Experimental Astronomy最新文献

{"title":"RAPOC: The Rosseland and Planck opacity converter","authors":"Lorenzo V. Mugnai,&nbsp;Darius Modirrousta-Galian","doi":"10.1007/s10686-022-09869-2","DOIUrl":"10.1007/s10686-022-09869-2","url":null,"abstract":"<div><p><span>RAPOC</span> (Rosseland and Planck Opacity Converter) is a Python 3 code that calculates Rosseland and Planck mean opacities (RPMs) from wavelength-dependent opacities for a given temperature, pressure, and wavelength range. In addition to being user-friendly and rapid, <span>RAPOC</span> can interpolate between discrete data points, making it flexible and widely applicable to the astrophysical and Earth-sciences fields, as well as in engineering. <span>RAPOC</span> uses <i>ExoMol</i>, <i>DACE</i>, or any user defined input data, provided that it is in a readable format. In this paper, we present the <span>RAPOC</span> code and compare its calculated Rosseland and Planck mean opacities with other values in the literature. <span>RAPOC</span> is open-source and available on Pypi and GitHub.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09869-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5639633","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Proton irradiation of SiPM arrays for POLAR-2","authors":"Slawomir Mianowski,&nbsp;Nicolas De Angelis,&nbsp;Johannes Hulsman,&nbsp;Merlin Kole,&nbsp;Tomasz Kowalski,&nbsp;Sebastian Kusyk,&nbsp;Hancheng Li,&nbsp;Zuzanna Mianowska,&nbsp;Jerzy Mietelski,&nbsp;Agnieszka Pollo,&nbsp;Dominik Rybka,&nbsp;Jianchao Sun,&nbsp;Jan Swakon,&nbsp;Damian Wrobel,&nbsp;Xin Wu","doi":"10.1007/s10686-022-09873-6","DOIUrl":"10.1007/s10686-022-09873-6","url":null,"abstract":"<div><p>POLAR-2 is a space-borne polarimeter, built to investigate the polarization of Gamma-Ray Bursts and help elucidate their mechanisms. The instrument is targeted for launch in 2024 or 2025 aboard the China Space Station and is being developed by a collaboration between institutes from Switzerland, Germany, Poland and China. The instrument will orbit at altitudes between 340km and 450km with an inclination of <span>({42}{^{circ }})</span> and will be subjected to background radiation from cosmic rays and solar events. It is therefore pertinent to better understand the performance of sensitive devices under space-like conditions. In this paper we focus on the radiation damage of the silicon photomultiplier arrays S13361-6075NE-04 and S14161-6050HS-04 from Hamamatsu. The S13361 are irradiated with 58MeV protons at several doses up to 4.96Gy, whereas the newer series S14161 are irradiated at doses of 0.254Gy and 2.31Gy. Their respective performance degradation due to radiation damage are discussed. The equivalent exposure time in space for silicon photomultipliers inside POLAR-2 with a dose of 4.96Gy is 62.9years (or 1.78years when disregarding the shielding from the instrument). Primary characteristics of the I-V curves are an increase in the dark current and dark counts, mostly through cross-talk events. Annealing processes at <span>({25}{^{circ }C})</span> were observed but not studied in further detail. Biasing channels while being irradiated have not resulted in any significant impact. Activation analyses showed a dominant contribution of <span>(beta ^{+})</span> particles around 511 keV. These resulted primarily from copper and carbon, mostly with decay times shorter than the orbital period.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09873-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4990127","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The 100-m X-ray test facility at IHEP","authors":"Yusa Wang,&nbsp;Zijian Zhao,&nbsp;Dongjie Hou,&nbsp;Xiongtao Yang,&nbsp;Can Chen,&nbsp;Xinqiao Li,&nbsp;Yuxuan Zhu,&nbsp;Xiaofan Zhao,&nbsp;Jia Ma,&nbsp;He Xu,&nbsp;Yupeng Chen,&nbsp;Guofeng Wang,&nbsp;Fangjun Lu,&nbsp;Shuangnan Zhang,&nbsp;Shu Zhang,&nbsp;Yong Chen,&nbsp;Yupeng Xu","doi":"10.1007/s10686-022-09872-7","DOIUrl":"10.1007/s10686-022-09872-7","url":null,"abstract":"<div><p>The 100-m X-ray Test Facility of the Institute of High Energy Physics (IHEP) was initially proposed in 2012 for the test and calibration of the X-ray detectors of the Hard X-ray Modulation Telescope (HXMT) with the capability to support future X-ray missions. The large instrument chamber connected with a long vacuum tube can accommodate the X-ray mirror, focal plane detector and other instruments. The X-ray sources are installed at the other end of the vacuum tube with a distance of 105 m, which can provide an almost parallel X-ray beam covering 0.2<span>(sim)</span>60 keV energy band. The X-ray mirror modules of the Einstein Probe (EP) and the enhanced X-ray Timing and Polarimetry mission (eXTP) and payload of the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) have been tested and calibrated with this facility. It has been also used to characterize the focal plane camera and aluminum filter used on the Einstein Probe. In this paper, we will introduce the overall configuration and capability of the facility, and give a brief introduction of some calibration results performed with this facility.