MICADO is the ELT first light instrument, an imager working at the diffraction limit of the telescope thanks to two adaptive optics (AO) modes: a single conjugate one (SCAO), available at the instrument first light and developed by the MICADO consortium, and a multi conjugate one (MCAO), developed by the MORFEO consortium. Although the project final design review process is about to be completed, the review board and ESO acknowledged that "the review of the final design can be considered complete for the majority of the MICADO sub-systems" and agreed that MICADO can start manufacturing. For the MICADO SCAO module, we have started the manufacturing of several parts: the majority of the SCAO optics and of the SCAO mechanics, the real-time computer software and the instrument control software. This manufacturing is ordered in several steps to allow the progressive integration of a first full AO close loop with the final SCAO parts. In this contribution, we will focus on the first two steps: on our AO Sesame bench and the so-called "beta flat configuration". We will present the status of this manufacturing and the first results obtained.

MICADO is a first light instrument for the Extremely Large Telescope (ELT), set to start operating later this decade. It will provide diffraction limited imaging, astrometry, high contrast imaging, and long slit spectroscopy at near-infrared wavelengths. During the initial phase operations, adaptive optics (AO) correction will be provided by its own natural guide star wavefront sensor. In its final configuration, that AO system will be retained and complemented by the laser guide star multi-conjugate adaptive optics module MORFEO (formerly known as MAORY). Among many other things, MICADO will study exoplanets, distant galaxies and stars, and investigate black holes, such as Sagittarius A* at the centre of the Milky Way. After their final design phase, most components of MICADO have moved on to the manufacturing and assembly phase. Here we summarize the final design of the instrument and provide an overview about its current manufacturing status and the timeline. Some lessons learned from the final design review process will be presented in order to help future instrumentation projects to cope with the challenges arising from the substantial differences between projects for 8-10m class telescopes (e.g. ESO-VLT) and the next generation Extremely Large Telescopes (e.g. ESO-ELT). Finally, the expected performance will be discussed in the context of the current landscape of astronomical observatories and instruments. For instance, MICADO will have similar sensitivity as the James Webb Space Telescope (JWST), but with six times the spatial resolution.

MICADO SCAO RTC hard real-time capabilities are provided by COSMIC, while the soft real-time features rely on the ESO RTC Toolkit. The RTC has actively begun the MAIT phase. For this purpose, a full-scale setup has been assembled to start the integration of the S-RTC and H-RTC. The setup is used with an additional simulation node running either COMPASS or ESO WFS simulator, allowing to validate the various implementations of the RTC in terms of AO performance and latency requirements. On top of that, an instance of the RTC has been deployed on the SESAME bench at LESIA. This paper will present the MICADO SCAO RTC architecture after final design review, the design choices and the current status of the MAIT activities related to the RTC. It will provide an overview of the H-RTC pipeline design, including performance benchmark and validation through simulation mode and on-bench results. It will also picture the current status of the RTC Toolkit integration activities for the S-RTC on multi-nodes cluster including the first implementation of telemetry consumption, data tasks, data storage, data visualization, H-RTC optimization and automation mechanisms.

MICADO is the ELT first light instrument, an imager working at the diffraction limit of the telescope thanks to two adaptive optics (AO) modes: a single conjugate one (SCAO), available at the instrument first light and developed by the MICADO consortium, and a multi conjugate one (MCAO), developed by the MORFEO consortium. This contribution presents an overview of the SCAO module while MICADO and its SCAO are in the last phase of their final design review. We focus on the SCAO architecture choices and present the final design of the SCAO subsystems: the Green Doughnut structure, the SCAO wavefront sensor, the SCAO calibration unit, the SCAO ICS (i.e. AOCS) and the SCAO RTC. We also present the SCAO global performance in terms of AO correction, obtained from an error budget that includes contributors estimated from AO end-to-end simulations as well as instrumental contributors. Finally, we present the current SCAO subsystems prototyping and the main milestones of the SCAO AIT plan.

