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Olivier Thizy Christian Buil François Cochard Coralie Neiner 《Planetary and Space Science》2008,56(14):1878-1881
Amateur spectroscopists are getting organized to contribute to professional astronomy work. We present here the work done within the AUDE association to design, manufacture and distribute the Lhires III high-resolution Littrow spectrograph, which fits usual amateur telescopes and CCD cameras. We also review how the communication is organized through the ARAS distribution list (Spectro-L), forums, and workshops to develop and promote spectroscopic work among amateurs. Last but not least, we introduce the Be stars spectra (BeSS) Virtual Observatory-compatible database and its use for the monitoring of Be stars in association with the COROT satellite. 相似文献
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The impulsive phase of the 23 July 2002 2B/X4.8 proton flare with a classical two-ribbon structure was observed with the Irkutsk
Large Solar Vacuum Telescope (LSVT) in spectropolarimetric mode, with high spatial, spectral, and time resolution. On the
basis of 49 spectrograms and 1200 spectral cuts across the flare ribbons, evidence for Hα line impact polarization has been obtained. A systematic change of the Stokes Q and U parameters has been detected across the ribbons for different flare regions measured with a scanning step of 0.85″. In the
eastern side of the ribbons, the degree of polarization is 4 – 8%; its plane is oriented toward the solar disk center (radial
direction). In the western side, the polarization degree runs up to 25%, and its plane is perpendicular to the disk center
direction (tangential direction). A comparison of these results with hard X-ray data (RHESSI) allows us to conclude that high-energy
electron beams reached the chromosphere during this flare. The observed changes of the direction of polarization and the vanishing
polarization within the ribbons mean that, at the chromospheric level, the energy of electrons remaining in the beam is about
200 eV. A shift of the peak position of polarization relative to the intensity maximum in the ribbons may result from the
inclination of the electron beam axis with respect to the solar surface. 相似文献
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We describe a design for a compact cooled spectrograph which incorporates two cameras and two collimators to achieve high throughput from 0.8 to 2.5m. The spectrograph utilizes multiple NICMOS 3 arrays, specially mounted to minimize their separation in the spectral dimension. This accommodates the broad wavelength range while providing extensive coverage in the spatial dimension. 相似文献
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The WIYN 3.5-meter telescope and its Multi-Object Spectrograph (MOS) have been used to obtain simultaneous spectra at many points in the coma of Comet Hale-Bopp. Between 1996 October and 1997 April in excess of 7500 individual spectra were obtained, typically 96 at a time. On six nights the “Hydra” fiber positioner was used to sample a ring pattern of points about the nucleus with a minimum spacing of 40 arc seconds and a maximum radius of 22.5 arc minutes. On four nights a new “Densepak” fiber cable was used. In this configuration a 7 × 13 rectangular pattern of 91, 3 arc second fibers on 4 arc second centers was used. In most cases the bench spectrograph was used in the echelle mode with an interference filter to isolate a single order. The wavelength range from 6100 Å to 6400 Å was recorded with resolution of approximately 15,000. This spectral region contains the emission features of [OI], C2, NH2and H2O+. From this mass of data we are beginning to extract the radial, azimuthal and temporal variations of many different spectral features. The radial profiles of [O I] λ6300 Å and NH2 are reasonably well representable by the Haser model formalism, that of H2O+ is not. 相似文献
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R. Foy A. Baranne C Bentolila A. Blazit F.-C Foy R. Leblondet D. Revest F. Tlévenin E. Thiébaut Ch. Thorn 《Experimental Astronomy》1994,5(3-4):329-354
We describe the multislit spectrograph SFM. It is designed to obtain simultaneously spectrograms of faint objects over a field of 10 arcminutes for an entrance aperture ratio f/10, or of 15 arcmin for f/8. The SFM makes the dispersed image of the entrance slits directly, without any fiber optics. The number of entrance slits can be as large as a few hundreds, depending on the distribution of the sources on the sky and on the wavelength range. The present reciprocal dispersion is 79Åmm–1 in the wavelength range 3600 – 6400Å. The SFM is expected to reachm
v22 with a signal to noise ratio of 10 for a spectral resolution of 3.3Å and an integration time of 5 hours, when used with the photon counting detector CP40.Radial velocities can be measured either by using calibration spectrograms or by the objective prism technique.The mask of entrance slits is made photochemically from a plate previously recorded of the field to be observed, taken during the same observing run. The auxiliary equipment Mascograph, specially designed for this purpose, is described.First spectrograms in the field of M15 obtained with the SFM using the Calar-Alto 3.50m telescope are presented.Based on observations collected at the Calar-Alto 3.5m telescope, operated by the German MPIfA (Heidelberg), and at the 3.60m CFHT, operated jointly by the Canadian SRC, the French CNRS and the University of Hawaii 相似文献
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讨论了如何将SOPC技术用于大天区多目标光纤光谱天文望远镜(LAMOST)项目的低分辨率光谱仪IP控制核的设计,并在NIOSⅡ软核基础上设计实现了光谱仪IP控制核。整个IP控制核主要分为底层电机控制单元和通信单元两部分。通过工业以太网,远程控制计算机可以方便地控制低分辨率光谱仪,使其完成指定动作。也可以从本地控制计算机上实行控制。设计中采用将步进电机控制器封装成IP再复用的方法,大大缩短了研发时间,减少错误的发生。通信控制中串口通信和以太网可以互为冗余,保证了通信的顺利进行。 相似文献