Paper II: Calibration of the Swift ultraviolet/optical telescope
A. A. Breeveld, P. A. Curran, E. A. Hoversten, S. Koch, W. Landsman, F. E. Marshall, M. J. Page, T. S. Poole, P. Roming, P. J. Smith, M. Still, V. Yershov, A. J… 展开作者
A. A. Breeveld, P. A. Curran, E. A. Hoversten, S. Koch, W. Landsman, F. E. Marshall, M. J. Page, T. S. Poole, P. Roming, P. J. Smith, M. Still, V. Yershov, A. J. Blustin, P. J. Brown, C. Gronwall, S. T. Holland, N. P. M. Kuin, K. McGowan, S. Rosen, P. Boyd, P. Broos, M. Carter, M. M. Chester, B. Hancock, H. Huckle, S. Immler, M. Ivanushkina, T. Kennedy, K. O. Mason, A. N. Morgan, S. Oates, M. de Pasquale, P. Schady, M. Siegel, D. Vanden Berk
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Accepted for publication in MNRAS. 15 pages, 21 figures, 4 tables
The Ultraviolet/Optical Telescope (UVOT) is one of three instruments onboard the Swift observatory. The photometric calibration has been published, and this paper follows up with details on other aspects of the calibration including a measurement of the point spread function with an assessment of the orbital variation and the effect on photometry. A correction for large scale variations in sensitivity over the field of view is described, as well as a model of the coincidence loss which is used to assess the coincidence correction in extended regions. We have provided a correction for the detector distortion and measured the resulting internal astrometric accuracy of the UVOT, also giving the absolute accuracy with respect to the International Celestial Reference System. We have compiled statistics on the background count rates, and discuss the sources of the background, including instrumental scattered light. In each case we describe any impact on UVOT measurements, whether any correction is applied in the standard pipeline data processing or whether further steps are recommended.
SNR 1E 0102.2-7219 as an X-ray Calibration Standard in the 0.5-1.0 keV Bandpass and Its Application to the CCD Instruments aboard Chandra, Suzaku, Swift and XMM-Newton
我们希望对以下天文台上的当前一代CCD仪器的绝对有效面积进行简单的比较：Chandra ACIS-S3，XMM-Newton（EPIC-MOS和EPIC-pn），Suzaku XIS和Swift XRT，并直接比较这些仪器在各自任务寿命期间的随时间变化的响应。我们一直在使用1 E 0102.2-7219，在小麦哲伦星云最明亮的超新星遗迹，以评估和修改这些仪器的响应模型。1 E 0102.2-7219具有低于1.5 keV的O、Ne和Mg的强谱线，并且几乎没有或没有Fe发射，从而使光谱复杂化。作为国际天文学高能定标联合会（IACHEC）活动的一部分，我们开发了1 E 0102.2-7219的标准光谱模型。该模型是经验的，因为它包括高斯识别线，在银河系中的吸收组件，在SMC的另一个吸收组件，和两个热连续分量。在我们的拟合中，该模型受到高度约束，因为仅允许四个最亮线/线复合体（O vi He $α$三重体、O vi Ly $α$线、Ne ix He $α$三重体和Ne x Ly $α$线）的标准化和总体标准化发生变化。我们已经检查了这些测得的线通量作为时间的函数，每个仪器后，应用最新的校准，占每个仪器的时间依赖性的响应。当辐射损伤和污染层处于最低限度时，我们与具有代表性的早期任务数据进行了有效面积比较。我们发现，这些线的测量通量一般同意在+/-10%的所有仪器，与我们的48个拟合归一化在…
Initial radiometric calibration of the High-Resolution EUV Imager ($\textrm{HRI}_\textrm{EUV}$) of the Extreme Ultraviolet Imager (EUI) instrument onboard Solar Orbiter
Royal Observatory of Belgium（比利时皇家天文台）；Institut d’Astrophysique Spatiale, CNRS, Univ. Paris-Sud, Université Paris-Saclay（空间天体物理研究所，法国国家科学研究中心，巴黎南大学，巴黎萨克雷大学）；European Commission, DG Energy, Directorate D: Nuclear Energy, Safety and ITER（欧盟委员会，能源总司，D局：核能、安全与ITER）；Laboratoire Charles Fabry, Institut d’Optique Graduate School, Université Paris-Saclay（夏尔·法布里实验室，高等光学研究院，巴黎萨克雷大学）；Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center（达沃斯物理气象观测站，世界辐射中心）；UCL-Mullard Space Science Laboratory（伦敦大学学院-穆拉德空间科学实验室）；Centre Spatial de Liège, Université de Liège（列日航天中心，列日大学）；Max Planck Institute for Solar System Research（马克斯·普朗克太阳系研究所）
Unraveling the Secrets of the lower Solar Atmosphere: One year of Operation of the Solar Ultraviolet Imaging Telescope (SUIT) on board Aditya-L1
Inter-University Centre for Astronomy and Astrophysics（大学间天文学与天体物理学中心）；Manipal Centre for Natural Sciences, Manipal Academy of Higher Education（马尼拉高等教育学院自然科学中心）；Department of Physics, University College, Research Centre, University of Kerala（喀拉拉大学研究学院物理系）；Tezpur University（特佐普尔大学）；Center of Excellence in Space Sciences India, Indian Institute of Science Education and Research Kolkata（印度空间科学卓越中心，加尔各答印度科学与教育研究所）
