Revisiting the Perseus Cluster II: Metallicity-Dependence of Massive Stars and Chemical Enrichment History

Abstract

The legacy Hitomi telescope has delivered the precise measurements of the chemical abundances in the Perseus Cluster, covering the Si-group (Si, S, Ar, Ca) and Fe-group elements (Cr, Mn, Ni). In Paper I (Leung et al., ApJ 2025), we examined the role of convection parameters and presented new core-collapse supernova (CCSN) explosion models at solar metallicity, which fit the observed abundance pattern. In this article, we extend our calculation for the stellar evolutionary models and CCSN models of the initial mass $15 - 60M_{\odot}$ and the metallicity $Z = 0 - Z_{\odot}$. The detailed pre- and post-explosion chemical profiles are calculated with a large post-processing network to capture the production of $α$-chain elements (e.g., Si, S, Ar), odd-number elements (e.g., P, K, Cl), and iron-group elements (e.g., Mn, Ni). We study the role of CCSNe in the production of these elements. We compare the galactic chemical evolution model based on the nucleosynthesis yield of the new massive stars and other yield tables from the literature. For each supernova yield, we perform parameter surveys and search for configurations that produce the best-fit model and best-rate model using the Perseus Cluster as the reference. From the survey, we study how individual chemical elements affect the contributions of massive stars and Type Ia supernovae in the cosmic chemical enrichment

Figures (7)

• Figure 1: The chemical composition of the model with $M=20 M_{\odot}$ and $Z=Z_{\odot}$ at the end of the O burning phase by directly solving the 127-isotope network in the MESA code (solid line) and by post-processing the thermodynamics trajectory from models using the 22-isotope network (dashed line).
• Figure 2: (top panel) The pre-collapse temperature profiles of M25Z0 (blue solid line), M25Z1e-1 (orange dashed line) and M25Z1 (green dotted line). (bottom panel) Same as the top panel but for the abundances of $^{16}$O (blue), $^{28}$Si (orange) and $^{56}$Fe (green). The line style corresponds to the initial metallicity.
• Figure 3: (top panel) The scaled mass fraction[X/$^{56}$Fe] for the stable isotopes after explosion of 15 $M_{\odot}$ progenitor assuming $1 \times 10^{51}$ erg, with $Z = 0$ (M15Z0, blue circles), $Z = 0.1 Z_{\odot}$ (M15Z1e-1, orange triangles) and $Z = Z_{\odot}$ (M15Z1, black squares). Isotopes from C to Zn are shown. The two horizontal lines refer to two times (upper line) and half (lower line) of the solar ratios. (middle panel) Same as the top panel, but for M20Z0, M20Z1e-1, and M20Z1. (bottom panel) Same as the top panel, but for M25Z0, M25Z1e-1, and M25Z1.
• Figure 4: (top panel) The scaled mass fraction[X/$^{56}$Fe] for the stable isotopes after explosion of 40 $M_{\odot}$ progenitor assuming $1 \times 10^{51}$ erg, with $Z = 0$ (M30Z0, blue circles), $Z = 0.1 Z_{\odot}$ (M30Z1e-1, orange triangles) and $Z = Z_{\odot}$ (M30Z1, black squares). Isotopes from C to Zn are shown. (middle panel) Same as the top panel, but for M40Z0, M40Z1e-1, and M40Z1. (bottom panel) Same as the top panel, but for M60Z0, M60Z1e-1, and M60Z1.
• Figure 5: (top left panel) The scaled mass fraction[X/Fe] for the stable isotopes after explosion of 15 $M_{\odot}$ progenitor assuming $1 \times 10^{51}$ erg, with $Z = 0$ (blue circles), $Z = 0.1 Z_{\odot}$ (orange triangles) and $Z = Z_{\odot}$ (black square). Elements from C to Zn are shown. Other panels are the same as the top left panel, but for M20Z0, M20Z1e-1, M20Z1 (top right panel), M25Z0, M25Z1e-1, M25Z1 (middle left panel), M30Z0, M30Z1e-1, M30Z1 (middle right panel), M40Z0, M40Z1e-1, M40Z1 (bottom left panel), M60Z0, M60Z1e-1, M60Z1 (bottom right panel).