Table 4
Expected rates.
| Model | Reference | Progenitor | #ν’s | #ν’s |
| mass (M⊙) | t < 380 ms | all times | ||
|
|
||||
| “Livermore” | (Totani et al. 1997) | 20 | 0.174 × 106 | 0.79 × 106 |
| “Garching LS-EOS 1d” | (Kitaura et al. 2006) | 8−10 | 0.069 × 106 | – |
| “Garching WH-EOS 1d” | (Kitaura et al. 2006) | 8−10 | 0.078 × 106 | – |
| “Garching SASI 2d” | (Marek et al. 2009) | 15 | 0.106 × 106 | – |
| “1987A at 10 kpc” | (Pagliaroli et al. 2009b) | 15 − 20 | (0.57 ± 0.18) × 106 | |
| “O-Ne-Mg 1d” | (Hüdepohl et al. 2010) | 8.8 | 0.054 × 106 | 0.17 × 106 |
| “Quark Star (full opacities)” | (Dasgupta et al. 2010) | 10 | 0.067 × 106 | – |
| “Black Hole LS-EOS” | (Sumiyoshi et al. 2007) | 40 | 0.395 × 106 | 1.03 × 106 |
| “Black Hole SH-EOS” | (Sumiyoshi et al. 2007) | 40 | 0.335 × 106 | 3.40 × 106 |
Notes. Number of recorded DOM hits in IceCube (≈’s) for various models of the supernova collapse and progenitor masses assuming a distance of 10 kpc, approximately corresponding to the center of our Galaxy. A normal neutrino hierarchy is assumed.
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