The masses of open star clusters and their tidal tails and the stellar initial mass function

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Table 2

Results of the models discussed in the present work.

Model name	$\frac{M_{S C, o b s}}{M_{S C, t o t}}$ $\[\frac{M_{\mathrm{SC}, \mathrm{obs}}}{M_{\mathrm{SC}, \mathrm{tot}}}\]$ (t = 300 Myr)	$\frac{M_{S C, d y n}}{M_{S C, t o t}}$ $\[\frac{M_{\mathrm{SC}, \mathrm{dyn}}}{M_{\mathrm{SC}, \mathrm{tot}}}\]$ (t = 300 Myr)	σ_z_,T1 (km/s)	σ_z_,T2 (km/s)	b	b_MLE
M1 (main model)	0.83	1.86	3.24	0.58	0.8 ± 0.3	0.9 ± 0.2
M2	0.82	2.81	2.81	0.54	1.5 ± 0.3	1.4 ± 0.3
M3	0.81	4.05	2.11	0.43	1.7 ± 0.4	1.2 ± 0.4
M4	0.78	17.52	1.70	0.27	1.8 ± 0.4	1.5 ± 0.5

Notes. The table lists the model name, the fraction of the total model mass an observer would deduce when determining the luminous mass of the SC at the end of the simulation ( $\frac{M_{S C, o b s}}{M_{S C, t o t}}$ $\[\frac{M_{\mathrm{SC}, \mathrm{obs}}}{M_{\mathrm{SC}, \mathrm{tot}}}\]$ ), the fraction of the total model mass an observer would deduce when determining the luminous mass of the SC at the end of the simulation ( $\frac{M_{S C, d y n}}{M_{S C, t o t}}$ $\[\frac{M_{\mathrm{SC}, \mathrm{dyn}}}{M_{\mathrm{SC}, \mathrm{tot}}}\]$ ), and the velocity dispersion in the z-direction averaged over the last 100 Myr of the simulation for T1 and T2 (σ_z_,T1, and σ_z_,T2 respectively). Additionally, the factor b from Eq. (26) is listed for both the fitting method and the MLE. All values are averages of the results of all models within one group (M1, M2, M3, or M4).

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