Aluminum mirror coatings for UVOIR telescope optics including the far UV

2015 ◽  
Author(s):  
Kunjithapatham Balasubramanian ◽  
John Hennessy ◽  
Nasrat Raouf ◽  
Shouleh Nikzad ◽  
Michael Ayala ◽  
...  
Keyword(s):  
Telescope Optics ◽  
Aluminum Mirror

scholarly journals Polarization calibration techniques and scheduling for the Daniel K. Inouye Solar Telescope

2014 ◽  
Vol 10 (S305) ◽  
pp. 102-107
Author(s):  
David F. Elmore
Keyword(s):  
Advanced Technology ◽  
Optical Coatings ◽  
Calibration Error ◽  
Solar Telescope ◽  
Critical Importance ◽  
Common Path ◽  
Solar Research ◽  
Telescope Optics ◽  
The Individual ◽  
Calibration Techniques

AbstractThe Daniel K. Inouye Solar Telescope (DKIST), formerly Advanced Technology Solar Telescope when it begins operation in 2019 will be by a significant margin Earth's largest solar research telescope. Science priorities dictate an initial suite of instruments that includes four spectro-polarimeters. Accurate polarization calibration of the individual instruments and of the telescope optics shared by those instruments is of critical importance. The telescope and instruments have been examined end-to-end for sources of polarization calibration error, allowable contributions from each of the sources quantified, and techniques identified for calibrating each of the contributors. Efficient use of telescope observing time leads to a requirement of sharing polarization calibrations of common path telescope components among the spectro-polarimeters and for those calibrations to be repeated only as often as dictated by degradation of optical coatings and instrument reconfigurations. As a consequence the polarization calibration of the DKIST is a facility function that requires facility wide techniques.

scholarly journals EUSO-SPB2 Telescope Optics and Testing

2021 ◽  
Author(s):  
Viktoria Kungel ◽  
"Randy Bachman" ◽  
"Jerod Brewster" ◽  
"Madeline Dawes" ◽  
"Julianna Desiato" ◽  
...  
Keyword(s):  
Telescope Optics

Thermal shaping of thin glass panels for hard X-ray telescope optics

2019 ◽  
Vol 40 (3) ◽  
Author(s):  
Vinita Navalkar ◽  
Kulinder PAL Singh ◽  
Mehernosh Press
Keyword(s):  
Thin Glass ◽  
X Ray ◽  
Glass Panels ◽  
Telescope Optics

scholarly journals Stellar Positions from CCD Images

1995 ◽  
Vol 167 ◽  
pp. 349-350
Author(s):  
A. R. Upgren ◽  
C. Abad ◽  
J. Stock
Keyword(s):  
Focal Length ◽  
Visual Image ◽  
Small Field ◽  
Yellow Filter ◽  
Perfect Adaptation ◽  
Ccd Detector ◽  
Focus Image ◽  
Telescope Optics ◽  
Blue Spectral Region ◽  
Double Cluster

The CIDA visual refractor of 65-cm aperture and focal length 10.5 m, has been used extensively for position determinations on photographic plates. The combination of Kodak D plates and a yellow filter permit an almost perfect adaptation to the focal curve of the telescope. It appeared of interest to test whether the telescope could be used for astrometric purposes with a CCD detector. As is well known, the spectral sensitivity of these detectors extends well into the infrared where the images formed by the telescope optics will be far out of focus. The blue spectral region where this would also be the case can easily be cut off by a yellow filter. There are no filters which would produce a similarly sharp cut-off towards the red region. On the other hand, given the small field covered by a CCD, the displacement of the red out-of-focus image with respect to the center of the visual image might be negligible. Recently obtained accurate positions in the area of the Perseus Double Cluster made this field suitable for the test of this possibility.

scholarly journals ECE Diagnostic for the initial Operation of Wendelstein 7-X

2019 ◽  
Vol 203 ◽  
pp. 03007 ◽  
Author(s):  
Matthias Hirsch ◽  
Udo Höfel ◽  
Johan Willem Oosterbeek ◽  
Neha Chaudhary ◽  
Joachim Geiger ◽  
...  
Keyword(s):  
Noise Source ◽  
Michelson Interferometer ◽  
Frequency Resolution ◽  
Line Of Sight ◽  
Initial Operation ◽  
Cold Source ◽  
Mode Of Operation ◽  
Standard Mode ◽  
Telescope Optics

