Black hole mass function shift in proto-stellar-clusters driven by gas accretion

Abstract

The James Webb Space Telescope (JWST) has observed compact, massive proto-stellar clusters of low metallicity in the Cosmic Gems arc galaxy at high redshift, which represent likely precursors to globular clusters. We model the mass growth of stellar black holes (BHs) during the first few Myr of the life of a massive, compact, gaseous stellar cluster before stellar feedback expels the primordial gas. At high redshift, in a lower metallicity environment stellar winds get weaker allowing for larger gas-depletion time-scales in the cluster despite of energetic pair-instability supernova (PISN) feedback for sufficiently compact clusters. Mass segregation drives the massive stellar progenitors of BHs in the center of the cluster where gas is most dense. We estimate the conditions for which the initial black hole mass function (BHMF), with a PISN-induced cut-off $<55{\mathrm{M}}_{\odot }$, gets shifted to values within the upper BH mass gap, $\sim 60-130{\mathrm{M}}_{\odot }$, or higher, as observed by Gravitational Wave (GW) experiments LIGO-Virgo-KAGRA. We find that the BHs are shifted by the end of gas depletion to values within and above the mass gap, well within the range of BH components of the recent GW-signal GW231123, depending on total mass, star formation efficiency, metallicity and compactness. The individual BH mass increase follows approximately a surprisingly steep power law with respect to initial BH mass with an exponent in the range $\approx 4-6$. This occurs in gaseous proto-stellar clusters that are sufficiently massive and compact, with typical values of total mass $\sim 10^6{\mathrm{M}}_{\odot }$ and size $\sim 1\mathrm{pc}$. Our analysis suggests that proto-stellar clusters at high redshift such as Cosmic Gems arc clusters have generated through early gas accretion, BHs as heavy as $\sim 10^2-10^3{\mathrm{M}}_{\odot }$.

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