The INT Wide Field Survey (WFS) is using the Wide Field Camera (~0.3 deg2 ) on the 2.5m Isaac Newton Telescope (INT). The project was initiated in August 1998 and is expected to have a duration of up to five years. The WFS is an umbrella for competitively judged science programmes which were assessed on the usual criteria plus the wider worth of the data set and the management competence of the proposing teams.
Multicolour data will be obtained over 200+ square degrees to a typical depth of ~25 mag (U through Z). Importantly, the data is publically accessible by the UK and NL communities from day one, with access to the rest of the world after one year. The preliminary processing and calibration (up to object catalogue generation) is the responsibility of the WFS project.
In recent years a number of major survey programmes covering a variety of wavelengths have been initiated. The 2Mass project is covering the entire sky at a resolution of 4 arcsec in the JHK bands (http://www.ipac.caltech.edu/2mass/) The Sloan Sky Survey (SDSS) (http://www.sdss.org/) will cover significant areas of the Northern Hemisphere. These wide area surveys are having a significant impact, both as target selectors for 8 m class telescopes and for inherent survey science programmes. The aim of the WFS is to provide deeper data than the SDSS, but still cover significant targeted coverage, typically of fields being observed by facilities at other frequencies.
The table below shows the survey wavebands and the typical survey detection limits. For more detailed information on the filters see the filters page.
|Waveband||Central Waveband||Banwidth FWHM||Exp Time||Detection Limit1||Surface Brightness Limit3|
|1: 5-sigma detection limit in 1" seeing (with PSF profile fitting)|
|2: 10-19 erg s-1cm-2A-1|
|3: 1-sigma limit per square arcsec|
|4: 10-20 erg s-1cm-2A-1|