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Gaia is an ambitious space observatory devoted to obtain the largest and most precise astrometric catalogue of astronomical objects from our Galaxy and beyond. On-board processing and transmission of the huge amount of data generated by the instruments is one of its several technological challenges. The measurement time tags are critical for the scientific results of the mission, so they must be measured and transmitted with the highest precision – leading to an important telemetry channel occupation. In this paper we present the optimization of time data, which has resulted in a useful software tool. We also present how time data is adapted to the packet telemetry standard. The several communication layers are illustrated and a method for coding and transmitting the relevant data is described as well. Although our work is focused on Gaia, the timing scheme and the corresponding tools can be applied to any other instrument or mission with similar operational principles. 相似文献
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William O’Mullane Xavier Luri Paul Parsons Uwe Lammers John Hoar Jose Hernandez 《Experimental Astronomy》2011,31(2-3):243-258
In recent years Java has matured to a stable easy-to-use language with the flexibility of an interpreter (for reflection etc.) but the performance and type checking of a compiled language. When we started using Java for astronomical applications around 1999 they were the first of their kind in astronomy. Now a great deal of astronomy software is written in Java as are many business applications. We discuss the current environment and trends concerning the language and present an actual example of scientific use of Java for high-performance distributed computing: ESA’s mission Gaia. The Gaia scanning satellite will perform a galactic census of about 1,000 million objects in our galaxy. The Gaia community has chosen to write its processing software in Java. We explore the manifold reasons for choosing Java for this large science collaboration. Gaia processing is numerically complex but highly distributable, some parts being embarrassingly parallel. We describe the Gaia processing architecture and its realisation in Java. We delve into the astrometric solution which is the most advanced and most complex part of the processing. The Gaia simulator is also written in Java and is the most mature code in the system. This has been successfully running since about 2005 on the supercomputer “Marenostrum” in Barcelona. We relate experiences of using Java on a large shared machine. Finally we discuss Java, including some of its problems, for scientific computing. 相似文献
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Jordi Portell Enrique García-Berro Xavier Luri Alberto G. Villafranca 《Experimental Astronomy》2006,21(3):125-149
Gaia is the most ambitious space astrometry mission currently envisaged and it will be a technological challenge in all its
aspects. Here we describe a proposal for the data compression system of Gaia, specifically designed for this mission but based
on concepts that can be applied to other missions and systems as well. Realistic simulations have been performed with our
Telemetry CODEC software, which performs a stream partitioning and pre-compression to the science data. In this way, standard
compressors such as bzip2 or szip boost their performance and decrease their processing requirements when applied to such pre-processed data. These simulations
have shown that a lossless compression factor of 3 can be achieved, whereas standard compression systems were unable to reach
a factor of 2.
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Santiago Torres Enrique García-Berro Jordi Isern Francesca Figueras 《Monthly notices of the Royal Astronomical Society》2005,360(4):1381-1392
One of the most promising space missions of the European Space Agency is the astrometric satellite Gaia , which will provide very precise astrometry and multicolour photometry, for all 1.3 billion objects to V ∼ 20 , and radial velocities with accuracies of a few km s−1 for most stars brighter than V ∼ 17 . Consequently, full homogeneous six-dimensional phase-space information for a huge number of stars will become available. Our Monte Carlo simulator has been used to estimate the number of white dwarfs potentially observable by Gaia . From this we assess the white dwarf luminosity functions that Gaia will obtain and discuss in depth the scientific returns of Gaia in the specific field of white dwarf populations. Scientifically attainable goals include, among others, a reliable determination of the age of the Galactic disc, a better knowledge of the halo of the Milky Way and the reconstruction of the star formation history of the Galactic disc. Our results also demonstrate the potential impact of a mission such as Gaia within the context of current understanding of white dwarf cooling theory. 相似文献
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A parameter database for large scientific projects: application to the Gaia space astrometry mission
