论文标题
毫匹马赛分离超质量的二进制黑洞的证据和类星体微透明的证据
Evidence for a milliparsec-separation Supermassive Binary Black Hole with quasar microlensing
论文作者
论文摘要
我们报告了重力镜头QJ0158-4325的15年长光光曲线的周期性振荡。在2003年至2010年之间，在高放大倍率的微透镜事件中加强了信号。我们测量了$ p_ {o} = 172.6 \ pm0.9 $天的周期。 We explore four scenarios to explain the origin of the periodicity: 1- the high magnification microlensing event is due to a binary star in the lensing galaxy, 2- QJ0158-4325 contains a massive binary black hole system in its final dynamical stage before merging, 3- the quasar accretion disk contains a bright inhomogeneity in Keplerian motion around the black hole, and 4- the accretion disk在进攻中。在这四种情况下，只有一个超级二进制黑洞可以通过振动磁盘向微透明腐蚀性的高量化区域的振荡来解释短期观察到的时期和信号的振幅。简短的测量周期意味着轨道的半轴为$ \ sim10^{ - 3} $ pc，并且合并时间尺度为$ t_ {coal} \ sim1000 $年，假设轨道的衰减是由重力浪潮发射的损失。观察到如此接近合并的系统的概率表明，超级质量黑洞二进制文件的人群要么大得多，要么比预期的，或者更有可能其他机制显着增加了合并时间尺度。二进制黑洞假设的三个测试包括：i）在任何图像中的任何未来微验证事件中，光度监测中振荡的复发，ii）频谱检测多普勒的频谱转移（高达0.01 $ c $），以及iii），以及通过脉冲驱动器$ 100的sim $ ska，例如，$ Ska的检测，例如，$ 100纳米赫兹排放。
We report periodic oscillations in the 15-year long optical light curve of the gravitationally lensed quasar QJ0158-4325. The signal is enhanced during a high magnification microlensing event undergone by the fainter lensed image of the quasar, between 2003 and 2010. We measure a period of $P_{o}=172.6\pm0.9$ days. We explore four scenarios to explain the origin of the periodicity: 1- the high magnification microlensing event is due to a binary star in the lensing galaxy, 2- QJ0158-4325 contains a massive binary black hole system in its final dynamical stage before merging, 3- the quasar accretion disk contains a bright inhomogeneity in Keplerian motion around the black hole, and 4- the accretion disk is in precession. Among these four scenarios, only a supermassive binary black hole can account for both the short observed period and the amplitude of the signal, through the oscillation of the accretion disk towards and away from high-magnification regions of a microlensing caustic. The short measured period implies that the semi-long axis of the orbit is $\sim10^{-3}$pc, and the coalescence timescale is $t_{coal}\sim1000$ years, assuming that the decay of the orbit is solely powered by the emission of gravitational waves. The probability of observing a system so close to coalescence suggests either a much larger population of supermassive black hole binaries than predicted, or, more likely, that some other mechanism significantly increases the coalescence timescale. Three tests of the binary black hole hypothesis include: i) the recurrence of oscillations in photometric monitoring during any future microlensing events in either image, ii) spectroscopic detection of Doppler shifts (up to 0.01$c$), and iii) the detection of gravitational waves through Pulsar Timing Array experiments, such as the SKA, which will have the sensitivity to detect the $\sim$100 nano-hertz emission.
