Table 3
The expected and observed ratios of SNe within galaxies host to 2, and host to 3 events.
Number of SNIa | N. CC | Expected ratio | Observed ratio (number of galaxies) |
|
|||
Galaxies host to 2 SNe | |||
0 | 2 | 0.40 ± 0.03 | 0.44 ± 0.06 (83) |
1 | 1 | 0.46 ± 0.03 | 0.39 ± 0.05 (72) |
2 | 0 | 0.14 ± 0.01 | 0.17 ± 0.04 (32) |
Galaxies host to 3 SNe | |||
0 | 3 | 0.49 ± 0.13 | 0.59 ± 0.25 (13) |
1 | 2 | 0.39 ± 0.09 | 0.23 ± 0.14 (5) |
2 | 1 | 0.10 ± 0.02 | 0.14 ± 0.11 (3) |
3 | 0 | 0.01 ± 0.00 | 0.05 ± 0.07 (1) |
|
|||
SNe in SF galaxies | |||
Galaxies host to 2 SNe | |||
0 | 2 | 0.45 ± 0.04 | 0.46 ± 0.04 (76) |
1 | 1 | 0.44 ± 0.03 | 0.41 ± 0.06 (68) |
2 | 0 | 0.11 ± 0.01 | 0.14 ± 0.03 (23) |
Galaxies host to 3 SNe | |||
0 | 3 | 0.61 ± 0.19 | 0.65 ± 0.28 (13) |
1 | 2 | 0.33 ± 0.25 | 0.25 ± 0.15 (5) |
2 | 1 | 0.06 ± 0.01 | 0.10 ± 0.09 (2) |
3 | 0 | 0.00 ± 0.00 | 0.00 ± 0.00 (0) |
|
|||
Number of SNIbc | N. SNII | Expected ratio | Observed ratio (number of galaxies) |
|
|||
Galaxies host to 2 SNe | |||
0 | 2 | 0.53 ± 0.05 | 0.61 ± 0.11 (54) |
1 | 1 | 0.39 ± 0.03 | 0.31 ± 0.07 (28) |
2 | 0 | 0.07 ± 0.00 | 0.08 ± 0.04 (7) |
Galaxies host to 3 SNe | |||
0 | 3 | 0.33 ± 0.09 | 0.63 ± 0.29 (10) |
1 | 2 | 0.44 ± 0.11 | 0.19 ± 0.15 (3) |
2 | 1 | 0.20 ± 0.04 | 0.13 ± 0.13 (2) |
3 | 0 | 0.03 ± 0.01 | 0.06 ± 0.10 (1) |
Notes. First the ratio of SNIa to CC is shown, both for the whole sample, then that excluding SNe within negative T-type host galaxies (SNe in star-forming galaxies). In the first column the number of SNIa is listed, and in the second the number of CC. We then list the expected percentage of events for each distribution, followed by that observed, with the number of galaxies in each distribution listed in brackets. We then list the expected and observed ratios of SNIbc to SNII. Errors on the expected ratios are calculated using the relative SN numbers within each sample, assuming Poisson statistics for distributions with more than 100 events, and using Gehrels (1986) for smaller size distributions. Errors on the observed ratios are calculated using the number of galaxies contributing to each distribution, again using Gehrels (1986) for smaller size distributions.
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