The star- and disk-formation process involves balancing gravity, turbulence, and magnetic fields. Turbulence and magnetic fields attempt to slow down the gravitational collapse. Thanks to high-angular resolution interferometric observations, much progress has been made in studying the disk properties. Unfortunately, little progress has been made in understanding the role of the environment in the formation and evolution of star- and disks and the role of feedback. We present NOMEA observations at 3mm that allow us to address different goals simultaneously. We will show the results of: (1) the first systematic estimate of the number of streamers on embedded protostars, (2) the first large-scale cosmic ray ionization rate and electron fraction maps, (3) a determination of the power spectrum of turbulence over more than 2-orders of magnitude for ions and neutrals down to the ambipolar diffusion scale, (4) the evidence for extended SiO and SO2 emission unrelated to outflows as evidence for large scale shocks, and (5) the comparison of typically used dense gas tracers in extragalactic studies. These results show that considering the interaction between parental cloud and YSOs is extremely important to understanding the star formation process.
