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Stars form in molecular clouds in the interstellar medium (ISM) with aturbulent kinematic state. Newborn stars therefore should retain the turbulentkinematics of their natal clouds. Gaia DR2 and APOGEE-2 surveys in combinationprovide three-dimensional (3D) positions and 3D velocities of young stars inthe Orion Molecular Cloud Complex. Using the full 6D measurements, we computethe velocity structure functions (VSFs) of the stars in six different groupswithin the Orion Complex. We find that the motions of stars in all diffusegroups exhibit strong characteristics of turbulence. Their first-order VSFshave a power-law exponent ranging from $\sim0.2-0.5$ on scales of a few to afew tens of pc, generally consistent with Larson's relation. On the other hand,dense star clusters, such as the Orion Nebula Cluster (ONC), have experiencedrapid dynamical relaxation, and have lost the memory of the initial turbulentkinematics. The VSFs of several individual groups and the whole Complex allshow features supporting local energy injection from supernovae. The measuredstrength of turbulence depends on the location relative to the supernovaepicenters and the formation history of the groups. Our detection of turbulencetraced by young stars introduces a new method of probing the turbulentkinematics of the ISM. Unlike previous gas-based studies with only projectedmeasurements accessible to observations, we utilize the full 6D information ofstars, presenting a more complete picture of the 3D interstellar turbulence.

Measuring Turbulence with Young Stars in the Orion Complex