Shapes of dark matter haloes with discrete globular cluster dynamics: The example of NGC 5128 (Centaurus A)

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Volume 687 (July 2024)

A&A, 687 (2024) A80

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Table 1.

Overview of the different magnitude ranges defined in this work.

	Mag cut	N_GC	$N_{GC}^{theo}$ $N_{\mathrm{GC}}^{\mathrm{theo}}$	$N_{GC}^{theo} / N_{GC}$ $N_{\mathrm{GC}}^{\mathrm{theo}}/N_{\mathrm{GC}}$	f_r ^( † )
All	–	2341	1450 ± 160	0.62 ± 0.07	0.48
A	r₀ < −9	338	124 ± 13	0.37 ± 0.04	0.36
B	−9 ≤ r₀ < −8.5	259	123 ± 13	0.48 ± 0.05	0.41
C ^( ⋆ )	−8.5 ≤ r₀ < −7.9	412	225 ± 24	0.55 ± 0.06	0.53
D	−7.9 ≤ r₀ < −7	1029	422 ± 46	0.41 ± 0.05	0.56
E ^( ‡ )	r₀ ≥ −7	303	554 ± 61	1.83 ± 0.2	0.35

Notes. The subsample name is shown in Col. 1. The r₀ band magnitude range of the corresponding subsample is in Col. 2 with the number of candidate GCs from the T17 dataset in Col. 3 and theoretical prediction based on the work by H21 in Col. 4. The ratio between the number of theoretically predicted GCs and candidate GCs ( $N_{GC}^{theo} / N_{GC}$ $N_{\mathrm{GC}}^{\mathrm{theo}}/N_{\mathrm{GC}}$ ) is shown in Col. 5. The last column shows the fraction of red GCs based on the separating magnitude of (u − z)₀ = 2.6. ^( † )Fraction of GCs with (u − z)₀ ≥ 2.6. ^( ⋆ )The most relaxed sample of GCs. ^( ‡ )This subsample is strongly affected by the magnitude completeness limit of the survey.

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