Table 1.
List of all models in the extended simulation set.
| Model | log10(M⋆) | F | l* | lg/l* | B | BAR |
|---|---|---|---|---|---|---|
| [M⊙] | [%] | [kpc] | [%] | |||
| G001M095F10L2B00 | 9.5 | 10 | 2 | 2 | 0 | Y |
| G002M095F10L2B10 | 9.5 | 10 | 2 | 2 | 10 | Y |
| G007M095F10L3B00 | 9.5 | 10 | 3 | 2 | 0 | N |
| G008M095F10L3B10 | 9.5 | 10 | 3 | 2 | 10 | N |
| G009M095F10L3B30 | 9.5 | 10 | 3 | 2 | 30 | N |
| G013M095F20L2B00 | 9.5 | 20 | 2 | 2 | 0 | Y |
| G014M095F20L2B10 | 9.5 | 20 | 2 | 2 | 10 | Y |
| G015M095F20L2B30 | 9.5 | 20 | 2 | 2 | 30 | N |
| G019M095F20L3B00 | 9.5 | 20 | 3 | 2 | 0 | N |
| G020M095F20L3B10 | 9.5 | 20 | 3 | 2 | 10 | N |
| G021M095F20L3B30 | 9.5 | 20 | 3 | 2 | 30 | N |
| G025M095F40L2B00 | 9.5 | 40 | 2 | 2 | 0 | Y |
| G026M095F40L2B10 | 9.5 | 40 | 2 | 2 | 10 | Y |
| G027M095F40L2B30 | 9.5 | 40 | 2 | 2 | 30 | Y |
| G031M095F40L3B00 | 9.5 | 40 | 3 | 2 | 0 | Y |
| G032M095F40L3B10 | 9.5 | 40 | 3 | 2 | 10 | N |
| G033M095F40L3B30 | 9.5 | 40 | 3 | 2 | 30 | N |
| G037M100F10L2B00 | 10 | 10 | 2 | 2 | 0 | Y |
| G038M100F10L2B10 | 10 | 10 | 2 | 2 | 10 | Y |
| G039M100F10L2B30 | 10 | 10 | 2 | 2 | 30 | Y |
| G045M100F10L3B00 | 10 | 10 | 3 | 2 | 0 | N |
| G046M100F10L3B10 | 10 | 10 | 3 | 2 | 10 | N |
| G053M100F20L2B00 | 10 | 20 | 2 | 2 | 0 | Y |
| G054M100F20L2B10 | 10 | 20 | 2 | 2 | 10 | Y |
| G055M100F20L3B30 | 10 | 20 | 2 | 2 | 30 | Y |
| G069M100F40L2B00 | 10 | 40 | 2 | 2 | 0 | N |
| G070M100F40L2B10 | 10 | 40 | 2 | 2 | 10 | Y |
| G105M105F10L3B00 | 10.5 | 10 | 3 | 2 | 0 | Y |
| G106M105F10L3B10 | 10.5 | 10 | 3 | 2 | 10 | Y |
| G137M105F20L3B00 | 10.5 | 20 | 3 | 2 | 0 | Y |
| G138M105F20L3B10 | 10.5 | 20 | 3 | 2 | 10 | Y |
| G161M110F10L5B00 | 11 | 10 | 5 | 2 | 0 | Y |
| G162M110F10L5B10 | 11 | 10 | 5 | 2 | 10 | N |
| G177M110F20L5B00 | 11 | 20 | 5 | 2 | 0 | Y |
| G178M110F20L5B10 | 11 | 20 | 5 | 2 | 10 | Y |
Notes. Columns from left to right are: label encapsulating the parameters used to set up the initial conditions, total stellar mass (M⋆, here in log10), gas mass fraction F (in %), stellar scale length l* (in kpc), scale length ratio lg/l* (gas over stellar scale lengths), and bulge mass fraction B (in %). The last column shows models that developed a bar (Y) or not (N) by the end of the run.
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