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09872-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4875265","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Classical novae with CUBES","authors":"Luca Izzo,&nbsp;Paolo Molaro,&nbsp;Piercarlo Bonifacio,&nbsp;Gabriele Cescutti,&nbsp;Massimo Della Valle,&nbsp;Pierluigi Selvelli","doi":"10.1007/s10686-022-09876-3","DOIUrl":"10.1007/s10686-022-09876-3","url":null,"abstract":"<div><p>Among the main science cases that have motivated the proposal of CUBES, a new high-resolution spectrograph for the Very Large Telescope at the European Southern Observatory, there is the study and the characterisation of the nucleosynthesis of beryllium. Classical novae have been proposed since the ’70s as one of the main factories of lithium in the Galaxy, but this hypothesis has been demonstrated on empirical basis only recently thanks to the direct identification of lithium in V1369 Cen and through the observations of the resonance transition of <span>(^{7})</span>Be II, the <span>(^{7})</span>Li parent, at 313.0 nm in the near-UV range. CUBES is then the ideal instrument to quantify the amount of <span>(^{7})</span>Be and therefore of <span>(^{7})</span>Li produced by the different novae types hosted in the different components of the Milky Way and also in its nearby satellite galaxies. As important by-product of high resolution spectroscopic observations obtained with CUBES, there are the study of the properties of nova ejecta abundances, the shocks evolution in novae and their connection with the high-energy emission observed in these transients, from satellites as Fermi and Swift.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4843562","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"New observables of the cosmic microwave background","authors":"Marco Lanucara,&nbsp;Robert J. Daddato","doi":"10.1007/s10686-022-09875-4","DOIUrl":"10.1007/s10686-022-09875-4","url":null,"abstract":"<div><p>We introduce new observables of the cosmic microwave background radiation, which can be measured through the detection of high order modes excited within an antenna feed system, coherently combined with those currently detected by space observatories. The use of such observables could potentially further constrain the validity of cosmological theories.\u0000</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09875-4.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4476482","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Investigation on the cosmic-ray shadow of planets and asteroids","authors":"Jun Li,&nbsp;Yi Zhang,&nbsp;X. Y. Huang,&nbsp;J. Y. He","doi":"10.1007/s10686-022-09874-5","DOIUrl":"10.1007/s10686-022-09874-5","url":null,"abstract":"<div><p>The moon shadow and sun shadow of cosmic rays are commonly used to calibrate the angular resolution of the instrument in extensive air shower experiments, measure the proton-antiproton ratio, and study the interplanetary magnetic field (IMF). The shadow effect of planets and asteroids in the solar system, on the other hand, has received little attention. If considerable shadow effects can be observed, a novel approach may be developed to calibrate the point spread function and investigate the IMF. In this work, we calculate the sensitivity of observing the shadow effects of planets and asteroids in the next hundred years using LHAASO’s instrumental response as an example. The result shows that the blocking impact of these celestial bodies is minimal; thus, their influence on the direction distribution of cosmic rays is negligible.