Dating bardou telescopes


25-Aug-2019 13:56

We then briefly discuss the necessity of an advanced data management system and data reduction pipeline. METIS, the Mid-nfrared E-ELT Imager and Spectrometer, will be providing high-sensitivity imaging and high-resolution spectroscopy in the mid-infrared (3-19 micrometer) to the E-ELT. If the Real-Time Computer is the heart of an AO system, the Wavefront Sensor (WFS) its eyes, the Deformable Mirror (DM) its hands and the control strategy its nervous system, the sum of all those parts is made into a harmonious entity thanks to calibrations. Here we present the new modules of SCEx AO, give an overview of the current commissioning status of each of the modules and present preliminary results.Giuliana Fiorentino; Davide Massari; Alan Mc Connachie; Peter B. In order to achieve the exceptional performance required by its driving science cases, exoplanets and proto-planetary disks, METIS will be featuring two Adaptive Optics (AO) systems — a first-light Single Conjugate Adaptive Optics (SCAO) system, complemented by a Laser Tomographic Adaptive Optics (LTAO) system, most likely, a few years after first light. This paper does not have the ambition to provide an overview of all the currently existing calibration strategies, but rather to focus on a few challenging problems and their recent evolution in the era of adaptive telescopes, mostly based on the experience of ESO's Adaptive Optics Instruments in general and the AO Facility in particular. Adaptive Optics (AO) that compensates for atmospheric turbulence is a standard tool for high angular resolution observations of the Sun at most ground-based observatories today.Mag AO's unique capabilities are simultaneous imaging in the visible and infrared with Vis AO and Clio, excellent performance at an excellent site, and a lean operations model. A detailed analysis on the score of success of the predictive capacities of the system have been carried out for all the astroclimatic as well as for the atmospherical parameters.Science results from Mag AO include the first ground-based CCD image of an exoplanet, demonstration of the first accreting protoplanets, discovery of a new wide-orbit exoplanet, and the first empirical bolometric luminosity of an exoplanet. Considering the excellent results that we obtained, this study proved the opportunity to implement on these two sites an automatic system to be run nightly in an operational configuration to support the scheduling of scientific programs as well as of astronomical facilities (particularly those supported by AO systems) of the VLT and the E-ELT.Here we report on the new Stereo-SCIDAR instrument installed on one of the Auxillary Telescope ports of the Very Large Telescope array at Cerro Paranal. The current main limitation was found to be vibrations attributed mainly to the rotation of the telescope.Paranal is located approximately 20 km from Cerro Armazones, the site of the E-ELT. Henry HARMONI is a visible and NIR integral field spectrograph, providing the E-ELT’s core spectroscopic capability at first light. Using the fast wavefront sensors, cameras and accelerometers, we managed to identify the origin of most of the vibrations degrading our performance. Mag AO has been in on-sky operation for 166 nights since installation in 2012. The principal aim of the project was to quantify the performances of an atmospherical non-hydrostatical mesoscale model (Astro-Meso-NH code) in forecasting all the main atmospherical parameters relevant for the ground-based astronomical observations and the optical turbulence (C and associated integrated astroclimatic parameters) above Cerro Paranal (site of the VLT) and Cerro Armazones (site of the E-ELT).

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These high resolution atmospheric parameters are critical for design studies and statistical evaluation of on-sky performance under real conditions. But even at that speed, we are still limited by low-frequency vibrations.

In this development phase, the IRIS science team has paid particular attention to the selection of filters, gratings, sensitivities of the entire system, and science cases that will benefit from the parallel mode of the IFS and imaging camera. We present in the following the MICADO-MAORY SCAO specifications, the current SCAO prototyping activities at LESIA for E-ELT scale pyramid wavefront sensor (WFS) and real-time computer (RTC), our activities on end-to-end AO simulations and the current preliminary design of SCAO subsystems. These solutions will not only improve significantly SCEx AOs performance, but will also help all the other instruments on the Subaru Telescope, especially the ones behind AO188. A recent addition is the RHEA spectrograph enabling spatially resolved high resolution spectroscopy of the surfaces of giant stars, for example.

We present new science cases for IRIS using the latest end-to-end data simulator on the following topics: Solar System bodies, the Galactic center, active galactic nuclei (AGN), and distant gravitationally-lensed galaxies. We finish by presenting the implementation and current design studies for the high-contrast imaging mode of MICADO, which will make use of the SCAO correction offered to the instrument. Ultimately, this study will also help the development of the TMT, as these two telescopes share very similar drives. New capabilities on the horizon include post-coronagraphic spectroscopy, spectral differential imaging, nulling interferometry as well as an integral field spectrograph and an MKID array.

We highlight the need for new algorithms to improve the modeling of the complex variation of the Point Spread Function (PSF) across the field of view. The LTAO system, consisting of up to 6 LGS and up to 3 low-order NGS WFS and located outside the cryostat, is designed to increase the sky coverage on arbitrary targets to E. This paper presents some aspects of the calibration plan that has been developed for NFIRAOS, the TMT first light MCAO system. The DKIST wavefront correction system will provide active alignment control and jitter compensation for all six of the DKIST science instruments.

Finally, we outline the role that large samples of stellar standards plays in providing a detailed description of the MCAO performance and in precise and accurate colour-magnitude diagrams. The plan consolidates the best practices from current 8-meter class AO instruments, while also addressing the specificities of NFIRAOS. Five of the instruments will also be fed by a conventional adaptive optics (AO) system, which corrects for high frequency jitter and atmospheric wavefront disturbances.

We use the large number of stars in the field of view to determine with high accuracy the PSF model for the profile fitting photometry. AO optimal control relies centrally on a stochastic model of the turbulence. The DKIST wavefront correction team has completed the design phase and is well into the fabrication phase.