Kinematic constraints on the ages and kick velocities of Galactic neutron star binaries

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Table 2

Estimated timescales of the Galactic BNS pulsars: the characteristic age (τ_c, Eq. (2)); kinematic age (τ_kin) for the first and second (χ₂) disc crossing, assuming either GC isotropy or LSR isotropy; and the merger time (τ_gw).

BNS pulsar	τ_c	τ_kin				τ_gw(a)
		χ₁		χ₂
		GC isotropy	LSR isotropy	GC isotropy	LSR isotropy
	(Myr)	(Myr)	(Myr)	(Myr)	(Myr)	(Myr)
J0737−3039A^(b)	204.49247(7)	$66_{- 38}^{+ 41}$ $66_{ - 38}^{ + 41}$	$40_{- 5}^{+ 4}$ $40_{ - 5}^{ + 4}$	$503_{- 338}^{+ 285}$ $503_{ - 338}^{ + 285}$	$96_{- 14}^{+ 14}$ $96_{ - 14}^{ + 14}$	85
J0737−3039B^(b)	49.3(4)	$66_{- 38}^{+ 41}$ $66_{ - 38}^{ + 41}$	$40_{- 5}^{+ 4}$ $40_{ - 5}^{ + 4}$	$503_{- 338}^{+ 285}$ $503_{ - 338}^{ + 285}$	$96_{- 14}^{+ 14}$ $96_{ - 14}^{ + 14}$	85
B1913+16	108.596(4)	$10_{- 2}^{+ 2}$ $10_{ - 2}^{ + 2}$	$7_{- 1}^{+ 1}$ $7_{ - 1}^{ + 1}$	$28_{- 2}^{+ 6}$ $28_{ - 2}^{ + 6}$	$37_{- 7}^{+ 11}$ $37_{ - 7}^{ + 11}$	301
J1913+1102	2457(1)	$45_{- 15}^{+ 45}$ $45_{ - 15}^{ + 45}$	$51_{- 16}^{+ 46}$ $51_{ - 16}^{ + 46}$	$68_{- 21}^{+ 69}$ $68_{ - 21}^{ + 69}$	$105_{- 39}^{+ 109}$ $105_{ - 39}^{ + 109}$	465
J0509+3801	153.02(4)	$4_{- 1}^{+ 1}$ $4_{ - 1}^{ + 1}$	$4_{- 1}^{+ 1}$ $4_{ - 1}^{ + 1}$	$72_{- 19}^{+ 27}$ $72_{ - 19}^{ + 27}$	$63_{- 15}^{+ 37}$ $63_{ - 15}^{ + 37}$	579
J1756-2251	443.494(1)	$3_{- 2}^{+ 31}$ $3_{ - 2}^{ + 31}$	$2_{- 2}^{+ 34}$ $2_{ - 2}^{ + 34}$	$58_{- 25}^{+ 63}$ $58_{ - 25}^{ + 63}$	$59_{- 15}^{+ 27}$ $59_{ - 15}^{ + 27}$	1457
B1534+12	248.0794(3)	$64_{- 46}^{+ 19}$ $64_{ - 46}^{ + 19}$	$55_{- 40}^{+ 13}$ $55_{ - 40}^{ + 13}$	$136_{- 45}^{+ 73}$ $136_{ - 45}^{ + 73}$	$105_{- 17}^{+ 67}$ $105_{ - 17}^{ + 67}$	2735
J1829+2456	13 152(6)	$32_{- 4}^{+ 1}$ $32_{ - 4}^{ + 1}$	$13_{- 3}^{+ 4}$ $13_{ - 3}^{ + 4}$	$51_{- 4}^{+ 35}$ $51_{ - 4}^{ + 35}$	$62_{- 7}^{+ 18}$ $62_{ - 7}^{ + 18}$	55 375^(c)
J1411+2551	10 300(600)	$42_{- 35}^{+ 84}$ $42_{ - 35}^{ + 84}$	$32_{- 17}^{+ 28}$ $32_{ - 17}^{ + 28}$	$164_{- 79}^{+ 140}$ $164_{ - 79}^{ + 140}$	$107_{- 32}^{+ 76}$ $107_{ - 32}^{ + 76}$	465446^(c)
J0453+1559	3900(2)	$10_{- 8}^{+ 138}$ $10_{ - 8}^{ + 138}$	$15_{- 7}^{+ 20}$ $15_{ - 7}^{ + 20}$	$86_{- 32}^{+ 137}$ $86_{ - 32}^{ + 137}$	$81_{- 15}^{+ 16}$ $81_{ - 15}^{ + 16}$	1456 721^(c)
J1518+4904	23 870(2)^(c)	$69_{- 49}^{+ 27}$ $69_{ - 49}^{ + 27}$	$24_{- 9}^{+ 13}$ $24_{ - 9}^{ + 13}$	$158_{- 66}^{+ 67}$ $158_{ - 66}^{ + 67}$	$85_{- 2}^{+ 11}$ $85_{ - 2}^{ + 11}$	8 826 539^(c)
J1930-1852	163.40(6)	$11_{- 2}^{+ 3}$ $11_{ - 2}^{ + 3}$	$9_{- 1}^{+ 2}$ $9_{ - 1}^{ + 2}$	$49_{- 14}^{+ 89}$ $49_{ - 14}^{ + 89}$	$66_{- 23}^{+ 77}$ $66_{ - 23}^{ + 77}$	10^8(c)

Notes. Quantities have been determined through a Monte Carlo estimation, as described in Sect. 2. The median values of the resulting distributions and their uncertainties are given in a manner similar to Table 3. ^(a)Lower bounds of the values determined following Peters (1964), similarly to Gaspari et al. (2024). ^(b)Two components of the double-pulsar binary J0737-3039A/B, which share the same τ_kin and τ_gw. ^(c)Exceeds a Hubble time.

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