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The interstellar medium (ISM) is turbulent on all scales and in all phases.In this paper, we study turbulence with different tracers in four nearbystar-forming regions: Orion, Ophiuchus, Perseus, and Taurus. We combine theAPOGEE-2 and Gaia surveys to obtain the full 6-dimensional measurements ofpositions and velocities of young stars in these regions. The velocitystructure functions (VSFs) of the stars show a universal scaling of turbulence.We also obtain H{\alpha} gas kinematics in these four regions from theWisconsin H-Alpha Mapper. The VSFs of the H{\alpha} are more diverse comparedto the stars. In regions with recent supernova activities, they showcharacteristics of local energy injections and higher amplitudes compared tothe VSFs of stars and of CO from the literature. Such difference in amplitudeof the VSFs can be explained by the different energy and momentum transportfrom supernovae into different phases of the ISM, thus resulting in higherlevels of turbulence in the warm ionized phase traced by H{\alpha}. In regionswithout recent supernova activities, the VSFs of young stars, H{\alpha}, and COare generally consistent, indicating well-coupled turbulence between differentphases. Within individual regions, the brighter parts of the H{\alpha} gas tendto have a higher level of turbulence than the low-emission parts. Our findingssupport a complex picture of the Milky Way ISM, where turbulence can be drivenat different scales and inject energy unevenly into different phases.

Turbulence in Milky Way Star-Forming Regions Traced by Young Stars and Gas