Table 4.
Results of the additional tests for the ten promising objects.
| Name | Red. (a) | Host separation | E(B - V)host | AGN (c) | Approx. | SN Ia? | Ib? | Ic? | IIP? | TDE? | ||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| error | (″) | (kpc) | (mag.)(b) | mag.(d) | ||||||||
| SN 2018grt( * ) | No | 0.36 ± 0.03 | 0.32 ± 0.02 | 0.21 – 0.36 | No | −16.5 | No (23) | No (23) | No (2) | No (3) | No (13) | |
| SN 2020pkj | No | 0.52 ± 0.02 | 0.28 ± 0.01 | 0.23 – 0.36 | No | −15.4 | Yes | Yes | Yes | No (23) | No (13) | |
| SN 2019ldf( * ) | No | 0.65 ± 0.04 | 0.78 ± 0.05 | ≤0.03 | No | −16.4 | No (123) | No (123) | No (123) | No (123) | No (13) | |
| SN 2019mse | No | 0.59 ± 0.05 | 1.09 ± 0.10 | 0 | No | −17.5 | No (2) | No (2) | No (2) | No (2) | Yes | |
| SN 2019rqn | No | 1.39 ± 0.08 | 2.21 ± 0.13 | ≤0.04 | No | −16.8 | No (13) | Yes | Yes | No (1) | No (13) | |
| SN 2019vzf | No | 3.89 ± 0.08 | 4.86 ± 0.10 | 0 | Yes | – | – | – | – | – | – | |
| SN 2020awr | Yes | 19.60 ± 0.04 | 31.65 ± 0.07 | – | – | – | – | – | – | – | – | |
| SN 2020alm | No | 0.67 ± 0.07 | 0.85 ± 0.09 | ≤0.05 | No | −16.9 | No (123) | No (12) | No (23) | No (123) | Yes | |
| SN 2020kzd | Yes | 4.67 ± 0.04 | 8.07 ± 0.07 | – | – | – | – | – | – | – | – | |
| SN 2020tfc( * ) | No | 0.21 ± 0.02 | 0.14 ± 0.01 | ≤0.12 | No | −16.8 | No (123) | No (12) | No (23) | No (123) | No (3) | |
Notes. The host separation is given in ″ and converted to kpc using the redshift given in Table 2 and the same cosmology as was used in Sect. 3.4.4. In the final five columns the similarity of each SN Ia with a late-time excess is compared to different transient classes to see if the late-time signal can be interpreted as another transient. This can be excluded based on an inconsistent colour (1), duration (2), and/or an excessive amount of host extinction (3) needed to obtain the observed magnitudes.
Reduction error: Comparison between the standard light curve reduction and scene modelling identified issues with the baseline correction (see Sect. 4.2.1).
Estimated assuming the main peak is a normal SN Ia. When correcting for Milky Way extinction and distance is enough to exceed an absolute g-band magnitude of −19.3, we quote a host E(B – V) = 0 mag.
The presence of an AGN was estimated using the WISE colours of the host and the criteria of Hviding et al. (2022).
Mean absolute magnitude of the r-band late-time excess after correction for Galactic and host extinction, averaged over the host extinction range considered.
( * )Our three final objects with suggested detections of late-time interaction.
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