Context: Instrumental profile (IP) is the basic property of a spectrograph. Accurate IP characterisation is the prerequisite of accurate wavelength solution. It also facilitates new spectral acquisition methods such as the forward modeling and deconvolution. Aims: We investigate an IP modeling method for the fibre-fed echelle spectrograph with the emission lines of the ThAr lamp, and explore the method to evaluate the accuracy of IP characterisation. Methods: The backbone-residual (BR) model is put forward and tested on the fibre-fed High Resolution Spectrograph (HRS) at the Chinese Xinglong 2.16-m Telescope, which is the sum of the backbone function and the residual function. The backbone function is a bell-shaped function to describe the main component and the spatial variation of IP. The residual function, which is expressed as the cubic spline function, accounts for the difference between the bell-shaped function and the actual IP. The method of evaluating the accuracy of IP characterisation is based on the spectral reconstruction and Monte Carlo simulation. Results: The IP of HRS is characterised with the BR model, and the accuracy of the characterised IP reaches 0.006 of the peak value of the backbone function. This result demonstrates that the accurate IP characterisation has been achieved on HRS with the BR model, and the BR model is an excellent choice for accurate IP characterisation of fibre-fed echelle spectrographs.
The Tartu Observatory Fiber-fed Echelle Spectrograph (TOFES) Data Reduction Pipeline
Tartu Observatory, University of Tartu（塔尔图大学塔尔图天文台）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；Institute for Theoretical and Computation Physics, Graz University of Technology（格拉茨工业大学理论与计算物理研究所）；Department of Physics and Astronomy, Uppsala University（乌普萨拉大学物理与天文学系）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文学系）；European Southern Observatory（欧洲南方天文台）
Experimental test of a 40 cm-long R=100 000 spectrometer for exoplanet characterisation
高分辨率光谱学是目前和未来天文仪器的关键要素。特别是，与高对比度成像仪和日冕仪相结合，高光谱分辨率能够实现更高的对比度，并已被确定为一个非常强大的组合来识别系外行星，从现在的巨型行星开始，到最终的类地行星。在这种情况下，我们提出了一个创新的阶梯光栅光谱仪的基础上使用VIPA（虚拟成像相控阵，白崎1996年）的实施。VIPA本身是一种特殊类型的法布里-珀罗干涉仪，用作具有比普通衍射光栅大得多的色散功率的角色散器。VIPA是一种高效的小型组件（3 cm x 2.4 cm），在多功能设计中充分利用了单模注入的优势。这里介绍的整个仪器是一个紧凑的，高分辨率（R > 80 000）光谱仪的概念验证，专用于H和K波段，在IPAG开发的高色散日冕项目的背景下。光具座的占地面积为40 cm x 26 cm ;它由两个单模光纤（SMF）馈电，一个专用于伴星，一个专用于恒星和/或校准通道，并冷却到80 K。本通讯首先介绍了该项目的科学和仪器背景，以及高分辨率光谱分析中单模操作的主要优点。在回顾了VIPA的物理结构及其在阶梯光谱仪设计中的实现之后，详细介绍了光谱仪的光学设计。总之，进一步的步骤（集成，校准，耦合与自适应光学）和可能的优化简要介绍。关键词：中阶梯光谱仪，高光谱分辨率，系外行星，高色散日冕照相术，红外，自适应光学，球
Design and Commissioning of an Iodine Cell for the ESPRESSO Spectrograph
National Institute of Standards and Technology（美国国家标准与技术研究院）；Imperial College London（帝国理工学院）；Carnegie Institution for Science, Earth & Planets Laboratory（卡内基科学学会地球与行星实验室）
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。
ANDES, the high-resolution spectrograph for the ELT: design and performance analysis of the YJH spectrograph
UK Astronomy Technology Centre, Royal Observatory Edinburgh（英国天文学技术中心，爱丁堡皇家天文台）；Université de Montréal（蒙特利尔大学）；Université Laval（拉瓦尔大学）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Uppsala University（乌普萨拉大学）；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 di Trieste（意大利国家天体物理研究所的里雅斯特天文台）
