Table 5.

Summary of the pros and cons of each of the progenitor systems considered for AT2018kzr.

UltrastrippedAccretion-inducedDouble WDMerger of a WD
core-collapse SNcollapse of an ONe WDmerger systemswith an NS/BH
Peak brightnessBadPossibleaGoodPossibleb
Light-curve evolutionBadPossiblecGoodGood
Velocity of ejectaGoodBadGoodGoodd
Ejecta massGoodGoodGoodPossiblee
Bulk compositionGoodBadBadGood
Fe/Ni ratioBadBadBadGood
UltrastrippedAccretion-inducedDouble WDMerger of a WD
core-collapse SNcollapse of an ONe WDmerger systemswith an NS/BH
Peak brightnessBadPossibleaGoodPossibleb
Light-curve evolutionBadPossiblecGoodGood
Velocity of ejectaGoodBadGoodGoodd
Ejecta massGoodGoodGoodPossiblee
Bulk compositionGoodBadBadGood
Fe/Ni ratioBadBadBadGood

aCapable of producing a magnetar, which can power the light curve.

bCapable of reaching the observed luminosity of AT2018kzr, with the help of high-velocity winds launched off the disc.

cLight-curve evolution too fast in the models discussed, but a higher ejecta mass would act to extend the light curve.

dThe bulk velocity of the ejecta material agrees with our photospheric estimates for ejecta velocity.

eThe ejecta mass obtained from light-curve modelling is lower than that estimated from the models discussed, but these values are dependent on the specific merger, which make it difficult to get good approximations.

Table 5.

Summary of the pros and cons of each of the progenitor systems considered for AT2018kzr.

UltrastrippedAccretion-inducedDouble WDMerger of a WD
core-collapse SNcollapse of an ONe WDmerger systemswith an NS/BH
Peak brightnessBadPossibleaGoodPossibleb
Light-curve evolutionBadPossiblecGoodGood
Velocity of ejectaGoodBadGoodGoodd
Ejecta massGoodGoodGoodPossiblee
Bulk compositionGoodBadBadGood
Fe/Ni ratioBadBadBadGood
UltrastrippedAccretion-inducedDouble WDMerger of a WD
core-collapse SNcollapse of an ONe WDmerger systemswith an NS/BH
Peak brightnessBadPossibleaGoodPossibleb
Light-curve evolutionBadPossiblecGoodGood
Velocity of ejectaGoodBadGoodGoodd
Ejecta massGoodGoodGoodPossiblee
Bulk compositionGoodBadBadGood
Fe/Ni ratioBadBadBadGood

aCapable of producing a magnetar, which can power the light curve.

bCapable of reaching the observed luminosity of AT2018kzr, with the help of high-velocity winds launched off the disc.

cLight-curve evolution too fast in the models discussed, but a higher ejecta mass would act to extend the light curve.

dThe bulk velocity of the ejecta material agrees with our photospheric estimates for ejecta velocity.

eThe ejecta mass obtained from light-curve modelling is lower than that estimated from the models discussed, but these values are dependent on the specific merger, which make it difficult to get good approximations.

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