Table 3.
Properties of the ALPAKA sample and description of the HST dataset.
| ID | M⋆ | SFR | ΔMS | Type | LIR | Iline | L′ CO/[CI] | HST filter | λrest, eff |
|---|---|---|---|---|---|---|---|---|---|
| (1010 M⊙) | (M⊙ yr−1) | (1012 L⊙) | (Jy km s−1) | (1010 K km s−1 pc2) | (Å) | ||||
| 1 | 1.1 ± 0.3 | 8 ± 2 |
 |
MS | 0.8 ± 0.2 | 0.32 ± 0.07 | 0.14 ± 0.03 | F160W | 9794 |
| 2 | 5.7 ± 0.5 | 28 ± 9 |
 |
MS | 2.8 ± 0.9 | 1.54 ± 0.05 | 0.37 ± 0.01 | F814W | 4921 |
| 3 | 3.2 ± 1.1 | 281 ± 18 |
 |
SB | 28 ± 2 | 3.2 ± 0.7 | 1.5 ± 0.3 | F814W | 3254 |
| 4 | 9 ± 4 | 220 ± 50 |
 |
SB | 22 ± 5 | 0.88 ± 0.07 | 2.5 ± 0.2 | F160W | 6236 |
| 5 | 3.6 ± 0.5 | 92 ± 24 |
 |
MS | 9 ± 2 | 0.67 ± 0.05 | 1.9 ± 0.1 | F160W | 6236 |
| 6 | 5.8 ± 1.0 | 67 ± 20 |
 |
MS | 6.7 ± 2.0 | 0.46 ± 0.07 | 1.3 ± 0.2 | F160W | 6210 |
| 7 | 7.6 ± 0.9 | 170 ± 30 |
 |
MS | 17 ± 3 | 0.75 ± 0.02 | 2.22 ± 0.06 | F160W | 6185 |
| 8 | 11 ± 3 | 141 ± 33 |
 |
MS | 14 ± 3 | 0.9 ± 0.2 | 2.6 ± 0.7 | F160W | 6185 |
| 9 | 3.9 ± 0.9 | 48 ± 11 |
 |
MS | 4.8 ± 1.2 | 0.48 ± 0.05 | 1.4 ± 0.1 | F160W | 6185 |
| 10 | 4.7 ± 0.4 | 229 ± 15 |
 |
SB | 23 ± 2 | 0.72 ± 0.09 | 2.15 ± 0.27 | F160W | 6160 |
| 11 ( * ) | 6.3 ± 0.8 | 174 ± 78 |
 |
SB | – | 1.19 ± 0.13 | 4.07 ± 0.44 | F160W | 5899 |
| 12 ( * ) | 5.9 ± 1.8 | 217 ± 82 |
 |
SB | – | 0.76 ± 0.14 | 2.75 ± 0.51 | F160W | 4759 |
| 13 | 12 ± 3 | 230 ± 56 |
 |
MS | 24 ± 10 | 1.96 ± 0.72 | 0.90 ± 0.33 | F160W | 5092 |
| 14 | 11 ± 3 | 441 ± 77 |
 |
MS | 44 ± 17 | 1.83 ± 0.06 | 2.8 ± 0.1 | F140W | 4279 |
| 15 | 25 ± 5 | 215 ± 40 |
 |
MS | 21.5 ± 5.2 | 0.8 ± 0.02 | 2.23 ± 0.06 | F160W | 4737 |
| 16 | – | 730 ± 300 | – | – | 73 ± 13 | 6.3 ± 0.8 | 3.4 ± 0.4 | F110W | 3384 |
| 17 | – | 1360 ± 680 | – | – | 136 ± 25 | 2.4 ± 0.5 | 1.3 ± 0.3 | F110W | 3384 |
| 18 | 12 ± 3 | 3150 ± 830 |
 |
SB | 315 ± 83 | 2.7 ± 0.2 | 4.3 ± 0.4 | F110W | 3285 |
| 19 | 8 ± 2 | 1100 ± 150 |
 |
SB | 110 ± 15 | 1.2 ± 0.1 | 4.1 ± 0.3 | F160W | 4377 |
| 20 | 32 ± 8 | 130 ± 170 |
 |
MS | 13 ± 17 | 0.5 ± 0.1 | 1.8 ± 0.3 | F160W | 4365 |
| 21 | 21 ± 6 | 323 ± 70 |
 |
MS | 32 ± 7 | 0.6 ± 0.1 | 2.2 ± 0.5 | F160W | 4352 |
| 22 | 7 ± 2 | 804 ± 313 |
 |
SB | 80 ± 31 | 1.2 ± 0.4 | 1.9 ± 0.7 | F160W | 3887 |
| 23 | 53 ± 30 | 898 ± 590 |
 |
MS | 90 ± 59 | 1.0 ± 0.5 | 4.9 ± 3.6 | – | – |
| 24 | – | – | – | – | – | 0.63 ± 0.09 | 3.0 ± 0.4 | – | – |
| 25 | 11 ± 5 | 704 ± 400 |
 |
SB | 70 ± 40 | 0.6 ± 0.2 | 2.8 ± 1.0 | – | – |
| 26 | 7 ± 4 | 916 ± 70 |
 |
SB | 92 ± 7 | 0.86 ± 0.06 | 1.7 ± 0.1 | – | – |
| 27 | 8.5 ± 4.0 | 2150 ± 210 |
 |
SB | 215 ± 21 | 2.2 ± 0.3 | 4.5 ± 0.7 | – | – |
| 28 | 13 ± 6 | 1848 ± 900 |
 |
SB | 184 ± 90 | 5.20 ± 0.05 | 8.16 ± 0.08 | F160W | 3299 |
Notes. Column 4 shows the distance of the ALPAKA galaxy with respect to the main-sequence relation, ΔMS = log(SFR/SFRMS), where SFRMS is the SFR defined by Schreiber et al. (2015) at fixed redshift and stellar mass. Column 5 indicates whether the galaxy is a main-sequence (MS) or a starburst (SB). To be conservative, galaxies with ID4, 11, 12, 25 are classified as starburst as their ΔMS values are ≳log(4) = 0.6 within the 1-σ uncertainties. Column 7 shows the flux for the CO or [CI] transitions listed in Table 1. The last column shows the rest-frame effective wavelength probed by the HST data. ( * )For targets 11 and 12, the M⋆ and SFR values are taken from Noble et al. (2017).
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