  We perform general relativistic simulations of magnetized, accreting disks
onto spinning binary black holes (BHBHs) with different mass ratios (MRs). The
magnitude of the individual BH spins are all $\chi= 0.26$ and lie either along
the initial orbital plane or $45^\circ$ above it. We evolve these systems
throughout the inspiral, merger and postmerger phases to identify the impact of
the BH spins and the MR on any jet and their electromagnetic (EM) signatures.
We find that incipient jets are launched from both BHs regardless of the MR and
along the spin directions as long as the force-free parameter
$B^2/(8\,\pi\rho_0)$ in the funnel and above their poles is larger than one. At
large distances the two jets merge into a single one what may prevent the EM
detection of individual jets. As the accretion rate reaches a quasistationary
state during predecoupling, we observe a sudden amplification of the outgoing
Poynting luminosity that depends on the MR. Following merger, the sudden change
in the direction of the spin of the BH remnant with respect to the spins of its
progenitors causes a reorientation of the jet, which drives a single,
high-velocity, outward narrow beam collimated by a tightly wound, helical
Bfield which, in turn, boosts the Poynting luminosity. This effect is nearly MR
independent. During this process, a kink is produced in the Bfield lines,
confining the jet. The kink propagates along the jet but rapidly decays,
leaving no memory of the spin-shift. Our results suggest that the merger of
misaligned, low-spinning, BHBH mergers in low-mass disks may not provide a
viable scenario to explain X-shaped radio galaxies if other features are not
taken into account. However, the sudden changes in the outgoing luminosity at
merger may help to identify mergers of BHs in active galactic nuclei, shedding
light on BH growth mechanisms and the observed co-evolution of their host
galaxies.
