Wide Field Camera 3

Wide Field Camera 3
🏢No image available
Organization information
Type	Space telescope instrument
Mission	Hubble Space Telescope
Operator	Space Telescope Science Institute

The Wide Field Camera 3 (WFC3) is an imaging instrument on board the Hubble Space Telescope that provides high-resolution observations in ultraviolet (UV), visible, and near-infrared (NIR) wavelengths. WFC3 was designed to expand Hubble’s scientific capabilities, including deep-field galaxy surveys, stellar population studies, and investigations of exoplanet atmospheres. Its observing modes enable both wide-area imaging and spectroscopy using multiple instrument channels.

Overview

The Wide Field Camera 3 is one of Hubble’s major instruments, complementing earlier cameras such as the Advanced Camera for Surveys (ACS) and the Wide Field and Planetary Camera 2 (WFPC2). Where those instruments supported a broad range of imaging and survey work, WFC3 emphasized improved sensitivity and wavelength coverage, particularly in the near-infrared. The instrument’s capabilities are therefore closely associated with Hubble’s role in frontier astronomy, including work highlighted by the Hubble Ultra Deep Field program.

WFC3 is typically discussed in connection with Hubble’s broader instrument suite and data systems, including the processes used to plan observations and calibrate measurements. Scientific use of WFC3 also relies on standardized data products produced by the Space Telescope Science Institute (STScI) and other Hubble operations workflows.

Instrument design and channels

WFC3 is commonly described as having multiple channels to cover different wavelength ranges. The UV and visible imaging capability is provided by a UV/visible channel, while a separate near-infrared channel extends sensitivity into the NIR regime. In addition to imaging, WFC3 supports spectroscopic observations, allowing researchers to infer physical properties such as composition, temperature, and redshifted emission features for distant astronomical targets.

The instrument’s channel architecture is particularly relevant for high-redshift astronomy, where rest-frame UV or optical light from early galaxies is redshifted into the near-infrared. Studies of these early systems often connect to larger programs such as the James Webb Space Telescope (JWST), which complements Hubble’s wavelength reach in related fields. However, WFC3 remains distinct for its combination of stable pointing on orbit and its high spatial resolution at visible wavelengths.

Observing modes and data use

WFC3 observations are carried out using a variety of filters, grisms, and observing templates depending on the scientific objective. Imaging programs may target star-forming regions, galaxy morphology, or gravitationally lensed systems, while spectroscopic programs can measure spectral features that help characterize stars and galaxies. The instrument’s output is typically processed into calibrated images and spectra suitable for scientific analysis.

Astronomers often integrate WFC3 data with observations from other Hubble instruments, such as ACS, to improve coverage in wavelength or field size. This multi-instrument approach is also used in studies of galaxy evolution that draw upon Hubble’s long-term legacy, including work spanning the same observational traditions as the Hubble Deep Field. In practice, WFC3 data analysis also depends on calibration reference files and standard pipelines distributed through Hubble’s data processing ecosystem.

Scientific impact

Since its deployment, WFC3 has contributed to numerous cornerstone results in extragalactic astronomy and observational cosmology. Its near-infrared sensitivity supports studies of distant galaxies whose light is shifted out of the optical bands. At the same time, its UV/visible imaging capability supports investigations of massive star populations, nearby stellar evolution, and the structure of galaxies in the local universe.

WFC3 has also been used to study exoplanets through transit observations, where instrument sensitivity and wavelength coverage can help constrain atmospheric properties. Research in exoplanet characterization frequently references methods developed across space-based platforms, including instruments on the Spitzer Space Telescope and current and upcoming work supported by facilities such as JWST. Within this context, WFC3 data are often combined with ground-based spectroscopy to improve interpretation of planetary atmospheres and host-star properties.

Maintenance, upgrades, and legacy

WFC3 was installed during the era of Hubble instrument servicing and has continued to operate as part of Hubble’s long-lived science program. Over time, instrument performance and calibration procedures have been monitored and updated to reflect changes in detector characteristics and on-orbit conditions. The instrument therefore has a well-established heritage of calibration and scientific use, spanning decades of Hubble observation cycles.

As Hubble continues its observational role, WFC3 data remain relevant for comparative studies with newer facilities. In many research programs, WFC3 imaging and spectroscopy are used as baseline measurements for targets that will later be examined in greater detail by JWST, especially for faint galaxies at high redshift. This continuity helps maintain Hubble’s legacy as a cornerstone observatory in modern astronomy.