First light: December 1984.
Designed and built by: Durham University and RGO.
Description: The Faint Object Spectrograph (FOS) is an efficient, fixed-format spectrograph with a CCD detector used for low resolution (15-20Å FWHM) spectrophotometry over the wavelength range 4000-10000Å. The optical design is a Schmidt camera without a collimator in the diverging beam from the Cassegrain focus. The dispersion is provided by a transmission grating and a cross-dispersing prism, which give a two-order format. The principal advantage of the FOS is its high throughput - 12% for the combination of atmosphere, telescope and FOS at 7000Å - some three times larger than that of the IDS with the same detector. It is highly appropiate for the study of emission-line objects such as quasars, radio galaxies, HII regions and planetary nebulae, but less useful for absorption-line objects (particularly those with narrow features) owing to its low resolution. There are four operating modes: beamswitching for point sources; beamswitching with a larger throw for extended objects; long slit (first order only) and 25 arc sec slit (both orders).
Faint Object Spectrograph for the 2.5-m Isaac Newton Telescope
Scientific and technical impact:
Publications (ING count: 11)