MICADO PSF-Reconstruction work package description
Matteo Simioni, Carmelo Arcidiacono, Andrea Grazian, Yann Clenet, Richard Davies, Marco Gullieuszik, Gijs Verdoes Kleijn, Fernando Pedichini, Roland Wagner, Ron… 展开作者
Matteo Simioni, Carmelo Arcidiacono, Andrea Grazian, Yann Clenet, Richard Davies, Marco Gullieuszik, Gijs Verdoes Kleijn, Fernando Pedichini, Roland Wagner, Ronny Ramlau, Werner W. Zeilinger, Fabrice Vidal, Benedetta Vulcani, Roberto Ragazzoni, Arnaud Sevin, Bernardo Salasnich, Andrea Baruffolo, Lorenzo Busoni, Simone Esposito, Éric Gendron, Roberto Piazzesi, Elisa Portaluri, Anita Zanella, Tapio Helin, Hanindyo Kuncarayakti, Seppo Mattila, Renato Falomo, Enrico Pinna
备注：
10 pages, 2 figures. Proceeding of the SPIE conference Adaptive Optics Systems VII, SPIE Astronomical Telescopes + Instrumentation 2020 Digital Forum, 14-18 December 2020 (paper 11448-169)
The point spread function reconstruction (PSF-R) capability is a deliverable of the MICADO@ESO-ELT project. The PSF-R team works on the implementation of the instrument software devoted to reconstruct the point spread function (PSF), independently of the science data, using adaptive optics (AO) telemetry data, both for Single Conjugate (SCAO) and Multi-Conjugate Adaptive Optics (MCAO) mode of the MICADO camera and spectrograph. The PSF-R application will provide reconstructed PSFs through an archive querying system to restore the telemetry data synchronous to each science frame that MICADO will generate. Eventually, the PSF-R software will produce the output according to user specifications. The PSF-R service will support the state-of-the-art scientific analysis of the MICADO imaging and spectroscopic data.
MICADO is a workhorse instrument for the ESO ELT, allowing first light capability for diffraction limited imaging and long-slit spectroscopy at near-infrared wavelengths. The PSF Reconstruction (PSF-R) Team of MICADO is currently implementing, for the first time within all ESO telescopes, a software service devoted to the blind reconstruction of the PSF. This tool will work independently of the science data, using adaptive optics telemetry data, both for Single Conjugate (SCAO) and Multi-Conjugate Adaptive Optics (MCAO) allowed by the MORFEO module. The PSF-R service will support the state-of-…
The MICADO first light imager for the ELT: the PSF Reconstruction Software
INAF-Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Incident Angle Oy；Max Planck Institut fuer extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；Finnish Centre for Astronomy with ESO (FINCA), University of Turku（图尔库大学欧洲南方天文台芬兰天文学中心）；Tuorla Observatory, Department of Physics and Astronomy, University of Turku（图尔库大学图奥拉天文台）；INAF-Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；INAF - Sezione Universitaria di Lecce（意大利国家天体物理研究所莱切大学分部）；INFN - Sezione di Lecce（意大利国家核物理研究所莱切分部）；Industrial Mathematics Institute, Johannes Kepler University Linz（林茨约翰内斯·开普勒大学工业数学研究所）；RICAM - Johann Radon Institute for Computational and Applied Mathematics（Johann Radon计算与应用数学研究所）
Current state-of-the-art adaptive optics (AO) provides ground-based, diffraction-limited observations with high Strehl ratios (SR). However, a detailed knowledge of the point spread function (PSF) is required to fully exploit the scientific potential of these data. This is even more crucial for the next generation AO instruments that will equip 30-meter class telescopes, as the characterization of the PSF will be mandatory to fulfill the planned scientific requirements. For this reason, there is a growing interest in developing tools that accurately reconstruct the observed PSF of AO systems, …
We present our investigation into the impact of wavefront errors on high accuracy astrometry using Fourier Optics. MICADO, the upcoming near-IR imaging instrument for the Extremely Large Telescope, will offer capabilities for relative astrometry with an accuracy of 50 micro arcseconds (μas). Due to the large size of the point spread function (PSF) compared to the astrometric requirement, the detailed shape and position of the PSF on the detector must be well understood. Furthermore, because the atmospheric dispersion corrector of MICADO is a moving component within an otherwise mostly static i…
Towards First Light for MICADO: Validation of the PSF-R service with real data
INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；ADaptive Optics National laboratory in Italy (ADONI)（意大利自适应光学国家实验室）；Dipartimento di Fisica e Astronomia ”G. Galilei”, Università di Padova（帕多瓦大学伽利略物理与天文系）；Johann Radon Institute for Computational and Applied Mathematics of the Austrian Academy of Sciences (RICAM)（奥地利科学院约翰·拉顿计算与应用数学研究所）；INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；INAF - Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天体物理与空间科学天文台）；MPE - Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理学研究所）；Finnish Centre for Astronomy with ESO, (FINCA), University of Turku（图尔库大学欧洲南方天文台芬兰天文学中心）；Tuorla Observatory, Department of Physics and Astronomy, University of Turku（图尔库大学物理与天文系图奥拉天文台）；Turku Collegium for Science, Medicine and Technology (TCSMT), University of Turku（图尔库大学科学与技术医学学院）；INAF - Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Industrial Mathematics Institute, Johannes Kepler University (JKU)（约瑟夫·开普勒大学工业数学研究所）
MICADO will be the first-light wide-field imager for the European Extremely Large Telescope (E-ELT) and will provide difiraction limited imaging (7mas at 1.2mm) over a ~53 arcsecond field of view. In order to support various consortium activities we have developed a first version of SimCADO: an instrument simulator for MICADO. SimCADO uses the results of the detailed simulation efforts conducted for each of the separate consortium-internal work packages in order to generate a model of the optical path from source to detector readout. SimCADO is thus a tool to provide scientific context to both…
Aims. In this work we aim to estimate the lowest stellar mass that MICADO at the ELT will be able to reliably detect given a stellar density and distance. We also show that instrumental effects that will play a critical role, and report the number of young clusters that will be accessible for IMF studies in the local Universe with the ELT. Methods. We used SimCADO, the instrument simulator package for the MICADO camera, to generate observations of 56 dense stellar regions with densities similar to the cores of young stellar clusters. We placed the cluster fields at distances between 8 kpc and …
AnisoCADO is a Python package for generating images of the point spread function (PSF) for the european extremely large telescope (ELT). The code allows the user to set many of the most important atmospheric and observational parameters that influence the shape and strehl ratio of the resulting PSF, including but not limited to: the atmospheric turbulence profile, the guide star position for a single conjugate adaptive optics (SCAO) solution, differential telescope pupil transmission, etc. Documentation can be found at https://anisocado.readthedocs.io/en/latest/
The MICADO first light imager for the ELT: Simulated Observations of Star Forming Clumps at Cosmic Noon
INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；INAF - Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛纳天文物理与空间科学观测站）；European Southern Observatory（欧洲南方天文台）
本文评估 ELT 的 MICADO 仪器通过模拟观测表征非透镜 z=2 星系中恒星形成团块的能力，证明其可探测至 R_e~20 pc 的团块，填补关键观测空白。
The InfraRed Imaging Spectrograph (IRIS) is a first-light instrument for the Thirty Meter Telescope (TMT) that will be used to sample the corrected adaptive optics field by the Narrow-Field Infrared Adaptive Optics System (NFIRAOS) with a near-infrared (0.8 - 2.4 $μ$m) imaging camera and integral field spectrograph. To better understand IRIS science specifications we use the IRIS data simulator to characterize relative photometric precision and accuracy across the IRIS imaging camera 34"x34" field of view. Because the Point Spread Function (PSF) varies due to the effects of anisoplanatism, we …
The scope of this paper is to compare the catalog extraction performances obtained using the new combination of SExtractor with PSFEx, against the more traditional and diffuse application of DAOPHOT with ALLSTAR; therefore, the paper may provide a guide for the selection of the most suitable catalog extraction software. Both software packages were tested on two kinds of simulated images having, respectively, a uniform spatial distribution of sources and an overdensity in the center. In both cases, SExtractor is able to generate a deeper catalog than DAOPHOT. Moreover, the use of neural network…
