Table 3
Photometric solutions for EF Aqr from the JKTEBOP code.
| u | v | b | y | |
|
|
||||
| i (°) | 88.40 | 88.46 | 88.44 | 88.49 |
| ± 7 | ± 6 | ± 5 | ± 5 | |
| rp | 0.1224 | 0.1213 | 0.1218 | 0.1212 |
| rs | 0.0875 | 0.0870 | 0.0873 | 0.0876 |
| k | 0.7152 | 0.7170 | 0.7168 | 0.7159 |
| ± 25 | ± 19 | ± 17 | ± 15 | |
| rp + rs | 0.2099 | 0.2084 | 0.2091 | 0.2080 |
| ± 6 | ± 5 | ± 5 | ± 5 | |
| up | 0.8107 | 0.7673 | 0.7369 | 0.6553 |
| us | 0.9223 | 0.8796 | 0.8323 | 0.7478 |
| yp | 0.6527 | 0.5648 | 0.4465 | 0.3791 |
| ys | 1.2437 | 0.8670 | 0.6904 | 0.5580 |
| Js/Jp | 0.2438 | 0.2851 | 0.3729 | 0.4251 |
| ± 27 | ± 21 | ± 19 | ± 19 | |
| Ls/Lp | 0.1184 | 0.1410 | 0.1834 | 0.2092 |
| σ (mmag) | 10.9 | 8.3 | 7.5 | 7.3 |
Notes. Linear limb darkening coefficients from Claret (2000) were adopted together with gravity darkening coefficients from Bloemen et al. (2011). A mass ratio of q = 0.761 from the spectroscopy was assumed, the orbit was assumed to be circular, and phase shift and magnitude normalisation were included as free parameters. The quoted errors are formal errors from the iterative least-squares solution procedure.
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