THESPITZERDEEP, WIDE-FIELD SURVEY

Abstract

The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 deg 2 in the Boötes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit-for the first time-the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z ∼ 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z ∼ 1.5. This paper explains the SDWFS observing strategy and data processing, presents the SDWFS mosaics and source catalogs, and discusses some early scientific findings. The publicly released, full-depth catalogs contain 6.78, 5.23, 1.20, and 0.96 × 10 5 distinct sources detected to the average 5σ , 4 -diameter, aperture-corrected limits of 19.77, 18.83, 16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0 μm, respectively. The SDWFS number counts and color-color distribution are consistent with other, earlier Spitzer surveys. At the 6 minute integration time of the SDWFS IRAC imaging, > 50% of isolated Faint Images of the Radio Sky at Twenty cm radio sources and > 80% of on-axis XBoötes sources are detected out to 8.0 μm. Finally, we present the four highest proper motion IRAC-selected sources identified from the multi-epoch imaging, two of which are likely field brown dwarfs of mid-T spectral class.

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

“…For the Bootes field, we compiled multiwavelength catalogues from the NOAO Deep-Wide Field Survey (Jannuzi & Dey 1999) DR3, SDSS DR9 (Ahn et al 2012), GALEX GR7 3 , FLAMINGOS Extragalactic Survey (Elston et al 2006), and the Spitzer Deep-Wide Field Survey (Ashby et al 2009). We use the LR method to match our X-ray catalogues to the appropriate selection band for each of these surveys, assigning secure matches from the surveys in the order of priority indicated in the Hard (2-10 keV) Figure 1.…”

The Spitzer Extragalactic Representative Volume Survey (SERVS): Survey Definition and Goals*

“…J.S. Dunlop), S-COSMOS, the Spitzer Deep Wide-Field Survey (SDWFS, Ashby et al 2009), the Spitzer-HETDEX Exploratory Large Area (SHELA, PID 80100, P.I. C. Papovich) Survey, SWIRE, the SPT-Spitzer Deep Field (SSDF, PID 80096, P.I.…”

Submillimeter number counts at 250 μm, 350 μm and 500 μm in BLAST data

“…Data in the submillimeter wavelength with increased sensitivity are thus needed to match the depth of infrared surveys, A&A 516, A43 (2010) conducted by Spitzer in the mid-and far-infrared with the MIPS instrument (Rieke et al 2004) at 24 μm, 70 μm and 160 μm (Chary et al 2004;Marleau et al 2004;Papovich et al 2004;Dole et al 2004;Frayer et al 2006a,b;Rodighiero et al 2006;Shupe et al 2008;Frayer et al 2009;LeFloc'h et al 2009;Béthermin et al 2010) as well as the near-infrared range with the IRAC instrument (Fazio et al 2004b) between 3.6 μm and 8.0 μm (Fazio et al 2004a;Franceschini et al 2006;Sullivan et al 2007;Barmby et al 2008;Magdis et al 2008;Ashby et al 2009). Infrared surveys have allowed the resolution of the CIB by identifying the contributing sources -directly at 24 μm and 70 μm, or indirectly trough stacking at 160 μm (Dole et al 2006;Béthermin et al 2010).…”