Because of bright starlight leakage in coronagraphic raw images, faint astrophysical objects such as exoplanets can only be detected using powerful point spread function (PSF) subtraction algorithms. However, these algorithms have strong effects on faint objects of interest, and often prevent precise spectroscopic analysis and scattering property measurements of circumstellar disks. For this reason, PSF-subtraction effects is currently the main limitations to the precise characterization of exoplanetary dust with scattered-light imaging. Forward-modeling techniques have long been developed for…
Lightstack: A Python Package for Creating Photometric Data Cubes
Universidade Federal do Rio Grande do Sul（南里奥格兰德联邦大学）；University of Hertfordshire（赫特福德大学）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）；European Southern Observatory（欧洲南方天文台）；Université Clermont Auvergne（克莱蒙奥弗涅大学）；University of California, Irvine（加州大学尔湾分校）
VST--Tube is a new software package designed to process optical astronomical images. It is an automated pipeline to go from the raw exposures to fully calibrated co-added images, and to extract catalogs with aperture and PSF photometry. A set of tools allow the data administration and the quality check of the intermediate and final products. VST-Tube comes with a Graphical User Interface to facilitate the interaction between data and user. We outline here the VST--Tube architecture and show some applications enlightening some of the characteristics of the pipeline.
We present an analysis of six independent on-sky datasets taken with the Keck-II/NIRC2 instrument. Using the off-axis point spread function (PSF) reconstruction software AIROPA, we extract stellar astrometry, photometry, and other fitting metrics in order to characterize the performance of this package. We test the effectiveness of AIROPA to reconstruct the PSF across the field of view in varying atmospheric conditions, number and location of PSF reference stars, stellar crowding and telescope position angle (PA). We compare the astrometric precision and fitting residuals between a static PSF …
The direct detection and characterization of planetary and substellar companions at small angular separations is a rapidly advancing field. Dedicated high-contrast imaging instruments deliver unprecedented sensitivity, enabling detailed insights into the atmospheres of young low-mass companions. In addition, improvements in data reduction and PSF subtraction algorithms are equally relevant for maximizing the scientific yield, both from new and archival data sets. We aim at developing a generic and modular data reduction pipeline for processing and analysis of high-contrast imaging data obtaine…
This paper presents an integrated modeling software to analyze the PSF of wide-field telescopes affected by misalignments. Even relatively small misalignments in the optical system of a telescope can significantly deteriorate the image quality by introducing large aberrations. In particular, wide-field telescopes are critically affected by these errors, insomuch that usually a closed-loop active optics system is adopted for a continuous correction, rather than for sporadic alignment procedures. Typically, a ray-tracing software such as Zemax OpticStudio is employed to accurately analyze the sy…
Context. The increase in sensitivity of Imaging Atmospheric Cherenkov Telescopes (IACTs) has lead to numerous detections of extended $γ$-ray sources at TeV energies, sometimes of sizes comparable to the instrument's field of view (FoV). This creates a demand for advanced and flexible data analysis methods, able to extract source information by utilising the photon counts in the entire FoV. Aims. We present a new software package, "SkyPrism", aimed at performing 2D (3D if energy is considered) fits of IACT data, possibly containing multiple and extended sources, based on sky images binned in en…
We introduce a new software package for modeling the point-spread function (PSF) of astronomical images, called Piff (PSFs In the Full FOV), which we apply to the first three years (known as Y3) of the Dark Energy Survey (DES) data. We describe the relevant details about the algorithms used by Piff to model the PSF, including how the PSF model varies across the field of view (FOV). Diagnostic results show that the systematic errors from the PSF modeling are very small over the range of scales that are important for the DES Y3 weak lensing analysis. In particular, the systematic errors from the…
