We propose a sociohistorical framework for better understanding the evolution in the use of telescopes. We define two regimes of use : a general-purpose (or survey) one, where the telescope governs research, and a dedicated one, in which the telescope is tailored to a specific project which includes a network of other tools. This conceptual framework is first applied to the history of the 80-cm telescope of Toulouse Observatory, which is initially anchored in a general-purpose regime linked to astrometry. After a transition in the 1930s, it is integrated in a dedicated regime centered on astrophysics. This evolution is compared to that of a very similar instrument, the 80-cm telescope of Marseille Observatory, which converts early on to the dedicated regime with the Fabry-Perot interferometer around 1910, and, after a period of idleness, is again used in the survey mode after WWII. To further validate our new concept, we apply it to the telescopes of Washburn Observatory, of Dominion Astrophysical Observatory and of Meudon Observatory. The uses of the different telescopes illustrate various combinations of the two regimes, which can be successive, simultaneous or alternating. This conceptual framework is likely to be applicable to other fields of pure and applied science.
WST -- Widefield Spectroscopic Telescope: addressing the instrumentation challenges of a new 12m class telescope dedicated to widefield Multi-object and Integral Field Spectroscopy
The DEdicated MONitor of EXotransits and Transients (DEMONEXT): System Overview and Year One Results from a Low-Cost Robotic Telescope for Follow-Up of Exoplanetary Transits and Transients
TRAPPIST: a robotic telescope dedicated to the study of planetary systems
我们在这里介绍一个新的机器人望远镜称为TRAPPIST（TRAnsiting Planets and PlanetesImals Small Telescope）。TRAPPIST配备了高质量的CCD相机，安装在0.6米的轻型光学管上，于2010年4月安装在ESO La Silla天文台（智利），现在正在开始其科学计划。TRAPPIST的科学目标是通过两种方法研究行星系：探测和研究系外行星以及研究彗星。我们在这里描述的项目目标，硬件，我们提出了一些在调试阶段获得的第一批成果。
A wide field X-ray telescope for astronomical survey purposes: from theory to practice
X射线反射镜通常采用Wolter I（抛物面-双曲面）结构。这种设计在轴上没有球面像差，但会受到场曲、彗差和像散的影响，因此角分辨率随着离轴角的增加而迅速下降。存在不同的反射镜设计，其中主反射镜和次反射镜轮廓被扩展为幂级数，以便在轴上性能的扩展下增加在大的离轴位置处的角分辨率。在这里，我们提出的设计和全局权衡研究的X射线镜系统的多项式光学的宽视场X射线望远镜（WFXT）的任务。WFXT的目标是在具有前所未有的通量灵敏度的软X射线波段进行扩展的宇宙学调查。为了实现这些目标，任务所需的角分辨率是非常苛刻的，在1度视场内的平均分辨率约为5角秒。此外，在1 keV时需要5-9000 cm ^2的有效面积。
Unveiling photometric transients with the ILMT and their follow-up using DOT
Aryabhatta Research Institute of Observational Sciences (ARIES)（阿亚巴塔观测科学研究所）；Physical Research Laboratory（物理研究实验室）；National University of Uzbekistan（乌兹别克斯坦国立大学）；Ulugh Beg Astronomical Institute of the Uzbek Academy of Sciences（乌兹别克斯坦科学院乌鲁伯格天体物理研究所）；Mahatma Jyotiba Phule Rohilkhand University（玛哈特马·乔特拉巴·普尔罗希勒坎德大学）；Liège University（列日大学）；The University of British Columbia（不列颠哥伦比亚大学）；Peking University（北京大学）；University of Calcutta（加尔各答大学）
Power Challenges of Large Scale Research Infrastructures: the Square Kilometer Array and Solar Energy Integration; Towards a zero-carbon footprint next generation telescope
