Design and Fabrication of a High Light Gathering Power Monochromator

1986 ◽  
Vol 15 (2) ◽  
pp. 54-61
Author(s):  
D. B. Jadhav ◽  
A. D. Tillu
1994 ◽  
Vol 161 ◽  
pp. 101-107
Author(s):  
U. Laux

The desire of astronomers for wide field telescope systems which surpass the RCC (1:8 max. 1.5 degree) in light gathering power and field of view are relative concrete today. For this type of telescope, detectors planned ARE CCDs in multichip arrangement.


Open Physics ◽  
2005 ◽  
Vol 3 (2) ◽  
Author(s):  
Anton Akhsakhalyan ◽  
Aram Akhsakhlyan ◽  
Alexander Kharitonov ◽  
Eugenie Kluenkov ◽  
Vladimir Murav’ev ◽  
...  

AbstractThis paper is an overview of the research activities carried out in the past five years at the Institute for Physics of Microstructures RAS and “X-ray” Company towards the manufacture of multilayer mirror systems capable of forming X-ray beams in the subnanometer range of wavelengths. The systems fabrication technology is presented, including techniques for producing supersmooth surfaces of specified shape, methods of graded multilayer structure deposition on such surfaces, and the principles of designing optimal mirror parameters. The characteristics of a quadrelliptical reflector—a novel high light-gathering power four-corner focusing system—are reported.


1988 ◽  
Vol 132 ◽  
pp. 425-427
Author(s):  
U. Pauls ◽  
N. Grevesse ◽  
M. C. E. Huber

The high resolution and the high light-gathering power of a Fourier–transform spectrometer (FTS) afford the observation of very weak lines in laboratory spectra. Thus it became possible to determine an accurate solar iron abundance from Fe II lines that are weak in the solar spectrum: we measured the branching fractions of a few such lines whose upper levels lifetimes are known.


The results of a study of the Raman spectra of nine aldehydes and of mesitylene are reported and discussed in this paper. Of these substances, only a few, namely, paraldehyde, acetaldehyde and benzaldehyde have been previously investigated by other authors and the rest receive attention for the first time. The experimental arrangements were the same as those described by Wood. Hilger’s quartz. E 2 and a two prism glass spectrograph of high light gathering power were used for studying the spectra. The liquids were mostly Kahlbaum’s or Merck’s extra pure and were further purified by distillation in vacuum before use. Capric, undecylic, and lauric aldehydes were, however, obtained from other sources and were used as received. In the following tables are given the wave-numbers and the intensities of the Raman lines, and the shifts in wave-numbers between them and the exciting lines. In the column ∆ v the letters a, b, c, d, e, f, g, h, k, l and m represent the exciting lines of the mercury spectrum λ A. U. 3650⋅1, 3654⋅8, 3663⋅3, 4046⋅6, 4077⋅8, 4339⋅2, 4347⋅5, 4358⋅3, 5460⋅7, 5769⋅5, 5790⋅5 respectively.


1949 ◽  
Vol 27a (6) ◽  
pp. 231-233 ◽  
Author(s):  
W. Petrie

The optics of the spectrograph consist of two f 2.5, 12 in. aircraft camera lenses, and a 15,000 lines per inch plane grating with ruled surface 4 in. by 4 in. The grating concentrates light in the second order spectrum; the dispersion in this order for normal incidence is 22 Å per mm. A few spectra were obtained during the spring of 1949, and the results appear to be most promising. These spectra include several interesting features, one of which is a strong radiation of wave length 4320 Å in the second order. This radiation is likely to be an intense first order infrared feature.


2003 ◽  
Vol 12 (2) ◽  
Author(s):  
G. Handler

AbstractI have investigated the value of the contribution of small telescopes to the success of a whole WET run. To this end, I have applied different data weighting schemes to two extreme WET test data sets. I find that weights proportional to the inverse local scatter in the light curves produce Fourier Transforms of best signal-to-noise. Weighting data stronger than their inverse scatter does not yield optimal results because of the reduction of the effective number of data points.The contribution of the small telescopes to the combined WET results was found to be very important. They do not only improve the spectral window, but they can reduce the noise in the total FT by more than their light gathering power would imply. Some suggestions for the optimal use of small telescopes in the WET are given.


During the past winter I have continued my studies on the spectrum of the night sky, and the connected subject of the auroral spectrum. The present paper reports the results obtained. The spectrographs used in this work are two of nearly identical construction. In designing them the paramount consideration was to obtain the greatest possible light gathering power, all other considerations being kept subordinate to this. It was accordingly decided to use the minimum number of optical pieces—one prism, one collimating lens, one camera lens, neither of the latter to be achromatic.


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