Red Giant Branch Bump Star Counts in Data and Stellar Models

TL;DR

This study compares stellar model predictions to observed star counts in the red giant branch bump (RGBB), revealing discrepancies that inform stellar interior models and suggest potential calibration issues in metallicity scales.

Contribution

It provides a detailed comparison of RGBB star counts between models and observations, highlighting the impact of metallicity scale assumptions and constraining deep mixing theories.

Findings

Model predictions exceed observed counts by 5-17% depending on the model.

Adjusting metallicity scales can reconcile model and data discrepancies.

RGBB star counts serve as a useful parameter for constraining stellar populations.

Abstract

We compare model predictions to observations of star counts in the red giant branch bump (RGBB) relative to the number density of first-ascent red giant branch at the magnitude of the RGBB, $EW_{RGBB}$. The predictions are shown to exceed the data by $(5.2 \pm 4.3)$% for the BaSTI models and by $(17.1 \pm 4.3)$% for the Dartmouth models, where the listed errors are purely statistical. These two offsets are brought to zero if the Galactic globular cluster metallicity scale is assumed to be overestimated by a linear shift of $\sim 0.11$ dex and $\sim 0.36$ dex respectively. This inference based on RGBB star counts goes in the opposite direction to the increase in metallicities of ${\Delta}$[M/H]$\approx$0.20 dex that would be required to fix the offset between predicted and observed RGBB luminosities. This comparison is a constraint on "deep mixing" models of stellar interiors, which predict decreased rather than increased RGBB star counts. We tabulate the predictions for RGBB star counts as a function of [Fe/H], [$\alpha$/Fe], CNONa, initial helium abundance, and age. Though our study suggests a small zero-point calibration issue, RGBB star counts should nonetheless be an actionable parameter with which to constrain stellar populations in the differential sense. The most significant outliers are toward the clusters NGC 5025 (M53), NGC 6723, and NGC 7089 (M2), each of which shows a $\sim 2 \sigma$ deficit in their RGBB star counts.