Massive star clusters in the semi-analytical galaxy formation model L-Galaxies 2020

Open Access

Table A.2

Variations in the initial half-mass radii of star clusters.

Model	Prescription
Fiducial	r_c,h = 1.0 pc
Compact	r_c,h = 0.1 pc
Density	r_c,h = 1 pc × (m_c/10⁴ M_⊙)^0.3
Empirical(a)	r_c,h = 2.37 pc × (m_c/10⁴ M_⊙)^0.18
Theoretical(b)	*(93)* $r_{c, h} \propto \sqrt{m_{c} / Σ_{g}}$ $Mathematical equation: ${r_{{\rm{c}},h}} \propto \sqrt {{m_c}/{\Sigma _{\rm{g}}}} $$

(a) Fitting results provided by Reina-Campos et al. (2023a) for the data of Brown & Gnedin (2021) when limiting the star cluster population to ages 1 Myr ≤ τ_c ≤ 10 Myr.

(b) Adopted from Choksi & Kruijssen (2021). To avoid extremely compact or extended clusters we introduce a lower and upper boundary to a star cluster’s half-mass radius of 0.1 and 100 pc, respectively.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.