Forbidden emission lines in protoplanetary disks signal potential disk accretion or wind, outflow, or jet ejection processes of the material that affects the angular momentum transport of the disk as a result. We report spatially resolved emission lines, namely, [\ion{O}{i}]~$\lambda\lambda$6300, 6363, [\ion{N}{ii}]~$\lambda\lambda$6548, 6583, H$\mathrm{\alpha}$, and [\ion{S}{ii}]\,$\lambda\lambda$6716, 6730 observed by the Multi Unit Spectroscopic Explorer (MUSE), at the Very Large Telescope (VLT). The forbidden emission lines analyzed here have their origin at the inner parts of the protoplanetary disk. From the maximum intensity emission along the outflow/jet in DL Tau, CI Tau, DS Tau, IP Tau, and IM Lup, we were able to reliably measure the PA$_\mathrm{outflow/jet}$ for most of the identified lines. We found that our estimates agree with PA$_\mathrm{dust}$ for most of the disks. These estimates depend on the signal-to-noise level and the collimation of the outflow (jet). The outflows/jets in CIDA 9, GO Tau, and GW Lup are too compact for a PA$_\mathrm{outflow/jet}$ to be estimated. Based on our kinematics analysis, we confirm that DL Tau and CI Tau host a strong outflow/jet with line-of-sight velocities much greater than 100 km~s$^{-1}$, whereas DS Tau, IP Tau, and IM Lup velocities are lower and their structures encompass low-velocity components to be more associated with winds. Our estimates for the mass-loss rate, $\dot{M}_{\mathrm{loss}}$, range between (1.1-6.5)~$\times$10$^{-7}$-10$^{-8}$~$M_{\odot}~yr^{-1}$ for the disk-outflow/jet systems analyzed here. The outflow/jet systems analyzed here are aligned within around 1$^{\circ}$ between the inner and outer disk.