共查询到20条相似文献，搜索用时 15 毫秒
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P. Barthol A. Gandorfer S. K. Solanki M. Sch��ssler B. Chares W. Curdt W. Deutsch A. Feller D. Germerott B. Grauf K. Heerlein J. Hirzberger M. Kolleck R. Meller R. M��ller T. L. Riethm��ller G. Tomasch M. Kn?lker B. W. Lites G. Card D. Elmore J. Fox A. Lecinski P. Nelson R. Summers A. Watt V. Mart��nez?Pillet J. A. Bonet W. Schmidt T. Berkefeld A. M. Title V. Domingo J. L. Gasent?Blesa J. C. del Toro?Iniesta A. L��pez?Jim��nez A. ��lvarez-Herrero L. Sabau-Graziati C. Widani P. Haberler K. H?rtel D. Kampf T. Levin I. P��rez?Grande A. Sanz-Andr��s E. Schmidt 《Solar physics》2011,268(1):1-34
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V. G. Klochkova V. E. Panchuk M. V. Yushkin D. S. Nasonov 《Astrophysical Bulletin》2008,63(4):386-394
Solutions are considered that allow the accuracy of stellar radial velocity measurements with the spectroscopic instruments of the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences to be improved. The factors that limit the accuracy of spectroscopic V r measurements are analyzed both in general and for the particular design of the telescope and its housing. 相似文献
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We present a novel approach to quality control during the processing of astronomical data. Quality control in the Astro-WISE Information System is integral to all aspects of data handing and provides transparent access to quality estimators for all stages of data reduction from the raw image to the final catalog. The implementation of quality control mechanisms relies on the core features in this Astro-WISE Environment (AWE): an object-oriented framework, full data lineage, and both forward and backward chaining. Quality control information can be accessed via the command-line awe-prompt and the web-based Quality-WISE service. The quality control system is described and qualified using archive data from the 8-CCD Wide Field Imager (WFI) instrument (http://www.eso.org/lasilla/instruments/wfi/) on the 2.2-m MPG/ESO telescope at La Silla and (pre-)survey data from the 32-CCD OmegaCAM instrument (http://www.astro-wise.org/~omegacam/) on the VST telescope at Paranal. 相似文献
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W. Cao N. Gorceix R. Coulter K. Ahn T. R. Rimmele P. R. Goode 《Astronomische Nachrichten》2010,331(6):636-639
The NST (New Solar Telescope), a 1.6 m clear aperture, off‐axis telescope, is in its commissioning phase at Big Bear Solar Observatory (BBSO). It will be the most capable, largest aperture solar telescope in the US until the 4 m ATST (Advanced Technology Solar Telescope) comes on‐line late in the next decade. The NST will be outfitted with state‐of‐the‐art scientific instruments at the Nasmyth focus on the telescope floor and in the Coudé Lab beneath the telescope. At the Nasmyth focus, several filtergraphs already in routine operation have offered high spatial resolution photometry in TiO 706 nm, Hα 656 nm, G‐band 430 nm and the near infrared (NIR), with the aid of a correlation tracker and image reconstruction system. Also, a Cryogenic Infrared Spectrograph (CYRA) is being developed to supply high signal‐to‐noise‐ratio spectrometry and polarimetry spanning 1.0 to 5.0 μm. The Coudé Lab instrumentation will include Adaptive Optics (AO), InfraRed Imaging Magnetograph (IRIM), Visible Imaging Magnetograph (VIM), and Fast Imaging Solar Spectrograph (FISS). A 308 sub‐aperture (349‐actuator deformable mirror) AO system will enable nearly diffraction limited observations over the NST's principal operating wavelengths from 0.4 μm through 1.7 μm. IRIM and VIM are Fabry‐Pérot based narrow‐band tunable filters, which provide high resolution two‐dimensional spectroscopic and polarimetric imaging in the NIR and visible respectively. FISS is a collaboration between BBSO and Seoul National University focussing on chromosphere dynamics. This paper reports the up‐to‐date progress on these instruments including an overview of each instrument and details of the current state of design, integration, calibration and setup/testing on the NST (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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A. Title 《Astronomische Nachrichten》2010,331(6):599-600
