Table 2.
CO emission line observations (ALMA band 3).
| Target | zCO(a) | CO | Synthesised beam | RMS | ICO(c) | FWHM (d) |  |
|---|---|---|---|---|---|---|---|
| line | Size (″)/PA (° ) | ((b)) | (mJy km s−1) | (km s−1) | (109 K km s−1 pc2) | ||
| J1322+0423 | 2.0800 (e) | 3–2 | 1.86 × 1.22/−50 | 59 | < 236 | – | < 5.82 |
| J0146–0220 | 2.1596 ± 0.0002 | 3–2 | 1.01 × 0.63/+59 | 71 | 373 ± 25 | 358 ± 61 | 9.82 ± 0.66 |
| J1415+2036 | 2.2448 ± 0.0004 | 3–2 | 0.87 × 0.62/+17 | 25 | < 304 ± 62 (g) | 332 ± 47 | < 8.57 ± 1.75 |
| J1249+1550 | 2.2926 ± 0.0009 | 3–2 | 0.74 × 0.51/+36 (f) | 28 | 193 ± 12 | 446 ± 115 | 5.64 ± 0.35 |
| J0006+2452 | 2.3800 ± 0.0003 | 3–2 | 0.81 × 0.52/+30 (f) | 45 | 906 ± 51 | 546 ± 107 | 28.3 ± 1.6 |
| J0850+1549 | 2.4235 (e) | 3–2 | 0.98 × 0.76/+30 | 45 | < 180 | – | < 5.78 |
| J1220–0051 | 2.4271 ± 0.0001 | 3–2 | 0.77 × 0.61/+34 | 28 | 240 ± 25 | 295 ± 46 | 7.74 ± 0.81 |
| J0950+0523 | 2.4538 ± 0.0006 | 3–2 | 0.50 × 0.36/+34 (f) | 36 | 470 ± 29 | 524 ± 138 | 15.4 ± 1.0 |
| J1220+0842 | 2.4698 (e) | 3–2 | 0.95 × 0.77/−35 | 65 | < 260 | – | < 8.63 |
| J1157+0113 | 2.5459 ± 0.0003 | 3–2 | 0.83 × 0.80/−71 | 25 | 237 ± 21 | 394 ± 95 | 8.29 ± 0.73 |
| J0121+0025 | 3.2445 (e) | 4–3 | 0.60 × 0.57/−45 | 30 | < 225 ± 65 (g) | – | < 6.63 ± 1.92 |
| J1316+2614 | 3.6122 (e) | 4–3 | 0.94 × 0.61/+10 | 27 | < 108 | – | < 3.79 |
Notes.
Redshifts derived from Gaussian fits of the detected CO emission line profiles (Sect. 3.2). For multiple components identified in the CO line profiles, we considered the component with the highest intensity to compute zCO, unless the multiple components have comparable intensities, then we considered the mean zCO of the components.
CO velocity-integrated intensities derived from CO moment-0 maps. For the CO non-detections, we considered 4σ upper limits based on the RMS noise level of moment-0 maps integrated over ∼ 350 km s−1 (Sect. 3.2).
Full-width half maximum derived from Gaussian fits of the detected CO emission line profiles (Sect. 3.2), and corrected for the final channel spacing of ∼ 45 km s−1 (see the ALMA Technical Handbook). For multiple blended components identified in the CO line profiles, we give the sum of the FWHM of all components.
Redshifts derived from optical nebular emission lines instead of a CO line that is either undetected or has a low S/N.
For these high S/N CO detections, we applied the Briggs weighting with the robust factor of 1.0 instead of the natural weighting.
J1415+2036 and J0121+0025 show patchy CO emission peaks at 4 − 5σ significance level spread within < 3″ (i.e. < 25 kpc) around the phase centre in the CO moment-0 maps, but their respective integrated CO line detections seem to be relatively robust (Figs. 1, A.1, and A.2, middle-right and right panels).
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