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home - overview glossary observing exposure time calculator (etc) survey processing pictures publications - external links eso - public surveys eso - vista surveys near ir surveys denis 2mass ukidss (in north) visible and infrared survey telescope for astronomy news building vista photos of vista images taken with vista past news overview - for potential users vista is a 4-m class wide field survey telescope for the southern hemisphere, equipped with a near infrared camera (1.65 degree diameter field of view at vista's nominal pixel size) containing 67 million pixels of mean size 0.34 arcsec and available broad band filters at z,y,j,h,k s and a narrow band filter at 1.18 micron. a wide field visible camera, if constructed, could also be used on vista. the telescope has an azimuth-altitude mount, and quasi-ritchey-chretien optics with a fast f/1 primary mirror giving an f/3.25 focus to the instrument at cassegrain. the instrument mounts to the rotator on the back of the primary mirror cell, and includes a wide-field corrector lens system (3 infrasil lenses), autoguider and active optics sensors. vista is located at eso's cerro paranal observatory in chile (latitude 24° 40' s - see google satellite picture ) on its own peak ( see picture ) about 1500m from the four vlts and the vst see either ( figure where vista is at top left ) or ( figure where vista is at bottom right ). the point spread function (psf) of the telescope+camera system (including pixels) is designed to have a full width at half maximum (fwhm) of 0.51 arcsec. seeing, and other weather realted statistics for cerro paranal are given at eso's astroclimatology of paranal pages and the vista site is expected to have similar conditions. the site, telescope aperture, wide field, and high quantum efficiency detectors will make vista the world's outstanding ground based near-ir survey instrument. time available 75% of the vista time available to eso will be available for large scale public surveys and the remaining 25% for smaller proprietary surveys. on the assumption that vista is unavailable ~10 nights a year for maintenance the corresponding numbers of nights per year are public surveys: ~236 nights, proprietary surveys: ~78 nights. in planning surveys it should be realised that the surveys as a whole (public + proprietary) have to effectively use the range of seeing and sky conditions ( sky brightness , extinction, wind speed ) available, as well as the ra range. one of the roles of the public survey panel for vista will be to ensure that the final public surveys form a realistic set in the light of these constraints. information on the conditions at the cerro paranal observatory can be found on the eso astroclimatology of paranal pages. for all observing time at eso telescopes eso assume 10 hours per night in odd periods (winter, 1 april to 30 september) and 8 hours per night in even periods (summer, 1 october to end of february). these numbers are used at submission time as approximate indications of time available (but not, for example, when later scheduling allocated service-mode observations). filters filter plot wavelength fwhm comment at 296k micron z transmission 0.88 0.12 manufactured y transmission 1.02 0.10 in camera j transmission 1.25 0.18 in camera h transmission 1.65 0.30 in camera ks transmission 2.15 0.30 in camera nb1.18 plot to be provided 1.18 0.01 in camera the only moving part in the camera is the filter wheel. with the current complement of z, y, j, h, k s and nb1.18 filters there is one filter wheel position available to hold a further set of 16 filters (1 per detector). purchase of other filters are under discussion by various groups - see vista twiki filters page field distortion the plate scale varies with distance from the field centre, getting larger from centre to edge, which is why the mean pixel size (of 0.339 arcsec) is quoted. the rectangular focal plane, when projected onto the sky, suffers barrel distortion. this means that a somewhat larger area of sky is seen by the detectors than if there was no distortion. a rectangular area of sky when imaged onto the focal plane suffers from pincushion distortion. this means that a somewhat smaller area of focal plane is covered by the sky than if there was no distortion. the distortions (of order 30 pixels at the edge) therefore increase overlap between adjacent tiles