Although high-mass (> 8 Msun) stars significantly impact their surroundings at all scales (envelope, cluster, cloud, and even galactic scales), a complete understanding of their feedback remains elusive. This is a direct consequence of their deeply embedded nature, which makes the observational study of high-mass protostars extremely challenging. This issue can be somewhat overcome by the detection of vibrational excited states, which have well constrained excitation conditions and arise at high temperatures (100s of K). In other words, vibrational excited states would allow us to pierce through and probe the inner core layers in close proximity to the protostellar surface and help us confine the temperature structure of hot cores. To carry this out, we have selected a sample of galactic hot cores observed by the ALMAGAL and TEMPO surveys, which offer high sensitivity and angular resolution (a few 1000 au) ALMA observations in band 6 (~1 mm) covering a variety of environmental conditions. We utilize the XCLASS package to fit the complex hot core spectra and derive their chemical composition, column densities, and excitation temperatures, which in turn allow us to model their radiative and mechanical feedback profiles. I will here present our preliminary results.
