The environment of a ULX in NGC 4559: an optical study

We have studied the candidate optical counterparts and the stellar population in the star-forming complex around the bright ULX in the western part of the spiral galaxy NGC4559, using HST/WFPC2, XMM-Newton/Optical Monitor, and ground-based data. We find that the ULX is located near a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant of mass ≈ 20M⊙ and age ≈ 10 Myr. A few other stars are resolved inside the error circle: mostly blue and red supergiants with inferred masses ≈ 10– 15M⊙ and ages ≈ 20 Myr. This is consistent with the interpretation of this ULX as a black hole (BH) accreting from a high-mass donor star in its supergiant phase, with mass transfer occurring via Roche-lobe overflow. The observed optical colors and the blue-to-red supergiant ratio suggest a low metal abundance for the stellar population: 0.2 . Z/Z⊙ . 0.4 (using the Padua tracks), or 0.05 . Z/Z⊙ . 0.2 (using the Geneva tracks). The age of the star-forming complex is . 30 Myr. Hα images show that this star-forming region has a ring-like appearance. We propose that it is an expanding wave of star formation, triggered by an initial density perturbation, in a region where the gas was only marginally stable to gravitational collapse. We also suggest that the most likely trigger was a collision with a satellite dwarf galaxy going through the gas-rich outer disk of NGC4559 less than 30 Myr ago. The culprit could be the dwarf galaxy visible a few arcsec north-west of the complex. If this is the case, this system is a scaled-down version of the Cartwheel galaxy. The X-ray data favour a BH more massive (M > 50M⊙) than typical Milky Way BH candidates. The optical data favour a “young” BH originating in the recent episode of massive star formation; however, they also rule out an association with young massive star clusters (none are present in the X7 field). We speculate that other mechanisms may lead to the formation of relatively massive BHs (perhaps M ∼ 50–100M⊙) from stellar evolution processes in low-metallicity environments, or when star formation is triggered by galactic collisions.