Harmoni is the ELT's first light visible and near-infrared integral field spectrograph. It will provide four different spatial scales, ranging from coarse spaxels of 60 x 30 mas best suited for seeing limited observations, to 4 mas spaxels that Nyquist sample the diffraction limited point spread function of the ELT at near-infrared wavelengths. Each spaxel scale may be combined with eleven spectral settings, that provide a range of spectral resolving powers from R 3500 to R 20000 and instantaneous wavelength coverage spanning the 0.47 - 2.45 μm wavelength range of the instrument. The consortium consists of several institutes in Europe under leadership of Oxford University. Harmoni is starting its Final Design Phase after a Preliminary Design Phase in November, 2017. The CRAL has the responsibility of the Integral Field Unit design linking the Preoptics to the 4 Spectrographs. It is composed of a field splitter associated with a relay system and an image slicer that create from a rectangular Field of View a very long (540mm) output slit for each spectrograph. In this paper, the preliminary design and performances of Harmoni Image Slicer will be presented including image quality, pupil distortion and slit geometry. It has been designed by CRAL for Harmoni PDR in November, 2017. Special emphases will be put on straylight analysis and slice diffraction. The optimisation of the manufacturing and slit geometry will also be reported.
METIS for ELT: optical alignment and testing of the IFU of the LM-band spectrometer
STFC - United Kingdom Astronomy Technology Centre（英国天体物理学技术中心）；NOVA optical infrared instrumentation group at ASTRON（ASTRON 的 NOVA 光学红外仪器组）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）
The 25.4m Giant Magellan Telescope (GMT) will be amongst the first in a new series of segmented extremely large telescopes (ELTs). The 25.4 m pupil is segmented into seven 8.4 m circular segments in a flower petal pattern. At the University of Arizona we have developed a novel pupil slicer that will be used for ELT extreme adaptive optics (ExAO) on the up and coming ExAO instrument, GMagAO-X. This comes in the form of a six-sided reflective pyramid with a hole through the center known as a "hexpyramid". By passing the GMT pupil onto this reflective optic, the six outer petals will be sent outw…
HARMONI is the first light visible and near-IR integral field spectrograph for the ELT covering a large spectral range from 450nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics modes-SCAO and LTAO-or with no AO. The project is preparing for Final Design Reviews. The laser Tomographic AO (LTAO) system provides AO correction with very high sky-coverage thanks to two systems: the Laser Guide Star Sensors (LGSS) and the Natural Guide Star Sensors (NGSS). LGSS is dedicated to the analysis of the wavefront coming from…
The High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI) is the visible and near-infrared (NIR), adaptive-optics-assisted, integral field spectrograph for ESO's Extremely Large Telescope (ELT). It will have both a single-conjugate adaptive optics (SCAO) mode (using a single bright natural guide star) and a laser tomographic adaptive optics (LTAO) mode (using multiple laser guide stars), providing near diffraction-limited hyper-spectral imaging with high performance and good sky coverage, respectively. A unique high-contrast adaptive optics (HCAO) c…
ELT-HARMONI is the first light visible and near-IR integral field spectrograph (IFS) for the ELT. It covers a large spectral range from 450nm to 2450nm with resolving powers from 3500 to 18000 and spatial sampling from 60mas to 4mas. It can operate in two Adaptive Optics modes - SCAO (including a High Contrast capability) and LTAO - or with NOAO. The project is preparing for Final Design Reviews. The High Contrast Module (HCM) will allow HARMONI to perform direct imaging and spectral analysis of exoplanets up to one million times fainter than their host star. Quasi-static aberrations are a lim…
