  In this manuscript, very blue-shifted broad H$\alpha$ with shifted velocity
$\sim$2200km/s is reported in the low redshift Type-1.9 AGN SDSS J1052+1036.
Blue-shifted broad emission lines may arise due to the presence of a rotating
gas disk around central black hole (BH), but may also be a signature of rare
phenomena such as gravitational wave recoil of a supermassive BH (rSMBH) or the
presence of a binary BH (BBH) system. Here, due to larger shifted velocity of
stronger and wider blue-shifted broad H$\alpha$, the BBH system is disfavoured.
Meanwhile, if this object contained a rSMBH, intrinsic obscuration with
E(B-V)$\le$0.6 should lead to a detectable broad H$\beta$, indicating the rSMBH
scenario not preferred. We find that the blue-shifted broad H$\alpha$ can be
well explained by emission from an AGN disk, indicating that SDSS J1052+1036 is
likely a disk-emitting AGN. In order to determine which scenario, a rSMBH or a
disk emitter, is more preferred, a re-observed spectrum in 2025 can provide
robust clues, with a disk emitter probably leading to clear variations of peak
positions, peak separations and/or peak intensity ratios in broad H$\alpha$,
but with a rSMBH scenario probably leading to no variations of peak separations
in broad H$\alpha$.