The ECE diagnostic at W7-X in its standard mode of operation measures in X2 mode polarization with a 32 channel radiometer in the frequency band around 140 GHz for central magnetic field 2.5T. The radiometer is calibrated by a noise source and the overall system absolutely calibrated by means of a hot-cold source placed outside the torus in front of a Gaussian telescope optics with identical geometry and transmission line as it is installed for the measurements in the plasma vessel. The system is supplemented with a 16 channel zoom device with 4 GHz span for higher frequency resolution at a suitable radial range and a Michelson interferometer for the characterization of higher harmonics sharing the same line of sight.

scholarly journals Corrected GSC: Reference catalogue for CCD observations. Now

1996 ◽  
Vol 172 ◽  
pp. 483-486
Author(s):  
A. Lopez Garcia ◽  
L.I. Yagudin
Keyword(s):  
Hubble Space Telescope ◽  
Systematic Errors ◽  
Reduction Model ◽  
Adjustment Procedure ◽  
Star Catalogue ◽  
Accuracy Level ◽  
Ccd Observations ◽  
Telescope Optics ◽  
Guide Star ◽  
Dependent Error

Astrometrical properties of the Hubble Space Telescope Guide Star Catalogue (GSC) were recently investigated by the same authors through its comparison with the PPM catalogue. In this paper, a new systematic plate-based magnitude dependent error produced by telescope optics and by the incompleteness of plate reduction model has been found after applying a simplified block adjustment procedure. New subroutine for correction of all systematic errors is developed and GSC can be used now as a dense reference catalogue on about 0.4″ accuracy level.

scholarly journals Expected performances of the Characterising Exoplanet Satellite (CHEOPS)

2020 ◽  
Vol 635 ◽  
pp. A23 ◽  
Author(s):  
D. Futyan ◽  
A. Fortier ◽  
M. Beck ◽  
D. Ehrenreich ◽  
A. Bekkelien ◽  
...  
Keyword(s):  
Time Series ◽  
Orbital Period ◽  
Satellite Orbit ◽  
Web Based ◽  
Telescope Optics ◽  
Exoplanetary Atmospheres ◽  
Design Options ◽  
Simulated Images ◽  
Spectroscopic Characterisation

Context. The CHaracterising ExOPlanet Satellite (CHEOPS) is a mission dedicated to the search for exoplanetary transits through high precision photometry of bright stars already known to host planets. The telescope will provide the unique capability of determining accurate radii for planets whose masses have already been measured from ground-based spectroscopic surveys. This will allow a first-order characterisation of the planets’ internal structure through the determination of the bulk density, providing direct insight into their composition. By identifying transiting exoplanets with high potential for in-depth characterisation, CHEOPS will also provide prime targets for future instruments suited to the spectroscopic characterisation of exoplanetary atmospheres. Aims. The CHEOPS simulator has been developed to perform detailed simulations of the data which is to be received from the CHEOPS satellite. It generates accurately simulated images that can be used to explore design options and to test the on-ground data processing, in particular, the pipeline producing the photometric time series. It is, thus, a critical tool for estimating the photometric performance expected in flight and to guide photometric analysis. It can be used to prepare observations, consolidate the noise budget, and asses the performance of CHEOPS in realistic astrophysical fields that are difficult to reproduce in the laboratory. Methods. The simulator has been implemented as a highly configurable tool called CHEOPSim, with a web-based user interface. Images generated by CHEOPSim take account of many detailed effects, including variations of the incident signal flux and backgrounds, and detailed modelling of the satellite orbit, pointing jitter and telescope optics, as well as the CCD response, noise and readout. Results. The simulator results presented in this paper have been used in the context of validating the data reduction processing chain, in which image time series generated by CHEOPSim were used to generate light curves for simulated planetary transits across real and simulated targets. Independent analysts were successfully able to detect the planets and measure their radii to an accuracy within the science requirements of the mission: for an Earth-sized planet with an orbital period of 50 days orbiting a Sun-like target with magnitude V = 6, the median measured value of the planet to star radius ratio, Rp/Rs, was 0.00923 ± 0.00054(stat) ± 0.00019(syst), compared to a true input value of 0.00916. For a Neptune-sized planet with an orbital period of 13 days orbiting a target with spectral type K5V and magnitude V = 12, the median measured value of Rp/Rs was 0.05038 ± 0.00061(stat) ± 0.00031(syst), compared to a true input value of 0.05.

Telescope Optics

2003 ◽  
pp. 31-59
Author(s):  
Chris Kitchin
Keyword(s):  
Telescope Optics
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