Red giant branch bump brightness in 7 metal-poor globular clusters obtained with GAIA DR2

Journal
Date Issued
2022
Author(s)
Song, Fen
•
Yuan, Zunli
•
Li, Yan
•
Wu, Xuchao
•
•
Poon, Helen
•
Wu, Tao
•
Nie, Jundan
•
Song, Hanfeng
•
Han, Cheng
•
Yang, Ye
•
Li, Yuxuan
•
Bai, Xingming
DOI
Abstract
The identification of the red giant branch bump brightness in metal-poor globular clusters is important for low-mass stellar evolution. The release of Gaia DR2 prompted us to revisit the red giant branch bump (RGBB) in galactic globular clusters. We apply a popular nonparametric density estimation approach, kernel density estimation (KDE), to explore the position of RGBB in 7 metal-poor globular clusters (GCs). The G and V magnitudes of the RGBB according to our clustering algorithm, GB,K and VB,K, respectively show the RGB bump magnitude detected by the KDE method in G band and V band. They show the overdensity location in the luminosity function of the RGB stars. Based on the results derived by KDE, a maximum-likelihood analysis via a Markov Chain Monte Carlo (MCMC) approach is adopted to detect the RGB bump feature and obtain more accurate RGBB brightnesses in G band and V band for the samples. We find that the red giant branch bump brightness becomes fainter as the global metallicity increases in clusters with [M/H]≤‑1.4. We present the empirical relation between the global metallicity [M/H] and absolute magnitude MV of the red giant branch bump for clusters with [M/H]≤‑1.4. We verify that discrepancies between observations and theory for metal-poor globular clusters with [M/H]≤‑1.4....
Volume
367
Issue
3
Uri
Url
Issn Identifier
0004-640X
Rights
open.access
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