HST spectrum and timing of the ultracompact X-ray binary candidate 47 Tuc X9

To confirm the nature of the donor star in the ultracompact X-ray binary candidate 47 Tuc X9, we obtained optical spectra (3000-10 000 angstrom) with the Hubble Space Telescope / Space Telescope Imaging Spectrograph. We find no strong emission or absorption features in the spectrum of X9. In particular, we place 3 sigma upper limits on the H alpha and He II lambda 4686 emission line equivalent widths -EWH alpha less than or similar to 14 angstrom and -EWHe II less than or similar to 9 angstrom, respectively. This is much lower than seen for typical X-ray binaries at a similar X-ray luminosity (which, for L2-10 keV approximate to 10(33)-10(34) erg s(-1) is typically -EWH alpha similar to 50 angstrom). This supports our previous suggestion, by Bahramian et al., of an H-poor donor in X9. We perform timing analysis on archival far-ultraviolet, V-and I-band data to search for periodicities. In the optical bands, we recover the 7-d superorbital period initially discovered in X-rays, but we do not recover the orbital period. In the far-ultraviolet, we find evidence for a 27.2 min period (shorter than the 28.2 min period seen in X-rays). We find that either a neutron star or black hole could explain the observed properties of X9. We also perform binary evolution calculations, showing that the formation of an initial black hole/He-star binary early in the life of a globular cluster could evolve into a present-day system such as X9 (should the compact object in this system indeed be a black hole) via mass-transfer driven by gravitational wave radiation.