The VISTA IR camera

Dalton, Gavin; Caldwell, M.; Ward, Kim; Whalley, Martin S.; Burke, Kevin; Lucas, John M.; Richards, Tony; Ferlet, Marc; Edeson, Ruben; Tye, Daniel; Shaughnessy, Bryan; Strachan, Mel; Atad-Ettedgui, Eli; Leclerc, Mélanie; Gallie, Angus; Bezawada, Nagaraja; Clark, Paul; Bissonauth, Nirmal; Luke, Peter; Dipper, N. A.; Berry, P.F.; Sutherland, William J.; Emerson, J. P.

doi:10.1117/12.551378

Cited by 12 publications

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“…The quantum efficiency of the CCD and the resulting bandpass of the camera are also plotted. The transmission of the V and I filters used at CTIO [19] are shown for comparison with our camera bandpasses f/1.3 lens which provided a 36°×36°field of view. The actual focal length in the near-IR was measured and found equal to 15.6 mm.…”

Section: Instrumentationmentioning

confidence: 99%

“…More recently, the initial stages in implementing VISTA (Visible and Infrared Survey Telescope for Astronomy) began at the Paranal Observatory. This 4m telescope will perform extensive surveys of the southern skies in the 0.85-2.3 micrometer spectral region [19,20]. Its field of view will be as large as 1.5°×1.0°in order to rapidly cover large areas of the sky and produce monitoring of selected objects.…”

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confidence: 99%

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Near-infrared sky background fluctuations at mid- and low latitudes

et al. 2008

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The emission of the upper atmosphere introduces an additional variable component into observations of astronomical objects in the NIR 700-3,000 nm range. The subtraction of this component is not easy because it varies during the night by as much as 100% and it is not homogeneous over the sky. A program aimed at measuring and understanding the main characteristics of the atmospheric NIR emission was undertaken. A 512×512 CCD camera equipped with a RG780/2 mm filter is used to obtain images of the sky in a 36°×36°field of view. The intensities of a given star and of the nearby region devoid of star in a 439 arcmin 2 area are monitored during periods of time of several hours. The sky intensity measured in the 754-900 nm bandpass, reduced to zenith and zero airmass is comprised between mag20 and mag18.5 per arcsecond 2 . A diminution by a factor of two during the night is frequently observed. Intensity fluctuations having an amplitude of 15% and periods of 5-40 min are present in the images with a structure of regularly spaced stripes. The fluctuations of the NIR sky background intensity are due to (1) the chemical evolution of the upper atmosphere composition during the night and (2) dynamical processes such as tides with periods of 3-6 h or gravity waves with periods of several tens of minutes. We suggest that a monitoring of the sky background intensity could be set up when quantitative observations of astronomical objects require exposure times longer than~10 min. The publication is illustrated with several video films accessible on the web site http://www.obs-besancon.fr/ nirsky/. Enter username: nirsky and password: skynir.

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Section: Instrumentationmentioning

confidence: 99%

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confidence: 99%

Near-infrared sky background fluctuations at mid- and low latitudes

et al. 2008

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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: 97%

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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“…This paper gives an overview of the requirements and design approach adopted for the VDFS, and is accompanied by two more detailed papers focussing on the (most immediate) case of WFCAM data, one by Irwin et al 1 on the pipeline processing, and one by Hambly et al 2 focussing on the science archive. 3 and VISTA are given elsewhere 4,5,6 .…”

Section: Introductionmentioning

confidence: 99%

VISTA data flow system: overview

et al. 2004

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Data from the two IR survey cameras WFCAM (at UKIRT in the northern hemisphere) and VISTA (at ESO in the southern hemisphere) can arrive at rates approaching 1.4 TB/night for of order 10 years. Handling the data rates on a nightly basis, and the volumes of survey data accumulated over time each present new challenges. The approach adopted by the UK's VISTA Data Flow System (for WFCAM & VISTA data) is outlined, emphasizing how the design will meet the end-to-end requirements of the system, from on-site monitoring of the quality of the data acquired, removal of instrumental artefacts, astrometric and photometric calibration, to accessibility of curated and user-specified data products in the context of the Virtual Observatory. Accompanying papers by Irwin et al 1 and Hambly et al 2 detail the design of the pipeline and science archive aspects of the project.

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The VISTA IR camera

Cited by 12 publications

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Near-infrared sky background fluctuations at mid- and low latitudes

Near-infrared sky background fluctuations at mid- and low latitudes

VISTA: status and performance

VISTA data flow system: overview

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