and do need not be considered in observation planning. covering an area of sky the sixteen 2048x2048 pixel ir detectors (raytheon virgo hgcdte 0.84-2.5 micron) in the camera are not buttable and are arranged as in the following figure which shows a diagram of the focal plane as would be seen looking directly down the camera body (down the z-axis which on the telescope points towards the sky). on the sky (in the default instrument rotator position) +y corresponds to n, and +x to east. below - photograph of the real focal plane. a single integration of length dit secs (or a coadded series of these known as an exposure) produces a sparsely sampled image of the sky known as a pawprint (in red in the following figure). the area of sky covered by the pixels of a pawprint is 0.6 sq degrees. for comparison the fields of view of nicmos, isaac, hawk-i and wfcam are shown below in figure 2 together with a crescent moon. and an mockup up of a pawprint showing the moon to 'fill-in' the gaps between the detectors to produce a single filled tile with reasonably uniform sky coverage the minimum number of pointed observations (with fixed offsets) required is 6 which is achieved first by observing at 3 positions offset in y i.e. so that after 3 positions in y an area of vertical side 5.275 detector widths (=4+3*0.425) is covered at least twice. this corresponds to 1.017 degrees (61 arcmin) at vista's mean pixel size. there is also a strip at the top and another at the bottom which is only covered once by this tiling pattern. these strips are each 0.475 of a detector height. each corresponding to 0.092 degrees (5.5 arcmin) at vista's mean pixel size. then a position shift is made in x as shown below so that the 2 positions in x cover a horizontal side 7.65 detector widths (=4+3*0.90+0.95) with no strips at the +/-x edges. this corresponds to 1.475 degrees (88.5 arcmin) at vista's nominal pixel size. the 3 steps in y are then repeated at the nex position in x. so after 3x2=6 steps an area of 5.275x7.65=40.354 detector areas corresponding to 1.017 deg x 1.475deg = 1.501 deg 2 sky is (almost) uniformly covered (by a minimum of 2 pixels) as shown in light green in the exposure time map below for a filled tile (no jitter). where dark green = 1, light green = 2, magenta = 3, red = 4, yellow = 6, in units of the single-pawprint exposure time. the dark green areas at top and bottom of the plot are each 1.475 deg x 0.092 deg =0.135 sq deg and can be overlapped by corresponding areas from adjacent tiles for many surveys. assigning only one of the two 0.092 deg overlap (top & bottom) to each of the two tiles involved in an overlap, the result is that each tile, when part of a filled larger area, would covers (1.017+0.092) x1.475 = 1.636 deg 2 which will be covered at least twice. summary of dimensions (unit of 2048 pixel side detecor) in x in y area det det sq det pawprint single detector 1 1 1 all 16 single detectors 4 4 16 outer boundary of (unfilled pawprint) 6.70 5.275 35.343 diagonal (unfilled pawprint) 8.5273 dets tile tile size covered twice 7.65 5.275 40.354 tile size at top (+y) covered once 7.65 0.475 3.634 tile size at bottom (-y) covered once 7.65 0.475 3.634 tile size covered twice if one of the two overlaps is matched by a nighbour tile in large survey 7.65 5.75 43.988 summary of dimensions (unit of degrees) in x in y area adopted mean pixel size 0.339 arsec deg deg sq deg pawprint single detector 0.193 0.193 0.037 all 16 single detectors 0.595 outer boundary (unfilled pawprint) 1.292 1.017 diagonal (unfilled pawprint) 1.6445 deg tile tile size all covered twi

URL analysis for vista.ac.uk

http://www.vista.ac.uk//glossary.htm#pawprint
http://www.vista.ac.uk//index.html
http://www.vista.ac.uk//glossary.htm#integration
http://www.vista.ac.uk//files/docs/arnaboldi-eso-surveys.pdf
http://www.vista.ac.uk//glossary.htm#jitter
http://www.vista.ac.uk//glossary.htm#microstep
http://www.vista.ac.uk///images/site/hires/01_aerial-view.jpg
http://www.vista.ac.uk//glossary.htm#exposure.html
http://www.vista.ac.uk//observing/index.html
http://www.vista.ac.uk///images/site/small/vista-at-sunrise-1600x1200.jpg
http://www.vista.ac.uk//glossary.htm
http://www.vista.ac.uk///vdfs/index.html
http://www.vista.ac.uk//glossary.htm#exposure
http://www.vista.ac.uk//pastnews.html
http://www.vista.ac.uk//images/site/hires/vistaandparanal.jpg

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