The light gathering power of optical systems with an electron optical member

1956 ◽  
Vol 6 (1) ◽  
pp. 21-21
Author(s):  
Antonín Vaško
Keyword(s):  
Optical Systems ◽  
Light Gathering Power ◽  
Light Gathering

High depth-of-field imaging without sacrificing light-gathering power and resolution

1997 ◽  
Author(s):  
Alan R. FitzGerrell ◽  
Edward R. Dowski, Jr.
Keyword(s):  
Depth Of Field ◽  
Light Gathering Power ◽  
Light Gathering ◽  
Field Imaging ◽  
High Depth

Merging Data from Large and Small Telescopes – Good or Bad? And: How Useful is the Application of Statistical Weights to Time-Series Photometric Measurements?

2003 ◽  
Vol 12 (2) ◽  
Author(s):  
G. Handler
Keyword(s):  
Fourier Transforms ◽  
Light Curves ◽  
Data Sets ◽  
Effective Number ◽  
Spectral Window ◽  
Light Gathering Power ◽  
Data Weighting ◽  
Light Gathering ◽  
Data Points ◽  
Photometric Measurements

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.

scholarly journals Wide-Field-Imaging 3-Mirror-Systems by High Light Gathering Power and a Wide-Field Optical System for the ‘Large Imaging Telescope’ (Lite)

1994 ◽  
Vol 161 ◽  
pp. 101-107
Author(s):  
U. Laux
Keyword(s):  
Optical System ◽  
High Light ◽  
Field Of View ◽  
Wide Field ◽  
Light Gathering Power ◽  
Imaging Telescope ◽  
Light Gathering ◽  
Field Imaging ◽  
Wide Field Imaging

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.

scholarly journals Further observations on the spectrum of the night sky

1923 ◽  
Vol 103 (720) ◽  
pp. 45-52 ◽  
Keyword(s):  
Camera Lens ◽  
The Past ◽  
Light Gathering Power ◽  
Identical Construction ◽  
Light Gathering ◽  
Minimum Number ◽  
Night Sky ◽  
Collimating Lens ◽  
Past Winter

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.

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
Keyword(s):  
High Light ◽  
Light Gathering Power ◽  
Light Gathering

scholarly journals Spectral Classification Studies of Cepheids Using a Small Telescope with an Image Tube Spectrograph

1973 ◽  
Vol 50 ◽  
pp. 30-32
Author(s):  
M. F. McCarthy
Keyword(s):  
Optical Design ◽  
Spectral Classification ◽  
Image Tube ◽  
Small Telescope ◽  
Light Gathering Power ◽  
Light Gathering ◽  
Large Telescopes ◽  
Absorption Features ◽  
Design Construction ◽  
Image Intensifiers

Most of the results reported thus far of image tube spectroscopy as applied in astronomy have been concerned with emission features and have been the result of a combination of the largest available light gathering power of large telescopes with the improved sensitivity of image intensifiers. We consider here the application of image tube techniques to moderate sized telescopes; concretely, we describe the first program of spectral classification using absorption features as carried out with the image tube spectrograph of the Vatican Observatory attached to the Zeiss 60-cm reflector at Castel Gandolfo. Treanor (1970) has described the optical design, construction and the first tests of this instrument. The receiver is an RCA cascaded image tube loaned to the Vatican Observatory by the Carnegie Image Tube Committee.

A FABRY-PEROT SPECTROMETER FOR AURORAL AND AIRGLOW OBSERVATIONS

1960 ◽  
Vol 38 (12) ◽  
pp. 1560-1569 ◽  
Author(s):  
G. G. Shepherd
Keyword(s):  
Preliminary Results ◽  
Grating Spectrometer ◽  
Light Gathering Power ◽  
Fabry Perot ◽  
Light Gathering ◽  
Mechanical Scanning ◽  
Low Order

A 1-in. Fabry-Perot interferometric spectrometer employing mechanical scanning has been constructed to operate at low order. Such an instrument gives a resolution similar to that of a grating spectrometer but has, at that resolution, a much higher light gathering power. The spectrometer is capable of resolving the sodium D lines in the twilight airglow, scanning once per minute. Some preliminary results on the variation of D2/D1 ratio during twilight are presented. This type of spectrometer should be useful for a number of other applications.

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