SWIRE: The SIRTF Wide‐Area Infrared Extragalactic Survey

By C. Lonsdale, H. Smith, M. Rowan‐Robinson, J. Surace, D. Shupe, C. Xu, S. Oliver, D. Padgett, F. Fang, T. Conrow and 27 more. 2001

568 citations recorded by the source corpus.

The SIRTF Wide‐Area Infrared Extragalactic Survey (SWIRE), the largest SIRTF Legacy program, is a wide‐area imaging survey to trace the evolution of dusty, star‐forming galaxies, evolved stellar populations, and active galactic nuclei (AGNs) as a function of environment, from redshifts z ∼ 3 to the current epoch. SWIRE will survey seven high‐latitude fields, totaling 60–65 deg2 in all seven SIRTF bands: Infrared Array Camera (IRAC) 3.6, 4.5, 5.6, and 8 μm and Multiband Imaging Photometer for SIRTF (MIPS) 24, 70, and 160 μm. Extensive modeling suggests that the Legacy Extragalactic Catalog may contain in excess of 2 million IR‐selected galaxies, dominated by (1) ∼150,000 luminous infrared galaxies (LIRGs; LFIR > 1011 L⊙) detected by MIPS (and significantly more detected by IRAC), ∼7000 of these with z>2; (2) 1 million IRAC‐detected early‐type galaxies (∼ 2 × 105 with z>1 and ∼10,000 with z>2); and (3) ∼20,000 classical AGNs detected with MIPS, plus significantly more dust‐obscured quasi‐stellar objects/AGNs among the LIRGs. SWIRE will provide an unprecedented view of the evolution of galaxies, structure, and AGNs. The key scientific goals of SWIRE are (1) to determine the evolution of actively star forming and passively evolving galaxies in order to understand the history of galaxy formation in the context of cosmic structure formation; (2) to determine the evolution of the spatial distribution and clustering of evolved galaxies, starbursts, and AGNs in the key redshift range 0.5<z<3 over which much of cosmic evolution has occurred; and (3) to determine the evolutionary relationship between “normal galaxies” and AGNs and the contribution of AGN accretion energy versus stellar nucleosynthesis to the cosmic backgrounds. The large area of SWIRE is important to establish statistically significant population samples over enough volume cells that we can resolve the star formation history as a function of epoch and environment, i.e., in the context of structure formation. The large volume is also optimized for finding rare objects. The SWIRE fields are likely to become the next generation of large “cosmic windows” into the extragalactic sky. They have been uniquely selected to minimize Galactic cirrus emission over large scales. The Galaxy Evolution Explorer will observe them as part of its deep 100 deg2 survey, as will Herschel. SWIRE includes ∼9 deg2 of the unique large‐area XMM Large Scale Structure hard X‐ray imaging survey and is partly covered by the UKIDSS deep J and K survey. An extensive optical/near‐IR imaging program is underway from the ground. The SWIRE data are nonproprietary; catalogs and images will be released twice yearly, beginning about 11 months after SIRTF launch. Details of the data products and release schedule are presented.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Chandra and Spitzer Unveil Heavily Obscured Quasars in the Chandra/SWIRE Survey (2006, methodology): “This field was selected for deep follow-up observations within the Spitzer WideArea Infrared Extragalactic (SWIRE) survey (Lonsdale et al. 2003, 2004) legacy project.”
THE TAURUS SPITZER SURVEY: NEW CANDIDATE TAURUS MEMBERS SELECTED USING SENSITIVE MID-INFRARED PHOTOMETRY (2009, methodology): “In the upper left of each Figure is the SWIRE (Spitzer Wide-area Infrared Extragalactic Survey; Lonsdale et al. 2003) ELAIS N1 extragalactic field4 (the c2d reduction – see Evans et al. 2007 – is used here, as in Rebull et al. 2007 and Padgett et al. 2008b).”
Dusty Star Forming Galaxies at High Redshift (2014, background): “Some of the deepest maps were in GOODS-N Dickinson (private communication) and COSMOS (Sanders et al., 2007) with SWIRE covering larger areas 50 deg2 to shallower depths of 280 µJy (Lonsdale et al., 2003).”
RESOLVING THE RADIO SOURCE BACKGROUND: DEEPER UNDERSTANDING THROUGH CONFUSION (2012, methodology): “This field in the Lockman Hole was originally selected by Owen & Morrison (2008) because it was covered by the Spitzer Wide-area InfraRed Extragalactic (SWIRE) legacy survey (Lonsdale et al. 2003), has exceptionally low infrared cirrus, and contains no strong radio sources.”
The VIMOS VLT deep survey - First epoch VVDS-deep survey: 11 564 spectra with 17.5 $\leq$ I$_\textit{\textbf{\small AB}}$ $\leq$ 24, and the redshift distribution over 0 $\leq$ z $\leq$ 5 (2004, unknown): “We have included the Chandra Deep Field South (CDFS, Giacconi et al. 2002), which is the target of Chandra, HST, XMM and Spitzer multi-wavelength observations, to complement the work of the GOODS consortium (Giavalisco et al. 2004).”
CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, methodology): “Spitzer/IRAC data Apart from the shallow (4 × 30s) IRAC coverage obtained by the Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE; Lonsdale et al. 2003), the UDS was surveyed as part of a Spitzer cycle-4 Legacy Program: the Spitzer UKIDSS Ultra Deep Survey (SpUDS hereafter; PI: J. Dunlop).”
EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, methodology): “Spitzer imaging and public catalogs in the four IRAC bands are available for 91 galaxies, from the GOODS-S survey (Dickinson et al. 2003), SWIRE survey (Lonsdale et al. 2003), AEGIS survey (Barmby et al. 2008) and SCOSMOS (Sanders et al. 2007).”
COSMOS PHOTOMETRIC REDSHIFTS WITH 30-BANDS FOR 2-deg2 (2008, methodology): “Polletta et al. selected their templates for fitting the VVDS sources (Le Fèvre et al. 2005) from the UVoptical (CFHTLS: McCracken et al. 2007) to the mid-IR (SWIRE: Lonsdale et al. 2003).”
THE EVOLVING RELATIONS BETWEEN SIZE, MASS, SURFACE DENSITY, AND STAR FORMATION IN 3 × 104 GALAXIES SINCE z = 2 (2009, methodology): “…the UKIDSS Ultra-Deep Survey Data Release 1 (UDS; Lawrence et al. 2007; Warren et al. 2007a), with overlapping BRi′z′ imaging from the Subaru-XMM Deep Survey (SXDS; Sekiguchi et al. 2004), and 3.6/4.5µm data from the Spitzer Wide-area Infrared Extragalactic (SWIRE) survey (Lonsdale et al. 2003).”
A 158 μm [C ii] LINE SURVEY OF GALAXIES AT z ∼ 1–2: AN INDICATOR OF STAR FORMATION IN THE EARLY UNIVERSE (2010, background): “These two sources are from the 2006 internal catalog of the Spitzer Wide-area Infrared Extragalactic (SWIRE) survey (Lonsdale et al. 2003).”
WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, methodology): “…et al. (2009) catalog usesJ and K-band data for the UKIDDS UDS Data Release 1 (Lawrence et al. 2007; Warren et al. 2007) in conjunction withB, R, i and z-band imaging from the SXDS (Furusawa et al. 2008) and 3.6µm and 4.5µm IRAC imaging data taken as part of the SWIRE survey (Lonsdale et al. 2003).”
The WIRCam Deep Survey I. Counts, colours, and mass-functions derived from near-infrared imaging in the CFHTLS deep fields (2011, methodology): “…chosen to overlap with the VIMOS-VLT Deep Survey (VVDS; Le Fèvre et al. 2005) and the Spitzer Wide-area Infrared Extragalactic Legacy Survey (SWIRE; Lonsdale et al. 2003, 2004), whilst the entir field overlaps with a portion of the XMM Large Scale Structure Survey (XMM-LSS; Pierre et al. 2004).”
Spectral Energy Distributions of Hard X-Ray Selected Active Galactic Nuclei in the XMM-Newton Medium Deep Survey (2007, unknown): “This region has also been observed as part of the Spitzer Wide-Area Infrared Extragalactic survey (SWIRE; Lonsdale et al. 2003) legacy program, of the VIMOS VLT Deep Survey (VVDS; McCracken et al. 2003; Le Fèvre et al. 2004), and of the CanadaFrance-Hawaii Telescope Legacy ‘‘Deep’’ (D1) Survey.”
THE GEMINI CLUSTER ASTROPHYSICS SPECTROSCOPIC SURVEY (GCLASS): THE ROLE OF ENVIRONMENT AND SELF-REGULATION IN GALAXY EVOLUTION AT z ∼ 1 (2011, methodology): “The z′ data for the SpARCS survey were obtained using the CFHT and CTIO 4m telescopes and the 3.6µm data used in SpARCS is taken from the 50 deg2 Spitzer Wide-area Extragalactic Sur- vey (SWIRE, Lonsdale et al. 2003).”
A TWO-PARAMETER MODEL FOR THE INFRARED/SUBMILLIMETER/RADIO SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES AND ACTIVE GALACTIC NUCLEI (2014, methodology): “In addition to the extant Spitzer IRAC and MIPS photometry for 5MUSES that is available from the SWIRE (Lonsdale et al. 2003) and First Look Surveys (Fadda et al. 2006; Frayer et al. 2006), we also have new Herschel 250, 350, and 500 µm SPIRE fluxes (Magdis et al. 2013).”
Photometric redshifts in the SWIRE Survey (2008, methodology): “Here we apply the template-fitting method of Rowan-Robinson (2003), Rowan-Robinson et al (2004, 2005), Babbedge et al (2004), to the data from the SPITZER-SWIRE Legacy Survey (Lonsdale et al 2003).”
The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 ≤ iAB ≤ 24.75 (2013, methodology): “Other multi-wavelength data are available in this field, with GALEX (Arnouts et al. 2005), XMM (Pierre et al. 2004), Spitzer-SWIRE (Lonsdale et al. 2003), and VLA (Bondi et al. 2003).”
Panchromatic spectral energy distributions of Herschel sources (2013, background): “…Space Observatory (ISO, e.g. ELAIS, Rowan-Robinson et al. 2004), Spitzer (e.g. Frayer et al. 2009; Le Floc’h et al. 2009; Magnelli et al. 2009; Lonsdale et al. 2003, 2004, Dickinson et al. 2001) and AKARI (e.g. Matsuura et al. 2009; Matsuhara et al. 2006) revealed the mid- and far-infrared…”