ERIS: revitalising an adaptive optics instrument for the VLT

Davies, Richard; Esposito, Simone; Schmid, Hans Martin; Taylor, W. D.; Agapito, Guido; Berbel, Alex Agudo; Baruffolo, A.; Biliotti, Valdemaro; Biller, Beth; Black, Martin; Boehle, Anna; Briguglio, B.; Buron, A.; Carbonaro, Luca; Cortes, Angela; Cresci, G.; Deysenroth, M.; Cianno, A. Di; Rico, G. Di; Doelman, David; Dolci, M.; Dorn, Reinhold J.; Eisenhauer, F.; Fantinel, D.; Ferruzzi, D.; Feuchtgruber, H.; Schreiber, N. Förster; Gao, Xiaofeng; Gemperlein, Hans; Genzel, R.; George, E. M.; Gillessen, S.; Giordano, Christophe; Glauser, Adrian M.; Glindemann, Andreas; Grani, Paolo; Hartl, Michael; Heijmans, Jeroen; Henry, David; Huber, Heinrich J.; Kasper, Markus; Keller, Christoph U.; Kenworthy, Matthew A.; Kühn, Jonas; Küntschner, H.; Lightfoot, J. F.; Lunney, D.; MacIntosh, Mike; Mannucci, F.; March, S.; Neeser, Mark; Patapis, Polychronis; Pearson, D.; Plattner, Markus; Puglisi, Alfio; Quanz, Sascha P.; Rau, C.; Riccardi, Armando; Salasnich, Bernardo; Snik, Frans; Sturm, E.; Valentini, Angelo; Waring, Chris; Wiezorrek, E.; Xompero, Marco

doi:10.1117/12.2311480

Cited by 20 publications

(10 citation statements)

References 26 publications

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“…( 6) gives EE core;OBS;uncorrected ¼ 0.36, in contrast with the observed value of EE core;OBS ¼ 0.43. The shape factor in this case results: E Q -T A R G E T ; t e m p : i n t r a l i n k -; e 0 0 9 ; 1 1 6 ; 4…”

Section: Appendix A: a Practical Relation Linking Sr Fwhm And Eementioning

confidence: 99%

“…In many scientific applications exploiting diffraction limit AO capabilities, [1][2][3][4][5][6] a serious challenge experienced during data analysis is the precise knowledge of the two-dimensional point spread function (PSF): approaching the diffraction limit of ground-based cornerstone facilities is not an easy task. A severe drawback in this sense is that the PSF of an AO system is a very complex entity, which has a high number of degrees of freedom involved, varies spatially in the field of view (FOV), is not constant in time, and behaves differently at each wavelength.…”

Section: Introductionmentioning

confidence: 99%

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Point spread function reconstruction for SOUL + LUCI LBT data

Simioni

Arcidiacono

Wagner

et al. 2022

J. Astron. Telesc. Instrum. Syst.

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Here, we present the status of an ongoing project aimed at developing a point spread function (PSF) reconstruction software for adaptive optics (AO) observations. In particular, we test for the first time the implementation of pyramid wave-front sensor data on our algorithms. As a first step in assessing its reliability, we applied the software to bright, on-axis, point-like sources using two independent sets of observations, acquired with the single-conjugated AO upgrade for the Large Binocular Telescope. Using only telemetry data, we reconstructed the PSF by carefully calibrating the instrument response. The accuracy of the results has been first evaluated using the classical metric: specifically, the reconstructed PSFs differ from the observed ones by <2% in Strehl ratio and 4.5% in full-width at half maximum. Moreover, the recovered encircled energy associated with the PSF core is accurate at 4% level in the worst case. The accuracy of the reconstructed PSFs has then been evaluated by considering an idealized scientific test-case consisting in the measurements of the morphological parameters of a compact galaxy. In the future, our project will include the analysis of anisoplanatism, low signal-to-noise ratio regimes, and the application to multi-conjugated AO observations.

