The silicon micro-strip detector plane for the LOFT/Wide Field Monitor
A. Goldwurm, P. Ferrando, D. Götz, P. Laurent, F. Lebrun, O. Limousin, S. Basa, W. Bertoli, E. Delagnes, Y. Dolgorouky, O. Gevin, A. Gros, C. Gouiffes, F. Jeann… 展开作者
A. Goldwurm, P. Ferrando, D. Götz, P. Laurent, F. Lebrun, O. Limousin, S. Basa, W. Bertoli, E. Delagnes, Y. Dolgorouky, O. Gevin, A. Gros, C. Gouiffes, F. Jeanneau, C. Lachaud, M. Llored, C. Olivetto, G. Prévôt, D. Renaud, J. Rodriguez, C. Rossin, S. Schanne, S. Soldi, P. Varniere
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Proceedings of SPIE, Vol. 8443, Paper No. 8443-89, 2012
The main objective of the Wide Field Monitor (WFM) on the LOFT mission is to provide unambiguous detection of the high-energy sources in a large field of view, in order to support science operations of the LOFT primary instrument, the LAD. The monitor will also provide by itself a large number of results on the timing and spectral behaviour of hundreds of galactic compact objects, Active Galactic Nuclei and Gamma-Ray Bursts. The WFM is based on the coded aperture concept where a position sensitive detector records the shadow of a mask projected by the celestial sources. The proposed WFM detector plane, based on Double Sided micro-Strip Silicon Detectors (DSSD), will allow proper 2-dimensional recording of the projected shadows. Indeed the positioning of the photon interaction in the detector with equivalent fine resolution in both directions insures the best imaging capability compatible with the allocated budgets for this telescope on LOFT. We will describe here the overall configuration of this 2D-WFM and the design and characteristics of the DSSD detector plane including its imaging and spectral performances. We will also present a number of simulated results discussing the advantages that this configuration offers to LOFT. A DSSD-based WFM will in particular reduce significantly the source confusion experienced by the WFM in crowded regions of the sky like the Galactic Center and will in general increase the observatory science capability of the mission.
The digital data processing concepts of the LOFT mission
大型X射线计时天文台（LOFT）是欧空局考虑用于M3任务的五个候选任务之一（发射机会在2022 - 2024年）。LOFT有两种仪器：大面积探测器（LAD）和宽视场监视器（WFM）。LAD是一种10 m 2级仪器，其收集面积约为迄今为止最大定时任务（RXTE）的15倍，首次结合CCD级光谱分辨率。WFM将持续监测天空并识别源状态的变化，检测瞬态和突发现象，并允许任务对此做出响应。使用LAD的有效面积观测最亮的X射线源会导致巨大的数据速率，这些数据速率需要在多个级别上进行处理，并在船上实时进行过滤和压缩。另一方面，WFM数据处理对数据速率的约束相当低，但需要算法来找到探测器上的光子相互作用位置，然后对探测器图像进行去卷积，以获得观测到的瞬态源的天空坐标。在下文中，我们将概述在研究阶段开发的数据处理概念。
Design and performance of the coded mask for the Lunar Electromagnetic Monitor in X-rays (LEM-X)
INAF, Istituto di Astrofisica e Planetologia Spaziali（意大利国家天体物理研究所，空间天体物理学与行星学研究所）；INFN, Sez. Roma Tor Vergata（意大利国家核物理研究所，罗马托维加塔分部）；University of Rome “La Sapienza”, Dept. of Physics（罗马大学，物理系）；INAF, Osservatorio Astronomico di Roma（意大利国家天体物理研究所，罗马天文台）；Agenzia Spaziale Italiana（意大利航天局）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所，天体物理学与空间科学观测站）；INFN, Sez. Bologna（意大利国家核物理研究所，博洛尼亚分部）
Simulations of a 2 x 1.5D coded aperture camera for X-ray astronomy
SRON Space Research Organization Netherlands（荷兰空间研究所）；INAF-IAPS Roma（罗马国家天体物理研究所）；Institute of Space Sciences (ICE-CSIC)（空间科学研究所）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院）
本文研究了用于X射线天文观测的2 x 1.5D编码孔径相机的设计与性能，采用IROS和MLM两种解码算法，旨在提高X射线源识别和观测精度。
The STRIP instrument of the Large Scale Polarization Explorer: microwave eyes to map the Galactic polarized foregrounds
本文讨论了“大尺度偏振探测器”（LSPE）实验中STRIP仪器的最新进展。LSPE是一个新颖的项目，它结合了地基（STRIP）和球载（SWIPE）的大角度尺度上的微波天空的偏振测量，试图探测宇宙微波背景偏振的“B模式”。STRIP将从特内里费岛的“Observatorio del Teide”观测大约25%的北方天空，使用43 GHz的49个相干偏振仪阵列，与1.5米全旋转交叉Dragone望远镜耦合。第二个频道有六个单元，频率为95千兆赫，将用作大气监测器。目前，STRIP仪器的大部分硬件已经在子系统级开发和测试。从2018年7月开始的系统级表征将使STRIP在年底内在观测站进行运输和安装。整个仪器的现场检定和校准将为STRIP进行为期2年的CMB偏振观测做好准备。
