Table 1
Rotational period, orbital period, companion mass, orbital eccentricity, and height above the Galactic plane for the six known eMSPs.
| PSR | P(ms) | Pb (days) | mc (M⊙) | e | |z| (kpc) | References |
|---|---|---|---|---|---|---|
| J0955−6150 | 2.00 | 24.6 | 0.22 | 0.11 | 0.22 | Camilo et al. (2015) |
| J1618−3921 | 11.99 | 22.7 | 0.20 | 0.027 | 0.75 | Edwards & Bailes (2001), Bailes (2010) |
| J1946+3417 | 3.17 | 27.0 | 0.2556(19) | 0.14 | 0.57 | Barr et al. (2013, 2017) |
| J1950+2414 | 4.30 | 22.2 | 0.30 | 0.08 | 0.15 | Knispel et al. (2015) |
| J2234+0611 | 3.58 | 32.0 | 0.23 | 0.13 | 0.60 | Deneva et al. (2013), Antoniadis et al. (2016) |
| J1903+0327 | 2.15 | 95.2 | 1.029(8) | 0.44 | 0.1 | Champion et al. (2008), Freire et al. (2011) |
Notes. Unlike otherpulsars in this table, PSR J1903+0327 is believed to have been formed by triple-star interaction and is therefore isolated in the list. The quoted masses are the median masses derived from the mass function assuming a pulsar mass of 1.35 M⊙ and a random distribution of orbital inclinations, except for PSR J1903+0327 and PSR J1946+3417, for which the pulsar and companion masses were determined through the measurement of post-Keplerian parameters. The height above the Galactic plane, z, was obtained from the ATNF pulsar catalog (see http://www.atnf.csiro.au/research/pulsar/psrcat, Manchester et al. 2005). The z values all assume the YMW16 model of Yao et al. (2017).
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