NAOMI: the adaptive optics system of the Auxiliary Telescopes of the VLTI

Woillez, J.; Abad, José Antonio; Abuter, R.; Carpentier, E. Aller; Alonso, Jaime; Andolfato, Luigi; Barriga, P.; Berger, J.‐P.; Beuzit, Jean-Luc; Bonnet, Henri; Bourdarot, Guillaume; Bourget, P.; Brast, R.; Caniguante, Luis; Cottalorda, Eric; Darré, Pascaline; Délabre, Bernard; Delboulbé, A.; Delplancke-Ströbele, F.; Dembet, R.; Donaldson, Rob; Dorn, Reinhold J.; Dupeyron, Jorge; Dupuy, Christophe; Egner, Sebastian; Eisenhauer, F.; Fischer, Gerhard W.; Frank, Christoph; Fuenteseca, Eloy; Gitton, Philippe B.; Gonté, Frederic; Guerlet, Thibaut; Guieu, S.; Gutierrez, P.; Haguenauer, Pierre; Haimerl, Andreas; Haubois, X.; Heritier, Cédric Taïssir; Huber, Stefan; Hubin, N.; Jolley, Paul; Jocou, L.; Kirchbauer, Jean-Paul; Kolb, Johann; Kosmalski, Johan; Krempl, P. W.; Bouquin, J.-B. Le; Louarn, Miska Le; Lilley, Paul; López, B.; Magnard, Y.; McLay, Stewart; Meilland, A.; Meister, Alexander; Mérand, A.; Moulin, T.; Pasquini, L.; Paufique, J.; Percheron, Isabelle; Pettazzi, Lorenzo; Pfuhl, O.; Phan, D. T.; Pirani, Werther; Quentin, J.; Rakich, Andrew; Ridings, R.; Riedel, Mario; Reyes, Javier Escalera; Rochat, S.; Tomás, Gonsalo Santos; Schmid, Christian; Schuhler, Nicolas; Shchekaturov, Pavel; Seidel, Matthias; Soenke, C.; Stadler, Eric; Stephan, Christian; Suárez, M.; Todorovic, Mirko; Valdes, G.; Vérinaud, Christophe; Zins, G.; Zúñiga-Fernández, S.

doi:10.1051/0004-6361/201935890

Cited by 28 publications

(8 citation statements)

References 19 publications

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“…Interferometric LM and N band data were obtained on 2019 July 9 and 11 using the instrument MATISSE (Lopez et al 2014) on the VLTI (Table 1). The Auxiliary Telescopes (ATs) were arranged in medium configuration and the New Adaptive Optics Module for Interferometry (NAOMI; Woillez et al 2019) was used. We simultaneously obtained visibility measurements on six baselines (baseline lengths between B = 30 and 95 m).…”

Section: O B S E Rvat I O N Smentioning

confidence: 99%

First L band detection of hot exozodiacal dust with VLTI/MATISSE

Kirchschlager

Wolf

Matter

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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For the first time we observed the emission of hot exozodiacal dust in L band. We used the new instrument MATISSE at the Very Large Telescope Interferometer to detect the hot dust around κ Tuc with a significance of 3σ to 6σ at wavelengths between 3.37 and 3.85 μm and a dust-to-star flux ratio of 5 to $7\,\mathrm{\%}$. We modelled the spectral energy distribution based on the new L band data alone and in combination with H band data published previously. In all cases we find 0.58 μm grains of amorphous carbon to fit the κ Tuc observations the best, however, also nanometre or micrometre grains and other carbons or silicates reproduce the observations well. Since the H band data revealed a temporal variability, while our L band data were taken at a different epoch, we combine them in different ways. Depending on the approach, the best fits are obtained for a narrow dust ring at a stellar distance in the 0.1 to 0.29 au range and thus with a temperature between 940 and 1430 K. Within the 1σ uncertainty dust location and temperature are confined to 0.032 − 1.18 au and 600 − 2000 K.

