HST spectrum and timing of the ultracompact X-ray binary candidate 47 Tuc X9
Maccarone, T. J.; Knigge, C.; van den Berg, M.; Heinke, C. O.; Bernardini, F.; Russell, D. M.; Miller-Jones, J. C. A.; Soria, R.; Sivakoff, G. R.; Bogdanov, S.; Strader, J.; Chomiuk, L.; Bahramian, A.; Plotkin, R. M.; Zurek, D. R.; Albrow, M. D.; Tudor, V.; Tauris, T. M.; Anderson, G. E.; Britt, C. T.
Australia, United Kingdom, United States, Germany, Canada, China, New Zealand, Netherlands, Italy, United Arab Emirates
Abstract
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 Å) 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 3σ upper limits on the H α and He II λ4686 emission line equivalent widths - EWH α ≲ 14 Å and -EW_{He {II}} ≲ 9 Å, respectively. This is much lower than seen for typical X-ray binaries at a similar X-ray luminosity (which, for L_2-10 keV ≈ 10^{33}-10^{34} erg s-1 is typically - EWH α ∼ 50 Å). 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.