HARMONI at ELT: line spread functions in a diffraction limited spectrometer
UKATC, Royal Observatory Edinburgh（英国天文技术控制中心，爱丁堡皇家天文台）；Oxford University（牛津大学）；Aix-Marseille Université, CNRS, CNES, LAM（艾克斯-马赛大学，法国国家科学研究中心，法国国家空间研究中心，拉格朗日实验室）；Université Lyon 1, CNRS, Centre de Recherche Astrophysique de Lyon (CRAL)（里昂第一大学，法国国家科学研究中心，里昂天体物理研究中心）；Instituto de Astrofísica de Canarias (IAC)（加那利天体物理学研究所）；Department of Physics, Durham University（杜伦大学物理系）
HARMONI at ELT: Reoptimization of the NGSS natural guide star sensors system for MCAO compatibility
Aix Marseille Univ, CNRS, CNES, LAM（艾克斯-马赛大学，法国国家科学研究中心，法国国家太空研究中心，天体物理学与行星学实验室）；Durham University, Centre for Advanced Instrumentation（杜伦大学，先进仪器中心）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心，西班牙高等科学研究理事会-国家航空航天技术研究所）；Université Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，天体物理与行星学研究所）；DOTA, ONERA（航天技术部门，法国航空与航天研究局）；Instituto de Astrofísica de Canarias (IAC), Universidad de La Laguna（加那利群岛天体物理研究所，拉帕鲁纳大学）
HARMONI is a visible and NIR integral field spectrograph, providing the E-ELT's core spectroscopic capability at first light. HARMONI will work at the diffraction limit of the E-ELT, thanks to a Classical and a Laser Tomographic AO system. In this paper, we present the system choices that have been made for these SCAO and LTAO modules. In particular, we describe the strategy developed for the different Wave-Front Sensors: pyramid for SCAO, the LGSWFS concept, the NGSWFS path, and the truth sensor capabilities. We present first potential implementations. And we asses the first system performanc…
Combining high-contrast imaging with medium-resolution spectroscopy has been shown to significantly boost the direct detection of exoplanets. HARMONI, one of the first-light instruments to be mounted on ESO's ELT, will be equipped with a single-conjugated adaptive optics system to reach the diffraction limit of the ELT in H and K bands, a high-contrast module dedicated to exoplanet imaging, and a medium-resolution (up to R = 17 000) optical and near-infrared integral field spectrograph. Combined together, these systems will provide unprecedented contrast limits at separations between 50 and 40…
In the present paper, we consider the optical design of a zoom system for the active refocusing in laser guide star wavefront sensors. The system is designed according to the specifications coming from the Extremely Large Telescope (ELT)-HARMONI instrument, the first-light, integral field spectrograph for the European (E)-ELT. The system must provide a refocusing of the laser guide as a function of telescope pointing and large decentring of the incoming beam. The system considers four moving lens groups, each of them being a doublet with one aspherical surface. The advantages and shortcomings …
Population III (Pop. III) stars, as of yet, have not been detected, however as we move into the era of extremely large telescopes this is likely to change. One likely tracer for Pop. III stars is the HeII$\lambda1640$ emission line, which will be detectable by the HARMONI spectrograph on the European Extremely Large Telescope (ELT) over a broad range of redshifts ($2\leq z\leq14$). By post-processing galaxies from the cosmological, AMR-hydrodynamical simulation NewHorizon with theoretical spectral energy distributions (SED) for Pop. III stars and radiative transfer (i.e. the Yggdrasil Models a…
Behind the Mask: can HARMONI@ELT detect biosignatures in the reflected light of Proxima b?
