Table A.2
Properties of SLSN sample used to plot the relations in Fig. 3.
| SLSN | Redshift | log M ⋆ | SFR | 12 +  |
References | |
| (M⊙) | (M⊙ yr-1) | M08 | ||||
|
|
||||||
| PTF11hrq | 0.057 | 8.55 |
0.20 |
8.28  |
4, 4 | |
| PTF10hgi | 0.098 | 7.95 |
0.04 ± 0.04 | 8.62 |
4, 3 | |
| PTF12dam | 0.1078 | 8.30 |
4.78 |
8.08 |
4, 4 | |
| PTF10nmn | 0.123 | 8.79 |
0.53 |
8.27 |
4, 4 | |
| SN1999as | 0.127 | 9.34 |
0.17 ± 0.19 | 8.78 |
1,3 | |
| SN2007bi | 0.127 | 8.13 |
0.02 ± 0.01 | 8.36 |
1,3 | |
| SN2011ke | 0.143 | 6.90 |
0.40 ± 0.03 | 7.86 |
4, 3 | |
| PTF10bfz | 0.175 | 8.65 |
0.39 |
8.02 |
4, 4 | |
| SN2012il | 0.169 | 8.45 |
0.38 ± 0.07 | 7.86 |
1, 3 | |
| PTF10vwg | 0.19 | 8.25 |
<0.07 | – | 4, 4 | |
| PTF11rks | 0.192 | 9.11 |
0.29 ± 0.13 | 8.70 |
4, 3 | |
| PTF10aagc | 0.206 | 8.98 |
0.47 |
8.33 |
4, 4 | |
| SN2010gx | 0.230 | 7.87 |
0.42 ± 0.17 | 7.78 |
4, 3 | |
| SN2011kf | 0.245 | 8.09 |
0.15 ± 0.05 | 8.14 |
1, 3 | |
| PTF09cnd | 0.258 | 8.32 |
0.23 ± 0.06 | 8.44 |
4, 3 | |
| SN2005ap | 0.283 | 8.46 |
– | – | 1, – | |
| PTF10uhf∗ | 0.289 | 10.6 |
5 |
8.98 |
4, 4 | |
| MLS12110 | 0.303 | 9.25 |
0.73 ± 0.02 | 8.54 |
1, 2 | |
| PTF12mxx | 0.33 | 8.16 |
0.11 |
8.69 |
4, 4 | |
| PTF09cwl | 0.349 | 7.85 |
< 0.06 | – | 4, 4 | |
| PTF10bjp | 0.359 | 9.21 |
0.93 |
8.24 |
4, 4 | |
| SN2006oz | 0.396 | 8.67 |
0.13 ± 0.11 | 8.46 |
1, 3 | |
| PTF10vqv | 0.45 | 8.08 |
1.36 |
8.51 |
4, 4 | |
| PTF09atu | 0.501 | 8.35 |
< 0.11 | – | 4, 4 | |
| PS1-12bqf | 0.522 | 9.45 |
1.05 ± 0.55 | 8.82 |
2, 2 | |
| PS1-11ap | 0.524 | 8.48 |
0.30 ± 0.18 | 8.42 |
2, 2 | |
| PS1-10bzj | 0.650 | 7.21 |
5.85 ± 2.10 | 7.76 |
2, 2 | |
| PS1-12zn | 0.674 | 8.34 |
4.50 ± 2.00 | 8.40 |
2, 2 | |
Notes. The table lists all SLSN hosts complying with our selection criteria (Sect. 2), even though only hosts with detected emission lines and measured metallicities are used for the plotting. Reported are SLSN designation, redshift, stellar mass, star formation rate, and nebular metallicity (in the M08 metallicity calibration). The last column gives the references from which the stellar masses and spectra were obtained, respectively. Masses and MB were adopted directly from the referenced works, while SFR and metallicities were measured as described in Sect. 2.
Reference. (1) Angus et al. (2016); (2) Lunnan et al. (2014); (3) Leloudas et al. (2015); (4) Perley et al. (2016b). (∗) Mass and SFR scaled by a factor of 4 to get the approximate values at the SLSN site, as suggested by (Perley et al. 2016b).
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