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Table 1.

Jeans model results.

3D Model 2D Model
All Young Old All
Adopted quantities
m–M (a) [mag] 18.49 18.49 18.49 18.49 18.49
Distance (a) [kpc] 49.9 49.9 49.9 49.9 49.9
Ltot(b) [109 L⊙] 1.31 1.31 1.31 1.31 1.31
M*/L [M⊙/L⊙] – 1.5 – – –
re(c) [arcmin] 98.7 98.7 98.7 98.7 98.7
Nstars 71 794 71 794 54 734 17 060 968 613
Fitted parameters
α0 [deg] 80.29 ± 0.04 80.26 ± 0.04 79.69 ± 0.05 80.99 ± 0.06 81.07 (d)
δ0 [deg] −69.25 ± 0.02 −69.26 ± 0.02 −69.16 ± 0.02 −69.23 ± 0.02 −69.41 (d)
μα0 [mas yr−1] 1.88 ± 0.01 1.88 ± 0.01 1.87 ± 0.01 1.88 ± 0.01 1.87 ± 0.01
μδ0 [mas yr−1] 0.32 ± 0.01 0.32 ± 0.01 0.29 ± 0.01 0.35 ± 0.01 0.36 ± 0.01
vlos0 [km s−1] 264.83 ± 0.16 264.70 ± 0.15 266.97 ± 0.25 264.42 ± 0.23 –
θ [deg] 25.5 ± 0.2 25.2 ± 0.2 26.9 ± 0.2 25.2 ± 0.3 34.0 ± 0.1
ψ(e) [deg] 124.0 ± 0.4 124.4 ± 0.5 124.4 ± 0.4 122.7 ± 0.5 104.2 ± 0.2
qproj 0.91 ± 0.01 0.91 ± 0.01 0.89 ± 0.01 0.91 ± 0.01 0.84 ± 0.01
log rs [pc] 4.02 ± 0.02 4.30 ± 0.03 4.06 ± 0.02 3.65 ± 0.01 3.66 ± 0.01
log ρs [M⊙ pc−3] −1.99 ± 0.03 −2.47 ± 0.04 −2.05 ± 0.02 −1.89 ± 0.03 −1.40 ± 0.01
κ 1.01 ± 0.01 1.00 ± 0.01 1.00 ± 0.01 1.02 ± 0.01 1.01 ± 0.01
βz 0.70 ± 0.01 0.64 ± 0.01 0.89 ± 0.01 0.69 ± 0.01 0.72 ± 0.01
Derived quantities
Nmem(Pmem > 0.8) 28 000 27 951 11 043 16 621 761 850
qintr 0.23 ± 0.01 0.20 ± 0.01 0.15 ± 0.01 0.26 ± 0.01 0.25 ± 0.01
Mencl(f) [1010 M⊙] 1.36 ± 0.01 1.34 ± 0.01 1.38 ± 0.03 1.30 ± 0.02 1.41 ± 0.01
M200 [1011 M⊙] 1.81 ± 0.10 4.34 ± 0.50 2.06 ± 0.25 1.45 ± 0.09 0.75 ± 0.01
R200 [kpc] 75 ± 2 156 ± 6 79 ± 4 68 ± 2 51 ± 0.4
V circ max $ V_{\mathrm{circ}}^{\mathrm{max}} $ [km s−1] 115 ± 2 126 ± 4 118 ± 4 109 ± 2 98 ± 0.2
(M/L)centre [M⊙/L⊙] 2.17 ± 0.03 2.35 ± 0.03 2.11 ± 0.05 2.33 ± 0.05 3.68 ± 0.02
(M/L)encl(f) [M⊙/L⊙] 11.5 ± 0.1 10.7 ± 0.1 11.7 ± 0.2 11.0 ± 0.1 11.8 ± 0.03
(M/L)total [M⊙/L⊙] 140 ± 10 330 ± 40 160 ± 20 110 ± 10 59 ± 1

Notes. Each column shows the best-fit Jeans model parameters for the following model setups: 3D model for all stars with NFW gravitational potential (fiducial model); 3D model for all stars with mixed potential (NFW + scaled stellar density); 3D model for the young stellar population with NFW potential; 3D model for the old stellar population with NFW potential; 2D model for all stars with NFW potential.

(a)

Distance modulus and corresponding distance from de Grijs et al. (2014), Crandall & Ratra (2015).

(b)

Total luminosity from the NED database.

(c)

Radius of the exponential surface brightness profile from Gallart et al. (2004).

(d)

Centre coordinates were kept fix to the estimate by Gaia Collaboration (2021a).

(e)

Line of nodes orientation angle measured from north to east.

(f)

Enclosed mass within the radial extent of the selected kinematic tracers (6.2 kpc).

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