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Section: O B S E Rvat I O N Smentioning

confidence: 99%

First L band detection of hot exozodiacal dust with VLTI/MATISSE

Kirchschlager

Wolf

Matter

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

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“…Actuator and modal gains are also known to depend on device temperature and can be compensated for with calibrated look-up tables, 16,24 although on-sky tests have shown that modal gains are uncorrelated with the DM housing temperature and are better estimated on-sky in the absence of an internal temperature sensor. 27 The drift of the DM membrane via creep contributes a time-dependent source of WFE to the system. In closed loop, creep is corrected as it arises, so we do not anticipate the need for a creep compensation scheme on the system woofer or the NCPC DM under most conditions.…”

Section: Alpao Shape Creepmentioning

confidence: 99%

Characterizing deformable mirrors for the MagAO-X instrument

Gorkom

Males

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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The MagAO-X instrument is a new extreme adaptive optics system for high-contrast imaging at visible and near-infrared wavelengths on the Magellan Clay Telescope. A central component of this system is a 2040-actuator microelectromechanical deformable mirror (DM) from Boston Micromachines Corp. that operates at 3.63 kHz for high-order wavefront control (the tweeter). Two additional DMs from ALPAO perform the low-order (the woofer) and non-common-path science-arm wavefront correction (the NCPC DM). Prior to integration with the instrument, we characterized these devices using a Zygo Verifire Interferometer to measure each DM surface. We present the results of the characterization effort here, demonstrating the ability to drive tweeter to a flat of 6.9 nm root mean square (RMS) surface (and 0.56 nm RMS surface within its control bandwidth), the woofer to 2.2 nm RMS surface, and the NCPC DM to 2.1 nm RMS surface over the MagAO-X beam footprint on each device. Using focus-diversity phase retrieval on the MagAO-X science cameras to estimate the internal instrument wavefront error (WFE), we further show that the integrated DMs correct the instrument WFE to 18.7 nm RMS, which, combined with a 11.7% pupil amplitude RMS, produces a Strehl ratio of 0.94 at Hα.

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“…The seeing, which represents the integrated strength of the turbulence along the line of sight, is the parameter used systematically for any instrument at the VLT to constrain the turbulence conditions, and this quantity can evolve rapidly in a matter of minutes. In addition, the use of adaptive optics (AO) systems at the VLT has expanded significantly in the past 3 years: all VLTI instruments are now AO-fed 2,3 and Unit Telescope 4 is a fully adaptive telescope. 4 In terms of operations, this means that new turbulence parameters have to be considered to ensure that these systems deliver their full performance.…”

Section: Supporting the Night Astronomer In Decision-making At Nightmentioning

confidence: 99%

Nowcasting the turbulence at the Paranal Observatory

Milli¹,

Gonzalez²,

Fluxa³

et al. 2019

Preprint

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At Paranal Observatory, the least predictable parameter affecting the short-term scheduling of astronomical observations is the optical turbulence, especially the seeing, coherence time and ground layer fraction. These are critical variables driving the performance of the instruments of the Very Large Telescope (VLT), especially those fed with adaptive optics systems. Currently, the night astronomer does not have a predictive tool to support him/her in decision-making at night. As most service-mode observations at the VLT last less than two hours, it is critical to be able to predict what will happen in this time frame, to avoid time losses due to sudden changes in the turbulence conditions, and also to enable more aggressive scheduling. We therefore investigate here the possibility to forecast the turbulence conditions over the next two hours. We call this "turbulence nowcasting", analogously with weather nowcasting, a term already used in meteorology coming from the contraction of "now" and "forecasting". We present here the results of a study based on historical data of the Paranal Astronomical Site Monitoring combined with ancillary data, in a machine learning framework. We show the strengths and shortcomings of such an approach, and present some perspectives in the context of the Extremely Large Telescope.

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NAOMI: the adaptive optics system of the Auxiliary Telescopes of the VLTI

Cited by 28 publications

References 19 publications

First L band detection of hot exozodiacal dust with VLTI/MATISSE

First L band detection of hot exozodiacal dust with VLTI/MATISSE

Characterizing deformable mirrors for the MagAO-X instrument

Nowcasting the turbulence at the Paranal Observatory

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