SN 2022lxg light curves

The fast decline of the light curve from peak (3.48+/-0.26mag(50d)^-1^ in g-band) implies that the ejecta mass must be low. Spectroscopically, until +35d there are similarities to some Type IIb SNe but then there is a transition to spectra that are more reminiscent of an interacting SN II. However, metal lines are largely absent in the spectra, even at epochs of ~80d.

Its remote location (~4.6kpc projected offset) from the presumed host galaxy, a dwarf with MB~-14.4mag, is consistent with our metallicity estimate -- close to the Small Magellanic Cloud value -- obtained from scaling relations. Furthermore, several lines of evidence (including intrinsic polarisation of p~(0.5-1.0)%) point to deviations from spherical symmetry. We suggest that a plausible way of uniting the observational clues is to consider a binary system that underwent case C mass transfer.

This failed to remove the entire H-envelope of the progenitor before it underwent core-collapse. In this scenario, the progenitor itself would be more compact and perhaps straddle the boundary between blue and yellow supergiants, tying in with the early spectroscopic similarity to Type IIb SNe.