Investigating the origin of the Milky Way streams - A revised look at their orbital pole distribution in light of precession effects

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Volume 702 (October 2025)

A&A, 702 (2025) A62

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Table 3.

Similar to Table 2, but for the full l-parameter space.

Distance cut	P (N = 100)	P (N = 300)	P (N = 500)
d < 100 kpc	$(4 . 26_{- 0.00}^{+ 6.83}) \times 10^{- 2}$ $(4.26^{+6.83}_{-0.00})\times 10^{-2}$ ( $(2 . 03_{- 0.43}^{+ 0.00}) σ$ $(2.03^{+0.00}_{-0.43})\sigma$ )	$(2 . 83_{- 0.00}^{+ 26.58}) \times 10^{- 2}$ $(2.83^{+26.58}_{-0.00})\times 10^{-2}$ ( $(2 . 19_{- 1.14}^{+ 0.00}) σ$ $(2.19^{+0.00}_{-1.14})\sigma$ )	$(1 . 86_{- 0.00}^{+ 12.76}) \times 10^{- 2}$ $(1.86^{+12.76}_{-0.00})\times 10^{-2}$ ( $(2 . 35_{- 0.90}^{+ 0.00}) σ$ $(2.35^{+0.00}_{-0.90})\sigma$ )
d < 150 kpc	$(4 . 54_{- 0.00}^{+ 7.74}) \times 10^{- 4}$ $(4.54^{+7.74}_{-0.00})\times 10^{-4}$ ( $(3 . 51_{- 0.27}^{+ 0.00}) σ$ $(3.51^{+0.00}_{-0.27})\sigma$ )	$(3 . 77_{- 0.00}^{+ 3.65}) \times 10^{- 8}$ $(3.77^{+3.65}_{-0.00})\times 10^{-8}$ ( $(5 . 50_{- 0.12}^{+ 0.00}) σ$ $(5.50^{+0.00}_{-0.12})\sigma$ )	$(3 . 38_{- 0.00}^{+ 6.79}) \times 10^{- 14}$ $(3.38^{+6.79}_{-0.00})\times 10^{-14}$ ( $(7 . 58_{- 0.14}^{+ 0.00}) σ$ $(7.58^{+0.00}_{-0.14})\sigma$ )
d < 200 kpc	$(1 . 96_{- 0.00}^{+ 3.87}) \times 10^{- 5}$ $(1.96^{+3.87}_{-0.00})\times 10^{-5}$ ( $(4 . 27_{- 0.25}^{+ 0.00}) σ$ $(4.27^{+0.00}_{-0.25})\sigma$ )	$(1 . 25_{- 0.00}^{+ 2.99}) \times 10^{- 10}$ $(1.25^{+2.99}_{-0.00})\times 10^{-10}$ ( $(6 . 43_{- 0.19}^{+ 0.00}) σ$ $(6.43^{+0.00}_{-0.19})\sigma$ )	≲1.68 × 10⁻¹² ((≳7.06σ))
d < 350 kpc	$(1 . 14_{- 0.00}^{+ 2.60}) \times 10^{- 6}$ $(1.14^{+2.60}_{-0.00})\times 10^{-6}$ ( $(4 . 87_{- 0.24}^{+ 0.00}) σ$ $(4.87^{+0.00}_{-0.24})\sigma$ )	$(7 . 36_{- 0.00}^{+ 15.62}) \times 10^{- 16}$ $(7.36^{+15.62}_{-0.00})\times 10^{-16}$ ( $(8 . 06_{- 0.14}^{+ 0.00}) σ$ $(8.06^{+0.00}_{-0.14})\sigma$ )	≲1.80 × 10⁻²⁰ ((≳8.54σ))

Notes. The last two lines in column P(N = 500) are only given as approximate values due to difficulties of the code in handling extremely low probabilities in a long-tailed probability distribution.

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