FGS/NIRISS
Fine Guidance Sensor / Near Infrared Imager and Slitless Spectrograph (FGS/NIRISS)
Quick Facts
FGS is a guider that locks on to bright stars in deep space to keep Webb on target creating sharp high quality images.
FGS allows Webb to determine its position, locate its celestial targets, track moving targets and remain steadily locked or pointed with very high precision on a specific celestial target.
FGS is so sensitive that it can detect a tiny angular displacement equivalent to the thickness of a human hair as seen from one kilometre away.
NIRISS enables scientists to determine the composition of exoplanets' atmospheres, observe distant galaxies, and examine objects that are very close together.
FGS/NIRISS operates over a wavelength range of 0.8 to 5.0 microns
Fine Guidance Sensor / Near Infrared Imager and Slitless Spectrograph (FGS/NIRISS)
The Fine Guidance Sensor (FGS) allows Webb to point precisely, so that it can obtain high-quality images. The Near Infrared Imager and Slitless Spectrograph part of the FGS/NIRISS is used to investigate the following science objectives: first light detection, exoplanet detection and characterization, and exoplanet transit spectroscopy.
FGS/NIRISS has a wavelength range of 0.8 to 5.0 microns, and is a specialized instrument with three main modes, each of which addresses a separate wavelength range. FGS is a "guider," which helps point the telescope.
Video: FGS/NIRISS 3d Diagram Rotation
FGS/NIRISS Image Gallery
Gallery of the development, testing and commissioning of the FGS/NIRISS in reverse chronological order.
The image below is a SLIDESHOW. Hover over the image to see the image title and controls. Click the image to go to a detail page with more info and the ability to download the image at various resolutions (click downward arrow in lower right corner).
Resources:
NIRSpec was developed by ...
NIRISS is a contribution of the Canadian Space Agency. Honeywell International designed and built the instrument in collaboration with a team at the Université de Montréal. Additional technical support was provided by the National Research Council of Canada’s Herzberg Astronomy and Astrophysics Research Centre.
