The secondary mirror concept for the European Extremely Large Telescope

2014 ◽  
Author(s):  
Michael Mueller ◽  
Marc Cayrel ◽  
Henri Bonnet ◽  
Emanuela Ciattaglia ◽  
Michael Esselborn ◽  
...  
Keyword(s):  
Large Telescope ◽  
Secondary Mirror

Method for optimizing the errors of the wavefront of recorded radiation for large-size information-measuring optical systems

2021 ◽  
pp. 57-61
Author(s):  
Victor V. Sychev ◽  
Andrey I. Klem
Keyword(s):  
Traditional Method ◽  
Optimization Problem ◽  
Optical Systems ◽  
Field Variation ◽  
Large Telescope ◽  
Size Information ◽  
Image Field ◽  
Advantages And Disadvantages ◽  
Large Size ◽  
Secondary Mirror

The article proposes a new method for increasing the information content of the image by minimizing the errors of the optical system of a large telescope using the redistribution of errors over the image field. Variation of the parameters of the secondary mirror is carried out to solve the optimization problem of uniform distribution of aberrations over the image field of a large telescope using the example of a cryotelescope with a diameter of 12 m in the Zemax-EE package. The results of calculations of optical schemes by the traditional method and by the method of optimization of the errors of the radiation wavefront are presented. The advantages and disadvantages are considered.

scholarly journals Mirror Compensator for Testing Convex Secondary

1984 ◽  
Vol 79 ◽  
pp. 131-133
Author(s):  
Pan Junhua
Keyword(s):  
West Germany ◽  
Large Telescope ◽  
Secondary Mirror ◽  
The Matrix ◽  
Convex Mirror

The testing of convex secondary mirror of large telescope is known as a difficault thing, because it needs for a large mirror or lens. In USA, they used to use Hindle sphere for testing convex hyperboloids, and in West Germany as I know, they often use concave matrix probe for testing convex mirrors. In the case of Hindle method, the diameter of testing sphere always is about 2 or 3 times as the convex mirror under testing, in the later case, the matrix probe must has the same size as the convex mirror, further more, the probe itself needs another testing facilities. Some other methods had been suggested by R. Wilson, E, Gaviola and others but they have rarely been used in practice.

B. Large Telescope Engineering Operations

1966 ◽  
Vol 27 ◽  
pp. 200-209
Keyword(s):  
Large Telescope ◽  
Advance Planning

Whitford : The next phase of the program has to do with advance planning of the instruments themselves, to make the logistics of operation simple and foolproof. I call first on Mr Rule to speak on ‘thinking ahead’.

scholarly journals Control oriented modelling and modal analysis of the deformable mirror M4 of the extremely large telescope

2021 ◽  
Vol 27 (1) ◽  
pp. 295-321
Author(s):  
Philip L. Neureuther ◽  
Kevin Schmidt ◽  
Thomas Bertram ◽  
Oliver Sawodny
Keyword(s):  
Modal Analysis ◽  
Deformable Mirror ◽  
Large Telescope

scholarly journals Successful application of PSF-R techniques to the case of the globular cluster NGC 6121 (M 4)

2020 ◽  
Vol 634 ◽  
pp. L5 ◽  
Author(s):  
D. Massari ◽  
A. Marasco ◽  
O. Beltramo-Martin ◽  
J. Milli ◽  
G. Fiorentino ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Globular Cluster ◽  
Hybrid Technique ◽  
Large Telescope ◽  
Point Spread ◽  
Accurate Knowledge ◽  
Viable Solution ◽  
Spread Function ◽  
Astronomical Images ◽  
Proper Analysis

Context. Precise photometric and astrometric measurements on astronomical images require an accurate knowledge of the point spread function (PSF). When the PSF cannot be modelled directly from the image, PSF-reconstruction techniques become the only viable solution. So far, however, their performance on real observations has rarely been quantified. Aims. In this Letter, we test the performance of a novel hybrid technique, called PRIME, on Adaptive Optics-assisted SPHERE/ZIMPOL observations of the Galactic globular cluster NGC 6121. Methods. PRIME couples PSF-reconstruction techniques, based on control-loop data and direct image fitting performed on the only bright point-like source available in the field of view of the ZIMPOL exposures, with the aim of building the PSF model. Results. By exploiting this model, the magnitudes and positions of the stars in the field can be measured with an unprecedented precision, which surpasses that obtained by more standard methods by at least a factor of four for on-axis stars and by up to a factor of two on fainter, off-axis stars. Conclusions. Our results demonstrate the power of PRIME in recovering precise magnitudes and positions when the information directly coming from astronomical images is limited to only a few point-like sources and, thus, paving the way for a proper analysis of future Extremely Large Telescope observations of sparse stellar fields or individual extragalactic objects.

Science with the re-baselined European Extremely Large Telescope

2012 ◽  
Author(s):  
J. Liske ◽  
P. Padovani ◽  
M. Kissler-Patig
Keyword(s):  
Large Telescope
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