Table 3.
Properties of the ordinary and millisecond pulsars that are investigated in this study.
| Pulsar | ObsID | tPN | tM1 | tM2 | bPN | bM1 | bM2 | P | D1 | D2 | log Ė | NH, 21 |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (ks) | (ks) | (ks) | (c/s) | (c/s) | (c/s) | (ms) | (kpc) | (kpc) | (erg s−1) | |||
| J0340+4130 | 0605470101 | 19.5 (6.3) | 20.7 (14.8) | 20.6 (15.0) | 0.4 (TN) | 0.35 (TN) | 0.35 (M) | 3 | 1.60( * ) | 1.73 | 33.9 | 1.5 |
| J1435−5954 | 0692050101 | 130.1 (90.0) | − | − | 0.4 (M) | − | − | 473 | 1.06 | 1.18 | 32.7 | 1.3 |
| J1535−4114 | 0652610201 | 101.4 (63.2) | 102.4 (84.6) | 102.4 (83.9) | 0.4 (TK) | 0.35 (TK) | 0.35 (TK) | 432 | 2.77 | 1.95 | 33.3 | 1.99 |
| J1622−0315 (B) | 0784770401 | 19.0 (4.8) | 20.6 (16.5) | 20.6 (16.1) | 0.4 (M) | 0.30 (M) | 0.35 (M) | 4 | 1.14 | 1.11 | 33.9 | 0.6 |
| J1643−1224 (B) | 0742520101 | 21.8 (9.3) | 23.4 (13.8) | 23.4 (11.1) | 0.4 (M) | 0.35 (M) | 0.35 (M) | 5 | 0.74( * ) | 2.40 | 33.8 | 1.87 |
| J1831−0952 | 0822330101 | − | 66.6 (6.2) | 66.6 (8.7) | − | 0.35 (M) | 0.35 (M) | 67 | 3.68 | 4.05 | 36.0 | 7.41 |
| J1857+0943 (B) | 0742520201 | 10.0 (5.3) | 11.6 (6.3) | 11.6 (8.8) | 0.4 (M) | 0.25 (M) | 0.25 (M) | 5 | 1.20( * ) | 1.17 | 33.6 | 0.40 |
| J1926−1314 | 0742620101 | 75.0 (56.6) | 76.6 (54.4) | 76.6 (74.7) | 0.4 (TN) | 0.35 (TN) | 0.35 (TN) | 4864 | 1.53 | 1.48 | 31.1 | 1.22 |
Notes. Pulsar names and their XMM-Newton obsid’s are given in the first and second column. The pulsars in binary systems are marked with (B). The following six column displays EPIC-pn and EPIC-MOS total and GTI-filtered exposure times (given in parentheses) and the GTI filter for the background light curve and the corresponding filters for each EPIC detector. “TN” is thin filter, “TK” is thick filter and “M” is medium filter. Source properties are noted in the last five columns. P is the spin period in seconds, D1 is the best estimate of the pulsar distance in kpc according to the ATNF pulsar catalog which uses the YMW+17 DM-based distance as default, log Ė is the common logarithm of the spin-down energy loss rate in erg s−1 and NH is the hydrogen column density in unit of 1021 cm−2 estimated from the DM as outlined in Sect. 2.4. Sources with parallactic distance are marked with ( * ).
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