University of Oxford（牛津大学）；Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；Université Côte d’Azur（蔚蓝海岸大学）；Instituto de Física Fundamental, CSIC（西班牙国家研究委员会基础物理研究所）；Aix Marseille Univ.（艾克斯-马赛大学）；Massachusetts Institute of Technology（麻省理工学院）；Carl Sagan Institute, Cornell University（康奈尔大学卡尔·萨根研究所）；Cornell University（康奈尔大学）
HARMONI@ELT: instrument design, performance, and science capabilities
LAM, Aix Marseille Univ., CNRS, CNES（LAM，艾克斯-马赛大学，法国国家科学研究中心，法国国家空间研究中心）；Univ. of Edinburgh（爱丁堡大学）；UK Astronomy Technology Centre, STFC（英国天体技术中心，英国科学与技术设施委员会）；Univ. of Durham（杜伦大学）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；University of Oxford（牛津大学）；Centre de Recherche en Astrophysique de Lyon（里昂天体物理研究中心）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家技术研究与发展总署/西班牙高等科学研究理事会）；University of Michigan（密歇根大学）；Institut de Planétologie et d’Astrophysique de Grenoble（格勒诺布尔行星学与天体物理学研究所）
CUBES: optical design and analysis of the VLT's high-resolution UV spectrograph past final design review
STFC - United Kingdom Astronomy Technology Centre (UK ATC)（英国科学技术设施委员会-英国天文学技术中心）；Durham University - Centre for Advanced Instrumentation - Department of Physics（杜伦大学-先进仪器中心-物理系）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所-布拉拉天文台）；Optical Lab Baader Planetarium GmbH（巴德尔天文馆有限公司光学实验室）；INAF-Osservatorio Astronomico di Trieste（意大利国家天体物理研究所-的里雅斯特天文台）
The SOUL project is upgrading the 4 SCAO systems of LBT, pushing the current guide star limits of about 2 magnitudes fainter thanks to Electron Multiplied CCD detector. This improvement will open the NGS SCAO correction to a wider number of scientific cases from high contrast imaging in the visible to extra-galactic source in the NIR. The SOUL systems are today the unique case where pyramid WFS, adaptive secondary and EMCCD are used together. This makes SOUL a pathfinder for most of the ELT SCAO systems like the one of GMT, MICADO and HARMONI of E-ELT, where the same key technologies will be e…
We present simulated observations of gas kinematics in galaxies formed in 10 pc resolution cosmological simulations with the hydrodynamical + N-body code RAMSES, using the new RAMSES2HSIM pipeline with the simulated observing pipeline (HSIM) for the ELT HARMONI IFU spectrograph. We post-process the galaxy's gas kinematics and Hα line emission for each simulation cell, and integrate the emission to produce an extinction-corrected input cube. We then simulate observations of the input cube with HARMONI, for a range of exposure times, spatial sampling, and spectral resolution. We analyze the mock…
Sky-coverage in laser-assisted AO observations largely depends on the system's capability to guide on the faintest natural guide-stars possible. Here we give an up-to-date status of our natural guide-star processing tailored to the European-ELT's visible and near-infrared (0.47 to 2.45 μm) integral field spectrograph - Harmoni. We tour the processing of both the isoplanatic and anisoplanatic tilt modes using the spatio-angular approach whereby the wave-front is estimated directly in the pupil plane avoiding a cumbersome explicit layered estimation on the 35-layer profiles we're currently using…
We present a study into the capabilities of integrated and spatially resolved integral field spectroscopy of galaxies at z=2-4 with the future HARMONI spectrograph for the European Extremely Large Telescope (E-ELT) using the simulation pipeline, HSIM. We focus particularly on the instrument's capabilities in stellar absorption line integral field spectroscopy, which will allow us to study the stellar kinematics and stellar population characteristics. Such measurements for star-forming and passive galaxies around the peak star formation era will provide a critical insight into the star formatio…
Current designs for all three extremely large telescopes show the overwhelming adoption of the pyramid wavefront sensor (P-WFS) as the WFS of choice for adaptive optics (AO) systems sensing on natural guide stars (NGS) or extended objects. The key advantages of the P-WFS over the Shack-Hartmann are known and are mainly provided by the improved sensitivity (fainter NGS) and reduced sensitivity to spatial aliasing. However, robustness and tolerances of the P-WFS for the ELTs are not currently well understood. In this paper, we present simulation results for the single-conjugate AO mode of HARMON…