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09874-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4439095","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The EUSO@TurLab project in the framework of the JEM-EUSO program","authors":"P. Barrillon,&nbsp;M. Battisti,&nbsp;A. Belov,&nbsp;M. Bertaina,&nbsp;F. Bisconti,&nbsp;S. Blin-Bondil,&nbsp;R. Bonino,&nbsp;F. Capel,&nbsp;R. Caruso,&nbsp;M. Casolino,&nbsp;G. Contino,&nbsp;G. Cotto,&nbsp;S. Dagoret-Campagne,&nbsp;F. Fenu,&nbsp;C. Fornaro,&nbsp;R. Forza,&nbsp;P. Gorodetzky,&nbsp;N. Guardone,&nbsp;A. Jung,&nbsp;P. Klimov,&nbsp;M. Manfrin,&nbsp;L. Marcelli,&nbsp;M. Mignone,&nbsp;H. Miyamoto,&nbsp;R. Mulas,&nbsp;M. Onorato,&nbsp;E. Parizot,&nbsp;L. Piotrowski,&nbsp;Z. Plebaniak,&nbsp;G. Prevot,&nbsp;J. Szabelski,&nbsp;G. Suino,&nbsp;Y. Takizawa,&nbsp;P. Tibaldi,&nbsp;C. Vigorito,&nbsp;A. Youssef","doi":"10.1007/s10686-022-09871-8","DOIUrl":"10.1007/s10686-022-09871-8","url":null,"abstract":"<div><p>The EUSO@TurLab project aims at performing experiments to reproduce Earth UV emissions as seen from a low Earth orbit by the planned missions of the JEM-EUSO program. It makes use of the TurLab facility, which is a laboratory, equipped with a 5 m diameter and 1 m depth rotating tank, located at the Physics Department of the University of Turin. All the experiments are designed and performed based on simulations of the expected response of the detectors to be flown in space. In April 2016 the TUS detector and more recently in October 2019 the Mini-EUSO experiment, both part of the JEM-EUSO program, have been placed in orbit to map the UV Earth emissions. It is, therefore, now possible to compare the replicas performed at TurLab with the actual images detected in space to understand the level of fidelity in terms of reproduction of the expected signals. We show that the laboratory tests reproduce at the order of magnitude level the measurements from space in terms of spatial extension and time duration of the emitted UV light, as well as the intensity in terms of expected counts per pixel per unit time when atmospheric transient events, diffuse nightlow background light, and artificial light sources are considered. Therefore, TurLab is found to be a very useful facility for testing the acquisition logic of the detectors of the present and future missions of the JEM-EUSO program and beyond in order to reproduce atmospheric signals in the laboratory.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09871-8.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4321827","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The CUBES science case","authors":"Chris Evans,&nbsp;Stefano Cristiani,&nbsp;Cyrielle Opitom,&nbsp;Gabriele Cescutti,&nbsp;Valentina D’Odorico,&nbsp;Juan Manuel Alcalá,&nbsp;Silvia H. P. Alencar,&nbsp;Sergei Balashev,&nbsp;Beatriz Barbuy,&nbsp;Nate Bastian,&nbsp;Umberto Battino,&nbsp;Pamela Cambianica,&nbsp;Roberta Carini,&nbsp;Brad Carter,&nbsp;Santi Cassisi,&nbsp;Bruno Vaz Castilho,&nbsp;Norbert Christlieb,&nbsp;Ryan Cooke,&nbsp;Stefano Covino,&nbsp;Gabriele Cremonese,&nbsp;Katia Cunha,&nbsp;André R. da Silva,&nbsp;Valerio D’Elia,&nbsp;Annalisa De Cia,&nbsp;Gayandhi De Silva,&nbsp;Marcos Diaz,&nbsp;Paolo Di Marcantonio,&nbsp;Heitor Ernandes,&nbsp;Alan Fitzsimmons,&nbsp;Mariagrazia Franchini,&nbsp;Boris T. Gänsicke,&nbsp;Matteo Genoni,&nbsp;Riano E. Giribaldi,&nbsp;Andrea Grazian,&nbsp;Camilla Juul Hansen,&nbsp;Fiorangela La Forgia,&nbsp;Monica Lazzarin,&nbsp;Wagner Marcolino,&nbsp;Marcella Marconi,&nbsp;Alessandra Migliorini,&nbsp;Pasquier Noterdaeme,&nbsp;Claudio Pereira,&nbsp;Bogumil Pilecki,&nbsp;Andreas Quirrenbach,&nbsp;Sofia Randich,&nbsp;Silvia Rossi,&nbsp;Rodolfo Smiljanic,&nbsp;Colin Snodgrass,&nbsp;Julian Stürmer,&nbsp;Andrea Trost,&nbsp;Eros Vanzella,&nbsp;Paolo Ventura,&nbsp;Duncan Wright,&nbsp;Tayyaba Zafar","doi":"10.1007/s10686-022-09864-7","DOIUrl":"10.1007/s10686-022-09864-7","url":null,"abstract":"<div><p>We introduce the scientific motivations for the development of the Cassegrain U-Band Efficient Spectrograph (CUBES) that is now in construction for the Very Large Telescope. The assembled cases span a broad range of contemporary topics across Solar System, Galactic and extragalactic astronomy, where observations are limited by the performance of current ground-based spectrographs shortwards of 400 nm. A brief background to each case is presented and specific technical requirements on the instrument design that flow-down from each case are identified. These were used as inputs to the CUBES design, that will provide a factor of ten gain in efficiency for astronomical spectroscopy over 300-405 nm, at resolving powers of <span>(R~sim)</span> 24,000 and <span>(sim)</span>7,000. We include performance estimates that demonstrate the ability of CUBES to observe sources that are up to three magnitudes fainter than currently possible at ground-ultraviolet wavelengths, and we place its predicted performance in the context of existing facillities.