Open AccessThe Faint Sky Variability Survey – I. Goals and data reduction process
Author(s) -
Groot P. J.,
Vreeswijk P. M.,
Huber M. E.,
Everett M. E.,
Howell S. B.,
Nelemans G.,
Van Paradijs J.,
Van Den Heuvel E. P. J.,
Augusteijn T.,
Kuulkers E.,
Rutten R. G. M.,
Storm J.
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06182.x
Subject(s) - physics , sky , brightness , astronomy , astrophysics , data reduction , latitude , telescope , sky brightness , remote sensing , geography , statistics , mathematics
The Faint Sky Variability Survey is aimed at finding photometric and/or astrometric variable objects in the brightness range between ∼16th and ∼24th mag on time‐scales between tens of minutes and years with photometric precisions ranging from 3 millimag for the brightest to 0.2 mag for the faintest objects. An area of ∼23 deg 2 , located at mid and high Galactic latitudes, has been covered using the Wide Field Camera on the 2.5‐m Isaac Newton Telescope on La Palma. Here we describe the main goals of the Faint Sky Variability Survey and the data reduction process.