Table 1.
Origin and evolutionary paths of gas ending up in clumps in the galaxy tail traced using Monte Carlo tracers.
| Tracer path | Definition |
|---|---|
| ISM → clumps | Gas, categorised as ISM at t = 1 Gyr, residing in tail clumps at the time of analysis. |
| CGM → clumps | Gas, categorised as CGM at t = 1 Gyr, residing in tail clumps at the time of analysis. |
| ICM → clumps | Gas, injected as ICM at t ≥ 1 Gyr, residing in tail clumps. |
| CGM → ISM → clumps | A subset of the category ‘CGM → clumps’, which passes through the galaxy’s ISM. |
| ICM → ISM → clumps | A subset of the category ‘ICM → clumps’, which passes through the galaxy’s ISM. |
Notes. The first three rows of paths are based on the properties of a tracer at t = 1 Gyr and at the time of the analysis. The two lower rows show paths with an intermediate phase in the galaxy’s ISM, which means gas characterised as ISM and residing no more than a distance of 1.1RHI downstream from the galaxy centre, where RHI is a measure of the HI extent of the gas disc.
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