Final published version including significant revisions. Twenty four pages, fourteen figures. Original version April 2006; final version published in MNRAS August 2007

/pdf/the-ukirt-infrared-deep-sky-survey-ukidss-3x4ktxmdiw.pdf

The UKIRT Infrared Deep Sky Survey (UKIDSS)

With digital equipment becoming increasingly networked, either on wired or wireless networks, for personal and professional use alike, distributed software systems have become a crucial element in information and communications technologies. The study of these systems forms the core of the ARLES' work, which is specifically concerned with defining new system software architectures, based on the use of emerging networking technologies. In this context, we concentrate on the study of distributed systems which bring to life the vision of ubiquitous computing systems, also known as ambient intelligence.

반도체 공정 overview

The UKIRT Infrared Deep Sky Survey is a set of v e surveys of complementary combinations of area, depth, and Galactic latitude, which began in 2005 May. The surveys use the UKIRT Wide Field Camera (WFCAM), which has a solid angle of 0.21deg 2 . Here we introduce and characterise the ZYJHK photometric system of the camera, which covers the wavelength range 0:83 2:37 m. We synthesise response functions for the v e passbands, and compute colours in the WFCAM, SDSS and 2MASS bands, for brown dwarfs, stars, galaxies and quasars of dieren t types. We provide a recipe for others to compute colours from their own spectra. Calculations are presented in the Vega system, and the computed osets to the AB system are provided, as well as colour equations between WFCAM lters and the SDSS and 2MASS passbands. We highlight the opportunities presented by the new Y lter at 0:97 1:07 m for surveys for hypothetical Y dwarfs (brown dwarfs cooler than T), and for quasars of very{high redshift, z > 6:4.

/pdf/the-ukirt-infrared-deep-sky-survey-zy-jhk-photometric-system-29gx4l3iay.pdf

The UKIRT Infrared Deep Sky Survey ZY JHK photometric system: passbands and synthetic colours

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 and Hambly et al detail the design of the pipeline and science archive aspects of the project.

/pdf/vista-data-flow-system-overview-1qsgqk5ako.pdf

VISTA data flow system: overview

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.

VISTA: status and performance

The VISTA IR Camera has now completed its detailed design phase and is on schedule for delivery to ESO’s Cerro Paranal Observatory in 2006. The camera consists of 16 Raytheon VIRGO 2048x2048 HgCdTe arrays in a sparse focal plane sampling a 1.65 degree field of view. A 1.4m diameter filter wheel provides slots for 7 distinct science filters, each comprising 16 individual filter panes. The camera also provides autoguiding and curvature sensing information for the VISTA telescope, and relies on tight tolerancing to meet the demanding requirements of the f/1 telescope design. The VISTA IR camera is unusual in that it contains no cold pupil-stop, but rather relies on a series of nested cold baffles to constrain the light reaching the focal plane to the science beam. In this paper we present a complete overview of the status of the final IR Camera design, its interaction with the VISTA telescope, and a summary of the predicted performance of the system.

The VISTA IR camera

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The VISTA IR camera