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Table 3.

Potentially observable glitching pulsars from IAR.

J name P0 S1400 W50(a) DM NG
[s] [mJy] [ms] [pc cm−3]
J0835−4510 ( † ) 0.08933 1050 1.4 67.97 19
J1644−4559 ( † ) 0.45506 300.0 8.0 478.8 3
J1731−4744 ( † ) 0.82983 27.00 17.1 123.056 7
J0742−2822 ( † ) 0.16676 26.00 4.2 73.728 7
J1721−3532 ( † ) 0.28042 16.80 29.8 496.0 1
J1709−4429 ( † ) 0.10246 12.10 5.7 75.68 1
J1803−2137 ( † ) 0.13367 9.60 13.1 233.99 5
J1818−1422 0.29149 9.60 17.1 622.0 1
J1705−1906 0.29899 9.30 154.2 22.907 1
J1048−5832 ( † ) 0.12367 9.10 4.8 128.679 3
J1740−3015 ( † ) 0.60689 8.90 2.4 151.96 36
J1757−2421 0.23411 7.20 9.6 179.454 1
J1801−2304 0.41583 7.00 128.3 1073.9 9
J1705−3423 0.25543 5.30 11.7 146.36 3
J1539−5626 0.24339 5.00 7.6 175.85 1
J1826−1334 0.10149 4.70 5.9 231.0 6
J1302−6350 0.04776 4.50 23.4 146.73 1
J1739−2903 0.32288 4.50 6.0 138.55 1
J1328−4357 0.53270 4.40 10.4 42.0 1
J1730−3350 0.13946 4.30 7.1 261.29 2
J1614−5048 0.23169 4.10 8.4 582.4 1
J1809−1917 0.08275 2.80 17.0 197.1 1
J1341−6220 0.19334 2.70 7.7 719.65 12
J0758−1528 0.68227 2.60 3.4 63.327 1
J1835−1106 0.16591 2.50 3.9 132.679 1
J1141−6545 0.39390 2.40 4.4 116.080 1
J1743−3150 2.41458 2.10 42.3 193.05 1

Notes. P0 is the barycentric period of the pulsar, S1400 the mean flux density at 1400 MHz, W50, width of pulse at 50% of peak (ms), D is the distance based on the Yao et al. (2017) electron density model, and NG is the number of glitches reported for the pulsar. Pulsars marked with a ( † ) are already being monitored at IAR.

(a)

Quoted values are indicative only, as the width of pulse at 50% of peak is a function of both observing frequency and time resolution.

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