We have discovered an accreting black hole (BH) in a spectroscopically confirmed globular cluster (GC) in NGC 1399 through the monitoring of its X-ray activity. The source, with a peak luminosity of LX ≃ 2 × 1039 erg s-1, reveals an order of magnitude change in the count rate within ≃10 ks in a Chandra observation. The BH resides in a metal-rich [Fe/H] ≃ 0.2 GC. After RZ 2109 in NGC 4472 this is only the second BH Xray source in a GC confirmed via rapid X-ray variability. Unlike RZ 2109, the X-ray spectrum of this BH source did not change during the period of rapid variability. In addition to the short-term variability the source also exhibits long-term variability. After being bright for at least a decade since 1993, within a span of two years it became progressively fainter, and eventually undetectable, or marginally detectable, in deep Chandra and XMM-Newton observations. The source also became harder as it faded. The characteristics of the long-term variability in itself provide sufficient evidence to identify the source as a BH. The long-term decline in the luminosity of this object was likely not recognized in previous studies because the rapid variability within the bright epoch suppressed the average luminosity in that integration. The hardening of the spectrum accompanying the fading would also make this BH source indistinguishable from an accreting neutron star in some epochs. Therefore, some low-mass X-ray binaries identified as neutron-star accretors in snapshot studies of nearby galaxies may also be BHs. Thus, the discovery of the second confirmed BH in an extragalactic GC through rapid variability at the very least suggests that accreting BHs in GCs are not exceedingly rare occurrences.
- Galaxies: individual (NGC 1399)
- Galaxies: star clusters: general
- X-rays: binaries