images (brightness scale in $\mu$Jy/arcsec$^2$, left panel) and 0.5/7keV images (right panel) of SDP.9 and SDP.11, overlaid with signal-to-noise ratio contours at 880 $\mu$m from the SMA (in steps of 3,6,9, Bussmann et al. 2013, Negrello et al. 2014).[]{data-label="fig:chandra_im"}](sdp11.png "fig:"){width="50.00000%"}

X-ray observations
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SDP.9 and SDP.11 were observed by in Cycle 16, with the ACIS-S3 CCD at the aimpoint, for a total exposure time of 55.3 ks (on January 10$^{th}$, 2015) and 19.8 ks (on February 28$^{th}$ and March 23$^{rd}$, 2015), respectively. Very-faint mode was used for the event telemetry format, and ASCA grade 0, 2, 3, 4 and 6 events were used in the analysis, which has been carried out using the [ciao]{} v4.7 software. Both sources are clearly detected, with 14 counts each in the 0.5–7 keV band within a circular region of 2 radius centered on the positions reported in $\S$2, and eight counts in the observed 2–7 keV band. The 0.5–7 keV images of SDP.9 and SDP.11, centered at those positions, are shown in Fig. \[fig:chandra\_im\]. Remarkably, the 0.5 arcsec on axis resolution is able to resolve the X-ray emission from the lensed components. The X-ray emission shows a better positional match with the SMA data 