Adaptive Optics corrected simulations of star-forming clumps observations at high-z for MORFEO/MICADO@ELT

In the framework of galaxy formation, the star-forming regions, typicaly dubbed as clumps, play an important role in the definition of the galaxy properties observed today. Clumps have been observed from cosmic noon (z ≈ 1) up to the highest redshift (up to z ≈ 10). To study them, high spatial resolution and sensitivity are needed, given their small size and faintness. In this work I focus on studying the possibility of observing and resolving star forming clumps using the ELT. In particular I focus on the simulation of the PSF that is expected to be obtained from the adaptive optics module MORFEO in the case of different natural guide star configurations, and on the effects that different configurations will have on the observations. Then I explore how the combination of different observing conditions and intrinsic properties of the targets (photometric filter, NGS asterism, source surface brightness and redshift) will impact the scientific performance of the Near-Infrared imager MICADO, fed with MORFEO-corrected wavefront. The scientific case taken into exam is the detection and characterization of star-forming clumps with size < 10 pc at different redshifts up to z=6. This will be accomplished through specific software developed for the prediction of adaptive optics PSF and for the simulation of MICADO+MORFEO data. Starting from well motivated assumptions on star forming clumps and their host galaxies, I produced simulated data of these systems in the I, J, H and K MICADO bands at different redshifts. Then I analyzed the simulated data to characterize how well the clumps can be detected and characterized on particular observing conditions and target properties. This work provides a first step for preparing to real on-sky observations of high-z star forming clumps in the near future.