Table B.1.
Summary of the properties of the hydrodynamical model galaxies by Chiosi & Carraro (2002).
| Model | MT | MD | MB | R200 | ⟨ρ⟩0 | Ms | Mg | Rs | σs | RDM | σD | Mg, esc | ΔMg, w |
 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Models with mean initial density ⟨ρ⟩≃200 × ρu(z) with z ≃ 5 | ||||||||||||||
| (1A) | 1e13 | 9.0e12 | 1.0e12 | 83 | 4e6 | 6.4e11 | 3.6e11 | 1.87 | 530 | 25 | 646 | 1.5e11 | 2.1e11 | 58 |
| (6A) | 1e9 | 9.0e8 | 1.0e8 | 4 | 4e6 | 3.2e7 | 6.8e7 | 0.07 | 17 | 1 | 20 | 2.4e7 | 4.5e7 | 66 |
| Models with mean initial density ⟨ρ⟩≃5 × ρu(z) with z ≃ 1 | ||||||||||||||
| (1B) | 5e13 | 4.5e13 | 5.0e12 | 681 | 4e4 | 4.4e12 | 0.6e12 | 29 | 365 | 276 | 654 | 4.0e11 | 2.0e11 | 33 |
| (2B) | 5e12 | 4.5e12 | 5.0e11 | 316 | 4e4 | 4.0e11 | 1.0e11 | 16 | 215 | 170 | 324 | 6.5e10 | 3.5e10 | 35 |
| (3B) | 1e12 | 9.0e11 | 1.0e11 | 184 | 4e4 | 6.4e10 | 3.6e10 | 9 | 98 | 63 | 153 | 1.9e10 | 1.7e10 | 47 |
| (4B) | 2e11 | 1.8e11 | 2.0e10 | 108 | 4e4 | 1.2e10 | 0.8e10 | 5 | 69 | 53 | 119 | 0.4e10 | 0.4e10 | 50 |
| (5B) | 1e10 | 9.0e9 | 1.0e9 | 40 | 4e4 | 4.0e8 | 6.0e8 | 2 | 33 | 19 | 55 | 2.5e8 | 3.5e8 | 58 |
| (6B)-LD | 1e9 | 9.0e8 | 1.0e8 | 35 | 5e3 | 1.3e7 | 8.7e7 | 9 | 3 | 1 | 13 | 1.5e7 | 0.8e7 | 35 |
| (6B)-ID | 1e9 | 9.0e8 | 1.0e8 | 19 | 4e4 | 2.5e7 | 7.5e7 | 1 | 6 | 10 | 15 | 3.0e7 | 4.5e7 | 60 |
| (6B)-HD | 1e9 | 9.0e8 | 1.0e8 | 16 | 6e4 | 7.7e7 | 2.3e7 | 0.3 | 5 | 19 | 19 | 6.4e7 | 2.3e7 | 24 |
| (7B) | 1e8 | 9.0e7 | 1.0e7 | 9 | 4e4 | 1.8e6 | 8.2e6 | 1 | 3 | 4 | 10 | 3.0e6 | 5.1e6 | 63 |
Notes. Left: initial conditions: MT is the total mass of the proto-galaxy, MD and MB the mass of DM and BM, respectively, R200 the initial radius, ⟨ρ⟩ the mean mass density. Masses are in M⊙, radii in kiloparsecs, and densities in M⊙ kpc−3. Middle: final results: the present day star Ms and gas Mg mass contents, the half-mass radius Rs and central velocity dispersion σs of the stellar mass, and half-mass radius RD and central velocity dispersion σD of DM. Right: galactic winds: Mg, esc amount of gas inside the radius at which the radial velocity is equal to the escape velocity; ΔMg, w amount of gas lost in the galactic wind; ΔMg, w/Mg percentage of gas lost in the wind with respect to the amount left over by star formation. Masses are in M⊙, radii in kiloparsecs, densities in M⊙ kpc−3, and velocity dispersions in km s−1.
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