SPARTA for the VLT: status and plans

Valles, M. Suárez; Fedrigo, Enrico; Donaldson, Robert H.; Soenke, C.; Zampieri, Stefano; Bourtembourg, Reynald; Helmut, Tischer,

doi:10.1117/12.925290

Cited by 13 publications

(7 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The RTC, named SPARTA, 23,24 is provided by ESO. SPARTA offers, as specified, a very modular and fine-grained RTC architecture.…”

Section: Real-time Computer and Algorithmsmentioning

confidence: 99%

“…A more detailed description can be found in Suárez Valles et al 24 In addition to classical integrator, an LQG control law has been implemented for tip/tilt mirror control in order to be able to deal with system and telescope vibrations and to ensure the smallest possible residual jitter. The LQG, also known as Kalman filter, and its associated online identification processes are detailed in Sec.…”

Section: Static Ultimate Performance Internal Sourcementioning

confidence: 99%

See 1 more Smart Citation

SAXO: the extreme adaptive optics system of SPHERE (I) system overview and global laboratory performance

Sauvage

Fusco

Petit

et al. 2016

J. Astron. Telesc. Instrum. Syst

Self Cite

View full text Add to dashboard Cite

International audienceThe direct imaging of exoplanet is a leading field of today’s astronomy. The photons coming from the planet carry precious information on the chemical composition of its atmosphere. The second-generation instrument, Spectro-Polarimetric High contrast Exoplanet Research (SPHERE), dedicated to detection, photometry and spectral characterization of Jovian-like planets, is now in operation on the European very large telescope. This instrument relies on an extreme adaptive optics (XAO) system to compensate for atmospheric turbulence as well as for internal errors with an unprecedented accuracy. We demonstrate the high level of performance reached by the SPHERE XAO system (SAXO) during the assembly integration and test (AIT) period. In order to fully characterize the instrument quality, two AIT periods have been mandatory. In the first phase at Observatoire de Paris, the performance of SAXO itself was assessed. In the second phase at IPAG Grenoble Observatory, the operation of SAXO in interaction with the overall instrument has been optimized. In addition to the first two phases, a final check has been performed after the reintegration of the instrument at Paranal Observatory, in the New Integration Hall before integration at the telescope focus. The final performance aimed by the SPHERE instrument with the help of SAXO is among the highest Strehl ratio pretended for an operational instrument (90% in H band, 43% in V band in a realistic turbulence r0, and wind speed condition), a limit R magnitude for loop closure at 15, and a robustness to high wind speeds. The full-width at half-maximum reached by the instrument is 40 mas for infrared in H band and unprecedented 18.5 mas in V band.L'imagerie directe d'exoplanètes est un domaine phare de l'astronomie actuelle. Les photons issus de la planète sont porteurs d'une information précieuse sur la composition chimique de son atmosphère. L'instrument de seconde génération SPHERE, Spectro-Polarimetri High-contrast Exoplanet Research, dédié à la détection la photométrie et la caractérisation spectrale de planètes joviennes, est maintenant en opération sur le très grand télescope Européen (VLT). Cet instrument repose sur une optique adaptative à très hautes performances (XAO) pour compenser les turbulences atmosphériques, comme les défauts optiques internes de l'instrument lui-même. Nous démontrons les très hauts niveaux de performance atteint par l'instrument SPHERE et son système de XAO SAXO, pendant la phase d'intégration (AIT). Pour pleinement caractériser les performances de l'instrument, deux périodes d'AIT ont été obligatoires. Dans la première phase à l'Observatoire de Paris, les performances de l'optique adaptative seule ont été obtenues. Dans la seconde phase à l'observatoire de Grenoble, l'opération de SAXO en interaction avec le reste de l'instrument ont été optimisées. En sus, une vérification finale a été faite au foyer du télescope. Les performances atteintes par SPHERE avec l'aide de SAXO sont parmi les plus hauts rapports de Strehl jamais at...

show abstract

“…The RTC, named SPARTA, 23,24 is provided by ESO. SPARTA offers, as specified, a very modular and fine-grained RTC architecture.…”

Section: Real-time Computer and Algorithmsmentioning

confidence: 99%

Section: Static Ultimate Performance Internal Sourcementioning

confidence: 99%

SAXO: the extreme adaptive optics system of SPHERE (I) system overview and global laboratory performance

