Table 2.
Properties and number of particles used to model the progenitor galaxies in GalMer experiments.
| Component | Parameter | gE0 | gS0 | gSa | gSb | gSd | dE0 | dS0 | dSa | dSb | dSd |
|---|---|---|---|---|---|---|---|---|---|---|---|
| Bulge | MB [2.3 × 109M⊙] | 70 | 10 | 10 | 5 | 0 | 7 | 1 | 1 | 0.5 | 0 |
| rB [kpc] | 4 | 2 | 2 | 1 | … | 1.3 | 0.6 | 0.6 | 0.3 | … | |
| Halo | MH [2.3 × 109M⊙] | 30 | 50 | 50 | 75 | 75 | 3 | 5 | 5 | 7.5 | 7.5 |
| rH [kpc] | 7 | 10 | 10 | 12 | 15 | 2.2 | 3.2 | 3.2 | 3.8 | 4.7 | |
| Disc | M⋆ [2.3 × 109M⊙] | 0 | 40 | 40 | 20 | 25 | 0 | 4 | 4 | 2 | 2.5 |
| Mg,D/M⋆ | … | … | 0.1 | 0.2 | 0.3 | 0 | 0 | 0.1 | 0.2 | 0.3 | |
| a⋆,D [kpc] | … | 4 | 4 | 5 | 6 | … | 1.3 | 1.3 | 1.6 | 1.9 | |
| h⋆,D [kpc] | … | 0.5 | 0.5 | 0.5 | 0.5 | … | 0.16 | 0.16 | 0.16 | 0.16 | |
| ag,D [kpc] | … | … | 5 | 6 | 7 | … | … | 1.6 | 1.9 | 2.2 | |
| hg,D [kpc] | … | … | 0.2 | 0.2 | 0.2 | … | … | 0.06 | 0.06 | 0.06 | |
| No. particles | Ng | … | … | 20 000 | 40 000 | 60 000 | … | … | 8000 | 16 000 | 24 000 |
| N⋆ | 80 000 | 320 000 | 60 000 | 40 000 | 20 000 | 32 000 | 32 000 | 24 000 | 16 000 | 8000 | |
| NDM | 40 000 | 160 000 | 40 000 | 40 000 | 40 000 | 16 000 | 16 000 | 16 000 | 16 000 | 16 000 | |
Notes. The masses and effective radii of the bulges in the progenitor galaxies (in all types, except for Sd’s) are referred as MB and rB. MH and rH represent analogous properties for their dark matter halos. M⋆,D, a⋆,D, and h⋆,D are the masses, effective radii, and scale-heights of the discs made of collisionless stellar particles (in progenitors from S0 to Sd types). From Sa to Sd types, the progenitors also contain discs of hybrid particles, totally gaseous at the start of the simulations, with analogous properties to stellar ones, but denoted as Mg,D, ag,D, and hg,D. The bottom row of the table indicates the number of particles in each component: NDM corresponds to the dark matter halo, N⋆ refers to the collisionless stellar particles distributed in the bulge and disc, and Ng to the hybrid particles in the initial gaseous disc.
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