]>SGRs and AXPs: Evidence for Delayed Amplification of Magnetic Field after Neutron Star Formation? : Table 1
Table 1: SGRs/AXPs data mainly from Gaensler et al. [5], Marsden et al. [4], the atnf pulsar catalog [12], and Camilo [13]; with updates as indicated by footnotes. Spin-down ages, 𝝉 S D , and SNR ages, 𝝉 S N R , in years.
Source 𝜏 S D 𝜏 S N R , l o w e r 𝜏 S N R , u p p e r 𝜏 S N R , m e a n Assoc. † 𝑑 k p c 𝑣 S N R (km/s) 𝑣 S D (km/s)
SGR1806 − 20 281 3500 30000 10300 S 1 ( < 1%) 1 5 2 100 3800
SGR1900 + 14 1050 9600 30000 17000 A 3 (4%) 7 2000 32000
SGR0525 − 66 1960 5000 16000 8940 S (0.2–0.7%) 50 800 3600
SGR1627 − 41 N/A 2600 30000 8830 A 4 (5%) 11 460 N/A
AXP1E1841 − 045 4510 500 2500 1120 S (0.01%) 7 < 890 < 220
AXP1845 − 0258 ‡ N/A 600 30000 4240 S (0.2%) < 20 < 870 N/A
AXP1E2259 + 586 228000 3000 17000 7140 S (0.05%) 3 7 < 360 < 11
AXP1E1048 − 5937 3 7 8 0 5 N/A N/A N/A N/A N/A N/A N/A
AXPRXS1708 − 4009 8960 N/A N/A N/A N/A N/A N/A N/A
TAXPXTEJ1810 − 197 1 1 3 0 0 6 N/A N/A N/A N/A N/A N/A N/A
TAXPJ0100 − 7211 6760 N/A N/A N/A N/A N/A N/A N/A
AXP1547 − 5408 1400 N/A N/A N/A N/AN/A N/A N/A
AXP4U0142 + 615 70200 N/A N/A N/A N/A N/A N/A N/A
1 Frail et al. [14]; 2 McClure-Griffiths and Gaensler [15]; 3 Vasisht et al. [16]; Lorimer and Xilouris [17]; 4 Smith et al. [18]; 5 based on ̇ 𝜈 prior to 2002 outburst [19]; 6 Camillo et al. [20]; 7 Kothes et al. [21]. † S for secure and A for ambiguous association (random association probability given in brackets); ‡ unconfirmed AXP.