2022MNRAS.511L..77S

We use the self-consistent stellar populations in the Binary Population And Spectral Synthesis (BPASS) models to assess whether NGC 1850-BH1 is a black hole (BH). Using search criteria based on reported physical properties in the literature, we purposefully search for suitable systems with a BH (or compact object) companion: we do not find any. Good matches to the observations are found in models where the bright component is a stripped star and the companion is natively (meaning we did not impose this in our search) 1-2.3 mag fainter than the primary in the optical bands. This alone can explain the lack of detection of the companion in the MUSE spectra without the need to invoke rapid rotation, although the conservative mass transfer exhibited by these particular models is likely to lead to rapidly rotating companions that could further smear their spectroscopic signatures. We advise that future claims of unseen BHs in binary systems would benefit from exploring detailed binary evolution models of stellar populations as a sanity check.