Table 1.
Parameters for the eMSPs known in the Galactic disk.
| PSR | P (ms) | Pb (d) | e | MT (M⊙) | Mp (M⊙) | Mc (M⊙) | Mtheo (M⊙) | References |
|---|---|---|---|---|---|---|---|---|
| J0955−6150 | 1.9993 | 24.5784 | 0.1175 | 1.96(3) | 1.71(2) | 0.254(2) | 0.271–0.300 | 1, 2 |
| J1618−3921 | 11.9873 | 22.7456 | 0.0274 | – | – | – | 0.269–0.297 | 3, 4 |
| J1946+3417 | 3.1701 | 27.0199 | 0.1345 | 2.094(22) | 1.827(13) | 0.2654(13) | 0.275–0.303 | 5, 6 |
| J1950+2414 | 4.3048 | 22.1914 | 0.0798 | 1.779(25) | 1.496(23) |
 |
0.268–0.296 | 7, 8 |
| J2234+0611 | 3.5766 | 32.0014 | 0.1293 |
 |
 |
 |
0.281–0.310 | 9, 10 |
| J1146−6610 | 3.7223 | 62.7712 | 0.0074 | – | – | – | 0.307–0.339 | 11 |
| J1903+0327 | 2.1499 | 95.1741 | 0.4367 | 2.697(29) | 1.667(21) | 1.029(8) | – | 12, 13 |
Notes. The parameters for the first five pulsars are similar, but they differ significantly from PSR J1903+0327. The first five systems and PSR J1146−6610 all have mass functions, spin periods, and period derivatives typical of MSPs with He WD companions. The 8th column states the He WD mass interval expected from the Pb − MWD correlation of Tauris & Savonije (1999). For PSR J1903+0327, the mass uncertainties refer to a 99.7 % confidence level; the companion of that pulsar is a main-sequence star. For the other systems, the companions are presumably He WDs; this has been confirmed in the case of PSR J2234+0611 by Antoniadis et al. (2016a).
References. (1) Camilo et al. (2015); (2) this work; (3) Octau et al. (2018); (4) Edwards & Bailes (2001); (5) Barr et al. (2013); (6) Barr et al. (2017); (7) Knispel et al. (2015); (8) Zhu et al. (2019); (9) Deneva et al. (2013); (10) Stovall et al. (2019); (11) Lorimer et al. (2021); (12) Champion et al. (2008); (13) Freire et al. (2011).
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