Table 1
The brightest persistent low mass X-ray binaries in the Galaxy with fluxes >1.4 × 10-10 erg s-1 cm-2 measured by UHURU (Forman et al. 1978).
| Name | Lx (2–10 keV) | Dist, kpc | Period, h |
| 1037 erg/s | |||
|
|
|||
| Sco X-1 | 37.4 | 2.81 | 18.94 |
| GX 5-1 | 26.1 | 92 | |
| GRS 1915+105 | 26.0 | 113 | 739.20 |
| Cyg X-2 | 19.4 | 11.65 | 236.27 |
| GX340+0 | 18.2 | 124 | |
| GX 349+2 | 15.3 | 8.56 | 22.5 |
| GX 17+2 | 14.9 | 7.57 | |
| GX 9+1 | 8.7 | 7.27 | |
| 4U1820-30 | 5.7 | 88 | 0.19 |
| Ser X-1 | 5.5 | 8.49 | 12.96 |
| GX 13+1 | 5.5 | 6.910 | 601.7 |
| 4U1735-44 | 4.9 | 9.111 | 4.65 |
| GX 3+1 | 3.4 | 4.512 | |
| 4U1624-49 | 3.1 | 1513 | 20.9 |
| 4U1636-53 | 2.4 | 5.910 | 3.79 |
| GX 9+9 | 1.8 | 5.07 | 4.20 |
| 4U1746-37 | 1.4 | 11.08 | 5.16 |
| 4U1705-32 | 1.18 | 1314 | |
| 1A1742-294 | 0.81 | 8.515 | |
| 4U1254-69 | 0.79 | 1116 | 3.93 |
| 4U0513-40 | 0.74 | 12.18 | 0.28 |
| 4U1823-00 | 0.61 | 6.317 | 3.19 |
| 4U1915-05 | 0.43 | 8.88 | 0.83 |
| 4U0614+09 | 0.34 | 3.218 | 0.81 |
| 4U1702-42 | 0.32 | 6.219 | |
| 4U1626-67 | 0.32 | 820 | 0.69 |
| GS1826-24 | 0.31 | 6.021 | 2.2522 |
| 4U1708-40 | 0.27 | 815 | |
| 4U1543-62 | 0.26 | 7.08 | 0.30 |
| 4U1724-30 | 0.17 | 9.58 | |
| 4U1850-08 | 0.17 | 8.28 | 0.34 |
| 4U1812-12 | 0.09 | 4.019 | |
| 4U1556-60 | 0.09 | 4.07 | |
| 4U1822-37 | 0.04∗ | 2.523 | 5.57 |
Notes. Orbital periods of systems are adopted from Ritter & Kolb (2003) and Liu et al. (2007).* – The source belongs to a group of so called accretion disk corona sources, in which we do not see the direct emission of the innermost parts of the accretion flow, therefore the observed X-ray luminosity of such a source is only a part of its intrinsic X-ray luminosity.
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