Table 3.
Radial extent of our sample.
| NGC | rgal, max | reff | r25 | rHI | |||
|---|---|---|---|---|---|---|---|
| or IC | CO | H I | |||||
| [kpc] | [kpc] | [kpc] | [kpc] | [kpc] | [reff] | [r25] | |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | |
| 1954 | 5 | 25 | 2.4 | 5.6 | 5.7 | ≈2 | ≈1 |
| 1512 | 10 | 120 | 4.8 | 23.1 | 65.3 | ≈14 | ≈3 |
| 1566 | 12 | 55 | 3.2 | 18.6 | 21.5 | ≈7 | ≈1 |
| 1672 | 18 | 75 | 3.4 | 17.4 | 26.3 | ≈8 | ≈2 |
| 3511 | 13 | 40 | 3.0 | 12.3 | 12.0 | ≈4 | ≈1 |
| 4535 | 11 | 45 | 6.3 | 18.7 | 20.0 | ≈3 | ≈1 |
| 5068 | 6 | 20 | 2.0 | 5.7 | 5.8 | ≈3 | ≈1 |
| 7496 | 8 | 25 | 3.8 | 9.1 | 15.0 | ≈4 | ≈2 |
| Aver. | 10 | 51 | 3.6 | 13.8 | 21.5 | 6 | 2 |
Notes. (1–2): The maximum value in galactocentric radius (rgal) for CO(2–1) (The maximum galactocentric radius of the CO(2–1) observations are sensitive to the ALMA FoV. We expect, however, that we recover ∼70 − 90% of the total CO emission (see Section 2.3).) and H I, for each galaxy. (3–4): reff and r25 in units of kpc, taken from Table 1. (5): rHI is defined as the ΣHI = 1 M⊙ pc−2 isophote. (6): The value of rHI in units of reff. For example, for NGC 1512 rHI = 65.3 kpc ≈ 14reff. (7): rHI in units of r25. For example, for NGC 1512 rHI ≈ 3r25.
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