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09864-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4056620","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"What are the fundamental modes of energy transfer and partitioning in the coupled Magnetosphere-Ionosphere system?","authors":"Jonathan Rae,&nbsp;Colin Forsyth,&nbsp;Malcolm Dunlop,&nbsp;Minna Palmroth,&nbsp;Mark Lester,&nbsp;Reiner Friedel,&nbsp;Geoff Reeves,&nbsp;Larry Kepko,&nbsp;Lucille Turc,&nbsp;Clare Watt,&nbsp;Wojciech Hajdas,&nbsp;Theodoros Sarris,&nbsp;Yoshifumi Saito,&nbsp;Ondrej Santolik,&nbsp;Yuri Shprits,&nbsp;Chi Wang,&nbsp;Aurelie Marchaudon,&nbsp;Matthieu Berthomier,&nbsp;Octav Marghitu,&nbsp;Benoit Hubert,&nbsp;Martin Volwerk,&nbsp;Elena A. Kronberg,&nbsp;Ian Mann,&nbsp;Kyle Murphy,&nbsp;David Miles,&nbsp;Zhonghua Yao,&nbsp;Andrew Fazakerley,&nbsp;Jasmine Sandhu,&nbsp;Hayley Allison,&nbsp;Quanqi Shi","doi":"10.1007/s10686-022-09861-w","DOIUrl":"10.1007/s10686-022-09861-w","url":null,"abstract":"<div><p>The fundamental processes responsible for energy exchange between large-scale electromagnetic fields and plasma are well understood theoretically, but in practice these theories have not been tested. These processes are ubiquitous in all plasmas, especially at the interface between high and low beta plasmas in planetary magnetospheres and other magnetic environments. Although such boundaries pervade the plasma Universe, the processes responsible for the release of the stored magnetic and thermal plasma energy have not been fully identified and the importance of the relative impact of each process is unknown. Despite advances in understanding energy release through the conversion of magnetic to kinetic energy in magnetic reconnection, how the extreme pressures in the regions between stretched and more relaxed field lines in the transition region are balanced and released through adiabatic convection of plasma and fields is still a mystery. Recent theoretical advances and the predictions of large-scale instabilities must be tested. In essence, the processes responsible remain poorly understood and the problem unresolved. The aim of the White Paper submitted to ESA’s Voyage 2050 call, and the contents of this paper, is to highlight three outstanding open science questions that are of clear international interest: (i) the interplay of local and global plasma physics processes: (ii) the partitioning during energy conversion between electromagnetic and plasma energy: and (iii) what processes drive the coupling between low and high beta plasmas. We present a discussion of the new measurements and technological advances required from current state-of-the-art, and several candidate mission profiles with which these international high-priority science goals could be significantly advanced.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09861-w.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5179206","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Design of the VLT-CUBES image slicers:","authors":"Ariadna Calcines,&nbsp;Martyn Wells,&nbsp;Kieran O’Brien,&nbsp;Simon Morris,&nbsp;Walter Seifert,&nbsp;Alessio Zanutta,&nbsp;Chris Evans,&nbsp;Paolo Di Marcantonio","doi":"10.1007/s10686-022-09866-5","DOIUrl":"10.1007/s10686-022-09866-5","url":null,"abstract":"<div><p>CUBES is a high efficiency spectrograph designed for a Cassegrain focus of the Very Large Telescope and is expected to be in operation in 2028. It is designed to observe point or compact sources in a spectral range from 300 to 405nm. CUBES will provide two spectral resolving powers: R<span>(ge)</span>20,000 for high resolution (HR) and R<span>(ge)</span>5,000 for low resolution (LR). This is achieved by using an image slicer for each resolution mode. The image slicers re-format a rectangular on-sky field of view of either 1.5arcsec by 10arcsec (HR) or 6arcsec by 10arcsec (LR) into six side-by-side slitlets which form the spectrograph slit. The slit dimensions are 0.19mm <span>(times)</span> 88mm for HR and 0.77mm <span>(times)</span> 88mm for LR. The on-sky and physical widths of the slicer mirrors are 0.25arcsec/0.5mm (HR) and 1arcsec/2mm (LR). The image slicers reduce the spectrograph entrance slit etendue and hence the size of the spectrograph optics without associated slit losses. Each of the proposed image slicers consists of two arrays of six spherical mirrors (slicer mirror and camera mirror arrays) which provide a straight entrance slit to the spectrograph with almost diffraction-limited optical quality. This paper presents the description of the image slicers at the end of the Phase A conceptual design, including their optical design and expected performance.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":null,"pages":null},"PeriodicalIF":3.0,"publicationDate":"2022-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09866-5.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4233930","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}