Table 2.
Maximum values predicted for bursts and values at equilibrium for models with constant SFR.
| Model | Burst (106 M⊙) | constant SFR= 1 M⊙ yr−1) | ||||||||
|---|---|---|---|---|---|---|---|---|---|---|
| ID | log(Q) | EW(Hβ) | log(ξion) | L1500 | MUV | log(Q) | log(ξion) | L1500 | MUV | κUV |
| [s−1] | [Å] | [erg−1 Hz] | [L⊙ Å−1] | [s−1] | [erg−1 Hz] | [L⊙ Å−1] | ||||
| Predictions including nebular emission: | ||||||||||
| BPASS-100 | 52.65 | 532 | 25.69 | 4.36e+05 | –16.16 | 53.32 | 25.15 | 5.13e+06 | –18.84 | 6.75e-01 |
| BPASS-300 | 52.93 | 654 | 25.79 | 6.89e+05 | –16.66 | 53.48 | 25.27 | 5.65e+06 | –18.94 | 6.13e-01 |
| VMS-150 | 52.81 | 530 | 25.74 | 5.90e+05 | –16.49 | 53.43 | 25.23 | 5.45e+06 | –18.90 | 6.35e-01 |
| VMS-200 | 52.90 | 557 | 25.77 | 6.39e+05 | –16.57 | 53.48 | 25.27 | 5.58e+06 | –18.93 | 6.21e-01 |
| VMS-300 | 52.99 | 579 | 25.79 | 7.34e+05 | –16.73 | 53.53 | 25.31 | 5.74e+06 | –18.96 | 6.04e-01 |
| VMS-400 | 53.04 | 588 | 25.80 | 7.50e+05 | –16.75 | 53.56 | 25.34 | 5.81e+06 | –18.97 | 5.96e-01 |
| Flatter-IMF-150 | 53.29 | 592 | 25.79 | 1.64e+06 | –17.60 | 53.86 | 25.41 | 9.87e+06 | –19.55 | 3.51e-01 |
| Flatter-IMF-400 | 53.56 | 636 | 25.84 | 2.22e+06 | –17.93 | 54.02 | 25.53 | 1.07e+07 | –19.64 | 3.23e-01 |
| VMS-only-150 | 54.17 | 712 | 25.91 | 9.89e+06 | –19.55 | 54.61 | 25.82 | 2.13e+07 | –20.38 | 1.63e-01 |
| VMS-only-400 | 54.15 | 689 | 25.89 | 7.79e+06 | –19.29 | 54.54 | 25.83 | 1.76e+07 | –20.17 | 1.97e-01 |
| PopIII (IMF C) | 54.05 | 753 | 26.18 | 3.94e+06 | –18.55 | 54.439 | 26.08 | 7.90e+06 | –19.30 | 0.438 |
| Predictions without nebular continuum emission: | ||||||||||
| BPASS-100 | 52.65 | 832 | 25.76 | 4.03e+05 | –16.07 | 53.32 | 25.17 | 4.93e+06 | –18.79 | 7.03e-01 |
| BPASS-300 | 52.93 | 1173 | 25.87 | 6.25e+05 | –16.55 | 53.48 | 25.29 | 5.35e+06 | –18.88 | 6.47e-01 |
| VMS-150 | 52.81 | 1067 | 25.85 | 5.08e+05 | –16.32 | 53.43 | 25.26 | 5.09e+06 | –18.83 | 6.81e-01 |
| VMS-200 | 52.90 | 1183 | 25.88 | 5.46e+05 | –16.40 | 53.48 | 25.30 | 5.16e+06 | –18.84 | 6.71e-01 |
| VMS-300 | 52.99 | 1286 | 25.91 | 6.01e+05 | –16.51 | 53.53 | 25.35 | 5.27e+06 | –18.86 | 6.57e-01 |
| VMS-400 | 53.04 | 1332 | 25.92 | 6.08e+05 | –16.52 | 53.56 | 25.38 | 5.31e+06 | –18.87 | 6.52e-01 |
| Flatter-IMF-400 | 53.56 | 1609 | 25.98 | 1.77e+06 | –17.68 | 54.02 | 25.60 | 9.26e+06 | –19.48 | 3.74e-01 |
| VMS-only-150 | 54.17 | 2209 | 26.08 | 7.92e+06 | –19.31 | 54.61 | 25.95 | 1.57e+07 | –20.05 | 2.21e-01 |
| VMS-only-400 | 54.15 | 2002 | 26.06 | 6.05e+06 | –19.01 | 54.54 | 25.97 | 1.29e+07 | –19.83 | 2.69e-01 |
Notes. Maximum values predicted for bursts (Columns 2–6) and values at equilibrium for models with constant SFR (Cols. 7–11). Predictions in the top-half of the table include nebular continuum emission, those below correspond to pure stellar emission. We also list the predictions for PopIII models with a top-heavy IMF (IMF C) from Raiter et al. (2010) for comparison. κUV is given in units of 10−28 M⊙ yr−1/(erg s−1 Hz−1). Burst models are normalized to a total mass of 106 M⊙, constant star formation to SFR = 1 M⊙ yr−1. “Flatter-IMF-X” refers to models with a slope α2 = −2.0 and an upper mass cut-off Mup=X.
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