共查询到20条相似文献，搜索用时 46 毫秒
1.
We describe the SCORPIO focal reducer that has been used since the fall of 2000 for observations on the 6-m Special Astrophysical Observatory telescope. We give parameters of the instrument in various observing modes (direct imaging, long-slit and multislit spectroscopy, spectropolarimetry, Fabry-Perot panoramic spectroscopy). Observations of various astronomical objects are used as examples to demonstrate the SCORPIO capabilities. 相似文献
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M. Balcells 《Astrophysics and Space Science》1998,263(1-4):361-364
EMIR is a near-infrared (NIR) multi-object spectrograph (MOS) proposed for first-generation common user instrument of the
Gran Telescopio Canarias GTC. It has three observing modes: imaging, multiobject spectroscopy and integral-field spectroscopy,
in the NIR Z, J, H and K bands. The design uses cryogenic multislit masks to allow simultaneous spectroscopy of up to approximately
50 objects. The spectral resolution R=5000 allows for effective "see through" the OH line forest that dominates the J and
H sky backgrounds. EMIR addresses one of the fundamental goals of large telescopes, the spectroscopy of large quantities of
faint sources. Science applications include young stellar objects embedded in molecular clouds, brown dwarfs, stellar clusters,
resolved population in external galaxies and distant galaxies. EMIR is being designed by a consortium of Spanish, UK and French
Institutes. Project updates and information will be posted at http://www.ucm.es/info/emir/.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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A. Quirrenbach J. Larkin M. Barczys T. Gasaway C. Iserlohe A. Krabbe M. McElwain I. Song J. Weiss S. Wright 《New Astronomy Reviews》2006,49(10-12):639
OSIRIS (OH-Suppressing Infra-Red Integral-field Spectrograph) is a new facility instrument for the Keck Observatory. After seeing first light in February 2005, OSIRIS is currently undergoing commissioning. OSIRIS provides the capability of performing three-dimensional spectroscopy in the near-infrared z, J, H, and K bands at the resolution limit of the Keck II telescope, which is equipped with adaptive optics and a laser guide star. The science case for OSIRIS is summarized, and the instrument and associated data reduction software are described. 相似文献
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Tobias Feger Michael J. Ireland Christian Schwab Joao Bento Carlos Bacigalupo David W. Coutts 《Experimental Astronomy》2016,42(3):285-300
We present RHEA, a compact and inexpensive single-mode spectrograph which is built to exploit the capabilities of modest-sized telescopes in an economic way. The instrument is fed by up to seven optical waveguides with the aim of achieving an efficient and modal-noise-free unit, suitable for attaining extreme Doppler precision. The cross-dispersed layout features a wavelength coverage from 430–650 nm, with spectral resolution of R ～75,000. When coupled to small telescopes using fast tip/tilt control, our instrument is well-suited to sensitive spectroscopy. Example science cases are accurate radial velocity studies of low to intermediate-mass giant stars with the purpose of searching for giant plants and using asteroseismology to simultaneously measure the host star parameters. In this paper we describe the final instrument design and present first results from testing the internal stability. 相似文献
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A magnetograph is an instrument which makes measurement of solar magnetic field by measuring Zeeman induced polarization in
solar spectral lines. In a typical filter based magnetograph there are three main modules namely, polarimeter, narrow-band
spectrometer (filter), and imager(CCD camera). For a successful operation of magnetograph it is essential that these modules
work in synchronization with each other. Here, we describe the design of instrument control system implemented for the Solar
Vector Magnetograph under development at Udaipur Solar Observatory. The control software is written in Visual Basic and exploits
the Component Object Model (COM) components for a fast and flexible application development. The user can interact with the
instrument modules through a Graphical User Interface (GUI) and can program the sequence of magnetograph operations. The integration
of Interactive Data Language (IDL) ActiveX components in the interface provides a powerful tool for online visualization,
analysis and processing of images. 相似文献
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介绍了最新的虚拟仪器开发平台LABVIEW的特点及应用 ,提出了利用LABVIEW实现低频时码信号的采集与显示的一种设计方法。该设计采用了软件设计技术 ,大大降低了测试设备系统的成本 ,并对于低频时码信号的分析与处理具有了更大灵活性。 相似文献
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Jordi Cepa 《Astrophysics and Space Science》1998,263(1-4):369-372
The characteristics of OSIRIS (Optical System for Imaging and low-Resolution Integrated Spectroscopy), an instrument for imaging
and low resolution spectroscopy proposed for the GTC 10m telescope, are described. OSIRIS is a multi-purpose instrument that
incorporates in a "classical design" several innovations, already tested in 4m-class telescopes, that will provide a powerful
first light instrument for the GTC.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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光电测微器是中－丹水平子午环最关键的部分．本文介绍了数据采集系统的设计思想．根据长期对仪器的测试和观测结果分析，表明系统完全达到设计要求，同时为下一步改装成ＣＣＤ终端，观测极限星等达１７ｍ．５提供了可行的方案． 相似文献
