Assessing the robustness of the Galactic rotation curve inferred from the Jeans equations using Gaia DR3 and cosmological simulations

Open Access

Fig. 5

Difference between the distributions of the second moments of υ_R, υ_ϕ, and υz (from left to right) for the BJz+ and BJz- samples. We use evenly spaced bins in x and y of width 0.5 kpc. The colour bars were limited to within the 1σ value of the distribution of calculated $Δ \sqrt{〈 v_{i}^{2} 〉}$ $\Delta \sqrt {\langle v_i^2\rangle }$ for the whole sample.

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