Identification of a Helium Donor Star in NGC 247 ULX-1
arXiv:2303.11639 · doi:10.3847/1538-4357/acc5eb
Abstract
With Very Large Telescope (VLT) Multi Unit Spectroscopic Explorer (MUSE) observations, we detected highly variable helium emission lines from the optical counterpart of the supersoft ultraluminous X-ray source (ULX) NGC 247 ULX-1. No Balmer lines can be seen in the source spectrum. This is the first evidence for the presence of a helium donor star in ULXs, consistent with a prediction that helium donor stars may be popular in ULXs. The helium lines with a FWHM of about 200 km/s are likely produced on the outer accretion disk. Their strong variation implies that the central X-ray source can be significantly obscured to the outer disk. Also, a ring or a double-ring structure is revealed in the MUSE image. It is unknown whether or not it is related to the progenitor of the ULX binary.
arXiv commentaccepted for publication in ApJ
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