efi|soft will be supervising all control command software developments on the projects below :

• HARMONI
  - The High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph, is one of the first-light instruments installed on the Extremely Large Telescope (ELT) and will function as the telescope's workhorse instrument for spectroscopy in the wavelength range 0.47–2.45 µm. This versatile instrument will offer a set of spatial scales to optimise observations for a wide range of science programmes and observing conditions. In particular, HARMONI will be optimised to exploit the best image quality delivered from a post-focal laser tomographic adaptive optics module.

• MICADO
  - The Multi-Adaptive Optics Imaging Camera for Deep Observations, is one of the first-light instruments for the Extremely Large Telescope (ELT) instrument and takes the Adaptive Optics technique to the next level. It will be the first dedicated imaging camera for the ELT and works with the multi-conjugate adaptive optics module, MAORY.

• MAORY
  is the post-focal adaptive optics module for ELT that will be installed on the Nasmyth platform A. It is designed to work with the imaging camera MICADO and with a second future instrument. MAORY will provide two adaptive optics modes to support MICADO: multi-conjugated and single-conjugated. In the Multi-Conjugate Adaptive Optics mode (MCAO), the ELT telescope deformable mirror M4 and at least another deformable mirror inside MAORY are conjugated to different altitudes in the atmosphere, to correct for different layers of turbulence. The MCAO mode has to be available at first light with at least one deformable mirror in MAORY, with provision for a second deformable mirror as an upgrade, implying that MAORY has to be designed for two deformable mirrors from the beginning.
  The MCAO mode is based on the use of six LGS for wave-front sensing. It measures the light from a configuration of six sodium laser guide stars, arranged in a circle on the sky, to obtain a kind of three-dimensional mapping of the turbulence. Three NGS are also required to supplement LGS measurements.
  In the Single-Conjugate Adaptive Optics mode (SCAO), the wave-front errors compensation is performed using M4 only. The high-order NGS sensing is performed using a dedicated wave-front sensor. LGS are not used. This mode is developed in collaboration with the MICADO consortium. In the current baseline design MAORY is composed by four modules: - The Post Focal Relay Optics (PFRO) module, which includes the mirrors, dichroic and LGS objective hosted by the main optical bench and the devices to monitor and control their movements;
  - The LOR WFS module, which is used in MCAO mode and it is composed by three units aimed to measure the wave front distortions of the natural guide stars; each unit includes a Low-order WFS and a Reference WFS;
  - The LGS WFS module, which is used in MCAO mode and it is an assembly of six wave-front sensor units aimed to measure the wave-front distortions on the laser guide stars;
  - The SCAO WFS module, which includes the wave front sensor for the (only one) NGS used in SCAO mode.
  Both the LOR WFS and SCAO WFS modules are hosted in the same structure, the so called Green Doughnut (GD), on top of MICADO instrument.

• MOSAIC
  - The workhorse instruments of the current 8-10m class observatories are multi-object spectrographs (MOS), providing comprehensive follow-up of ground-based and space-borne imaging data. With the advent of even deeper imaging surveys from, e.g., HST, VISTA, JWST and Euclid, many science cases require complementary spectroscopy with high sensitivity and good spatial resolution to identify the objects and to measure their astrophysical parameters. The light-gathering power of the 39m ELT and its spatial resolution, combined with a MOS, will enable the large samples necessary to tackle some of the key scientific drivers of the ELT project, ranging from studies of stellar populations out to the highest-redshift galaxies. Consequently, a MOS-facility is foreseen within the ELT instrumentation plan.

• HIRES
  - The Mid-infrared ELT Imager and Spectrograph (METIS), will be the third instrument on the Extremely Large Telescope (ELT). It will make full use of the giant, 39-metre main mirror of the telescope and focus on five scientific goals: exoplanets, proto-planetary disks, Solar System bodies, active galactic nuclei, and high-redshift infrared galaxies.

• ELT-PCS
  - spectrographe imageur dédié à l'observation des exo-planètes.