Determining cosmological growth parameter for stellar-mass black holes

Abstract

ABSTRACT It has recently been suggested that black holes (BHs) may grow with time, so that their mass is proportional to the cosmological scale factor to the power n, with suggested values n ≈ 3 for supermassive BHs in elliptical galaxies. Here, we test these predictions with stellar-mass BHs in X-ray binaries using their masses and ages. We perform two sets of tests to assess the compatible values of n. First, we assume that no compact object grows over the Tolman–Oppenheimer–Volkoff limit which marks the borderline between neutron stars and BHs. We show that half of BHs would be born with a mass below this limit if n = 3 applies. The possibility that all BHs were born above the limit is rejected at $4\, \sigma$ if n = 3 applies. In the second test, we assume that masses of BHs at their formation stay the same over cosmic history. We compare the mass distribution of the youngest BHs, which could have not grown yet, to their older counterparts. Distributions are compatible for $n = -0.9^{+1.3}_{-4.6}$, with n = 3 excluded formally with 87 per cent confidence. This result may be biased, because massive BHs tend to have a massive companion. Correcting for this bias yields n ≈ 0. We can therefore conclude that while our results are not a clear rejection of BH scaling with n = 3, we show that n = 0 is much more consistent with the data.