Table 1.
Galaxies identified as gravitationally interacting with a companion in the (e)LARS samples.
| ID | Interacting | Close-pair (a) | morphopt(b) | morphHI(c) | vHα(d) |
|---|---|---|---|---|---|
| LARS01 | ◼ | ◼ | |||
| LARS02 | ◼ | ◼ | ◼ | ||
| LARS03 | ◼ | ◼ | ◼ | ◼ | |
| LARS04 | ◼ | ◼ | ◼ | ◼ | |
| LARS05 | – | ||||
| LARS06 | ◼ | ◼ | ◼ | ◼ | ◼ |
| LARS07 | ◼ | ◼ | |||
| LARS08 | ◼ | ◼ | ◼ | ||
| LARS09 | ◼ | ◼ | ◼ | ◼ | |
| LARS10 | ◼ | ◼ | – | ||
| LARS11 | ◼ | ◼ | – | ||
| LARS12 | ◼ | ◼ | – | ◼ | |
| LARS13 | ◼ | ◼ | – | ◼ | |
| LARS14 | ◼ | ◼ | – | ◼ | |
| eLARS01 | ◼ | ◼ | ◼ | ◼ | ◼ |
| eLARS02 | |||||
| eLARS03 | ◼ | ◼ | ◼ | ||
| eLARS04 | ◼ | ◼ | |||
| eLARS05 | ◼ | ◼ | ◼ | ||
| eLARS06 | ◼ | ◼ | |||
| eLARS07 | ◼ | ◼ | ◼ | ◼ | |
| eLARS08 | |||||
| eLARS09 | ◼ | ◼ | |||
| eLARS10 | ◼ | ◼ | ◼ | ||
| eLARS11 | ◼ | ◼ | |||
| eLARS12 | |||||
| eLARS13 | ◼ | – | ◼ | ||
| eLARS14 | |||||
| eLARS15 | ◼ | ◼ | |||
| eLARS16 | |||||
| eLARS17 | ◼ | ◼ | |||
| eLARS18 | |||||
| eLARS19 | ◼ | ◼ | ◼ | – | |
| eLARS20 | – | ||||
| eLARS21 | ◼ | ◼ | |||
| eLARS22 | ◼ | ◼ | ◼ | ◼ | |
| eLARS23 | ◼ | ◼ | |||
| eLARS24 | |||||
| eLARS25 | |||||
| eLARS26 | ◼ | ◼ | ◼ | ||
| eLARS27 | |||||
| eLARS28 | ◼ | ◼ | ◼ | ||
| Ninteracting | 31 | 18 | 16 | 13 | 11 |
| finteracting | 74% | 43% | 38% | 39% | 26% |
| finteracting | 83% | 33% | 50% | 63% | 33% |
| LAE | |||||
| finteracting | 70% | 47% | 33% | 32% | 23% |
| non-LAE | |||||
Notes. Galaxies identified as interacting using the methods indicated in the columns are shown by a black square. Galaxies that were not considered for a given method due to lack of data or detection are indicated by a dash.
Galaxies with a close companion identified spectroscopically in SDSS, using the definition in Ventou et al. (2019).
Galaxies showing optical features in HST (Melinder et al. 2023) or DECaLS (Dey et al. 2019) imaging characteristic of a galaxy interaction.
Galaxies showing disturbed HI envelopes characteristic of a galaxy interaction (see e.g., eLARS01 in Fig. 2) or envelopes with extensions encompassing a companion (e.g., LARS02 in Fig. 2 and in the online figure showing the moment maps for this galaxy). Note: for this method, we display the fractions related only to galaxies detected in HI.
Galaxies with Hα kinematics deviating strongly from a rotating disk case, identified in Herenz et al. (2024). In the last rows, we present the total number and fraction of interacting galaxies for the different identification methods. The last two lines show the fraction of interacting galaxies for galaxies that are Lyα-emitters (EWLyα ≥ 20 Å) and non or weak-emitters EWLyα < 20 Å).
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