RX J1131 is a distant supermassive black hole containing quasar located about 6 billion light years from Earth in the constellation Crater.
In 2014, astronomers found that the X-rays being emitted are coming from a region inside the accretion disk located about three times the radius of the event horizon. This implies that the black hole must be spinning incredibly fast to allow the disk to survive at such a small radius. The measurement of the black hole’s rotation is the first time astronomers have been able to directly measure the rotational speed of any black hole.
This determination was made by a team led by Rubens Reis of the University of Michigan using NASA’s Chandra X-ray Observatory and the European Space Agency’s XMM-Newton telescopes. The team observed the X-rays generated in the innermost regions of the disk circling and feeding the black hole that powers the quasar. By measuring the radius of the disk, the astronomers were able to calculate the black hole’s rotational speed, which was almost half the speed of light. The rapid spin of the quasar indicates that the black hole is being fed by a vast supply of gas and dust.
However, the measurements would not have been possible without a rare alignment of the quasar and a giant elliptical galaxy (which is itself part of a cluster of other galaxies in line with the quasar) which lies between Earth and RX J1131. This line-up provided a quadruple gravitational lens which magnified the light coming from the quasar. The strong gravitational lensing effect associated with J1131 has also produced measured time delays; that is, in one image the lensed object will be observed before the other image.