With the upcoming giant class of telescopes, Adaptive Optics (AO) has become more essential than ever before to get access to the full potential offered by those telescopes. The complexity of such AO systems is reaching extreme heights, and disruptive developments will have to be made in order to build them. One of the critical component of a AO system is the Real Time Controller (RTC) which will have to compute the slopes and the Deformable Mirror (DM) commands at high frequency, in a range of 0.5 to several kHz. Since the complexity of the computations involved in the RTC is increasing with the size of the telescope, fulfilling RTC requirements for Extremely Large Telescope (ELT) class is a challenge. As an example, the MICADO SCAO (Single Conjugate Adaptive Optics) system requires around 1 TMAC/s for the RTC to get sufficient performance. This complexity brings the need for High Performance Computing (HPC) techniques and standards, such as the use of hardware accelerator like GPU. On top of that, building a RTC is often project-dependent as the components and the interfaces change from one instrument to an other. The COSMIC platforms aims at developing a common AO RTC platform which is meant to be powerful, modular and available to the AO community. This development is a joint effort between Observatoire de Paris and the Australian National University (ANU) in collaboration with the Subaru Telescope. We focus here on the current status of the core hard real-time component of this platform. The H-RTC pipeline is composed of Business Units (BU): each BU is an independent process in charge of one particular operation, such as Matrix Vector Multiply (MVM) or centroid computation, that can be made on CPU or on GPU. BUs read and write data on Shared Memory (SHM) handled by the CACAO framework. Synchronization between each BU can then be made either by using semaphore or by busy waiting on the GPU to ensure very low jitter. The RTC pipeline can then be controlled through a Python interface. One of the key point of this architecture is that the interfaces of a BU with the various SHM is abstracted, so adding a new BU in the collection of available ones is straight forward. This approach allows a high performance, scalable, modular and configurable RTC pipeline that could fit the needs of any AO system configuration. Performance has been measured on a MICADO SCAO scale RTC pipeline with around 25,000 slopes by 5,000 actuators on a DGX-1 system equipped with 8 Tesla V100 GPUs. The considered pipeline is composed of two BUs : the first one takes an input the raw pyramid WFS image (produced by simulator), applies on it dark and flat references, and then extract the useful pixel from the image. The second BU performs the MVM and the integration of the commands following a classical integrator command law. Synchronization between the BU is made through GPU busy waiting on the BU inputs. Performance obtained shows a mean latency up to 235 μs using 4 GPUs, with a jitter of 4.4 μs rms and a maximum jitter of 30 μs

MICADO is the ELT near-infrared first light imager. It will provide diffraction limited images using the singleconjugate adaptive optics (SCAO) mode developed inside the MAORY AO module. Although the MICADOMAORY SCAO mode uses during regular operations the ELT wavefront correction capabilities (M4 & M5 adaptive mirrors), the SCAO system will not be able to work with them until the final instrument commissioning. Since it is crucial to test and validate the SCAO system during various AITs phases in Europe, the need of a high order deformable mirror with comparable number of degrees of freedom is required to test both spatial and temporal behaviour of the SCAO mode. For that purpose, the SCAO AITs in Europe will use the newly developed ALPAO 64×64 actuators deformable mirror (DM). Before using this deformable mirror in the context of the SCAO mode (i.e controlled by a non-linear pyramid WFS, we built a classical Shack-Hartmann WFS to ensure a proper linear wavefront measurement in the lab and perform the DM characterisation of its 3228 actuators. We present the preliminary results of the tests performed on this DM in a classical closed loop scheme. In particular we study the spatial wavefront correction, actuators additivity and linear response, maximum amplitude range (stroke), hysteresis and temporal stability.

Here, we present a cubesat space mission dedicated to the detection and characterization of meteors. The detection of meteors brings information on the flux of meteoroids and space debris in Earth environment and on the nature of the meteoroids that come from two reservoirs: comets and asteroids [1]. Such study brings information on the formation of the solar system. Several methods have been developed from Earth ground and airborne to detect meteors or space debris. However, the advantage of a space mission dedicated to meteors observation is to be able to probe a large volume of the Earth atmosphere and to avoid weather constraints [2]. The primary objective is to assess a robust statistics on meteoroids and space debris that enter into the Earth atmosphere. At present, their fluxes and properties are not yet determined accurately [3]. These estimates will allow to quantify the delivery of extraterrestrial material on Earth, and possible consequences on aeronomy (e.g. noctilucent clouds and atomic layer). These estimations are also crucial to estimate impact risks for artificial satellites during meteor showers. There are several secondary objectives such as to bring information on ablation, fragmentation, rotation processes by photometry variation; to determine the trajectory in connection with Earth- ground network such as FRIPON network developed in France in order to find the dynamical origin of the meteoroid; and to detect other fainter luminous atmospheric. This cubesat is a 3U developed by students from Sorbonne University and the project is presently in phase B [4]. The launch would be scheduled in four years. Support from CNES-JANUS, ESEP, and IDEX Sorbonne Universites are acknowledged. [1] Jenniskens, P., 2006, Meteor Showers and their Parent Comets. Ed. Cambridge University Press, Cambridge, U.K. [2] Bouquet A., Baratoux D., Vaubaillon J., et al. 2014, Simulation of the capabilities of an orbiter for monitoring the entry of interplanetary matter into the terrestrial atmosphere, Planetary and Space Science 103 (2014) 238-249 [3] Zolensky, M., Bland, P., Brown, P., and Halliday, I. 2006, Meteorites and the Early Solar System II, 869 [4]Meteorix, A student nanosatellite Project by UPMC - Sorbonne Universites, Phase A review, MET_MGT_HO_0068_v1r1_11092017