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.
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