Table 6.
Multi-wavelength emission properties of the confirmed and candidate tMSPs in the sub-luminous accretion disk state; other systems properties are also listed.
| Confirmeda |
Candidatesb |
||||||
|---|---|---|---|---|---|---|---|
| J18245 | J1023 | J12270 | J1544 | J0427 | J1748 | J1109 | |
| Optical propertiesc | |||||||
| Magntitude | – | G ∼ 16.3 | V ∼ 16.1 | G ∼ 18.6 | G ∼ 17.7 | – | G ∼ 20.1 |
| Short-term variability | – | ✓ | ✓ | ✓ | ✓ | – | ✓ |
| Orbital modulation | – | ✓ | ✓ | ✓ | ✓ | – | – |
| Spectral emission lines | – | ✓ | ✓ | ✓ | ✓ | – | ✓ |
| Pulsations | – | ✓(in high, flare modes) | – | – | – | – | – |
| X-ray propertiesd | |||||||
| ΓX | 1.44 ± 0.05 | 1.62 ± 0.02 | 1.70 ± 0.02 | 1.63 ± 0.02 |
 |
1.5 ± 0.1 | 1.63 ± 0.02 |
| LX (1033 erg s−1) | 11.2 ± 0.5 | 5.2 ± 0.1 | 12 ± 2 | 16.5 ± 0.6 | 6.3 ± 0.4 | 6.5 ± 0.3 | 21.6 ± 0.4 |
| LX, high (1033 erg s−1) | 13.1 ± 0.6 | 7.9 ± 0.1 | 13 ± 3 | 25.1 ± 0.7 | 10.3 ± 0.8 | – | 27.2 ± 0.6 |
| LX, low (1033 erg s−1) | 2.0 ± 0.3 | 0.87 ± 0.04 | 2.0 ± 0.4 | 1.4 ± 0.3 | 3.6 ± 0.4 | – | 3 ± 1 |
| Pulsations | ✓ | ✓(in high mode) | ✓(in high mode) | – | – | – | – |
| Red noise power law slope | 1.18 ± 0.01 | 1.05 ± 0.05 | 1.39 ± 0.06 | 1.41 ± 0.04 | 1.5 ± 0.1 | – | 1.3 ± 0.1 |
| Gamma-ray propertiese | |||||||
| Γγ | – | 2.41 ± 0.10 | 2.36 ± 0.06 | 2.48 ± 0.05 | 2.48 ± 0.06 | – | 2.58 ± 0.15 |
| (2.53 ± 0.05) | (2.39 ± 0.06) | ||||||
| Lγ (1033 erg s−1) | – | 12.5 ± 0.4 | 21.9 ± 0.7 | 24.7 ± 0.2 | 6.5 ± 0.4 | – | 15 ± 2 |
| Radio propertiesf | |||||||
| Γr | 0.39 ± 0.06 | 0.09 ± 0.18 | −0.1 ± 0.1 | – | – | – | – |
| Lr (1027 erg s−1) | 112 | 0.97 | 5.4 | – | – | – | < 2.5 |
| Lr [high X-ray mode] (1027 erg s−1) | – | 0.63 | – | – | – | – | < 4.0 |
| Lr [low X-ray mode] (1027 erg s−1) | 112 | 1.9 | – | – | – | – | < 10.0 |
| Other propertiesg | |||||||
| Spin period (ms) | 3.93 | 1.69 | 1.69 | – | – | – | – |
| Orbital period (h) | 11.03 | 4.75 | 6.91 | 5.80 | 8.80 | – | – |
| Spin-down luminosity (1034 erg s−1) | – | 4.8 ± 0.5 | 8.3 ± 1.8 | – | – | – | – |
| NS dipolar magnetic field (108 G) | – | 1.9 | 2.3 | – | – | – | – |
| System inclination (°) | – | 46 ± 2 | 46–55 | 7 ± 1 | 78 ± 2 | – | – |
| Spectral type of the companion | – | Mid-G V | G5 | K6–7V | mid-to-late K | – | – |
| NS mass (M⊙) | – |
 |
– | – | 1.86 ± 0.11 | – | – |
| Companion mass (M⊙) | 0.20 ± 0.01 | 0.22 ± 0.03 | ≥0.27 | ≲0.7 | 0.65 ± 0.08 | – | – |
Notes. Values are not reported for those cases where the corresponding counterpart is uncertain, has not been identified yet or was not observed during the sub-luminous accretion disk state, and also where the X-ray modes and the slope of the red noise component have not been clearly singled out. (a)Systems that have been observed to undergo a state transition. (b)Systems that have not been observed to undergo a state transition so far. (c)Optical magnitudes are not corrected for extinction and are taken from the second Gaia data release, except for XSS J12270−4859 which persisted in a rotation-powered state since the satellite launch in 2013 December. (d)All X-ray luminosities were re-computed in this work over the 0.3–79 keV energy band adopting the abundances of Wilms et al. (2000) for the absorption model, to allow a direct comparisons among the different systems. We assumed isotropic emission at the following distances: 5.5 kpc for IGR J18245−2452 (Harris 1996), 1.37 kpc for PSR J1023+0038 (Deller et al. 2015), 1.6 kpc for XSS J12270−4859 (Jennings et al. 2018), 3.8 kpc for 1RXS J154439.4−112820 (Britt et al. 2017), 2.4 kpc for 1SXPS J042749.2−670434 (Strader et al. 2016), 5.9 kpc for CXOGlb J174804.5−244641 (Lanzoni et al. 2010) and 4 kpc for J1109 (this work). The luminosities of IGR J18245−2452 and CXOGlb J174804.5−244641, for which no observations exist in the hard X-ray band during the sub-luminous accretion disk state, were obtained extrapolating the best-fitting absorbed power law model for the soft X-ray emission and assuming no spectral cut-off up to 79 keV. Uneclipsed luminosities are reported for 1SXPS J042749.2−670434. (e)The value for the simple power law model is reported for both PSR J1023+0038 and XSS J12270−4859, although evidence for an exponential cut-off was found in both systems (Torres et al. 2017; Xing et al. 2018). The value reported on the Fermi/LAT eight-year point source list is also quoted in parentheses. Uncertainties are statistical only. Gamma-ray luminosities are evaluated over the 0.1–300 GeV energy band and for the same distances as in (d). Uncertainties are statistical only. (f)Radio luminosities are evaluated at a frequency of 5 GHz and for the same distances as in (d). Upper limits are evaluated assuming a flat spectrum. (g)See also Strader et al. (2019).
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