The MICADO first light imager for the ELT: overview, operation, simulation

Davies, Richard; Alves, J.; Clénet, Y.; Lang-Bardl, Florian; Nicklas, H.; Pott, Jörg-Uwe; Ragazzoni, Roberto; Tolstoy, Eline; Amico, Paola; Anwand-Heerwart, H.; Barboza, Santiago; Barl, L.; Baudoz, Pierre; Bender, Ralf; Bezawada, Naidu; Bizenberger, Peter; Boland, W.; Bonifacio, P.; Borgo, Bruno; Buey, T.; Chapron, F.; Chemla, Fanny; Cohen, Mathieu; Czoske, O.; Déo, Vincent; Disseau, K.; Dreizler, S.; Dupuis, Olivier; Fabricius, Maximilian; Falomo, R.; Fédou, P.; Schreiber, N. Förster; Garrel, Vincent; Geis, N.; Gemperlein, Hans; Gendron, É.; Genzel, R.; Gillessen, S.; Glück, Martin; Grupp, Frank; Hartl, Michael; Hauser, M. G.; Hess, Hans-Joachim; Hofferbert, R.; Hopp, U.; Hörmann, Veronika; Hubert, Z.; Huby, Elsa; Huet, Jean-Michel; Hutterer, Victoria; Ives, Derek; Janssen, A.; Jellema, Willem; Kausch, W.; Kerber, F.; Kravcar, H.; Ruyet, Bertrand Le; Leschinski, Kieran; Mandla, Christopher; Manhart, M.; Massari, D.; Mei, S.; Merlin, Francesca; Mohr, Lars; Monna, A.; Muench, Norbert; Müller, Friedrich; Musters, Gert; Navarro, Ramón; Neumann, Udo; Neumayer, Nadine; Niebsch, Jenny; Plattner, Markus; Przybilla, N.; Rabien, S.; Ramlau, Ronny; Ramos, J.; Ramsay, Suzanne; Rhode, P.; Richter, Amon; Richter, Josef; Rix, H. W.; Rodeghiero, Gabriele; Rohloff, R. R.; Rosensteiner, Matthias; Rousset, G.; Schlichter, Jörg; Schubert, J.; Sevin, Arnaud; Stuik, Remko; Sturm, E.; Thomas, Jens; Tromp, Niels; Verdoes-Kleijn, Gijs; Vidal, Fabrice; Wagner, Roland; Wegner, Michael; Zeilinger, W. W.; Ziegleder, J.; Ziegler, B.; Zins, G.

doi:10.1117/12.2311483

Cited by 17 publications

(5 citation statements)

References 24 publications

(16 reference statements)

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“…Further optical observations of these targets with dedicated observations or matched objects in Gaia or LSST object lists will allow us to constrain the radio optical offsets. The identified offset-AGN candidates can then be further investigated with dedicated follow-up at milliarcsecond angular resolution at the radio wavelengths with SKA-VLBI (Paragi et al 2015) and at the optical/near-infrared wavelengths with future adaptive optics instrumentation, such as MICADO at the Extremely Large Telescope (E-ELT, Massari et al 2016;Davies et al 2018).…”

Section: Tracing the Evolution Of Active Galaxies Using Large Samplesmentioning

confidence: 99%

Constraining VLBI−optical offsets in high redshift galaxies using strong gravitational lensing

Spingola

Barnacka

2020

Monthly Notices of the Royal Astronomical Society

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We present a multi-wavelength analysis of two highly magnified strong gravitationally lensed galaxies, CLASS B0712+472 and CLASS B1608+656, at redshifts 1.34 and 1.394, respectively, using new VLBI and archival HST observations. We reconstruct the positions of the radio and optical emissions with their uncertainties using Monte Carlo sampling. We find that in CLASS B0712+472 the optical and radio emissions are co-spatial within 2 ± 5 mas (17 ± 42 pc at redshift of 1.34). But, in CLASS B1608+656, we reconstruct an optical-radio offset of 25 ± 16 mas (214 ± 137 pc at redshift of 1.394), the smallest offset measured for an AGN at such high redshift. The spectral features indicate that CLASS B1608+656 is a post-merger galaxy, which, in combination with the optical-VLBI offset reported here, makes CLASS B1608+656 a promising candidate for a high-z offset-AGN. Furthermore, the milliarcsecond angular resolution of the VLBI observations combined with the precise lens models allow us to spatially locate the radio emission at 0.05 mas precision (0.4 pc) in CLASS B0712+472, and 0.009 mas precision (0.08 pc) in CLASS B1608+656. The search for optical-radio offsets in high redshift galaxies will be eased by the upcoming synoptic all-sky surveys, including E-ELT and SKA, which are expected to find ∼ 10 5 strongly lensed galaxies, opening an era of large strong lensing samples observed at high angular resolution.

