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We present a continuum radiative transfer model grid for fitting observedspectral energy distributions (SEDs) of massive protostars. The model grid isbased on the paradigm of core accretion theory for massive star formation withpre-assembled gravitationally-bound cores as initial conditions. In particular,following the Turbulent Core Model, initial core properties are set primarilyby their mass and the pressure of their ambient clump. We then model theevolution of the protostar and its surround structures in a self-consistentway. The model grid contains about 9000 SEDs with 4 free parameters: initialcore mass, the mean surface density of the environment, the protostellar mass,and the inclination. The model grid is used to fit observed SEDs via chi^2minimization, with the foreground extinction additionally estimated. Wedemonstrate the fitting process and results using the example of massiveprotostar G35.20- 0.74. Compared with other SED model grids currently used formassive star formation studies, in our model grid, the properties of theprotostar and its surrounding structures are more physically connected, whichreduces the dimensionality of the parameter spaces and the total number ofmodels. This excludes possible fitting of models that are physicallyunrealistic or that are not internally self-consistent in the context of theTurbulent Core Model. Thus, this model grid serves not only as a fitting toolto estimate properties of massive protostars, but also as a test of coreaccretion theory. The SED model grid is publicly released with this paper.

Radiation Transfer of Models of Massive Star Formation. IV. The Model Grid and Spectral Energy Distribution Fitting