The ADF and the t$^2$ formalism in H II regions based on the upper mass limit of the IMF for the MW

TL;DR

This study investigates how the upper mass limit of the initial mass function influences predicted element abundances in the Milky Way's H II regions, comparing models with observations to constrain M$_{ m up}$.

Contribution

It introduces a novel approach by analyzing the impact of M$_{ m up}$ on chemical abundances using both direct and temperature independent methods, providing new constraints on the IMF upper mass limit.

Findings

DM predicts M$_{ m up}$ = 25-45 M$_{ m \,odot}$

TIM predicts M$_{ m up}$ = 70-110 M$_{ m \,odot}$

Galaxies similar to the MW have M$_{ m up} \,\sim 100$ M$_{ m \,odot}$

Abstract

We study in depth the abundance discrepancy problem in H II regions, this time from a different perspective than the usual one: by studying the effect of the upper mass limit (M$_{\rm up}$) of the initial mass function (IMF) on the O, C, and He predicted by chemical evolution models for the Milky Way. We use abundances determined with the direct method (DM) and with the temperature independent method (TIM). We compare the predicted abundances at the present time with observations of Orion, M17, and M8 to determine the M$_{\rm up}$ value of the galactic IMF. From the DM abundances, the models predict an M$_{\rm up}$ = 25-45 M$_{\odot}$, while from the TIM, CEMs derive an M$_{\rm up}$ = 70-110 M$_{\odot}$. Spiral galaxies with the stellar mass and star formation rate of the MW are predicted to have an M$_{\rm up} \sim100$ M$_{\odot}$. These results support that abundances derived from the TIM are better than those derived from the DM.