The High-contrast End-to-End Performance Simulator (HEEPS): influence of ELT/METIS instrumental effects

Delacroix, Christian; Absil, Olivier; Xivry, Gilles Orban de; Shinde, Muskan; Pathak, Prashant; Cantalloube, F.; Carlomagno, Brunella; Christiaens, Valentin; Boné, André; Dolkens, Dennis; Kenworthy, Matthew A.; Doelman, David

doi:10.1117/12.2630341

Cited by 2 publications

(2 citation statements)

References 16 publications

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“…The excellent optical performance of the METIS AO system (section 4.2) enables efficient coronagraphy and high contrast imaging [33], [34]. Since the theoretical contrast curves are generally quite optimistic for the real environment at the telescope, we have included several likely perturbations in our simulations, such as pupil drift, Talbot effect, residual non common path aberrations (NCPA) and the effect of a cluster of 7 slightly misaligned ELT M1 segments.…”

Section: High Contrast Imaging Performancementioning

confidence: 99%

Status update on the development of METIS, the mid-infrared ELT imager and spectrograph

Brandl¹,

Bettonvil

Boekel

et al. 2022

Ground-Based and Airborne Instrumentation for Astronomy IX

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The Mid-Infrared ELT Imager and Spectrograph (METIS) is one of the first generation science instruments on ESO's 39m Extremely Large Telescope (ELT). METIS will provide diffraction-limited imaging and medium resolution slitspectroscopy from 3 -13 microns (L, M, and N bands), as well as high resolution (R ~ 100,000) integral field spectroscopy from 2.9 -5.3 microns. Both imaging and IFU spectroscopy can be combined with coronagraphic techniques. After passing its preliminary design review (PDR) in May 2019, and the final design review (FDR) of its optical system in June 2021, METIS is now preparing for the FDR of its entire system in the fall of 2022, while the procurements of many optical components have already started. First light at the telescope is expected in 2028, after a comprehensive assembly integration and test phase. In this paper we focus mainly on the various design aspects, and present a status update on the final optical and mechanical design of METIS. We describe the conceptual setup of METIS, its key functional components, and the resulting observing modes. Last but not least, we present the expected scientific performance, in terms of sensitivity, adaptive optics, and high contrast imaging performance.

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Section: High Contrast Imaging Performancementioning

confidence: 99%

Status update on the development of METIS, the mid-infrared ELT imager and spectrograph

Brandl¹,

Bettonvil

Boekel

et al. 2022

Ground-Based and Airborne Instrumentation for Astronomy IX

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“…To model this incoherent emission, we take small test apertures of radius a as representative of independent point sources in the telescope pupil. We propagate these test apertures, one by one, through the METIS CVC, using the HCI end-to-end performance simulator (HEEPS 27 ), to infer their associated fluxes on the detector. Then we sum the contributions of all these small apertures to get the total flux on the detector, which is basically the VCG.…”

Section: Simulationsmentioning

confidence: 99%

Modeling the vortex center glow in the ELT/METIS vortex coronagraph

Shinde¹,

Delacroix²,

Xivry³

et al. 2022

Modeling, Systems Engineering, and Project Management for Astronomy X

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The Mid-infrared ELT Imager and Spectrograph (METIS) is among the first three scientific instruments commissioned at the ELT. It will implement vortex coronagraphy to achieve high-contrast imaging (HCI) at small angular separations from bright, nearby stars. An important unresolved problem with vortex coronagraphy is the vortex center glow (VCG) effect, where the thermal emission from the warm environment around the entrance pupil is partially diffracted into the image of the pupil by the vortex phase mask (VPM), which shows up as a diffuse bright spot in the center of the image. This effect has proven to be a significant nuisance in previous mid-infrared observations. Here, we use physical optics propagation to model the VCG for the first time and evaluate its strength with respect to the background flux in standard noncoronagraphic imaging in the context of ELT/METIS. Through our end-to-end simulations we find that the VCG peaks at about 70% of the standard background flux at an angular separation of 1 λ/D from the star and reduces to about 20% at 5 λ/D from the star. We apply the same method to model the VCG for the VLT/VISIR configuration, and show our model to be in agreement with the actual VCG measured in VISIR data, where the peak of the VCG is about twice as bright as the thermal background. In case the VCG turns out to be larger than anticipated in METIS, we propose two methods to mitigate it: (i) adding pupil stops in the pupil plane upstream to the VPM to block all of the thermal emission, and (ii) adding undersized Lyot stops in the image plane to block part of the diffracted light.

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The High-contrast End-to-End Performance Simulator (HEEPS): influence of ELT/METIS instrumental effects

Cited by 2 publications

References 16 publications

Status update on the development of METIS, the mid-infrared ELT imager and spectrograph

Status update on the development of METIS, the mid-infrared ELT imager and spectrograph

Modeling the vortex center glow in the ELT/METIS vortex coronagraph

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