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| Spitzer Space Telescope Infrared Array Camera | |
|---|---|
| Name | Infrared Array Camera |
| Mission | Spitzer Space Telescope |
| Operator | NASA |
| Manufacturer | Jet Propulsion Laboratory |
| Launch | 2003-08-25 |
| Wavelength | 3.6–8.0 μm |
| Detectors | 256×256 InSb and Si:As arrays |
| Mass | 14.0 kg |
Spitzer Space Telescope Infrared Array Camera The Infrared Array Camera was a four-channel imaging instrument flown on the Spitzer Space Telescope that provided broadband photometry across mid-infrared wavelengths, enabling observations of Andromeda Galaxy, Orion Nebula, Galactic Center (Milky Way), NGC 1333 and numerous exoplanet host stars. Designed and built under the auspices of the Jet Propulsion Laboratory and managed by NASA, the instrument supported programs led by teams at the California Institute of Technology, Harvard–Smithsonian Center for Astrophysics, University of Arizona, Cornell University and international partners from institutions such as the European Space Agency and Centre National d'Études Spatiales. Its data were archived at the Infrared Processing and Analysis Center and used extensively by researchers affiliated with the Space Telescope Science Institute, Max Planck Institute for Astronomy, University College London and other observatories.
The Infrared Array Camera (IRAC) consisted of four broadband channels centered near 3.6, 4.5, 5.8 and 8.0 micrometers and operated throughout the cryogenic and warm phases of the Spitzer Space Telescope mission, enabling surveys of star formation regions, protoplanetary disks, brown dwarfs, active galactic nuclei, high-redshift galaxies and solar system targets such as Jupiter and Comet 73P/Schwassmann–Wachmann 3. IRAC observations complemented data from instruments aboard observatories like the Hubble Space Telescope, Chandra X-ray Observatory, Galaxy Evolution Explorer, WISE, ALMA, Kepler, James Webb Space Telescope and ground facilities including the Keck Observatory, Very Large Telescope and Subaru Telescope. Principal investigators, instrument scientists, and project managers from the California Institute of Technology, Jet Propulsion Laboratory, NASA Ames Research Center and international institutes coordinated observing programs and archival deliveries.
IRAC employed four detector arrays: two indium antimonide (InSb) arrays and two arsenic-doped silicon (Si:As) arrays, each 256×256 pixels, cooled by the Spitzer cryogenic system during the primary mission and operated in a reduced mode after the cryogen was exhausted, analogous to instrument operations on missions like COBE and ISO. The optical design used dichroic beamsplitters and pickoff mirrors modeled with tools from the California Institute of Technology and fabricated under contracts with aerospace firms overseen by the Jet Propulsion Laboratory and Lockheed Martin. Electronics heritage traced to designs used at the National Radio Astronomy Observatory and in instruments developed for the Herschel Space Observatory and SOFIA. Thermal control, stray light suppression, and vibration mitigation used engineering practices common to missions led by NASA centers and contractors collaborating with the European Space Agency.
IRAC supported imaging, high-dynamic-range frames, and subarray modes for bright targets, with frame times optimized for observations of transiting exoplanets and brown dwarf variability campaigns conducted by teams at Harvard–Smithsonian Center for Astrophysics and University of Arizona. Sensitivity and point-spread function (PSF) performance were characterized during in-orbit checkout using calibration fields including the SWIRE and GOODS survey regions, and comparisons with data from the Sloan Digital Sky Survey, Two Micron All Sky Survey, COSMOS field and Spitzer Deep Wide-Field Survey informed observing strategies. The instrument achieved background-limited performance on faint galaxy surveys and sub-millijansky sensitivity in deep integrations, enabling photometry for targets observed also by the Hubble Ultra Deep Field, Spitzer Extragalactic Representative Volume Survey and follow-up of candidates from Kepler and TESS.
IRAC calibration used ground test data from the Jet Propulsion Laboratory and in-flight calibration programs tied to standard stars cataloged by the Infrared Astronomical Satellite and photometric systems used by the Two Micron All Sky Survey and WISE. Data processing pipelines were developed by the Spitzer Science Center at the Infrared Processing and Analysis Center and implemented into the Spitzer Heritage Archive; pipelines produced Basic Calibrated Data (BCD), mosaics, and source catalogs used by the Astrophysics Data System community. Calibration tasks included flat-fielding, dark-current subtraction, array location-dependent corrections, pixel-phase correction, muxbleed mitigation and detector linearity adjustments, with algorithms refined through collaborations involving the Space Telescope Science Institute, University of California, Berkeley, Massachusetts Institute of Technology, Max Planck Institute for Extraterrestrial Physics and instrument teams.
IRAC enabled discovery and characterization of thousands of exoplanet atmospheres via secondary-eclipse and phase-curve photometry for systems such as HD 209458 b, HD 189733 b and numerous Kepler candidates; it revealed disk structures in systems like TW Hydrae and HL Tauri and mapped polycyclic aromatic hydrocarbon emission in star-forming regions including the Orion Nebula and Carina Nebula. Surveys such as GLIMPSE, SAGE, SWIRE and GOODS used IRAC to trace stellar mass assembly, measure luminosity functions of quasars and detect massive galaxies at redshifts greater than 6 in synergy with Subaru Telescope and Keck Observatory spectroscopy. IRAC identified free-floating planetary-mass objects, provided mid-infrared light curves of variable stars and contributed to studies of asteroid and Kuiper Belt Object thermal properties that complemented measurements from the NEOWISE program and spacecraft missions like New Horizons.
IRAC operated from the Spitzer launch in 2003 through the end of the cryogenic mission in 2009 and continued in a "warm mission" phase using the two shorter-wavelength channels, similar to operational transitions experienced by missions such as Hubble Space Telescope servicing cycles and Chandra X-ray Observatory calibration phases. Instrument teams coordinated with the Spitzer Science Center, NASA Headquarters, and international partners to schedule Legacy programs, General Observer campaigns, and Director's Discretionary Time observations. Data releases and pipeline updates occurred periodically, driven by instrument characterization work and science priorities set by community panels involving representatives from the National Science Foundation, European Southern Observatory and academic consortia.
IRAC's extensive catalog of mid-infrared images and photometry has become a cornerstone of archival research in astrophysics, influencing instrument designs for the James Webb Space Telescope's Near Infrared Camera and Mid-Infrared Instrument, the Wide Field Infrared Survey Telescope (now Nancy Grace Roman Space Telescope) planning, and ground-based infrared cameras on telescopes such as the Very Large Telescope and Keck Observatory. The techniques, calibration strategies, and survey science developed with IRAC informed follow-up campaigns using ALMA, JWST, HST and next-generation facilities operated by institutions including the Max Planck Society, European Space Agency and major universities worldwide. Category:Spitzer Space Telescope instruments