Sauvage

Fusco

Petit

et al. 2016

J. Astron. Telesc. Instrum. Syst

Self Cite

View full text Add to dashboard Cite

show abstract

“…A dedicated RTC application optimized for GRAVITY will be built on the newly developed SPARTA-Light platform, the low-cost implementation of ESO's Standard Platform for Adaptive Optics Real Time Applications (SPARTA). 12 Detailed AO performance simulations were performed for this optimization, examining the number of subapertures, operating frequency, centroiding window and algorithm, given different atmospheric conditions, WFS bandpasses, guide star magnitudes and WFS operational modes. Key results from these simulations are presented in Section 3.…”

Section: Adaptive Optics Real-time Controlmentioning

confidence: 99%

GRAVITY Coudé Infrared Adaptive Optics (CIAO) system for the VLT Interferometer

Kendrew¹,

Hippler²,

Brandner³

et al. 2012

SPIE Proceedings

Self Cite

View full text Add to dashboard Cite

GRAVITY is a second generation instrument for the VLT Interferometer, designed to enhance the near-infrared astrometric and spectro-imaging capabilities of VLTI. Combining beams from four telescopes, GRAVITY will provide an astrometric precision of order 10 micro-arcseconds, imaging resolution of 4 milli-arcseconds, and low and medium resolution spectro-interferometry, pushing its performance far beyond current infrared interferometric capabilities. To maximise the performance of GRAVITY, adaptive optics correction will be implemented at each of the VLT Unit Telescopes to correct for the effects of atmospheric turbulence. To achieve this, the GRAVITY project includes a development programme for four new wavefront sensors (WFS) and NIR-optimized real time control system. These devices will enable closed-loop adaptive correction at the four Unit Telescopes in the range 1.4-2.4 µm. This is crucially important for an efficient adaptive optics implementation in regions where optically bright references sources are scarce, such as the Galactic Centre. We present here the design of the GRAVITY wavefront sensors and give an overview of the expected adaptive optics performance under typical observing conditions. Benefiting from newly developed SELEX/ESO SAPHIRA electron avalanche photodiode (eAPD) detectors providing fast readout with low noise in the near-infrared, the AO systems are expected to achieve residual wavefront errors of ≤400 nm at an operating frequency of 500 Hz.

show abstract

“…ERIS is intended to upgrade the couple NAOS-CONICA + SINFONI and, to this extent, it was conceived as a modular device, with an adaptive optics (AO) module that can feed two different scientific instruments: an imaging camera (NIX) 2 and a spectrograph (SPIFFIER) 3 . The partners involved in the construction are: INAF for the AO module 4 , 5 and the calibration unit (CU), 6 Max Planck Institute for SPIFFIER; STFC, ETH, and NOVA for the NIX camera; ESO itself for the wave front sensor (WFS) cameras and the real-time computing framework named SPARTA 7 . A picture of the entire unit is shown in Fig.…”

Section: Introductionmentioning

confidence: 99%

Reliability, availability, and maintainability analysis of the Enhanced Resolution Imager and Spectrograph adaptive optics module and lesson learned before commissioning

Xompero

Briguglio

Grani

et al. 2023

J. Astron. Telesc. Instrum. Syst.

View full text Add to dashboard Cite

Enhanced Resolution Imager and Spectrograph is an instrument currently under commissioning at the Cassegrain focus of the Very Large Telescope UT4. Its mission is to replace the suite of instruments NAOS-CONICA and SINFONI and push to the edge the capabilities of this 8-meter class telescope, by leveraging the adaptive optics module. The instrument has been designed for maximum lifetime and reliability and minimum downtime. We will present the instrument constraints and our approach to the reliability, availability, and maintainability (RAM) analysis. We identified the main actors in the system, then for each of them, we compiled a database of reliability parameters in order to build-up the reliability diagram, describing the failure sources. Starting from this information, we computed the system-wide reliability parameters and compared them with the requirements by the customer. Such a scheme is very general and may be taken as an example of RAM analysis for astronomical instrumentation; it may be also customized for the needs of other projects. In the end, we summarize the lessons learned.

show abstract

SPARTA for the VLT: status and plans

Cited by 13 publications

References 0 publications

SAXO: the extreme adaptive optics system of SPHERE (I) system overview and global laboratory performance

SAXO: the extreme adaptive optics system of SPHERE (I) system overview and global laboratory performance

GRAVITY Coudé Infrared Adaptive Optics (CIAO) system for the VLT Interferometer

Reliability, availability, and maintainability analysis of the Enhanced Resolution Imager and Spectrograph adaptive optics module and lesson learned before commissioning

Contact Info

Product

Resources

About