Atmospheric dispersion correctors at the Cassegrain focus

Wynne, C. G.; Worswick, S. P.

doi:10.1093/mnras/220.3.657

Cited by 36 publications

(17 citation statements)

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“…1). At the focus of a telescope, this will produce a linear dispersion with a well defined direction (Wynne & Worswick 1986). For simplification purposes but with no loss of generality, we will assume that this displacement is along the x-axis of the guiding camera, while the displacement along the y-axis will remain constant.…”

Section: Star and Fiber Simulationsmentioning

confidence: 99%

The impact of atmospheric dispersion in the performance of high-resolution spectrographs

Wehbé

Cabral

Martins

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Differential atmospheric dispersion is a wavelength-dependent effect introduced by the atmosphere. It is one of the instrumental errors that can affect the position of the target as perceived on the sky and its flux distribution. This effect will affect the results of astronomical observations if not corrected by an atmospheric dispersion corrector (ADC). In high-resolution spectrographs, in order to reach a radial velocity (RV) precision of 10 cm/s, an ADC is expected to return residuals at only a few tens of milli-arcseconds (mas). In fact, current state-of-the-art spectrographs conservatively require this level of residuals, although no work has been done to quantify the impact of atmospheric dispersion. In this work we test the effect of atmospheric dispersion on astronomical observations in general, and in particular on RV precision degradation and flux losses. Our scientific objective was to quantify the amount of residuals needed to fulfil the requirements set on an ADC during the design phase. We found that up to a dispersion of 100 mas, the effect on the RV is negligible. However, on the flux losses, such a dispersion can create a loss of ∼2% at 380 nm, a significant value when efficiency is critical. The requirements set on ADC residuals should take into consideration the atmospheric conditions where the ADC will function, and also all the aspects related with not only the RV precision requirements but also the guiding camera used, the tolerances on the flux loss, and the different melt data of the chosen glasses.

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Section: Star and Fiber Simulationsmentioning

confidence: 99%

The impact of atmospheric dispersion in the performance of high-resolution spectrographs

Wehbé

Cabral

Martins

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Among the many types of ADC designs, the rotating double Amici prism design is most widely used in astronomy. 29,30 Design. As shown in Fig.…”

Section: Atmospheric Dispersion Correctormentioning

confidence: 99%

Design and development of an adaptive optics system in visible and near-infrared for Inter-University Centre for Astronomy and Astrophysics 2-meter telescope

Paul

Das

Ramaprakash

et al. 2019

J. Astron. Telesc. Instrum. Syst.

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Robo-AO is the first robotic autonomous laser-guided adaptive optics (AO) system operating in the sky. It is a very economical AO system especially suitable for observations with 1-to 3-m class telescopes. A second Robo-AO system, which works both in the visible and near-infrared wavelengths, has been developed to improve the image quality of the 2-m diameter telescope at Inter-university Centre for Astronomy and Astrophysics Girawali Observatory in India. We present the optomechanical design and development of the Laser Guide Star Facility (LGSF) and the Cassegrain AO facility with various test results. Effects of different projection geometries of the LGSF have been discussed with modeling results. Comprehensive study of an atmospheric dispersion corrector with dispersion model and development of a generic software are elaborated with experimental results. Toward the end, AO loop test results in the presence of artificial turbulence generated in the laboratory are presented.

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“…The aberration study of such prisms in a converging beam is studied by Wynne and Worswick. 36 In the meantime, the aligning strategy will focus on a short waveband centered at 889 nm due to a narrowband methane filter. The differential refraction between the reference targeting and scientific wavelengths of interest can be evaluated with the help of atmospheric dispersion models.…”

Section: Optical Designmentioning

confidence: 99%

Conception of a near-infrared spectrometer for ground-based observations of massive stars

Kintziger

Desselle

Loicq

et al. 2017

J. Astron. Telesc. Instrum. Syst

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Conception of a nearinfrared spectrometer for ground-based observations of massive stars," J. Abstract. In our contribution, we outline the different steps in the design of a fiber-fed spectrographic instrument for stellar astrophysics. Starting from the derivation of theoretical relationships from the scientific requirements and telescope characteristics, the entire optical design of the spectrograph is presented. Specific optical elements, such as a toroidal lens, are introduced to improve the instrument's efficiency. Then the verification of predicted optical performances is investigated through optical analyses, such as resolution checking. Eventually, the star positioning system onto the central fiber core is explained.

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Atmospheric dispersion correctors at the Cassegrain focus

Cited by 36 publications

References 0 publications

The impact of atmospheric dispersion in the performance of high-resolution spectrographs

The impact of atmospheric dispersion in the performance of high-resolution spectrographs

Design and development of an adaptive optics system in visible and near-infrared for Inter-University Centre for Astronomy and Astrophysics 2-meter telescope

Conception of a near-infrared spectrometer for ground-based observations of massive stars

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