ABSTRACT

In the past decade strong gravitational lensing has become a fundamental method to investigate the Universe and the structures inside it, i.e. revealing dark matter substructures in the lens (on galaxy scales or in clusters), or by exploiting the lens as a magnifying glass to detect structures and clumps in high-z galaxies, allowing detailed kinematical and morphological studies of the components wherein (stars, ISM, dust) in different stages of their evolution. This has been possibile thanks to the always increasing number of discovered lensing phenomenon in surveys, and with the implementation of reliable and robust lens modelling and source reconstruction techniques, applied in every domain of the electromagnetic spectrum. Here we report the physical properties of the ISM in the strongly lensed galaxy J091043.0-000322 (SDP.11), at redshift 1.78, which was discovered in the H-ATLAS survey, by means of a multi-wavelength suite of observations which were carried out in the near-infrared with the Hubble Space Telescope, in the sub-millimeter with the Atacama Large Millimeter/submillimeter Array (ALMA) and the Submillimeter Array(SMA), and in the millimeter regime with Plateau de Bure Interferometer (PdBI). We build a robust model for the lens from the modelling, in the uv-plane, of the dust continuum emission in ALMA Band 9 which we use to reconstruct the lensed emission from all our observations. This high resolution observations allow us to probe scales down to 300-700 pc at the redshift of the source, where the gas emission breaks into several clumps none of which is associated with the more compact dust emission. We use the reconstructed kinematics to investigate the nature of SDP.11, finding evidence that the source is undergoing a major-merging event.

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