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Section: Appendix A: a Practical Relation Linking Sr Fwhm And Eementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Point spread function reconstruction for SOUL + LUCI LBT data

Simioni

Arcidiacono

Wagner

et al. 2022

J. Astron. Telesc. Instrum. Syst.

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“…The Enhanced Resolution Imager and Spectrograph (ERIS) will be installed in the Cassegrain focus of UT4 at the Very Large Telescope in the near future [85,86]. ERIS is a 1-5 m instrument with an imager (NIX) operating from -band and an IFS (SPIFFIER) in -band with R∼8000.…”

Section: Vlt/erismentioning

confidence: 99%

Vector-apodizing phase plate coronagraph: design, current performance, and future development [Invited]

et al. 2021

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Over the last decade, the vector-apodizing phase plate (vAPP) coronagraph has been developed from concept to on-sky application in many high-contrast imaging systems on 8-m class telescopes. The vAPP is an geometric-phase patterned coronagraph that is inherently broadband, and its manufacturing is enabled only by direct-write technology for liquid-crystal patterns. The vAPP generates two coronagraphic PSFs that cancel starlight on opposite sides of the point spread function (PSF) and have opposite circular polarization states. The efficiency, that is the amount of light in these PSFs, depends on the retardance offset from half-wave of the liquid-crystal retarder. Using different liquid-crystal recipes to tune the retardance, different vAPPs operate with high efficiencies (> 96%) in the visible and thermal infrared (0.55 µm to 5 µm). Since 2015, seven vAPPs have been installed in a total of six different instruments, including Magellan/MagAO, Magellan/MagAO-X, Subaru/SCExAO, and LBT/LMIRcam. Using two integral field spectrographs installed on the latter two instruments, these vAPPs can provide lowresolution spectra (R∼30) between 1 m and 5 m. We review the design process, development, commissioning, on-sky performance, and first scientific results of all commissioned vAPPs. We report on the lessons learned and conclude with perspectives for future developments and applications.

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“…The Enhanced Resolution Imager and Spectrograph (ERIS) will be installed in the Cassegrain focus of UT4 at the Very Large Telescope in the near future [85,86]. ERIS is a 1-5 𝜇m instrument with an imager (NIX) operating from 𝐽-𝑀 𝑝 band and an IFS (SPIFFIER) in 𝐽-𝐾 band with R∼8000.…”

Section: Vlt/erismentioning

confidence: 99%

The vector-apodizing phase plate coronagraph: design, current performance, and future development

Doelman,

Snik,

Por

et al. 2021

Preprint

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Over the last decade, the vector-apodizing phase plate (vAPP) coronagraph has been developed from concept to on-sky application in many high-contrast imaging systems on 8-m class telescopes. The vAPP is an geometric-phase patterned coronagraph that is inherently broadband, and its manufacturing is enabled only by direct-write technology for liquid-crystal patterns. The vAPP generates two coronagraphic PSFs that cancel starlight on opposite sides of the point spread function (PSF) and have opposite circular polarization states. The efficiency, that is the amount of light in these PSFs, depends on the retardance offset from half-wave of the liquid-crystal retarder. Using different liquid-crystal recipes to tune the retardance, different vAPPs operate with high efficiencies (> 96%) in the visible and thermal infrared (0.55 µm to 5 µm). Since 2015, seven vAPPs have been installed in a total of six different instruments, including Magellan/MagAO, Magellan/MagAO-X, Subaru/SCExAO, and LBT/LMIRcam. Using two integral field spectrographs installed on the latter two instruments, these vAPPs can provide lowresolution spectra (R∼30) between 1 𝜇m and 5 𝜇m. We review the design process, development, commissioning, on-sky performance, and first scientific results of all commissioned vAPPs. We report on the lessons learned and conclude with perspectives for future developments and applications.

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ERIS: revitalising an adaptive optics instrument for the VLT

Cited by 20 publications

References 26 publications

Point spread function reconstruction for SOUL + LUCI LBT data

Point spread function reconstruction for SOUL + LUCI LBT data

Vector-apodizing phase plate coronagraph: design, current performance, and future development [Invited]

The vector-apodizing phase plate coronagraph: design, current performance, and future development

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