(a) Spatial radial velocity distribution for strongest emission lines in SBS 0335−052 in the northwest‐southeast direction. For comparison, the spatial wavelength distribution for the night‐sky emission line [O I] λ5577 is shown; this line does not show significant variations along the slit. We do not detect a significant gradient in velocity distribution except for a slight increase of velocity by 50 km s⁻¹ in the outer parts of the H II region. (b) Distribution of FWHM for the strongest emission lines in SBS 0335−052. For the Hβ λ4861 emission line width, the error bars are also shown. The FWHM for night‐sky [O I] λ5577 emission is shown for comparison. Note that the Hβ λ4861 line is narrower than other lines and could be subject to underlying stellar absorption from A stars. The gradient in Hβ λ4861 and [O III] λ5007 emission line width could be explained by turbulent velocity increasing in the northwest direction.