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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.
We show early results from the commissioning and address future implications of the results. Wright; Gregory Walth; Tuan Do; Daniel Marshall; James E. Moore; Mate Adamkovics; David Andersen; Lee Armus; Aaron Barth; Patrick Cote; Jeff Cooke; Eric M. The IRIS instrument design includes a near-infrared (0.85 - 2.4 micron) integral field spectrograph (IFS) and imager that are able to conduct simultaneous diffraction-limited observations behind the advanced adaptive optics system NFIRAOS. MICADO will also come with a SCAO capability, jointly developed by MICADO and MAORY. We are working with the telescope team to tune the motor drives and reduce the impact of the elevation encoder. It offers high Strehl ratios at near-IR wavelengths (y-K band) with stable pointing and coronagraphs with extremely small inner working angles, optimized for imaging faint companions very close to the host.
The IRIS science cases have continued to be developed and new science studies have been investigated to aid in technical performance and design requirements. SCAO will be the first AO mode to be tested at the telescope, in a phased approach of AO integration at the E-ELT. A Linear Quadratic Gaussian controller (LQG, or Kalman filter) is also being implemented inside SCEx AO to control these vibrations. In the visible, it has several interferometric imagers which offer polarimetric and spectroscopic capabilities.
Stereo-SCIDAR has demonstrated the capability to resolve turbulent layers with the required vertical resolution to support wide-field ELT instrument designs. The Subaru Coronagraphic Extreme Adaptive Optics (SCEx AO) instrument, under development for the Subaru Telescope, has currently the fastest on-sky wavefront control loop, with a pyramid wavefront sensor running at 3.5 k Hz.
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.
Follette; Enrico Pinna; Alfio Puglisi; Jennifer Vezilj; Marco Xompero; Ya-Lin Wu ”Mag AO" is the adaptive optics instrument at the Magellan Clay telescope at Las Campanas Observatory, Chile. Comparison to coetaneous profiles estimated with the Durham Stereo-SCIDAR instrument (DSS) are analysed.
We will focus the discussion on photometric precision and accuracy reached nowadays. A trade-off has been made between both visible versus infrared wave front sensing as well as Pyramid versus Shack-Hartmann, under various observing conditions and target geometries, taking into account performance, target availability, reliability and technology readiness level. New loops come into play like the one to minimize LGS Jitter and the one taking over the telescope active optics by means of offloading the DM low orders, and they all require calibration. Dedicated wavefront sensors for observations of solar prominences off the solar limb with AO have been deployed.
This enables instrument performance calibration, optimisation and data analysis of, for example, the ESO Adaptive Optics facility and the Next Generation Transit Survey. Ghez; Lei Hao; Yutaka Hayano; Michael Liu; Enrique Lopez-Rodriguez; Jessica R. Tan; Tsuyoshi Terai; Tommaso Treu; Luc Simard; Jason L. In particular, we describe the strategy developed for the different Wave-Front Sensors: pyramid for SCAO, the LGSWFS concept, the NGSWFS path, and the truth sensor capabilities. Multi-conjugate adaptive optics (MCAO) will be the primary AO mode of MICADO, driving the design of the instrument. Different approaches are being implemented to take care of these issues.
It will also be used to validate atmospheric models for turbulence forecasting. Weiss; James Wincentsen; Michael Wong; Kai Zhang The Thirty Meter Telescope (TMT) first light instrument IRIS (Infrared Imaging Spectrograph) will complete its preliminary design phase in 2016. It will be provided by MAORY, the E-ELT first-light AO module. The PID control of the image rotator has been tuned to reduce their high-frequency contribution. Hayashi SCEx AO is the premier high-contrast imaging platform for the Subaru Telescope.
Many of these instruments are already well into the design phase meaning these profies are required immediately to ensure they are optimised for the unique conditions likely to be observed. Such a feature is particularly crucial for all WFAO systems that require such detailed information on the OT vertical stratification on the whole 20 km above the ground.
Stereo-SCIDAR is a generalised SCIDAR instrument which is used to characterise the profile of the atmospheric optical turbulence strength and wind velocity using triangulation between two optical binary stars. This important achievement tells us that all the WFAO systems can rely on automatic systems that are able to support their optimized use.
Although the surface layer of the turbulence will be different for the two sites due to local geography, the high-altitude resolution profiles of the free atmosphere from this instrument will be the most accurate available for the E-ELT site. HARMONI will work at the diffraction limit of the E-ELT, thanks to a Classical and a Laser Tomographic AO system. Low-frequency vibrations are coming from the telescope drive in azimuth and elevation, as well as the elevation encoders when the target is at transit.