SIEGE - IV. Compact star clusters in cosmological simulations with a high star formation efficiency and subparsec resolution

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Volume 699 (July 2025)

A&A, 699 (2025) A31

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Table 1

Relevant properties of clumps across redshift.

z	15.5	13	10.5	10	9	8	7	6.14
N_clump	4	104	207	320	369	408	436	358
Total stellar mass M_⋆,tot (10⁶ M_⊙)	0.07	1.81	6.58	12.56	19.08	28.49	46.83	72.27
Total clump mass M_clump,tot (10⁶ M_⊙)	0.039	0.423	0.874	1.51	1.51	1.67	1.76	3.69
Clump mass fraction f_clump	0.57	0.23	0.13	0.12	0.08	0.06	0.04	0.05
CMF slope α	−	$- {2.03}_{- 0.09}^{+ 0.09}$ $\[-2.03_{-0.09}^{+0.09}\]$	$- {2.15}_{- 0.07}^{+ 0.07}$ $\[-2.15_{-0.07}^{+0.07}\]$	$- {2.15}_{- 0.09}^{+ 0.09}$ $\[-2.15_{-0.09}^{+0.09}\]$	$- {2.19}_{- 0.11}^{+ 0.11}$ $\[-2.19_{-0.11}^{+0.11}\]$	$- {2.18}_{- 0.18}^{+ 0.18}$ $\[-2.18_{-0.18}^{+0.18}\]$	$- {2.20}_{- 0.15}^{+ 0.15}$ $\[-2.20_{-0.15}^{+0.15}\]$	$- {2.17}_{- 0.18}^{+ 0.18}$ $\[-2.17_{-0.18}^{+0.18}\]$
young CMF slope α_{50 Myr}	−	$- {2.07}_{- 0.19}^{+ 0.19}$ $\[-2.07_{-0.19}^{+0.19}\]$	$- {2.02}_{- 0.08}^{+ 0.08}$ $\[-2.02_{-0.08}^{+0.08}\]$	$- {2.02}_{- 0.15}^{+ 0.15}$ $\[-2.02_{-0.15}^{+0.15}\]$	$- {2.15}_{- 0.15}^{+ 0.15}$ $\[-2.15_{-0.15}^{+0.15}\]$	$- {1.98}_{- 0.23}^{+ 0.23}$ $\[-1.98_{-0.23}^{+0.23}\]$	$- {1.60}_{- 0.18}^{+ 0.18}$ $\[-1.60_{-0.18}^{+0.18}\]$	$- {1.73}_{- 0.22}^{+ 0.22}$ $\[-1.73_{-0.22}^{+0.22}\]$
log R_e − log M_⋆ relation (m_{R_eff–M_⋆}), q_{R_eff–M_⋆})	(0.32, −1.48)	(0.44, −1.59)	(0.46, −1.55)	(0.30, −0.93)	(0.36, −1.07)	(0.53, −1.57)	(0.38, −1.02)	(0.39, −1.08)

Notes. From top to bottom: the considered redshift z; the total number of clumps identified at the end of the procedure described in Section 4, N_clump; the total stellar mass in the simulation volume M_⋆,tot; the total stellar mass in clumps M_clump,tot; the clump mass fraction f_clump; the slope α of the CMF ( $\frac{d N}{d M_{⋆}} \propto M_{⋆}^{α}$ $\[\frac{\mathrm{d} N}{\mathrm{~d} M_{\star}} \propto M_{\star}^{\alpha}\]$ ) of all clumps and the slope α_{50 Myr} of the CMF obtained considering only clumps younger than 50 Myr; and the values of m_{R_eff–M_⋆} and q_{R_eff–M_⋆}, which result from the fits to the size-mass relation outlined in Section 5.4.

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