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Using the line profiles of [Fe x] 6374 å and [Fe XIV] 5303 å emission lines observed during five total solar eclipses, we address the problem whether the solar corona is static or contains moving features. Many of the profiles of both emission lines have complicated shapes, which we interpret as an evidence for the existence of many, small, moving features in the corona. The line-of-sight velocities observed by other investigators (e.g. Desai, Chandrasekhar & Angreji 1982) also support this view. On the other hand, about 15 recent interferometric and multislit investigations of coronal emission lines have not shown evidence of moving elements. We suggest that this is due to insufficient spatial resolution. 相似文献
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HERMES, a fibre‐fed high‐resolution (R = 85000) échelle spectrograph with good stability and excellent throughput, is the work‐horse instrument of the 1.2‐m Mercator telescope on La Palma. HERMES targets building up time series of high‐quality data of variable stellar phenomena, mainly for asteroseismology and binary‐evolution research. In this paper we present the HERMES project and discuss the instrument design, performance, and a future upgrade. We also present some results of the first four years of HERMES observations. We illustrate the value of small telescopes, equipped with efficient instrumentation, for high‐resolution spectroscopy. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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Remko Stuik Roland Bacon Ralf Conzelmann Bernard Delabre Enrico Fedrigo Norbert Hubin Miska Le Louarn Stefan Strbele 《New Astronomy Reviews》2006,49(10-12):618
MUSE, the Multi-Unit Spectroscopic Explorer, is an adaptive optics (AO)-assisted Integral Field Spectrograph, currently in the Preliminary Design Phase as a second generation instrument for the VLT. MUSE will feature two modes, each with an associated AO mode. The first mode is the wide field mode, mainly aiming at the study of high redshift galaxies. For this mode, the AO system has to deliver an improvement of at least a factor of two over the full 1′ × 1′ field of view. The second mode, the narrow field mode, aims at the high-resolution spectroscopy of nearby extended objects, for example, galaxies and globular clusters. For this mode, the AO system will have to deliver near-diffraction limited performance over a small field of view. In this paper, we discuss the trade-offs in the current design of GALACSI – the MUSE AO system – and illustrate with a number of simulations the expected performance in the wide- and narrow field modes. 相似文献
17.
R. J. García López 《Astrophysics and Space Science》1998,263(1-4):365-368
ODIN is an international consortium constituted to design and build a first-light multi-purpose optical intermediate dispersion
spectrograph for the Gran Telescopio Canarias (GTC, 10-m) to be installed at the Observatorio del Roque de los Muchachos (La
Palma). This instrument should fulfill an important fraction of the needs of the Spanish astronomical community in optical
spectroscopy performed at large telescopes, and must be highly competitive in a variety of research fields. We are proposing
a spectrograph that will be capable of providing multi-object observations by means of optical fibers, integral field spectroscopy,
and also multi-integral fields. It will be mounted at the Nasmyth focus of the GTC. One of the main drivers of our proposal
is to cover the whole visible range allowed by the atmospheric cut-off with the highest efficiency, particularly at the UV
end.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
18.
《天文和天体物理学研究(英文版)》2015,(6)
As a facility used for astronomical research, the Lijiang 2.4-m telescope of Yunnan Astronomical Observatories, requires the ability to change one auxiliary instrument with another in as short a time as possible. This arises from the need to quickly respond to scientific programs(e.g. transient observation, time domain studies) and changes in observation conditions(e.g. seeing and weather conditions). In this paper, we describe the design, construction and test of hardware and software in the rapid instrument exchange system(RIES) for the Cassegrain focal station of this telescope, which enables instruments to be quickly changed at night without much loss of observing time. Tests in the laboratory and at the telescope show that the image quality and pointing accuracy of RIES are satisfactory.With RIES, we observed the same Landolt standard stars almost at the same time with the Princeton Instruments VersA rray 1300 B Camera(PICCD) and the Yunnan Faint Object Spectrograph and Camera(YFOSC), while both were mounted at the Cassegrain focus. A quasi-simultaneous comparison shows that the image quality of the optical system inside the YFOSC is comparable with that provided by the PICCD. 相似文献
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P. Felenbok J. Guérin R. Bellenger M. Dreux A. Fernandez 《Astrophysics and Space Science》1990,171(1-2):297-300
We are presenting a multi-object instrument for spectrography in a large field. It is of the arm design as MX or ARGUS. The MEFOS (Meudon-ESO Fiber Optical System) version is built to be used at the ESO 3.60 m prime focus with the triplet corrector. The FIFI (Franco-Italian Fiber Instrument) version, a copy of MEFOS, is shared between the Bologna Observatory and the Paris-Meudon Observatory and will be used, on a visitor basis, at the CFHT prime focus. The instrument carries 30 independent arms with an imaging capability on each arm. It is a modular design with its electronic implemented on each arm. The system is under control of anti-collision software and the whole instrument is driven by an PC/XT-type computer.Paper presented at the 11th European Regional Astronomical Meetings of the IAU on New Windows to the Universe, held 3–8 July, 1989, Tenerife, Canary Islands, Spain. 相似文献