Weighing the black holes in ultraluminous X-ray sources through timing
P. CasellaAstronomical Institute 'Anton Pannekoek', University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the NetherlandsG. PontiAPC Université Paris 7 Denis Diderot, 75205 Paris Cedex 13, FranceAlessandro PatrunoAstronomical Institute ‘Anton Pannekoek’, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, the NetherlandsT. BelloniINAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate (LC), ItalyG. MiniuttiAPC Université Paris 7 Denis Diderot, 75205 Paris Cedex 13, FranceL. ZampieriINAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy
2008en
ABI
Annotatsiya
We describe a new method to estimate the mass of black holes in Ultraluminous X-ray Sources (ULXs). The method is based on the recently discovered ‘variability plane’, populated by Galactic stellar-mass black-hole candidates (BHCs) and supermassive active galactic nuclei (AGNs), in the parameter space defined by the black-hole mass, accretion rate and characteristic frequency. We apply this method to the two ULXs from which low-frequency quasi-periodic oscillations have been discovered, M82 X-1 and NGC 5408 X-1. For both sources we obtain a black-hole mass in the range 100–1300 M⊙, thus providing evidence for these two sources to host an intermediate-mass black hole.
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