What mechanisms dissipate energy in plasma turbulence is an important open question in heliophysics. Which mechanisms are at play under varied plasma conditions, and what consequences they have in the system are aspects that can start addressing this topic. Here we overview the partitioning of dissipated energy between ions and electrons in a set of three-dimensional (3D) gyrokinetic turbulence simulations. The partition of the dissipated energy between the species varies markedly with plasma beta, with the ratio of ion to electron heating decreasing as beta decreases from 1 to 0.01. While there is evidence of Landau damping in all of the systems, whether magnetic reconnection operates has not been studied until recently. In this work, we investigate reconnection activity in detail in the beta of 0.01 simulation, where electrons dominate energy dissipation. Using a newly developed method based on magnetic flux transport (MFT), we can accurately identify reconnection in turbulence in both simulations and in-situ observations. Reconnection takes place in small-scale current sheets formed between turbulent flux ropes as they interact, in the form of flux rope merging, and in elongated current sheets inside flux ropes, which produces smaller-scale flux ropes. Contrary to ideas of patchy and unpredictable reconnection in 3D turbulence, spatially extended active reconnection X-lines, extending on the order of the system size, are present. Plenty of these reconnection X-lines develop in the 3D volume, concurrent with the time of strong energy transfer from turbulence to plasma. Application of this method to MMS observations provides evidence for MFT signature of active reconnection in magnetosheath turbulence, in both ion- and electron-scale current sheets, and under varying plasma conditions throughout Earth’s magnetosphere. MFT is applicable to both kinetic and magnetohydrodynamic turbulence simulations, and in situ measurements from single- and multi-spacecraft missions, representing a new opportunity to study reconnection in heliospheric plasmas.