The exciting new high resolution images from the one meter Sunrise balloon telescope and the first images from the 1.6 meter Big Bear telescope together with the continuing data from the 1 meter Swedish Solar Observatory demonstrate the promise of the new generation of multimeter solar telescopes. While the promise of the new generation of telescopes is great the technical challenges to build them will require the efforts of a significant fraction of the solar community. In this talk I will emphasize the need for an integrated systems approach to the development of the telescope, its instruments, its software, and its operations and management structures. The experience of several decades of space mission has taught us a great deal about the value of planning mission development from the definition of the primary scientific objectives to the delivery of the data to the science community. Much of these lessons learned, often painfully, should provide guidance to those in developing the new telescope systems (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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Toshinori Maihara 《Astrophysics and Space Science》1989,160(1-2):313-323
The principal features of the JNLT as an infrared telescope are presented along with its ultimate performance of detectivity in typical methods of imagery and spectroscopy. Some infrared instruments: infrared camera, grating spectrometer, and Fabry-Pérot-based imager, currently proposed as the first generation instruments are also discussed in relation to the scientific objectives of the JNLT.Paper presented at the Symposium on the JNLT and Related Engineering Developments, Tokyo, November 29–December 2, 1988. 相似文献
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The 1.6 m clear aperture solar telescope in Big Bear is operational and with its adaptive optics (AO) system it provides diffraction limited solar imaging and polarimetry in the near-infrared (NIR). While the AO system is being upgraded to provide diffraction limited imaging at bluer wavelengths, the instrumentation and observations are concentrated in the NIR. The New Solar Telescope (NST) operates in campaigns, making it the ideal ground-based telescope to provide complementary/supplementary data to SDO and Hinode. The NST makes photometric observations in Hα (656.3 nm) and TiO (705.6 nm) among other lines. As well, the NST collects vector magnetograms in the 1565 nm lines and is beginning such observations in 1083.0 nm. Here we discuss the relevant NST instruments, including AO, and present some results that are germane to NASA solar missions. 相似文献
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C. Denker O. von der Lühe A. Feller K. Arlt H. Balthasar S.‐M. Bauer N. Bello Gonzlez Th. Berkefeld P. Caligari M. Collados A. Fischer T. Granzer T. Hahn C. Halbgewachs F. Heidecke A. Hofmann T. Kentischer M. Klva&#x;a F. Kneer A. Lagg H. Nicklas E. Popow K.G. Puschmann J. Rendtel D. Schmidt W. Schmidt M. Sobotka S.K. Solanki D. Soltau J. Staude K.G. Strassmeier R. Volkmer T. Waldmann E. Wiehr A.D. Wittmann M. Woche 《Astronomische Nachrichten》2012,333(9):810-815
In this review, we look back upon the literature, which had the GREGOR solar telescope project as its subject including science cases, telescope subsystems, and post‐focus instruments. The articles date back to the year 2000, when the initial concepts for a new solar telescope on Tenerife were first presented at scientific meetings. This comprehensive bibliography contains literature until the year 2012, i.e., the final stages of commissioning and science verification. Taking stock of the various publications in peer‐reviewed journals and conference proceedings also provides the “historical” context for the reference articles in this special issue of Astronomische Nachrichten/Astronomical Notes (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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AKARI, formerly known as ASTRO-F, is the second Japanese space mission to perform infrared astronomical observations. AKARI was launched on 21 February 2006 (UT) and