The strong feedback processes of massive stars influence the surrounding ISM both locally and on large scales. An important question to be answered is the one of cooling and heating in massive star forming regions. There, heating is provided mostly by far-UV (FUV) and infra-red radiation. Cooling is mostly provided by emission in the fine structure lines of [CII] and [OI]. There are, however, molecular lines such as CO, OH and H_2O which can become significant coolants in the dense, embedded regions. To understand the heating and cooling balance, one has to consider the contributions of various radiative and dynamical processes such as FUV radiation, shocks, and the PDRs where the radiation impinges on the molecular material. The tracers of these processes can be observed in the far-infrared, a wavelength range that is now accessible at unprecedented high spectral and spatial resolution with the Herschel Space Observatory. Our approved 3 hour Herschel GT project was designed to cover all the major coolants in one massive star forming region, IRAS 12326-6245. H_2O and [CII] were obtained at high spectral resolution with HIFI, [OI] and OH lines will be observed with PACS and the CO ladder with SPIRE. This luminous, massive, region, located at 4.4 kpc, contains a hot core inside a ˜ 1600Mȯ dust envelope and has one of the most massive outflows observed (Dedes et al. 2011). In this contribution, we will present first results of the radiative transfer modeling of the continuum emission, the H_2O lines modeling, and the derivation of physical conditions of the gas obtained from CH_3OH, 13CO and C18O lines. Despite its apparent simplicity in the ground based CO line profiles, Herschel observations of the source show a complicated velocity structure in the water lines, with many lines contributing to absorption from foreground clouds. High spectral resolution measurements from CH^+ and H_2O^+ are used to assign the velocity components to the source and foreground material.Read less <