an estimated column density of at least $10^{23}$ cm$^{-2}$, as observed in other bright submm galaxies (Johnson et al. 2013).

For SDP.11, we combined the photons of the two observations into a single spectrum. As for SDP.9, a powerlaw model provides an apparently flat spectrum, with $\Gamma=1.0\pm{0.9}$. If $\Gamma=1.8$ was assumed, the column density would be $3.2\times10^{22}$ cm$^{-2}$ (3$\sigma$ upper limit of $\approx2.4\times10^{23}$ cm$^{-2}$). The observed 2–10 keV flux is $\approx1.2\times10^{-14}$ [${\rm erg~cm}^{-2}~{\rm s}^{-1}$]{}, and the apparent rest-frame 2–10 keV luminosity (again corrected for the absorption but not for the magnification) is $\approx1.2\times10^{44}$ [erg s$^{-1}$]{}.

![ALMA high resolution continuum 1.3mm observations of SDP9.[]{data-label="fig:alma_continuum"}](continuum.pdf){width="50.00000%"}

![SDP9 CO(6-5) 0, 1, and 2 momenta of the line distribution, corresponding to the integrated brightness, and velocity distributions and the velocity dispersion.[]{data-label="fig:alma_momenta"}](COmom0.pdf "fig:"){width="9cm"} ![SDP9 CO(6-5) 0, 1, and 2 momenta of the line distribution, corresponding to the integrated brightness, and velocity distributions and the velocity dispersion.[]{data-label="fig:alma_momenta"}](COmom1.pdf "fig:"){width="9cm"} ![SDP9 CO(6-5) 0, 1, and 2 momenta of the line distribution, corresponding to the integrated brightness, and velocity distributions and the velocity dispersion.[]{data-label="fig:alma_momenta"}](COmom2.pdf "fig:"){width="9cm"}

Once corrected for the magnification factors, the intrinsic X-ray luminosities are $\approx5.9\times10^{42}$ [erg s$^{-1}$]{} and $\approx1.5\times10^{43}$ [erg s$^{-1}$]{} for SDP.9 and SDP.11, respectively. We can 