≤9
AS2COS8.1	3.581	≤1.05	≤8	≤0.75	≤6
AS2COS13.1	2.608	0.41 $_{- 0.19}^{+ 0.16}$ $^{+0.16}_{-0.19}$	2.9 $_{- 1.4}^{+ 1.2}$ $^{+1.2}_{-1.4}$	–	–
AS2COS14.1	2.921	0.74 $_{- 0.21}^{+ 0.25}$ $^{+0.25}_{-0.21}$	5.8 $_{- 1.7}^{+ 2.0}$ $^{+2.0}_{-1.7}$	0.98 $_{- 0.31}^{+ 0.35}$ $^{+0.35}_{-0.31}$	7.7 $_{- 2.4}^{+ 2.8}$ $^{+2.8}_{-2.4}$
AS2COS23.1	4.341	≤1.89	≤13	1.11 ± 0.44	7.6 ± 3.0
AS2COS28.1	3.097	0.66 $_{- 0.27}^{+ 0.28}$ $^{+0.28}_{-0.27}$	5.1 $_{- 2.1}^{+ 2.2}$ $^{+2.2}_{-2.1}$	–	–
AS2COS31.1	3.643	≤5.26	≤39	≤0.44	≤3.4
AS2COS54.1	3.174	≤1.60	≤12	–	–
AS2COS65.1	2.414	≤0.68	≤5.6	0.38 ± 0.11	3.1 ± 0.9
AS2COS66.1	3.247	≤2.09	≤17	–	–
AS2COS139.1	2.219	≤1.08	≤8	–	–
AS2UDS10.0	3.169	≤3.65	≤28	–	–
AS2UDS11.0	4.073	≤2.37	≤38	–	–
AS2UDS12.0	2.520	≤0.80	≤6.6	0.40 ± 0.19	3.3 ± 1.6
AS2UDS126.0	2.436	0.97 $_{- 0.25}^{+ 0.37}$ $^{+0.37}_{-0.25}$	8.0 $_{- 2.1}^{+ 3.1}$ $^{+3.1}_{-2.1}$	0.64 ± 0.28	5.3 ± 2.3
AEG2	3.668	≤1.43	≤12	–	–
CDFN1	3.149	≤0.80	≤6	–	–
CDFN2	4.422	≤1.35	≤9	–	–
CDFN8	4.144	≤0.89	≤6	–	–

AS2COS2.1	4.595	–	–	2.30 $_{- 1.25}^{+ 1.90}$ $^{+1.90}_{-1.25}$	15 $_{- 8}^{+ 12}$ $^{+12}_{-8}$
AS2UDS.26	3.296	–	–	0.67 $_{- 0.30}^{+ 0.31}$ $^{+0.31}_{-0.30}$	5.1 $_{- 2.3}^{+ 2.4}$ $^{+2.4}_{-2.3}$

Notes. The sizes were derived from the uv-plane modelling using a 5 kλ radial bin size and were integrated over ±1 FWHM bandwidth (we adopted the mid-J CO line widths from Birkin et al. 2021; Chen et al. 2022). For galaxies for which a point-source solution is preferred, the upper limit was based on the 95th percentile from the posterior of the exponential model. At the bottom of the table, we include two sources that have not been detected in the CO(1–0) emission, but have [C I](1–0) detections. The [C I] line in AS2COS66.1 falls partially outside the ALMA tuning and is not used in our analysis.

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