Metal-poor Stars Observed with the Automated Planet Finder Telescope. III. CEMP-no Stars are the Descendant of Population III Stars

TL;DR

This paper investigates the origins of CEMP-no stars by comparing their chemical abundances with supernova models, suggesting they descend from Population III stars with specific mass and explosion energy ranges, and analyzing their galactic kinematics.

Contribution

It provides a probabilistic analysis linking CEMP-no stars to Population III supernova progenitors based on abundance ratios and kinematic data.

Findings

Progenitor stars likely had masses between 11-22 solar masses.

Explosion energies of progenitors estimated between 0.3-1.8 x 10^{51} erg.

CEMP-no stars are not associated with known Gaia halo remnants.

Abstract

In this study, we report a probabilistic insight into the stellar mass and supernovae (SNe) explosion energy of the possible progenitors of five CEMP-no stars. This was done by a direct comparison between the abundance ratios [X/Fe] of the light-elements and the predicted nucleosynthetic yields of SN of high-mass metal-free stars. This comparison suggests possible progenitors with stellar mass range of 11 - 22\,M$_{\odot}$ and explosion energies of $0.3 - 1.8 \times 10^{51}$\,erg. The coupling of the chemical abundances with kinematics derived from $Gaia$ DR2 suggests that our sample do not enter the outer-halo region. In addition, we suggest that these CEMP-no stars are not $Gaia$-Sausage nor $Gaia$-Sequoia remnant stars, but another accretion event might be responsible for the contribution of these stars to the Galactic Halo of the Milky-Way.