Table 2
Power-law slopes β and γ describing the cumulative luminosity distribution (see Sects. 2.3.1 and 2.3.2) for the known UCXB population based on the RXTE ASM data.
Name | Porb (min) | β | γ |
|
|||
4U 1820–30 | 11.42 | −7.4 | −3.7 |
4U 0513–40 | 17 | −2.0 | −2.3 |
2S 0918–549 | 17.4 | −1.03 | −2.5 |
4U 1543–624 | 18.2 | −3.8 | −4.3 |
4U 1850–087 | 20.6 | −1.9 | −2.1 |
M 15 X-2 | 22.58 | −1.6 | −3.0 |
XTE J1807–294 | 40.07 | −2.4 | N/A |
4U 1626–67 | 41.4 | −3.0 | −2.5 |
XTE J1751–305 | 42.42 | −2.5 | −0.55 |
XTE J0929–314 | 43.58 | −2.8 | N/A |
4U 1916–05 | 49.48 | −2.8 | −2.5 |
SWIFT J1756.9–2508 | 54.70 | −1.3 | −1.7 |
|
|||
4U 1728–34 | 10.77? | −6.3 | −0.66 |
4U 0614+091 | 51.3? | −3.2 | −4.1 |
Notes. The two systems below the line are UCXB candidates, with an uncertain orbital period. If no γ-value is given, the source is too faint on average for this method to work.
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