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Methods: An adapted version of the WHO Maternal Near Miss Screening Tool was used to identify maternal near-miss cases. These were compared with unmatched controls (uncomplicated deliveries) in a ratio of 1:2.

Results: Out of 8433 live births, 288 maternal near-miss cases and 62 maternal deaths were identified. In all, 454 healthy controls were recruited for comparison. Maternal near-miss and maternal death incidence ratios were 34.2 (95% CI 30.2-38.1) and 7.4 (95% CI 5.5-9.2) per 1000 live births, respectively with a maternal near-miss to mortality ratio of 4.6:1. Cause of near-miss was pre-eclampsia/eclampsia (41.0%), haemorrhage (12.2%), maternal sepsis (11.1%) and ruptured uterus (4.2%). A major factor associated with maternal near-miss was maternal fever within the 7 days before birth (OR 5.95, 95%CI 3.754-9.424). Spontaneous onset of labour was protective against near-miss (OR 0.09 95% CI 0.057-0.141).

Conclusion: For every maternal death, there were nearly five maternal near-misses. Women having a fever in the 7 days before delivery were six times more likely to experience a near-miss than women not having fever.

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In the following we report the first measurement of the next relativistic effect in the orbit of S2, namely the in-plane, prograde precession of its pericentre angle, the Schwarzschild precession (Misner et al. 1973).

We expect only modest further improvement of the significance of our result as our monitoring continues and S2 moves away from pericentre, because our result already now is limited by the precision with which we have measured the pre-pericentre orbit with AO data.

Fig. A.3.Astrometric (left) and spectroscopic (right) 1tag_hash_109 statistical measurement uncertainties of S2 over time. Left panel: almost 100-fold improvement in astrometric precision in RA and Dec, from the early period of speckle imagery with SHARP on the 3.5 m NTT (until 2001), then the AO imagery with NACO on the 8 m VLT (> 2002), and then, since 2016.7, the interferometric astrometry of GRAVITY combining all four 8 m telescopes of the VLT. The grey vertical lines are the two pericentre passages (2002.33 and 2018.38) covered by our data set.

We used the binary fitting method in our previous publications (GRAVITY Collaboration 2018a,b, 2019). The quantities used are the visibility amplitudes and the closure phases, both of which measure the internal source structure. We omit the visibility phases here, because they mostly contain information about the location of the phase centre and only to a lesser degree about the source internal structure. One of the parameters describing the source structure is the desired binary separation.

where k labels the telescope and xk denotes its position, E0 is the amplitude of the unperturbed electric field, and s is the source position on the sky. The scaling in amplitude and the phase shift are functions of the source position with respect to the field centre and differ for each telescope.

In Fig. E.2 we show selected correlation plots from the posterior distribution, which are worth discussing in the context of fSP. The strongest correlation for fSP is with the pericentre time. This is not surprising, given the discussion in Appendix B, where we showed that near pericentre the SP acts like a shift in time. The second strongest correlation for fSP is with the RA offset of the coordinate system. This explains why including the NACO flare data helps determining fSP: the flares essentially measure the offset of the coordinate system.

The parameter fSP is also weakly correlated with the semi-major axis a and it is anti-correlated with the eccentricity e of the orbit. The former can be understood in the following way: If the orbit were slightly larger on sky, a stronger precession term would be required in order to achieve the same amount of kink (in mas on sky) at pericentre. The latter is understood similarly: A higher eccentricity leads to a narrower orbit figure, and hence less of the precession term would be needed. Interestingly, fSP is almost uncorrelated with the argument of periapsis tag_hash_124 (i.e. the angle describing the orientation of the orbital ellipse in its plane), despite that the SP changes exactly that parameter.

Astrometric (left) and spectroscopic (right) 1tag_hash_127 statistical measurement uncertainties of S2 over time. Left panel: almost 100-fold improvement in astrometric precision in RA and Dec, from the early period of speckle imagery with SHARP on the 3.5 m NTT (until 2001), then the AO imagery with NACO on the 8 m VLT (> 2002), and then, since 2016.7, the interferometric astrometry of GRAVITY combining all four 8 m telescopes of the VLT. The grey vertical lines are the two pericentre passages (2002.33 and 2018.38) covered by our data set.

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