The parallel development of many aspects of a complex space science mission like Gaia, which includes numerous participants in ESA, industrial companies, and a large and active scientific collaboration throughout Europe, makes keeping track of the many design changes, instrument and operational parameters, and numerical values for the data analysis and simulations, a challenging but crucially important problem. A comprehensive, easily-accessible, up-to-date, and definitive compilation of a large range of numerical quantities is required, and the Gaia parameter database has been established to satisfy these needs. The database is a centralised repository containing, besides mathematical, physical, and astronomical constants, many satellite and subsystem design parameters. Version control provides both a ‘live’ version with the most recent parameters, as well as previous ‘reference’ versions of the full database contents. Query results are formatted by default in HTML, while an important feature is that data can also be retrieved as Java, ANSI-C, C++, Ruby, or XML structures for direct inclusion into software codes, such that all collaborating scientists can use the retrieved database parameters and values directly linked to computational routines. 相似文献
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P. G. Niarchos 《Astrophysics and Space Science》2006,304(1-4):387-390
The space experiment Gaia, the approved cornerstone 6 ESA mission, will observe up to a billion stars in our Galaxy and obtain their astrometric positions on a micro-arcsec level, multi-band photometry as well as spectroscopic observations. It is expected that about one million Eclipsing Binaries (EBs) (with V ≤ 16 mag) will be discovered and the observing fashion will be quite similar to Hipparcos/Tycho mission operational mode. The combined astrometric, photometric and spectroscopic data will be used to compute the physical parameters of the observed EBs. From a study of a small sample of EBs, it is shown that the agreement between the fundamental stellar parameters, derived from ground-based and Hipparcos (Gaia-like) observations, is more than satisfactory and the Gaia data will be suitable to obtain accurate binary solutions. 相似文献
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Michael Perryman 《Astronomy and Astrophysics Review》2011,19(1):1-16
The Hipparcos satellite was launched in 1989. It was the first, and remains to date the only, attempt at performing large-scale astrometric measurements from space. Hipparcos marked a fundamentally new approach to the field of astrometry, revolutionising our knowledge of the positions, distances, and space motions of the stars in the solar neighbourhood. In this retrospective, I look back at the processes which led to the mission??s acceptance, provide a short summary of the underlying measurement principles and the experiment??s scientific achievements, and a conclude with a brief summary of its principal legacy??the Gaia mission. 相似文献
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时间尺度的连续性要求对原子钟信号进行必要的预测,预测的实质是建立一个模型来逼近原子钟的信号,前向神经网络具有良好的副近非线性 函数的能力,用神经网络模型来预测原子钟信号,并与AD模型的预测结果作了比较。 相似文献
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Gerald Hechenblaikner Marc-Peter Hess Marianna Vitelli Jan Beck 《Experimental Astronomy》2014,37(3):481-501
STE-QUEST is a fundamental science mission which is considered for launch within the Cosmic Vision programme of the European Space Agency (ESA). Its main scientific objectives relate to probing various aspects of Einstein’s theory of general relativity by measuring the gravitational red-shift of the earth, the moon and the sun as well as testing the weak equivalence principle to unprecedented accuracy. In order to perform the measurements, the system features a spacecraft equipped with two complex instruments, an atomic clock and an atom interferometer, a ground-segment encompassing several ground-terminals collocated with the best available ground atomic clocks, and clock comparison between space and ground via microwave and optical links. The baseline orbit is highly eccentric and exhibits strong variations of incident solar flux, which poses challenges for thermal and power subsystems in addition to the difficulties encountered by precise-orbit-determination at high altitudes. The mission assessment and definition phase (Phase-A) has recently been completed and this paper gives a concise overview over some system level results. 相似文献
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Claus Braxmaier Hansj?rg Dittus Bernard Foulon Ertan G?klü Catia Grimani Jian Guo Sven Herrmann Claus L?mmerzahl Wei-Tou Ni Achim Peters Benny Rievers étienne Samain Hanns Selig Diana Shaul Drazen Svehla Pierre Touboul Gang Wang An-Ming Wu Alexander F. Zakharov 《Experimental Astronomy》2012,34(2):181-201
ASTROD I is a planned interplanetary space mission with multiple goals. The primary aims are: to test General Relativity with an improvement in sensitivity of over 3 orders of magnitude, improving our understanding of gravity and aiding the development of a new quantum gravity theory; to measure key solar system parameters with increased accuracy, advancing solar physics and our knowledge of the solar system; and to measure the time rate of change of the gravitational constant with an order of magnitude improvement and the anomalous Pioneer acceleration, thereby probing dark matter and dark energy gravitationally. It is envisaged as the first in a series of ASTROD missions. ASTROD I will consist of one spacecraft carrying a telescope, four lasers, two event timers and a clock. Two-way, two-wavelength laser pulse ranging will be used between the spacecraft in a solar orbit and deep space laser stations on Earth, to achieve the ASTROD I goals.For this mission, accurate pulse timing with an ultra-stable clock, and a drag-free spacecraft with reliable inertial sensor are required. T2L2 has demonstrated the required accurate pulse timing; rubidium clock on board Galileo has mostly demonstrated the required clock stability; the accelerometer on board GOCE has paved the way for achieving the reliable inertial sensor; the demonstration of LISA Pathfinder will provide an excellent platform for the implementation of the ASTROD I drag-free spacecraft. These European activities comprise the pillars for