共查询到20条相似文献,搜索用时 93 毫秒
1.
Ana I. Gómez?de?Castro Jesús Maíz Pablo Rodriguez Maite Gómez Juan A. Larruquert José A. Méndez Tomas Belenguer Victor Rodrigo-Gudiel Fátima López-Martínez Paola Sestito 《Astrophysics and Space Science》2011,335(1):283-289
ISSIS is the Imaging and Slitless Spectroscopy Instrument for the World Space Observatory-Ultraviolet (WSO-UV) mission. ISSIS
is a multipurpose instrument designed to carry out high resolution (<0.1 arcsec) imaging in the far UV with fields of view
≥2×2 arcmin2. ISSIS has two acquisition channels: the High Sensitivity Channel (HSC) and the Channel for Surveys (CfS). The HSC is equipped
with an MCP-type detector to guarantee high sensitivity in the 1150–1750 ? range and high rejection of lower energy radiation.
The CfS is equipped with a large CCD detector (4k×4k) to obtain images from the far UV to the red (1150–8500 ?); the CfS is
implemented to allow observing UV bright sources such as reflection nebulae or nearby massive star forming regions. The design
drivers and the current status of the instrument are described in this contribution. 相似文献
2.
We are developing a web-based interactive software to simulate crowded-field imaging with ISSIS on board the future WSO-UV. This new tool is aimed to prepare WSO-UV/ISSIS proposals to observe multicomponent targets and dense fields. For a given combination of UV channel, filters and exposure time, the user creates a set of point-like and extended sources (source model). This source model produces a final image, which takes into account a pixelated field of view, a realistic conversion between physical flux and counts per second, the convolution with the expected point spread function, a sky background and noise fluctuations. The current version of the simulator is available at the Glendama website, and it allows users to specify all relevant parameters of each point-like or extended source, drag-and-drop sources by using a mouse or a fingertip/stylus on a touchscreen, change the frame size or the brightness scale, etc. 相似文献
3.
Gravitationally lensed QSOs (GLQs) at 1≤z≤2 play a key role in understanding the cosmic evolution of the innermost parts of active galaxies (black holes, accretion
disks, coronas and internal jets), as well as the structure of galaxies at intermediate redshifts. With respect to studies
of normal QSOs, GLQ programmes have several advantages. For example, a monitoring of GLQs may lead to unambiguous detections
of intrinsic and extrinsic variations. Both kinds of variations can be used to discuss central engines in distant QSOs, and
mass distributions and compositions of lensing galaxies. In this context, UV data are of particular interest, since they correspond
to emissions from the immediate surroundings of the supermassive black hole. We describe some observation strategies to analyse
optically bright GLQs at z∼1.5, using ISSIS (CfS) on board World Space Observatory-Ultraviolet. 相似文献
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SOHM-4型氢原子钟的设计改进与初步性能 总被引:1,自引:3,他引:1
氢原子钟是一种最稳定的 (除极短测量时间间隔之外 )频率标准 ,但是环境温度变化及微波谐振腔老化会引起原子钟输出频率的变化 ,从而导致氢原子钟长期性能变差。为了减小这些影响 ,可借助一种自动调谐器来确保谐振腔的频率始终工作在所需的频率上 ,并采用新的温度控制系统来改善氢原子钟的长期性能。针对这些年来许多氢钟出现的有关问题 ,上海天文台在借鉴国外氢钟实验室经验的基础之上 ,对原有氢钟进行了技术改造 ,并为国家授时中心研制了SOHM - 4型氢原子钟。对该型氢原子钟技术改造特点作了介绍 ,并给出了期望的性能指标及初步的测试结果 相似文献
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8.
A. Maselli B. Ciardi A. Kanekar 《Monthly notices of the Royal Astronomical Society》2009,393(1):171-178
In this paper, we report on the improvements implemented in the cosmological radiative transfer code crash . In particular, we present a new multi-frequency algorithm for spectra sampling which makes use of coloured photon packets: we discuss the need for the multi-frequency approach, describe its implementation and present the improved crash performance in reproducing the effects of ionizing radiation with an arbitrary spectrum. We further discuss minor changes in the code implementation which allow for more efficient performance and an increased precision. 相似文献
9.
为了探索对较暗目标进行成像的新方法,我们在TI公司生产的带有增益寄存器的EMCCD(Electron Multiply CCD)芯片基础上,构建了一套成像系统,主要用于对此芯片进行性能测试,为将来构建天文观测用相机做准备。本文主要介绍了EMCCD的结构特点、工作原理,并且详细介绍实验室采用TI公司的EMCCD搭建的成像系统,以及在此系统基础上对EMCCD进行地评测。 相似文献
10.