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Section: Tracing the Evolution Of Active Galaxies Using Large Samplesmentioning

confidence: 99%

Constraining VLBI−optical offsets in high redshift galaxies using strong gravitational lensing

Spingola

Barnacka

2020

Monthly Notices of the Royal Astronomical Society

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“…Due to the combination of increased angular resolution and collecting aperture, diffraction-limited ELT observations will at the same time access smaller angular separations, and achieve higher astrometric precision at angular separations accessible to 8m-class imagers. Assuming that all the astrometric uncertainties listed in Table 6 scale as λ∕D, we also estimated a calibration error budget for a high-contrast imaging instrument on the ELT operating in the H band, which is covered by the Multi-adaptive optics Imaging Camera for Deep Observations (MICADO) 63 and the High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI), 64 and in the L 0 band, which is covered by the Mid-infrared ELT Imager and Spectrograph (METIS). 65 Under this assumption and assuming that the measurement uncertainties in the position of detected companions are small compared to the calibration uncertainty (i.e., companions detected with S/N larger than the ratio of the PSF width over the calibration uncertainty), we expect that sub-mas precisions should be achieved with exoplanet imaging instruments on the ELT.…”

Section: Discussionmentioning

confidence: 99%

“…MICADO is the only instrument for which the design is driven by astrometric requirements for the observation of the Galactic Center and wide stellar fields. 63 The requirements in regular imaging are 50 μas, with a goal of 20 μas. 68 This will be achieved thanks to a dedicated astrometric stability by design and built-in calibration strategy.…”

Section: Exoplanet Imaging With the Eltmentioning

confidence: 99%

Lessons learned from SPHERE for the astrometric strategy of the next generation of exoplanet imaging instruments

Maire

Langlois

Delorme

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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Measuring the orbits of directly imaged exoplanets requires precise astrometry at the milliarcsec level over long periods of time due to their wide separation to the stars (≳10 au) and long orbital period (≳20 yr). To reach this challenging goal, a specific strategy was implemented for the instrument Spectro-Polarimetric High-contrast Exoplanet Research (SPHERE), the first dedicated exoplanet imaging instrument at the Very Large Telescope of the European Southern Observatory (ESO). A key part of this strategy relies on the astrometric stability of the instrument over time. We monitored for five years the evolution of the optical distortion, pixel scale, and orientation to the True North of SPHERE images using the near-infrared instrument IRDIS. We show that the instrument calibration achieves a positional stability of ∼1 mas over 2″ field of views. We also discuss the SPHERE astrometric strategy, issues encountered in the course of the on-sky operations, and lessons learned for the next generation of exoplanet imaging instruments on the Extremely Large Telescope being built by ESO. © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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“…The telescope-born distortions are characterized by low-order terms; the warm MAORY optics have larger distortions (with respect to the ELT) but higher optomechanical stability, whereas the cold MICADO optics have even higher distortions due to the magnifying optics, but extreme stability. For instruments such as MICADO 14 and IRIS, 15 the common figure of merit for the relative astrometry at single-and multi-epoch observations is 50 μas in the near-infrared (NIR) for sources ∼1 as apart. The origin and fundamental limits of achieving 50 μas-level astrometry with the ELT/MICADO was discussed by Pott et al 16 Generally, NIR refers to a wavelength range of 0.8 to 2.4 μm where typically higher AO performances (and boosted astrometry) are achieved at the red side of this range (H-K band).…”

Section: Introductionmentioning

confidence: 99%

“…MICADO is targeted to be the synthesis of the best characteristics of the previous astrometric imagers in terms of optomechanical stability located at the Nasmyth focus and the sensitivity gain from the ELT. Although the instrument design is astrometry oriented 14 and it provides an imaging channel with no moving parts to ensure the highest stability, several systematics notch the astrometric precision at different levels. The astrometric error budget takes into account the nominal distortion by design, the as-built manufacturing residuals, the tolerances, and the AO corrections.…”

Section: Introductionmentioning

confidence: 99%

Performance and limitations of using ELT and MCAO for 50 μas astrometry

Rodeghiero

Arcidiacono

Pott

et al. 2021

J. Astron. Telesc. Instrum. Syst.

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Multi-conjugated adaptive optics (MCAO) is essential for performing astrometry with the Extremely Large Telescope (ELT). Unlike most of the 8-m class telescopes, the ELT will be a fully adaptive telescope, and a significant portion of the adaptive optics (AO) dynamic range will be depleted by the correction and stabilization of the telescope aberrations and instabilities. MCAO systems are of particular interest for ground-based astrometry since they stabilize the low-order field distortions and transient plate scale instabilities, which originate from the telescope and in the instrument. All instruments have several optical elements relatively far away from the pupil that can potentially challenge the astrometric precision of the observations with their residual mid-spatial frequencies errors. Using a combined simulation of ray tracing and AO numerical codes, we assess the impact of these systematic errors at different field-ofview (FoV) scales and fitting scenarios. The distortions have been assessed at different sky position angles (PA) and indicate that over large FoVs only small PA ranges (AE1 deg to 3 deg) are accessible with astrometric residuals ≤50 μas. A full compliance with the astrometric requirement, at any PA, is achievable for 2 arc sec 2 FoV patches already with a third-order polynomial. The natural partition of the optical system into three segments, i.e., the ELT, the MAORY MCAO module, and the MICADO instrument, resembles a splitting of the astrometric problem into the three subsystems that are characterized by different distortion amplitudes and calibration strategies. The result is a family portrait of the different optical segments with their specifications, dynamic motions, conjugation height, and AO correctability, leading to tracing their role in the bigger puzzle of the 50-μas as astrometric endeavor. © The Authors. Published by SPIE under a Creative Commons Attribution 4.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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The MICADO first light imager for the ELT: overview, operation, simulation

Cited by 17 publications

References 24 publications

Constraining VLBI−optical offsets in high redshift galaxies using strong gravitational lensing

Constraining VLBI−optical offsets in high redshift galaxies using strong gravitational lensing

Lessons learned from SPHERE for the astrometric strategy of the next generation of exoplanet imaging instruments

Performance and limitations of using ELT and MCAO for 50 μas astrometry

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