2021MNRAS.507..484J

A galaxy merger is expected to cause the formation of a supermassive black hole (SMBH) binary, which itself eventually coalesces through the anisotropic emission of gravitational waves. This may result in the merged SMBH receiving a recoil kick velocity ∼100-1000 kms^–1, causing it to oscillate in the gravitational potential of the host galaxy. The luminous quasar E1821+643, identified as an SMBH recoil candidate via spectropolarimetry observations, shows Doppler shifting of the broad emission lines in direct and scattered light, consistent with a relative velocity of 2100 km s^–1 between the quasar nucleus and host galaxy. In this paper, we attempt to detect the expected spatial displacement using a combination of optical spectroastrometry and Hubble Space Telescope (HST) narrow-band images. The spectroastrometry reveals a relative spatial displacement between the quasar nucleus and the gas emitting the [O III] λλ4959, 5007 lines of ∼130 mas (∼580 pc) to the north-west. Our HST images resolve the [O III] emission on sub-arcsecond scales, showing that it is asymmetrically distributed, extending to radial distances ∼0.5-0.6 arcsec from the nucleus in a wide arc running from the north-east around to the west. A simulated spectroastrometry observation based on the HST [O III] image indicates that only a small fraction of the measured displacement can be attributed to the asymmetric [O III] emission. This displacement therefore appears to be a real spatial offset of the quasar nucleus with respect to the narrow-line region, presumed to be located at the host galaxy centre, further supporting the interpretation that a post-merger gravitational recoil of the SMBH has occurred in E1821+643.