J. Wang X. M. Meng X. H. Han H. B. Cai L. Cao J. S. Deng Y. L. Qiu S. Wang J. Y. Wei J. Y. Hu 《Astrophysics and Space Science》2015,360(1):10
We here report the photometric performance of Lunar-based Ultraviolet telescope (LUT), the first robotic telescope working on the Moon, for its 18-months operation. In total, 17 IUE standards have been observed in 51 runs until June 2015, which returns a highly stable photometric performance during the past 18 months (i.e., no evolution of photometric performance with time). The magnitude zero point is determined to be \(17.53\pm0.05~\mbox{mag}\), which is not only highly consistent with the results based on its first 6-months operation, but also independent on the spectral type of the standard from which the magnitude zero point is determined. The implications of this stable performance is discussed, and is useful for next generation lunar-based astronomical observations. 相似文献
11.
Jean-Pierre Rivet Laurent Koechlin Truswin Raksasataya Paul Deba Ren�� Gili 《Experimental Astronomy》2011,30(2-3):149-164
The Fresnel Diffractive Array Imager (FDAI) is a new optical concept proposed for large telescopes in space. To evaluate its performance on real sky objects, we have built a new testbed of FDAI, especially designed for on-sky operation. It is an evolution of the laboratory setup previously used to validate the concept on artificial sources. In order to observe celestial objects, this new two-module testbed was installed in July 2009 at Observatoire de la Côte d??Azur (Nice, France). The two modules of the testbed (the Fresnel array module and the receiver module), were secured at both ends of the 19 m long tube of an historical refractor, used as an optical bench on an equatorial mount. In this article, we focus on the evolution steps from a laboratory experiment to the first observation prototype, and on the targets chosen for performance assessment. We show the first on-sky results of a FDAI, although they do not reflect the nominal performances of the final testbed. These nominal performances have been attained only with the latest and most sophisticated prototype, and are presented in a separate article in this special issue. 相似文献
12.
传统铷原子钟和铯原子钟已在卫星导航定位系统中作为星载原子钟获得重要应用.卫星导航定位系统的更新和新发展要求更高精度更小型的新型星载原子钟.该文介绍采用新物理原理和先进技术在下-代卫星导航定位系统有应用前景的新原子钟的产生和发展以及它们目前的进展. 相似文献
13.
《天文和天体物理学研究(英文版)》2021,(9)
In the past few years,Chinese astronomical community is actively testing astronomical sites for several new optical/infrared ground-based telescopes.These site testing campaigns conducted were mainly focused on fundamental performances of the sites,such as cloud coverage,seeing,temperature,etc.With increasing interests in sodium laser guide star adaptive optics for these new telescopes in the Chinese astronomical community,it is interesting to investigate the performance of the laser guide star at these sites,especially considering that the sodium laser guide star's on-sky performance is significantly influenced by sites' local performances,such as geomagnetic field,sodium layer dynamics,density of air molecule,etc.In this paper,we studied sodium laser guide star's performance of a 20 W class Quasi Continuous Wave(QCW) pulsed laser developed by TIPC with numerical simulation for five selected sites in China. 相似文献
14.
K. P. Singh G. C. Stewart N. J. Westergaard S. Bhattacharayya S. Chandra V. R. Chitnis G. C. Dewangan A. T. Kothare I. M. Mirza K. Mukerjee V. Navalkar H. Shah A. F. Abbey A. P. Beardmore S. Kotak N. Kamble S. Vishwakarama D. P. Pathare V. M. Risbud J. P. Koyande T. Stevenson C. Bicknell T. Crawford G. Hansford G. Peters J. Sykes P. Agarwal M. Sebastian A. Rajarajan G. Nagesh S. Narendra M. Ramesh R. Rai K. H. Navalgund K. S. Sarma R. Pandiyan K. Subbarao T. Gupta N. Thakkar A. K. Singh A. Bajpai 《Journal of Astrophysics and Astronomy》2017,38(2):29
The Soft X-ray focusing Telescope (SXT), India’s first X-ray telescope based on the principle of grazing incidence, was launched aboard the AstroSat and made operational on October 26, 2015. X-rays in the energy band of 0.3–8.0 keV are focussed on to a cooled charge coupled device thus providing medium resolution X-ray spectroscopy of cosmic X-ray sources of various types. It is the most sensitive X-ray instrument aboard the AstroSat. In its first year of operation, SXT has been used to observe objects ranging from active stars, compact binaries, supernova remnants, active galactic nuclei and clusters of galaxies in order to study its performance and quantify its characteriztics. Here, we present an overview of its design, mechanical hardware, electronics, data modes, observational constraints, pipeline processing and its in-orbit performance based on preliminary results from its characterization during the performance verification phase. 相似文献
15.
《Chinese Astronomy and Astrophysics》2020,44(4):519-535
Two-Way Satellite Time and Frequency Transfer (TWSTFT) is one of the time transfer methods with the highest accuracy at present, and it is also the main method to compare the atomic time scale among the time-keeping laboratories participated in the international atomic time calculation. Improving the short-term stability of TWSTFT links and reducing the influence of Diurnal on the link time transfer result have practical significance for optimizing the performance of TAI (International Atomic Time). In this paper, a method of TWSTFT link performance optimization based on conditional adjustment is proposed. Firstly, the optimized network of TWSTFT link performance (hereinafter briefly called as optimized network) is established according to the noise level and spectrum analysis result of TWSTFT link measurements, and then the weight coefficient matrix is set according to the analysis result of measurement noises of all the links in the optimized network to establish the conditional adjustment model. The Two-Way Satellite Time and Frequency Transfer link between the National Institute of Metrology (NIM) and the National Time Service Center (NTSC) of Chinese Academy of Sciences in the Asia-Pacific region is selected as the link to be optimized, and the TWSTFT links among NTSC, NIM, and Physikalisch-Technische Bundesanstalt (PTB) are used to compose the optimized network. The networking method and conditional adjustment model are verified by experiments. The results show that the short-term stability of the link to be optimized after adjustment is improved, and the influence of Diurnal is reduced about 24.6%. Using this method, the time transfer performance of the link to be optimized can be improved effectively. 相似文献
16.
