CUBES, the Cassegrain U-Band Efficient Spectrograph: towards final design review
Matteo Genoni, Hans Dekker, Stefano Covino, Roberto Cirami, Marcello Agostino Scalera, Lawrence Bissel, Walter Seifert, Ariadna Calcines, Gerardo Avila, Julian … 展开作者
Matteo Genoni, Hans Dekker, Stefano Covino, Roberto Cirami, Marcello Agostino Scalera, Lawrence Bissel, Walter Seifert, Ariadna Calcines, Gerardo Avila, Julian Stuermer, Christopher Ritz, David Lunney, Chris Miller, Stephen Watson, Chris Waring, Bruno Vaz Castilho, Marcio De Arruda, Orlando Verducci, Igor Coretti, Luca Oggioni, Giorgio Pariani, Edoardo Alberto Maria Redaelli, Matteo D'Ambrogio, Giorgio Calderone, Matteo Porru, Ingo Stilz, Rodolfo Smiljanic, Guido Cupani, Mariagrazia Franchini, Andrea Scaudo, Vincent Geers, Vincenzo De Caprio, Domenico D' Auria, Mina Sibalic, Cyrielle Opitom, Gabriele Cescutti, Valentina D' Odorico, Ruben Sanchez Janssen, Andreas Quirrenbach, Beatriz Barbuy, Stefano Cristiani, Paolo Di Marcantonio
发表信息：
Proceedings Volume 13096, Ground-based and Airborne Instrumentation for Astronomy X; 130967T (2024)
In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high instrumental efficiency ( $>$ 37\%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R $>$ 20, 000 (with a lower-resolution, sky-limited mode of R $\sim$ 7, 000). With the design focusing on maximizing the instrument throughput (ensuring a Signal to Noise Ratio -SNR- $\sim$ 20 per spectral resolution element at 313 nm for U $\sim$ 17.5 mag objects in 1h of observations), it will offer new possibilities in many fields of astrophysics: i) access to key lines of stellar spectra (e.g. lighter elements, in particular Beryllium), extragalactic studies (e.g. circumgalactic medium of distant galaxies, cosmic UV background) and follow-up of explosive transients. We present the CUBES instrument design, currently in Phase-C and approaching the final design review, summarizing the hardware architecture and interfaces between the different subsystems as well as the relevant technical requirements. We describe the optical, mechanical, electrical design of the different subsystems (from the telescope adapter and support structure, through the main opto-mechanical path, including calibration unit, detector devices and cryostat control, main control electronics), detailing peculiar instrument functions like the Active Flexure Compensation (AFC). Furthermore, we outline the AITV concept and the main instrument operations giving an overview of its software ecosystem. Installation at the VLT is planned for 2028-2029 and first science operations in late 2029.
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）
SIMLA: The Spitzer Infrared Spectrograph Mapping Legacy Archive
University of Toledo（托莱多大学）；University of California, San Diego（加州大学圣地亚哥分校）；University of Texas at Arlington（德克萨斯大学阿灵顿分校）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
CARMENES. I. A radial-velocity survey for terrestrial planets in the habitable zones of M dwarfs. A historical overview
CARMENES（Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and optical Echelle Spectrographs）是由西班牙和德国11个机构组成的财团为Calar Alto天文台的3.5米望远镜建造的下一代仪器。用完成的仪器对300 M矮星进行为期五年的系外行星调查是该项目的一个组成部分。CARMENES仪器由两个独立的阶梯光栅摄谱仪组成，覆盖550至1700 nm的波长范围，光谱分辨率为R= 82，000，由来自望远镜卡塞格伦焦点的光纤馈电。光谱仪被安置在真空罐中，提供必要的温度稳定环境，以实现1 m/s的径向速度精度，同时使用发射线灯进行校准。
Mock Observations for the CSST Mission: Integral Field Spectrograph--GEHONG: A Package for Generating Ideal Datacubes
Hebei Normal University（河北师范大学）；Guoshoujing Institute of Astronomy, Hebei Normal University（河北师范大学郭守敬天文研究所）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
Design evolution for the Wide-field Spectroscopic Telescope
Astralis, Australian Astronomical Optics, Macquarie University（澳大利亚光学天文台，麦考瑞大学）；Université Claude Bernard Lyon 1, CNRS, CRAL（里昂第一大学，法国国家科学研究中心，CRAL）；Leibniz-Institut für Astrophysik Potsdam（波茨坦阿佩尔天体物理研究所）；UK Astronomy Technology Centre（英国天文学技术中心）；Advanced Instrumentation Technology Centre, ANU, Canberra（堪培拉国立大学先进仪器技术中心）
Progress of the design of the 12-m optical, Wide-field Spectroscopic Telescope (WST)
Centre de Recherche Astrophysique de Lyon（里昂天体物理研究中心）；Australian National University（澳大利亚国立大学）；Science and Technology Facilities Council (STFC)（科学与技术设施委员会）；Laboratoire Matériaux Avancés- IP2I, CNRS UCB Lyon（里昂UCB-CNRS先进材料实验室-IP2I）；Istituto Nazionale di Astrofisica（意大利国家天体物理研究所）；Queen Mary University London（伦敦玛丽女王大学）；University College London（伦敦大学学院）；NOVA optical infrared instrumentation group at ASTRON（荷兰ASTRON天文台的NOVA光学红外仪器组）；Universität Wien（维也纳大学）；Astralis - MQ AB（Astralis-MQ公司）
ESO-VLT BlueMUSE instrument - Conceptual Design for Phase A
Universite Claude Bernard Lyon 1, CRAL UMR5574, ENS de Lyon, CNRS（里昂第一大学克劳德·贝尔纳，CRAL UMR5574，巴黎高等师范学校里昂分校，法国国家科学研究中心）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；Instituto de Astrofísica e Ciências do Espaço, U. Lisboa（里斯本大学空间科学与天体物理研究所）；Ecole Polytechnique Federale de Lausanne (EPFL)（洛桑联邦理工学院）；Australian Astronomical Optics, Macquarie Univ.（澳大利亚天文光学中心，麦考瑞大学）；Centre for Advanced Instrumentation, Department of Physics, Durham University（杜伦大学物理系先进仪器中心）；Dpt d'Astronomie, Univ. de Geneve（日内瓦大学天文学系）；Universite Paris-Saclay, CEA, IRFU（巴黎萨克雷大学，法国原子能和替代能源委员会，核物理研究创新实验室）；Stockholm University（斯德哥尔摩大学）；Instituto de Astrofísica e Ciências do Espaço, U.Porto（波尔图大学空间科学与天体物理研究所）
