Table A.2.
Galaxy sample studied in this paper.
| log(M⋆/M⊙) | log(SFR/[M⊙ yr−1]) | Vmin/[km s−1] | Vmax/[km s−1] | centre | bar | spiral | |
|---|---|---|---|---|---|---|---|
| IC1954 | 9.7 | -0.44 | 900 | 1175 | 1 | 1 | 1 |
| IC5273 | 9.7 | -0.27 | 1150 | 1400 | 1 | 1 | 0 |
| IC5332 | 9.7 | -0.39 | 625 | 750 | 1 | 0 | 0 |
| NGC0628 | 10.3 | 0.24 | 600 | 700 | 1 | 0 | 1 |
| NGC0685 | 10.1 | -0.38 | 1225 | 1450 | 0 | 1 | 0 |
| NGC1087 | 9.9 | 0.12 | 1375 | 1625 | 0 | 1 | 0 |
| NGC1097 | 10.8 | 0.68 | 1000 | 1550 | 1 | 1 | 1 |
| NGC1300 | 10.6 | 0.07 | 1400 | 1700 | 1 | 1 | 1 |
| NGC1317 | 10.6 | -0.32 | 1825 | 2025 | 1 | 1 | 0 |
| NGC1365 | 11.0 | 1.23 | 1400 | 1850 | 1 | 1 | 1 |
| NGC1385 | 10.0 | 0.32 | 1350 | 1600 | 0 | 0 | 1 |
| NGC1433 | 10.9 | 0.05 | 925 | 1175 | 1 | 1 | 0 |
| NGC1511 | 9.9 | 0.36 | 1150 | 1475 | 1 | 0 | 0 |
| NGC1512 | 10.7 | 0.11 | 725 | 1025 | 1 | 1 | 1 |
| NGC1546 | 10.4 | -0.08 | 1050 | 1450 | 1 | 0 | 0 |
| NGC1559 | 10.4 | 0.58 | 1100 | 1450 | 0 | 1 | 0 |
| NGC1566 | 10.8 | 0.66 | 1325 | 1650 | 1 | 1 | 1 |
| NGC1637 | 9.9 | -0.19 | 600 | 825 | 1 | 1 | 1 |
| NGC1672 | 10.7 | 0.88 | 1200 | 1450 | 1 | 1 | 1 |
| NGC1792 | 10.6 | 0.57 | 1050 | 1375 | 1 | 0 | 0 |
| NGC1809 | 9.8 | 0.76 | 1125 | 1400 | 1 | 0 | 0 |
| NGC2090 | 10.0 | -0.39 | 700 | 1100 | 1 | 0 | 1 |
| NGC2283 | 9.9 | -0.28 | 725 | 925 | 1 | 1 | 1 |
| NGC2566 | 10.7 | 0.94 | 1475 | 1775 | 1 | 1 | 1 |
| NGC2775 | 11.1 | -0.06 | 1100 | 1575 | 1 | 0 | 0 |
| NGC2835 | 10.0 | 0.09 | 750 | 975 | 1 | 1 | 1 |
| NGC2903 | 10.6 | 0.49 | 300 | 775 | 1 | 1 | 0 |
| NGC2997 | 10.7 | 0.64 | 925 | 1225 | 1 | 0 | 1 |
| NGC3059 | 10.4 | 0.38 | 1150 | 1325 | 0 | 1 | 0 |
| NGC3137 | 9.9 | -0.31 | 950 | 1225 | 1 | 0 | 0 |
| NGC3239 | 9.2 | -0.41 | 648 | 848 | 0 | 0 | 0 |
| NGC3351 | 10.4 | 0.12 | 625 | 950 | 1 | 1 | 0 |
| NGC3507 | 10.4 | -0.00 | 875 | 1075 | 1 | 1 | 1 |
| NGC3511 | 10.0 | -0.09 | 925 | 1250 | 1 | 1 | 0 |
| NGC3521 | 11.0 | 0.57 | 550 | 1050 | 1 | 0 | 0 |
| NGC3596 | 9.7 | -0.52 | 1100 | 1275 | 1 | 0 | 0 |
| NGC3621 | 10.1 | -0.00 | 575 | 875 | 1 | 0 | 0 |
| NGC3626 | 10.5 | -0.67 | 1200 | 1675 | 1 | 1 | 0 |
| NGC3627 | 10.8 | 0.58 | 500 | 950 | 1 | 1 | 1 |
| NGC4207 | 9.7 | -0.72 | 480 | 720 | 0 | 0 | 0 |
