Hidden Population III Descendants in Ultra-Faint Dwarf Galaxies

TL;DR

This study uses a chemical evolution model of the ultra-faint dwarf galaxy Boötes I to identify potential descendants of the first stars, revealing rare candidates with signatures of early supernovae and emphasizing the importance of detailed modeling.

Contribution

The paper introduces a data-calibrated chemical evolution model to identify and analyze potential Pop III star descendants in ultra-faint dwarf galaxies, highlighting their chemical signatures and rarity.

Findings

Low metal retention in UFDs due to SNe feedback

Higher Pop III SN energy leads to lower metal retention

Identified three candidate stars as Pop III descendants in Boötes I

Abstract

The elusive properties of the first (Pop III) stars can be indirectly unveiled by uncovering their true descendants. To this aim, we exploit our data-calibrated model for the best-studied ultra-faint dwarf (UFD) galaxy, Bo\"otes I, which tracks the chemical evolution (from carbon to zinc) of individual stars from their formation to the present day. We explore the chemical imprint of Pop III supernovae (SNe), with different explosion energies and masses, showing that they leave distinct chemical signatures in their descendants. We find that UFDs are strongly affected by SNe-driven feedback resulting in a very low fraction of metals retained by their gravitational potential well ($<2.5\%$). Furthermore, the higher the Pop III SN explosion energy, the lower the fraction of metals retained. Thus, the probability to find descendants of energetic Pair Instability SNe is extremely low in these systems. Conversely, UFDs are ideal cosmic laboratories to identify the fingerprints of less massive and energetic Pop III SNe through their [X/Fe] abundance ratios. Digging into the literature data of Bo\"otes I, we uncover three hidden candidates for Pop III descendants: one mono-enriched and two multi-enriched. These stars show the chemical signature of Pop III SNe in the mass range $[20-65] \rm M_{\odot}$, spanning a wide range in explosion energies $[0.3- 10]10^{51}$ erg. In conclusion, candidates for Pop III descendants are hidden in ancient UFDs but those mono-enriched by a single Pop III SN are extremely rare. Thus, self-consistent models such as the one presented here are required to uncover these precious fossils and probe the properties of the first Pop III supernovae.