《天文和天体物理学研究(英文版)》2021,(7)
Trying to achieve the best surface accuracy control with the fewest actuators, this article mainly studies the distribution of actuators and the method of panel design. The influence of the number of faulty actuators on the accuracy of the surface shape is demonstrated. In addition, the method incorporating a triangular panel, node index and the fitting solution method of a single panel is also given. This method provides a reference for the design and realization of an active surface or a deformable sub-reflector for high performance large aperture radio telescopes. 相似文献
17.
Automatic Short-Term Solar Flare Prediction Using Machine Learning and Sunspot Associations 总被引:2,自引:0,他引:2
In this paper, a machine-learning-based system that could provide automated short-term solar flare prediction is presented.
This system accepts two sets of inputs: McIntosh classification of sunspot groups and solar cycle data. In order to establish
a correlation between solar flares and sunspot groups, the system explores the publicly available solar catalogues from the
National Geophysical Data Center to associate sunspots with their corresponding flares based on their timing and NOAA numbers.
The McIntosh classification for every relevant sunspot is extracted and converted to a numerical format that is suitable for
machine learning algorithms. Using this system we aim to predict whether a certain sunspot class at a certain time is likely
to produce a significant flare within six hours time and if so whether this flare is going to be an X or M flare. Machine
learning algorithms such as Cascade-Correlation Neural Networks (CCNNs), Support Vector Machines (SVMs) and Radial Basis Function
Networks (RBFN) are optimised and then compared to determine the learning algorithm that would provide the best prediction
performance. It is concluded that SVMs provide the best performance for predicting whether a McIntosh classified sunspot group
is going to flare or not but CCNNs are more capable of predicting the class of the flare to erupt. A hybrid system that combines
a SVM and a CCNN is suggested for future use. 相似文献
18.
卫星双向时间传递(Two-Way Satellite Time and Frequency Transfer, TWSTFT)是目前精度最高的时间传递方法之一,同时也是参与国际原子时计算的守时实验室之间比较原子时尺度的一种主要方法.提高TWSTFT链路的短期稳定度,降低周日效应对链路时间传递结果的影响,对优化TAI (International Atomic Time)的性能具有现实意义.提出了一种基于条件平差的TWSTFT链路性能优化方法,先依据TWSTFT链路测量噪声水平与谱分析结果建立TWSTFT链路性能优化网络(简称优化网络),再根据优化网络中各链路测量噪声分析结果设置权系数阵,建立条件平差模型.选取亚太地区的中国计量科学研究院(National Institute of Metrology, NIM)-中国科学院国家授时中心(National Time Service Center, NTSC)卫星双向时间传递链路作为待优化链路,以NTSC、NIM以及德国联邦物理技术研究所(Physikalisch-Technische Bundesanstalt,PTB)之间的TWSTFT链路组成优化网络,对优化网络的组网方法和条件平差模型进行实验验证.结果表明,平差后待优化链路短期稳定度得到了改善,同时其受周日效应的影响降低了约24.6%.使用该方法,能够有效提高待优化链路的时间传递性能. 相似文献
19.
《New Astronomy》2015
The New Vacuum Solar Telescope (NVST) is a 1-m solar telescope that aims to observe the fine structures in both the photosphere and the chromosphere of the Sun. The observational data acquired simultaneously from one channel for the chromosphere and two channels for the photosphere bring great challenges to the data storage of NVST. The multi-channel instruments of NVST, including scientific cameras and multi-band spectrometers, generate at least 3 terabytes data per day and require high access performance while storing massive short-exposure images. It is worth studying and implementing a storage system for NVST which would balance the data availability, access performance and the cost of development. In this paper, we build a distributed data storage system (DDSS) for NVST and then deeply evaluate the availability of real-time data storage on a distributed computing environment. The experimental results show that two factors, i.e., the number of concurrent read/write and the file size, are critically important for improving the performance of data access on a distributed environment. Referring to these two factors, three strategies for storing FITS files are presented and implemented to ensure the access performance of the DDSS under conditions of multi-host write and read simultaneously. The real applications of the DDSS proves that the system is capable of meeting the requirements of NVST real-time high performance observational data storage. Our study on the DDSS is the first attempt for modern astronomical telescope systems to store real-time observational data on a low-cost distributed system. The research results and corresponding techniques of the DDSS provide a new option for designing real-time massive astronomical data storage system and will be a reference for future astronomical data storage. 相似文献