| NGC4254 | 10.4 | 0.49 | 2250 | 2525 | 1 | 0 | 1 |
| NGC4293 | 10.5 | -0.29 | 775 | 1075 | 1 | 1 | 0 |
| NGC4298 | 10.0 | -0.34 | 1000 | 1275 | 1 | 0 | 0 |
| NGC4303 | 10.5 | 0.73 | 1450 | 1675 | 1 | 1 | 1 |
| NGC4321 | 10.7 | 0.55 | 1425 | 1725 | 1 | 1 | 1 |
| NGC4424 | 9.9 | -0.52 | 350 | 550 | 0 | 0 | 0 |
| NGC4457 | 10.4 | -0.51 | 786 | 986 | 1 | 1 | 0 |
| NGC4496A | 9.5 | -0.21 | 1625 | 1825 | 0 | 1 | 0 |
| NGC4535 | 10.5 | 0.33 | 1800 | 2100 | 1 | 1 | 1 |
| NGC4536 | 10.4 | 0.54 | 1600 | 2000 | 1 | 1 | 1 |
| NGC4540 | 9.8 | -0.78 | 1200 | 1375 | 1 | 1 | 0 |
| NGC4548 | 10.7 | -0.28 | 350 | 650 | 1 | 1 | 1 |
| NGC4569 | 10.8 | 0.12 | -425 | 0 | 1 | 1 | 0 |
| NGC4571 | 10.1 | -0.54 | 225 | 450 | 1 | 0 | 0 |
| NGC4579 | 11.1 | 0.34 | 1300 | 1725 | 1 | 1 | 1 |
| NGC4654 | 10.6 | 0.58 | 850 | 1225 | 0 | 1 | 0 |
| NGC4689 | 10.2 | -0.39 | 1500 | 1800 | 1 | 0 | 0 |
| NGC4694 | 9.9 | -0.81 | 1060 | 1300 | 0 | 0 | 0 |
| NGC4731 | 9.5 | -0.22 | 1375 | 1600 | 0 | 1 | 1 |
| NGC4781 | 9.6 | -0.32 | 1100 | 1400 | 0 | 1 | 0 |
| NGC4826 | 10.2 | -0.69 | 200 | 625 | 1 | 0 | 0 |
| NGC4941 | 10.2 | -0.35 | 900 | 1300 | 1 | 1 | 0 |
| NGC4951 | 9.8 | -0.45 | 1025 | 1350 | 1 | 0 | 0 |
| NGC5042 | 9.9 | -0.22 | 1250 | 1525 | 1 | 0 | 0 |
| NGC5068 | 9.4 | -0.56 | 625 | 725 | 1 | 1 | 0 |
| NGC5128 | 11.0 | 0.09 | 200 | 850 | 1 | 0 | 0 |
| NGC5134 | 10.4 | -0.34 | 1625 | 1860 | 1 | 1 | 0 |
| NGC5248 | 10.4 | 0.36 | 1000 | 1325 | 1 | 1 | 1 |
| NGC5530 | 10.1 | -0.48 | 1025 | 1350 | 1 | 0 | 0 |
| NGC5643 | 10.3 | 0.41 | 1050 | 1325 | 1 | 1 | 1 |
| NGC6300 | 10.5 | 0.28 | 900 | 1300 | 1 | 1 | 0 |
| NGC6744 | 10.7 | 0.38 | 625 | 1025 | 1 | 1 | 1 |
| NGC7456 | 9.6 | -0.43 | 1050 | 1310 | 1 | 0 | 0 |
| NGC7496 | 10.0 | 0.35 | 1525 | 1750 | 1 | 1 | 0 |
Notes. Stellar mass and star formation rates of the galaxies studied in this paper (Leroy et al. 2021a). Vmin and Vmax indicate the velocity range (LSRK) over which the ALMA cubes were integrated in order to obtain the intensity maps used in this paper. The last three columns indicate the morphological components included in the environmental masks. All galaxies with a spiral mask have a corresponding interarm mask, whereas the rest have a generic disc component.
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