Low-velocity components (LVCs, |v| < 100 km s−1) in optical forbidden line profiles are used as a proxy for protoplanetary disk winds. We aim to study the line properties of LVCs that potentially affect disk dispersal. Using Subaru-HDS, we obtained high spectral resolution spectra (Δv ∼ 2.5 km s−1) for DG Tau A and detected 23 optical forbidden lines ([N I], [N II], [O I], [O II], [O III], [S II], [Ca II], [Fe II]) from 4800 Å to 7500 Å and also three permitted lines (Hα, Hβ, He I). Among these lines, LVCs were observed in the [O I] 5577, 6300, 6364 Å, [S II] 6716, 6731 Å lines. Our analysis reveals that the LVCs can be divided into three subcomponents: LVC-H, LVC-M, and LVC-L. These components may trace turbulent gas, a wide-angled wind, and an upper disk atmosphere, respectively. With 12-70 au wind lengths measured using spectroastrometry, we estimate a lower limit to the wind mass-loss rate of ∼10^−8 M⊙ yr−1. Comparisons between our observation and available photoevaporative wind, D-wind, and X-wind models suggest the need for more extensive synthetic observations of combined wind models to identify the driving mechanism. In addition to the LVCs, we identified one or two high-velocity components (HVCs, |v| > 100 km s−1) associated with the collimated jet in all 26 lines. The one downstream (∼1", ne ∼10^4 cm−3) is associated with an internal shock surface, while the other at the base (0".06 - 0".25) may be a stationary shock component.