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Table 3.

Main results and priors for MAMPOSST-PM runs, using the merged sample from the cleaned HST, Gaia and MUSE datasets.

Model rβ β(r) Σ Nfree R−1 β0 βout rscale n MBH MCUO MGC −Δlnℒmax ΔAICc ΔBIC
[pc] [arcmin] [M] [103 M] [104 M]
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15) (16)
1 iso S 8 0.003 0 0 18.82 29.62 8.90
2 gOM S 11 18.25 34.49 34.81
3 TAND gOM S 10 0.007 18.45 32.89 26.20
4 TAND gOM S 9 0.005 0 18.50 30.98 17.28
5 TAND gOM S 9 0.003 0 18.85 31.68 17.98
6 iso S 11 0.017 0 0 7.09 12.17 12.49
iso S 0 0
7 iso S 7 0.002 0 0 25.98 41.93 14.20
8 iso S 10 0.009 0 0 13.68 23.35 16.66
iso S 0 0
9 iso S 10 0.007 0 0 10.09 16.17 9.48
iso P 0 0
10 iso S 9 0.002 0 0 9.86 13.70
iso P 0 0
11 iso S 9 0.004 0 0 11.14 16.26 2.56
iso H 0 0
12 iso S 10 0.012 0 0 9.69 15.37 8.68
iso S 0 0
13 TAND gOM S 11 9.92 17.83 18.15
gOM P 0 0
14 iso S 12 0.014 0 0 7.33
iso S 0 0
iso P 0 0
15 TAND gOM S 16 0.009 −0.56 6.91 42.29
TAND gOM S
iso P 0 0

Notes. Columns are (1): run number; (2): anisotropy radius (where TAND is tied anisotropy number density, rβ = rscale); (3): velocity anisotropy model (“iso” for isotropic); (4): surface density model (“S” for Sérsic, “P” for Plummer, “H” for Hernquist); (5): number of free parameters; (6): MCMC convergence criterion (R−1 ≤ 0.02 is considered as properly converged, worse convergence runs are shown in bold red); (7): anisotropy value at r = 0; (8): anisotropy value at rout = 8′; (9): scale radius (effective – half projected number – radius Re for Sérsic, otherwise radius of 3D density slope −2, with r−2 = 1.63 Re for Plummer and r−2 = 0.28 Re for Hernquist); (10): Sérsic index; (11): black hole mass; (12): mass of inner subcluster of unresolved objects (CUO); (13): mass of the stellar population considered; (14): difference in minus natural logarithm of the maximum likelihood relative to model 14; (15): difference in AIC (Eq. (25)) relative to best value; (16): difference in BIC (Eq. (26)) relative to best value. Blue bold zeros for −Δlnℒmax, ΔAICc and ΔBIC represent the reference values among all runs, for each column, respectively. Values in bold gray were fixed parameters. The values of Cols. (9)–(13) are at maximum likelihood (black) or medians (orange and italics, when the MLE is outside the 16−84 percentiles). The uncertainties are from the 16th and 84th percentiles of the marginal distributions. The number of stars in each subset is 8255, the maximum allowed PM error (Eq. (12)) for those runs is 0.197 mas yr−1, the distance was considered as 2.39 kpc, and the GC center was that of Goldsbury et al. (2010). For models considering two main-sequence populations, the parameters of the brighter (fainter) population is displayed first (next).

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