Table 4.
Geometric parameters of the ALPAKA galaxies.
| ID | PAHST | iHST | PAALMA | iALMA | PAkin | KC |
|---|---|---|---|---|---|---|
| (deg) | (deg) | (deg) | (deg) | (deg) | ||
| 1 | 253 ± 38 | 53 ± 6 | 244  |
47  |
259 ± 7 | D |
| 2 | 223 ± 33 | 60 ± 5 | 210  |
77  |
215 ± 8 | D |
| 3 ( * ) | 129 ± 19 | 84 ± 1 | 116  |
28  |
134 ± 11 | D |
| 4 | 167 ± 25 | 37 ± 11 | 168  |
52  |
175 ± 16 | U |
| 5 | 357 ± 54 | 37 ± 11 | 290  |
26  |
328 ± 20 | U |
| 6 | 216 ± 32 | 46 ± 8 | 199  |
43  |
213 ± 8 | D |
| 7 | 272 ± 41 | 37 ± 11 | 319  |
35  |
294 ± 3 | D |
| 8 | 206 ± 31 | 37 ± 11 | 201  |
48  |
195 ± 20 | D |
| 9 | 128 ± 19 | 46 ± 8 | 130  |
44  |
120 ± 3 | D |
| 10 | 103 ± 15 | 46 ± 8 | 92  |
30  |
74 ± 23 | U |
| 11 | 113 ± 17 | 26 ± 18 | 118  |
31  |
111 ± 9 | D |
| 12 | 95 ± 14 | 66 ± 4 | 102  |
70  |
103 ± 10 | D |
| 13 | −16 ± 2 | 37 ± 11 | 10  |
24  |
37 ± 4 | D |
| 14 | 13 ± 2 | 53 ± 6 | 323  |
58  |
309 ± 10 | U |
| 15 | 92 ± 14 | 60 ± 5 | 112  |
42  |
132 ± 20 | D |
| 16 ( * ) | 17 ± 3 | 78 ± 2 | 13  |
73  |
15 ± 10 | U |
| 17 ( * ) | 354 ± 53 | 66 ± 4 | 359  |
65  |
1 ± 20 | M |
| 18 ( * ) | 267 ± 40 | 26 ± 18 | 267  |
27  |
248 ± 15 | D |
| 19 | 309 ± 46 | 56 ± 5 | 359  |
71  |
11 ± 9 | D |
| 20 | 154 ± 23 | 46 ± 8 | 144  |
56  |
141 ± 8 | D |
| 21 | 14 ± 2 | 26 ± 18 | 52  |
36  |
7 ± 5 | U |
| 22 ( * ) | 107 ± 16 | 66 ± 4 | 173  |
26  |
157 ± 30 | D |
| 23 | – | – | 86  |
70  |
97 ± 9 | D |
| 24 | – | – | 16  |
75  |
19 ± 4 | D |
| 25 | – | – | 76  |
74  |
87 ± 12 | D |
| 26 | – | – | 317  |
38  |
340 ± 30 | U |
| 27 | – | – | 142  |
62  |
97 ± 19 | M |
| 28 ( * ) | 93 ± 14 | 53 ± 6 | 133  |
52  |
140 ± 5 | D |
Notes. Columns 2–5: values of the position and inclination angles, as derived by GALFIT using the HST data (when available) and CANNUBI using the ALMA total-flux map. Column 6: kinematic position angles derived by 3DBAROLO. Column 7: kinematic class (KC) of each ALPAKA source (D: disk, U: uncertain, M: merger). Galaxies for which the HST filter covers the rest-frame wavelength at λrest,eff ≲ 4000 Å (Table 3) are marked with an asterisk ( * ). In these cases, the geometric parameters (PAHST and iHST) may be not representative of the bulk of stellar emission.
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