In order to maximize the scientific return of the telescopes located at the Paranal Observatory, we analyse the properties of the atmosphere above Paranal in the near-infrared (NIR). We estimate atmospheric extinction in the spectral range 1.10-2.30 um (J, Js, H, and Ks) using standard stars that were observed during photometric and clear nights with ISAAC on the Very Large Telescope UT1 between 2000 and 2004. We have built a database consisting of hundreds of observations, which allows us to examine how extinction varies with airmass and the column density of water vapour. In addition, we use theoretical models of the atmosphere to estimate Rayleigh scattering and molecular absorption in order to quantify their fractional contribution to the total extinction in each filter. Finally, we have observed 8 bright red standard stars to evaluate filter color terms. We find that extinction coefficients are < 0.1 mag/airmass in all the considered bands. The extinction coefficient in the J-band strongly depends on the column density of water vapour. Molecular absorption dominates the extinction in J, H and Ks, while Rayleigh scattering contributes most to the extinction in Js. We have found negligible color terms for J, H and Ks and a non-negligible color term for Js.
Detection of a 14-days atmospheric perturbation peak at Paranal associated with lunar cycles
在本文中，我们研究了在帕拉纳尔天文台的大气扰动和智利海岸潮汐，这主要是由14天的朔望日月潮汐周期调制之间的相关性。为此，我们从AQUA卫星下载了15年（2003-2017年）的云覆盖数据，其中包括欧洲极大望远镜所在地Armazones的矩阵。通过对这些数据进行快速傅立叶变换，我们检测到大约14天的周期性峰值。我们研究了2017年海洋海岸Chanaral De Las Animas的潮汐周期，并将其与Paranal和月相的大气扰动相关联。我们发现了一个显着的相关性（96%）之间的现象，短的持续时间和强度（1-3天）和潮汐周期在Chanaral。然后，我们表明，大气扰动发生在帕拉纳尔伴随着低潮，预计满月（或新）的3-4天。这一结果可以通过引入月球变量来改进目前天文观测站的天气预报模型。
Pollux: decisions affecting the optical architecture of a high-resolution spectrograph and polarimeter for the Habitable Worlds Observatory
Department of Physics, University of Oxford（牛津大学物理系）；Space Research Institute, Austrian Academy of Sciences（奥地利科学院空间研究所）；LIRA, Observatoire de Paris, Universite PSL, CNRS, Sorbonne Universite, Universite Paris Cite, CY Cergy Universite（巴黎天文台 LIRA 实验室（隶属于 PSL 大学、CNRS、索邦大学、巴黎西岱大学、CY 塞尔吉大学））；Aix Marseille Univ, CNRS, CNES, LAM, Marseille（艾克斯-马赛大学）
Daytime seeing variations in Paranal through a SHABAR system. Description of the method and first measurements from the PoET solar telescope
Instituto de Astrofísica e Ciências do Espaço, CAUP, Universidade do Porto（波尔图大学空间科学与天体物理研究所）；Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto（波尔图大学理学院物理与天文系）；Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa（里斯本大学空间科学与天体物理研究所）；Departamento de Física, Faculdade de Ciências, Universidade de Lisboa（里斯本大学理学院物理系）；University of North Carolina, Chapel Hill（北卡罗来纳大学教堂山分校）
Exoplanets through extreme optics: from PLATO to SHARK-NIR
在过去的几年里，帕多瓦天文台（Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Padova）和帕多瓦大学大规模参与了地面和天基系外行星搜索项目。关于我博士学位的活动在空间项目框架内和地面仪器领域都得到了利用。PLATO是“行星凌日和恒星振荡”的首字母缩写，是欧空局的一项任务，目标是利用它们在明亮恒星上的凌日来探测和表征系外行星。总体仪器布局包括一个多望远镜概念仪器，由几十个望远镜单元组成，它已经开发了一个全折射光学解决方案。这些器件的特点是具有非常大的视场（一侧>20度），光学质量可将大部分能量融入单个传感器像素。我参与了望远镜光学单元原型的组装、集成和验证（AIV），以验证AIV程序和望远镜飞行条件下的光学性能。SHARK-NIR是“具有从R到K波段的高阶自适应光学的日冕照相系统-近红外”的首字母缩写，是一种设计用于在近红外域中以日冕照相直接成像和光谱模式搜索和表征年轻系外行星系统和恒星形成区的仪器。它已被选为第二代大型双目望远镜（LBT）仪器，它将利用LBT极限自适应光学（XAO）校正的优异性能，这是SHARK-NIR实现最佳日冕性能所必需的，这是探测围绕明亮恒星运行的微弱行星的强制性要求。关于SHARK，我的工作是进行光学校准和仪器鉴定。
