The Infrared Array Camera (IRAC) for the Spitzer Space Telescope

By G. Fazio, J. Hora, L. Allen, M. Ashby, Pauline Barmby, L. Deutsch, J.-S. Huang, S. Kleiner, M. Marengo, S. Megeath and 55 more. 2004

299 citations recorded by the source corpus.

The Infrared Array Camera (IRAC) is one of three focal plane instruments on the Spitzer Space Telescope. IRAC is a four-channel camera that obtains simultaneous broadband images at 3.6, 4.5, 5.8, and 8.0 μm. Two nearly adjacent 5.′2 × 5.′2 fields of view in the focal plane are viewed by the four channels in pairs (3.6 and 5.8 μm; 4.5 and 8 μm). All four detector arrays in the camera are 256 × 256 pixels in size, with the two shorter wavelength channels using InSb and the two longer wavelength channels using Si:As IBC detectors. IRAC is a powerful survey instrument because of its high sensitivity, large field of view, and four-color imaging. This paper summarizes the in-flight scientific, technical, and operational performance of IRAC.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/4594db45d86c71c0878e246e9ad946918e4cdac6

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Citations in the corpus

In-flight performance and calibration of the Infrared Array Camera (IRAC) for the Spitzer Space Telescope (2004, background): “See Fazio et al.2 for transmission plots and the isophotal wavelengths.”
ANDROMEDA'S DUST (2013, methodology): “M31 has been mapped using the IRAC (Fazio et al. 2004) and MIPS (Rieke et al. 2004) cameras on Spitzer Space Telescope (Werner et al. 2004).”
CANDELS: THE EVOLUTION OF GALAXY REST-FRAME ULTRAVIOLET COLORS FROM z = 8 TO 4 (2011, methodology): “The issue of correlations between β and the UV M/L ratio could potentially be alleviated by including photometry from the Spitzer Space Telescope Infrared Array Camera (IRAC Fazio et al. 2004) when measuring the stellar mass.”
Transit timing observations from Kepler - III. : Confirmation of four multiple planet systems by a Fourier-domain study of anticorrelated transit timing variations (2012, background): “Kepler–25c, Kepler–25b, and Kepler–26c were observed during several transits with Warm-Spitzer/IRAC (Werner et al. 2004; Fazio et al. 2004) at 4.5 µm (program ID 60028).”
STELLAR POPULATIONS OF Lyα EMITTERS AT z ∼ 6–7: CONSTRAINTS ON THE ESCAPE FRACTION OF IONIZING PHOTONS FROM GALAXY BUILDING BLOCKS (2010, background): “Ouchi et al. (2009a) have reported the discovery of a giant LAE at z = 6.595, Himiko, with a Spitzer/Infrared Array Camera (IRAC; Fazio et al. 2004) counterpart, and estimated its stellar mass to be (0.9 – 5.0) ×1010M⊙.”
The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, methodology): “Given that the FWHM of the IRAC Point Spread Function (PSF) is 1.8-2.0′′ (Fazio et al. 2004a), and that the PSFs are very sharp and stable, almost all sources are point-like in the 4 channels, and objects can be resolved for separations of the order of ∼1′′.”
Absolute Calibration and Characterization of the Multiband Imaging Photometer for Spitzer. I. The Stellar Calibrator Sample and the 24 μm Calibration (2007, methodology): “…on board the Spitzer Space Telescope (Werner et al. 2004) are calibrated against celestial sources: for example, the Infrared Array Camera (IRAC; Fazio et al. 2004), with photometric bands from ∼ 3− 8 µm, is calibrated against stars (Reach et al. 2005), as is the Infrared Spectrograph (IRS;…”
A SPITZER SURVEY OF YOUNG STELLAR CLUSTERS WITHIN ONE KILOPARSEC OF THE SUN: CLUSTER CORE EXTRACTION AND BASIC STRUCTURAL ANALYSIS (2009, background): “…resolution comparable to those of near-infrared surveys at midinfrared wavelengths with onboard imaging instruments the Infrared Array Camera (IRAC; Fazio et al. 2004) at 3–8 μm 18 No. 1, 2009 YOUNG CLUSTER SURVEY 19 and the Mid-Infrared Photometer for Spitzer (MIPS; Rieke et al. 2004) at 24–160…”
The Disk Population of the Chamaeleon I Star-forming Region (2008, methodology): “Observations For our census of the disk population in Chamaeleon I, we use images at 3.6, 4.5, 5.8, and 8.0 µm obtained with Spitzer’s Infrared Array Camera (IRAC; Fazio et al. 2004a) and images at 24 µm obtained with the Multiband Imaging Photometer for Spitzer (MIPS; Rieke et al. 2004).”