Underlying data for the paper "Efficient black hole seed formation in low metallicity and dense stellar clusters with implications for JWST sources"

Here we provide the underlying data for the 5 extremely dense MOCCA star cluster models simulated as part of the preprint: https://arxiv.org/abs/2508.14260 For each model, the following 5 files are provided (where x is the of the VMS): 1. history-x.dat The first 207 lines are header lines describing the model. Line 208 is a header line which describes the column in this file. All header lines begin with #. This file contains the complete history of events for the star which becomes the VMS and subsequently an IMBH. Key columns: Column 1: Linetype - String to describe the event for which the information is provided in the line (e.g., SIN_EVOL is single stellar evolution, COLLISION is a 2-body collision, BIN_STAR is binary single interaction) Column 4: Time [Myr] Column 6: Star ID Column 10: Initial stellar mass before interaction [M⊙] Column 11: Final stellar mass after interaction [M⊙] Column 13: Distance from cluster center [pc] Column 19: Stellar type (SSE/BSE) Column 20: Stellar type of the merging star (if there is a COLLISION event in column 1) Column 26: Mass of the merging star (if there is a COLLISION event in column 1) [M⊙] Column 29: Final radius of the VMS [R⊙] 2. evol-sin-restart-x.datThis file contains detailed stellar evolution data for the VMS at time step. Columns (in order): Time [Myr] Star ID Stellar type (SSE/BSE) Mass [M⊙] Radius [R⊙] Physical time [Myr] SSE/BSE epoch Bolometric luminosity [L⊙] Core mass [M⊙] Core radius [R⊙] Envelope mass [M⊙] Envelope radius [R⊙] Stellar age = (physical time – epoch) [Myr] 3. system.datStandard MOCCA output file containing global cluster properties over time. Column descriptions are provided in the file header that are prefixed with # and describe each column. The first 2498 lines are these header lines which describe the 572 columns that are in this output file. The physical time of the simulation in Myr is in column 2. 4. lagrangi.datTracks the evolution of Lagrangian radii (with and without the VMS/IMBH). Column descriptions are provided in the header lines which start with #. There are 47 columns which are described in the first 190 lines of this file. 5. escape-5myr.datLists stars escaping from the cluster within the first 5 Myr. Columns in order: Escape time [Myr] Mass of component 1 [M⊙] Mass of component 2 [M⊙] (0.0 for single escapers) Stellar type of component 1 (SSE/BSE) Stellar type of component 2 (SSE/BSE) Total escaping mass [M⊙] The integer values for SSE/BSE stellar types are explained below:0 - Fully convective low-mass MS star (M < 0.7 M⊙)1 - Main Sequence star (M > 0.7 M☉)2 - Hertzsprung Gap (subgiant star)3 - First Giant Branch4 - Core Helium Burning5 - First Asymptotic Giant Branch6 - Second Asymptotic Giant Branch7 - Main Sequence Naked Helium star8 - Hertzsprung Gap Naked Helium star9 - Giant Branch Naked Helium star10 - Helium White Dwarf11 - Carbon/Oxygen White Dwarf12 - Oxygen/Neon White Dwarf13 - Neutron Star14 - Black Hole