Table 3.
Log of the classification spectra for the 42 SNe IIn in our sample.
| SN | Epoch | SN age, relative to | Telescope | Instrument |
|---|---|---|---|---|
| (MJD) | peak (days, rest frame) | |||
| PTF09tm | 55037 | 8 | Lick | Kast |
| PTF09uy | 55008 | −23 | Keck I | LRIS |
| PTF09bcl | 55055 | 9 | WHT | ISIS |
| PTF10cwl | 55270 | 4 | Keck I | LRIS |
| PTF10cwx | 55273 | 1 | P200 | DBSP |
| PTF10ewc | 55285 | −14 | WHT | ISIS |
| PTF10fjh | 55300 | −8 | Gemini North | GMOS |
| PTF10flx | 55299 | −6 | Gemini North | GMOS |
| PTF10gvd | 55322 | 9 | Keck I | LRIS |
| PTF10gvf | 55323 | −13 | Keck I | LRIS |
| PTF10oug | 55396 | −30 | P200 | DBSP |
| PTF10qwu | 55421 | – | P200 | DBSP |
| PTF10tel | 55434 | −11 | Gemini North | GMOS |
| PTF10tyd | 55443 | −23 | P200 | DBSP |
| PTF10vag | 55454 | −10 | Lick | Kast |
| PTF10weh | 55502 | −2 | Lick | Kast |
| PTF10xgo | 55477 | −2 | P200 | DBSP |
| PTF10abui | 55536 | −10 | P200 | DBSP |
| PTF10achk | 55547 | −5 | UH | SNIFS |
| PTF10acsq | 55574 | – | P200 | DBSP |
| PTF11fzz | 55736 | −51 | P200 | DBSP |
| PTF11mpg | 55833 | 6 | Keck II | DEIMOS |
| PTF11oxu | 55872 | −37 | WHT | ISIS |
| PTF11qnf | 55892 | −76 | Keck I | LRIS |
| PTF11qqj | 55895 | −7 | P200 | DBSP |
| PTF11rfr | 55916 | −30 | P200 | DBSP |
| PTF11rlv | 55953 | 20 | Kitt Peak | RC Spec |
| PTF12cxj | 56035 | −14 | Gemini North | GMOS |
| PTF12frn | 56124 | 4 | Keck II | DEIMOS |
| PTF12glz | 56123 | −58 | P200 | DBSP |
| PTF12ksy | 56238 | −14 | P200 | DBSP |
| iPTF13agz | 56442 | 26 | Apache Point | DIS |
| iPTF13aki | 56395 | −7 | P200 | DBSP |
| iPTF13asr | 56421 | 2 | Keck I | LRIS |
| iPTF13cuf | 56545 | – | Keck II | DEIMOS |
| iPTF14bcw | 56803 | −16 | Keck II | DEIMOS |
| iPTF14bpa | 56832 | −28 | P200 | DBSP |
| iPTF15aym | 57176 | −13 | NOT | ALFOSC |
| iPTF15bky | 57196 | −8 | NOT | ALFOSC |
| iPTF15blp | 57226 | 17 | P200 | DBSP |
| iPTF15eqr | 57362 | −10 | Keck I | LRIS |
| iPTF16fb | 57445 | 4 | P200 | DBSP |
Notes. Epochs are given in MJD (=JD – 2 400 000.5). The spectra were taken at epochs −11 ± 20 d (1σ Gaussian spread) relative to light-curve peak (Table 6). For our spectroscopy, we used the following telescopes (with spectrographs given in parenthesis): Apache Point 3.5 m (DIS, Dual Imaging Spectrograph), Gemini North 8.1 m (GMOS, Gemini Multi-Object Spectrograph), Keck I 10 m (LRIS, Low-Resolution Imaging Spectrometer), Keck II 10 m (DEIMOS, DEep Imaging Multi-Object Spectrograph), Kitt Peak 4 m (Ritchey-Chretien Spectrograph), Lick 3 m Shane telescope (Kast Double Spectrograph), Nordic Optical Telescope (NOT) 2.5 m (ALFOSC, Alhambra Faint Object Spectrograph and Camera), P200 5.1 m Hale telescope (DBSP, Double Spectrograph), University of Hawaii (UH) 2.2 m (SNIFS, Supernova Integral Field Spectrograph) and William Herschel Telescope (WHT) 4.2 m (ISIS, Intermediate-dispersion Spectrograph and Imaging System). For SNe with age – when the spectrum was taken, no peak epoch was determined.
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