building up the mission and make the technologies needed ready. A second mission, ASTROD or ASTROD-GW (depending on the results of ASTROD I), is envisaged as a three-spacecraft mission which, in the case of ASTROD, would test General Relativity to one part per billion, enable detection of solar g-modes, measure the solar Lense-Thirring effect to 10 parts per million, and probe gravitational waves at frequencies below the LISA bandwidth, or in the case of ASTROD-GW, would be dedicated to probe gravitational waves at frequencies below the LISA bandwidth to 100?nHz and to detect solar g-mode oscillations. In the third phase (Super-ASTROD), larger orbits could be implemented to map the outer solar system and to probe primordial gravitational-waves at frequencies below the ASTROD bandwidth. This paper on ASTROD I is based on our 2010 proposal submitted for the ESA call for class-M mission proposals, and is a sequel and an update to our previous paper (Appouchaux et al., Exp Astron 23:491?C527, 2009; designated as Paper I) which was based on our last proposal submitted for the 2007 ESA call. In this paper, we present our orbit selection with one Venus swing-by together with orbit simulation. In Paper I, our orbit choice is with two Venus swing-bys. The present choice takes shorter time (about 250?days) to reach the opposite side of the Sun. We also present a preliminary design of the optical bench, and elaborate on the solar physics goals with the radiation monitor payload. We discuss telescope size, trade-offs of drag-free sensitivities, thermal issues and present an outlook. 相似文献
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The mission Gaia by European Space Agency (ESA) is expected to fly at the end of 2011 and to perform an all-sky, magnitude-limited survey for 5 years. The probe will not use an input catalogue, and will get high accuracy astrometry and photometry for all sources of magnitude V<20. Low-resolution spectra will also be available. Moving Solar System objects will be observed as well, and their observations will be processed by a specific pipeline in order to retrieve the physical and dynamical characteristics of each object. In this contribution we will mainly focus on the impact of Gaia observations on asteroid dynamics. A dramatic improvement of orbital elements is expected, as well as the measurement of subtle effects such as those related to general relativity (GR). Gaia observations will also be supported by a network of ground-based observation sites, capable of providing follow-up for newly discovered objects that will not receive an adequate coverage from space. Specific strategies for follow-up are being planned and tested. These will need to take into account the peculiar observing geometry (large parallax effect due to the orbit of Gaia around L2) and the time constraints dictated by data processing. 相似文献
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Wang Ji-gang Hu Yong-huiHe Zai-min Wu Jian-feng Ma Hong-jiaoWang Kang 《Chinese Astronomy and Astrophysics》2011,35(3):318
The prediction of the clock errors of atomic clocks plays an important role in the work on time and frequency. Each of the prediction models often used at present has its own merits and shortages. A combination of the predicted results obtained by means of these models can be used to synthesize the characteristics of various kinds of prediction models. In the light of the problem which occurs when the linear combination model is used to make the prediction of clock errors, the concept of learning weight is proposed and the modified combination prediction model is made by taking advantage of various kinds of pieces of accuracy information. For verifying the efficiency of this method the clock error sequences of the IGS (International GNSS Service) of 4 GPS satellites are selected and the predicted results of the quadratic polynomial and grey model are combined. The result shows that the modified model can further improve the stability and accuracy based on the guarantee of the reliability. 相似文献
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本文主要介绍基于科学CCD的低纬子午环数据采集系统的硬件构成及软件设计。为了能绝对而又精确地确定天体的位置 ,低纬子午环需要配备多种精密的测量装置 ,如 :GPS与时钟、 9路Reticon线阵、视频CCD、科学CCD、圆感应同步器、光栅线性位移传感器等。为了能有序地控制并采集这些装置的数据 ,我们设计了一个包含 3个PC机的数据采集与控制系统。文中将描述测量装置的功能 ,然后介绍数据采集方法及软件设计 相似文献
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F. Mignard A. Cellino K. Muinonen P. Tanga M. Delbò A. Dell’Oro M. Granvik D. Hestroffer S. Mouret W. Thuillot J. Virtanen 《Earth, Moon, and Planets》2007,101(3-4):97-125
According to current plans of the European space agency, Gaia will be launched in 2011. By performing a systematic survey of the whole sky down to magnitude V = 20, this mission will provide a fundamental contribution in practically all branches of modern Astrophysics. Gaia will be able to survey with repeated observations spanning over 5 years several 100,000 s asteroids. It will directly measure sizes of about 1,000 objects, obtain the masses of about 100 of them, derive spin properties and overall shapes of more than 10,000 objects, yield much improved orbits and taxonomic classification for most of the observed sources. The final harvest will very likely include new discoveries of objects orbiting at heliocentric distances less than 1 AU. At the end of the mission, we will know average densities of about 100 objects belonging to all the major taxonomic classes, have a much more precise knowledge of the inventory and size and spin distributions of the population, of the distribution of taxonomic classes as a function of heliocentric distance, and of the dynamical and physical properties of dynamical families. 相似文献
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