brought into a sun-synchronous polar orbit at an altitude of 700 km by a JAXA M-V rocket. AKARI has a telescope with a primary-mirror aperture size of 685 mm together with two focal-plane instruments on board: the Infrared Camera (IRC), which covers the spectral range 2–26 μm and the Far-Infrared Surveyor (FIS), which operates in the range 50–180 μm. The telescope mirrors are made of sandwich-type silicon carbide, specially developed for AKARI. The focal-plane instruments and the telescope are cooled by a unique cryogenic system that kept the telescope at 6K for 550 days with 180 l super-fluid liquid Helium (LHe) with the help of mechanical coolers on board. Despite the small telescope size, the cold environment and the state-of-the-art detectors enable very sensitive observations at infrared wavelengths. To take advantage of the characteristics of the sun-synchronous polar orbit, AKARI performed an all-sky survey during the LHe holding period in four far-infrared bands with FIS and two mid-infrared bands with IRC, which surpasses the IRAS survey made in 1983 in sensitivity, spatial resolution, and spectral coverage. AKARI also made over 5,000 pointing observations at given targets in the sky for approximately 10 min each, for deep imaging and spectroscopy from 2 to 180 μm during the LHe holding period. The LHe ran out on 26 August 2007, since which date the telescope and instrument are still kept around 40K by the mechanical cooler on board, and near-infrared imaging and spectroscopic observations with IRC are now being continued in pointing mode. 相似文献
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M. Collados F. Bettonvil L. Cavaller I. Ermolli B. Gelly A. Prez H. Socas‐Navarro D. Soltau R. Volkmer the EST team 《Astronomische Nachrichten》2010,331(6):615-619
In this paper, the present status of the development of the design of the European Solar Telescope is described. The telescope is devised to have the best possible angular resolution and polarimetric performance, maximizing the throughput of the whole system. To that aim, adaptive optics and multi‐conjugate adaptive optics are integrated in the optical path. The system will have the possibility to correct for the diurnal variation of the distance to the turbulence layers, by using several deformable mirrors, conjugated at different heights. The present optical design of the telescope distributes the optical elements along the optical path in such a way that the instrumental polarization induced by the telescope is minimized and independent of the solar elevation and azimuth. This property represents a large advantage for polarimetric measurements. The ensemble of instruments that are planned is also presented (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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望远镜的曝光时间计算器对于远程观测以及不熟悉整个观测系统的观测人员尤为重要,因为它可以帮助观测者制定合理的观测计划。设计并实现了高美古2.4m望远镜系统的曝光时间计算器(exposuretimecalculator,ETC),它可以根据望远镜及其终端设备的参数,通过计算给出待测天体曝光时间的参考值。这为观测者了解现有条件下极限观测能力,设置曝光时间或者是给定星等和曝光时间计算信噪比提供了依据。将ETC计算结果与实际测光标准星的数据进行了比较,结果表明ETC对测光标准星的计算结果是可靠的。 相似文献
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A. K. Tickoo R. Koul S. K. Kaul I. K. Kaul C. L. Bhat N. G. Bhatt M. K. Kothari H. C. Goyal N. K. Agarwal S. R. Kaul 《Experimental Astronomy》1999,9(2):81-101
A PC-based drive-control system has been developed for the altitude-azimuth mounted TACTIC -ray telescope to control the speed and direction of motion of its 2-axes. Details of various hardware components chosen for the telescope, including hybrid-stepper motor, 16-bit absolute encoder and CAMAC-based programmable stepper motor controller, are discussed in this paper. The telescope-control strategy, based on the position-loop with a proportional type control for the source-seek mode and the on/off type control for the tracking mode, is explained in detail. Some important performance features of the telescope, including its blind-spot size, drive-system backlash and encoder-error compensation, are also presented. The drive system has been extensively field-tested and has been operating satisfactorily during observation campaigns carried out since March 1997 with the TACTIC Imaging Element. A tracking accuracy of ±3 arc-minutes has been achieved. A test report of its performance, with regard to its tracking accuracy on the basis of successful detection of TeV -rays from the active galaxy Markarian 501 in April–May 1997, is also presented. 相似文献
