Table 5.
Details of the comparison transients used to test if late-time detections could be explained by another transient at a similar sky position.
| Type | Name | Peak abs. Mr (mag.) | Reference |
|---|---|---|---|
| SN Ia | SN 2011fe | −18.4 to −19.4 | Mazzali et al. (2014) |
| SN Ib | SN 2019yvr | −17.9 | Kilpatrick et al. (2021) |
| SN Ic | SN 2021krf | −17.3 | Ravi et al. (2023) |
| SN IIP | SN 2020jfo | −17.8 | Ailawadhi et al. (2023) |
| SN IIP | SN 2017gmr | −18.7 | Andrews et al. (2019) |
| TDE | AT 2018hco | −22.1 | van Velzen et al. (2021) |
| TDE | AT 2018zr | −20.1 | van Velzen et al. (2021) |
Notes. The first column shows the assumed type of transient, the second shows the transients used to represent each type, the third has the approximate absolute extinction-corrected r-band peak magnitudes, and the fourth the reference for each event.
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