SED modeling of Young Massive Stars

TL;DR

This paper reviews a spectral energy distribution fitting tool for studying young massive stars, discussing its current limitations, potential improvements, and applications in understanding massive star formation.

Contribution

It introduces a spectral energy distribution modeling tool and analyzes its limitations, proposing future enhancements to better understand massive star formation.

Findings

Current models cannot distinguish between competing star formation theories.

The tool provides insights into stellar mass and multiplicity.

Future model improvements will address existing limitations.

Abstract

In this contribution, I review the applications and potential limitations of the spectral energy distribution fitting tool that I have developed, with a strong emphasis on the limits to which this tool can be used to improve our understanding of massive star formation. I discuss why our current grid of models cannot be used to distinguish between the several competing theories of massive star formation. I also discuss stellar mass determinations, artificial correlations between parameters in the grid of models, multiplicity, confusion, dust assumptions, and unique fits. I briefly review the improvements we intend to carry out for our next grid of models, which will eliminate many of these limitations. Finally, I show examples of applications of this tool to massive young stars.