formation should occur primarily at low energies. This would produce an apparently lower value for the measured nuclear obscuration in low-counting statistics spectra as those of SDP.9 and SDP.11, making the intrinsic X-ray luminosities quoted for the two objects likely lower limits.

![image](channels.pdf){width="\textwidth"}

![image](COmom0_cont_SE.pdf){width="47.00000%"} ![image](COmom0_cont_NW.pdf){width="47.00000%"}

ALMA mm observations
====================

The two targets were included in a low-resolution observation with ALMA in Cycle 1 (2012.1.00915, PI:Lupu). On the basis of those data, Oteo et al. (2017) investigate dense circumnuclear region emissions through HCN(3-2), HCO$^+$(3-2), HNC(3-2) and CO(3-2) transitions properties. HCN(3-2), HCO$^+$(3-2) and CO(3-2) lines have been detected with ALMA for both the targets while HNC(3-2) was detected only in SDP.9. These spectral line intensity ratios and their relation with the continuum emission suggest that the presence of intense star formation could be associated with massive dense molecular gas reservoirs and high dense molecular gas fractions.

High resolution ($<0.1$ arcsec) observations have been carried out for both our targets. The observations are still on going for the SDP.11 (2015.1.01362.S, PI:Gordon). In the following we report our reduction, imaging, analysis of the data for SDP.9 available in the ALMA Science archive of Cycle 4 project, performed with a different approach with respect to 