Table 6
Best-fit orbital profile parameters in units of the orbital phase.
| Source | φi | τi | φe | τe | θe | θe,old |
| (deg) | (deg) | |||||
|
|
||||||
| LMC X-4 | 0.951(4) | 0.020(1) | 0.039(3) | 0.012(2) | 15.8(8) | 27(2)a |
| Cen X-3 | 0.922(1) | 0.019(1) | 0.077(1) | 0.0187(6) | 27.9(3) | 33(1)b |
| 4U 1700-377 | 0.912(4) | 0.0185(5) | 0.0894(4) | 0.0126(2) | 32(1) | 29(2)c |
| 4U 1538-522 | 0.936(4) | 0.018(2) | 0.052(4) | 0.0147(5) | 21(1) | 29(2)d |
| SMC X-1 | 0.939(9) | 0.0139(4) | 0.066(5) | 0.007(2) | 23(2) | 28(2)a |
| SAX J1802.7-2017 | 0.94(1) | 0.038(9) | 0.11(1) | 0.012(7) | 31(2) | 35(5)e |
| XTE J1855-026 | 0.920(5) | 0.0129(3) | 0.097(6) | 0.016(4) | 32(1) | 42(6)f |
| Vela X-1 | 0.9202(4) | 0.0209(1) | 0.0899(2) | 0.0084(2) | 30.5(1) | 33(3)g |
| EXO 1722-363 | 0.94(2) | 0.013(8) | 0.088(4) | 0.004(2) | 26(4) | 32(2)h |
| OAO 1657-415 | 0.933(1) | 0.0184(6) | 0.049(2) | 0.0352(1) | 20.9(4) | 30(1)i |
Notes. For each source we indicate with θe the semi-eclipse angle measured from our ISGRI light curves (17−40 keV energy band), φi,e is the defined as the phase at which 99% of the source flux is occulted at eclipse ingress or egress, and τi,e the corresponding transition phase width. The values of the semi-eclipse angles reported in the last column, θe,old, are taken from the literature. We indicate in brackets the uncertainties at 1σ c.l. on the last digits of each reported value.
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