Aspects of concurrent design during the VISTA IR camera detailed design phase

Caldwell, M.; Whalley, Martin S.; Woodhouse, Guy F.W.; Edeson, Ruben; Burke, Kevin; Lucas, John M.; Shaughnessy, Bryan; Richards, Tony; Ward, Kim; Dalton, Gavin; Leclerc, Mélanie; Gallie, Angus; Clark, Paul

doi:10.1117/12.550907

Cited by 5 publications

(1 citation statement)

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“…The design of the camera is covered by Dalton et al 32,33 , Egan et al 34 , Caldwell et al 35 , Beard et al 36 , and Edeson et al 37 , and Dalton et al 38 report on the camera commissioning at this meeting.…”

Section: Cameramentioning

confidence: 98%

VISTA: status and performance

Emerson

Sutherland

2010

SPIE Proceedings

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VISTA, the Visible and Infrared Survey Telescope for Astronomy, is a 4-m class 1.65-degree wide field near-IR survey telescope with 0.34 arcsec pixels. VISTA was successfully commissioned and has been making surveys since 15 October 2009, and was formally accepted as a part of ESO's Cerro Paranal Observatory on 10 December 2009. We summarise the design and build process, report on commissioning and the as-built status. The most novel aspects of the system design have proved to all work well. We report the measured on-sky system performance that confirms that VISTA works as expected.

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Section: Cameramentioning

confidence: 98%

VISTA: status and performance

Emerson

Sutherland

2010

SPIE Proceedings

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The Mid-Infrared Instrument for theJames Webb Space Telescope, I: Introduction

Rieke¹,

Wright²,

Böker³

et al. 2015

Publications of the Astronomical Society of the Pacific

362

167

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MIRI (the Mid-Infrared Instrument for the James Webb Space Telescope (JWST)) operates from 5 to 28.5 µm and combines over this range: 1.) unprecedented sensitivity levels; 2.) sub-arcsec angular resolution; 3.) freedom from atmospheric interference; 4.) the inherent stability of observing in space; and -3 -5.) a suite of versatile capabilities including imaging, low and medium resolution spectroscopy (with an integral field unit), and coronagraphy. We illustrate the potential uses of this unique combination of capabilities with various science examples: 1.) imaging exoplanets; 2.) transit and eclipse spectroscopy of exoplanets; 3.) probing the first stages of star and planet formation, including identifying bioactive molecules; 4.) determining star formation rates and mass growth as galaxies are assembled; and 5.) characterizing the youngest massive galaxies.

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