The Sagittarius stellar stream embedded in a fermionic dark matter halo

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Table 1

Fit coefficients.

Coefficient	$μ_{Λ_{⊙}}$ ${{\mu }_{{{\Lambda }_{\odot }}}}$	$μ_{B_{⊙}}$ ${{\mu }_{{{B}_{\odot }}}}$	V_los
a₁	1.1842	−1.2360	277.4481
a₂	−1.5639π/180	1.0910π/180	0.1088
a₃	−0.39917	0.3633	1.1807
a₄	−1.9307	−1.3412	0.0400
a₅	−8.0606 · 10⁻⁴	7.3022 · 10⁻³	−0.0145
a₆	3.2441 · 10⁻⁵	−4.3315 · 10⁻⁵	−106.0409
a₇	–	–	0.4529
a₈	–	–	0.0110

Notes. Coefficients of the different functions given in Eqs. (1) and (2) used to fit the distributions of proper motion and line-of-sight velocities of stars as a function of the longitude, Λ_⊙.

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