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Steven H. Pravdo Richard J. Terrile Christ Ftaclas George D. Gatewood Eugene H. Levy 《Astrophysics and Space Science》1994,212(1-2):433-440
The Astrometric Imaging Telescope (AIT) is a proposed spaceborne observatory whose primary goal is the detection and study of extra-solar planetary systems. It contains two instruments that use complementary techniques to address the goal. The first instrument, the Coronagraphic Imager, takes direct images of nearby stars and Jupiter-size planets. It uses a telescope with scattering-compensated optics and a high-efficiency coronagraph to separate reflected planet light from the central star light. Planet detections take hours; confirmations occur in months. With a program duration of about 2 years, about 50 stars are observed. The second instrument, the Astrometric Photometer, shares the same telescope and focal plane. It uses a Ronchi ruling that is translated across the focal plane to simultaneously measure the positions of each target star and about 25 reference stars with sufficient accuracy to detect Uranus-mass planets around hundreds of stars. Enough stars of several spectral types are observed to obtain a statistically significant measurement of the prevalence of planetary systems. This observing program takes about 10 years to complete. The combination of both instruments in a single telescope system results from a number of innovative solutions that are described in this paper.Paper presented at the Conference onPlanetary Systems: Formation, Evolution, and Detection held 7–10 December, 1992 at CalTech, Pasadena, California, U.S.A. 相似文献
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T. Herbst 《Astrophysics and Space Science》2003,286(1-2):45-53
The Large Binocular Telescope (LBT) will be the largest single telescope in the world when it is completed in 2005. The unique structure of the telescope incorporates two, 8.4 meter diameter primary mirrors on a 14.4 meter center-to-center mounting. This configuration provides the equivalent collecting area of a 12 meter telescope, and when combined coherently, the two optical paths offer very interesting possibilities for interferometry. Two initial interferometric instruments are planned for the LBT. A group based at the University of Arizona is constructing LBTI, a pupil-plane, nulling beam combiner operating in the thermal infrared N band. This instrument will search for and measure zodiacal light in candidate stellar systems for the Terrestrial Planet Finder (TPF) and Darwin missions. Expansion ports can accomodate additional instruments. A second group, based in Heidelberg, Arcetri, and Köln, is building LINC-NIRVANA, a near-infrared Fizeau-mode beam combiner. This type of observation preserves phase information and allows true imagery over a wide field of view. Using state-of-the-art detector arrays, coupled with advanced adaptive optics, LINC-NIRVANA will deliver the sensitivity of a 12 m telescope and the spatial resolution of a 23 m telescope, over a field of view up to 2 arc minutes square. 相似文献
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1m太阳望远镜的方位驱动控制系统采用液压轴承,液压系统正常工作时望远镜才能实现平稳旋转。可通过油压、油温监测液压系统的工作状态。针对原有液压系统不能提供其工作状态实时监测和自动化程度较低的缺陷,设计了液压监控系统并将其集成到望远镜控制系统中,可实现油压油温数据采集、油压异常报警、油泵自动启停等功能,保证液压轴承的安全运转。介绍了该监控系统的结构和工作原理,阐述了油压、油温数据采集系统的软硬件实现并给出了相应的实验数据和运行结果。理论分析和实验结果表明系统工作正常,数据采集速度快、分辨率高,精度可满足要求,能长期稳定运行。 相似文献
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K. -W. Hodapp 《Experimental Astronomy》1994,3(1-4):251-253
The U.S. Air Force Phillips Laboratory will build the 3.63 m Advanced Electro Optical System (AEOS) telescope on Haleakala, Maui. The Institute for Astronomy will participate in this project and will develop astronomical instruments optimized for using the AEOS telescope in survey projects. As part of this instrument development program 1024×1024 HgCdTe near-infrared detector arrays will be developed at the Rockwell International Science Center. 相似文献