THE SPITZER DEEP, WIDE-FIELD SURVEY

By M. Ashby, Daniel Stern, M. Brodwin, R. Griffith, P. Eisenhardt, S. Kozłowski, C. Kochanek, J. Bock, C. Borys, K. Brand and 23 more. 2009

162 citations recorded by the source corpus.

The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 deg2 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 × 105 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.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/46a7a78e91600be93e1bf1e98540dfdfa90bba46

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Citations in the corpus

WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF THE EVOLUTION OF MASSIVE STAR-FORMING REGIONS (2012, methodology): “To calculate the rate of contamination in our YSO samples, we used three non-Galactic plane fields (the Boötes SDWFS field of Ashby et al. 2009 and two polar fields, all of ≈10 deg2).”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL’DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY (2012, methodology): “The Spitzer/IRAC imaging data are processed from the standard online pipeline system and analyzed as described in Ashby et al. (2009); NEWFIRM data are reduced using the FATBOY pipeline (Eikenberry et al. 2006).”
MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER. I. CHARACTERIZING WISE-SELECTED ACTIVE GALACTIC NUCLEI IN COSMOS (2012, methodology): “Prior to the launch of WISE, Ashby et al. (2009) suggested W1−W2 ≥ 0.5 would robustly identify AGN while Assef et al. (2010) suggested a color cut of W1−W2 ≥ 0.85.”
LOW-RESOLUTION SPECTRAL TEMPLATES FOR ACTIVE GALACTIC NUCLEI AND GALAXIES FROM 0.03 TO 30 μm (2010, methodology): “Ashby et al. (2009) estimated a high surface density but used a bluer cut of [3.4]–[4.6] which will introduce significant contamination by ULIRGS and starforming galaxies at low and intermediate redshifts.”
MID-INFRARED SELECTION OF ACTIVE GALACTIC NUCLEI WITH THE WIDE-FIELD INFRARED SURVEY EXPLORER. II. PROPERTIES OF WISE-SELECTED ACTIVE GALACTIC NUCLEI IN THE NDWFS BOÖTES FIELD (2012, methodology): “The Spitzer Deep, Wide-Field Survey (SDWFS; Ashby et al. 2009) quadrupled this exposure, reaching 5σ depths of 19.3, 18.5, 16.3 and 15.6 mag for [3.6], [4.5], [5.8] and [8.0], respectively.”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, methodology): “These observations are reduced following the methodology of Ashby et al. (2009).”
THE ERA OF STAR FORMATION IN GALAXY CLUSTERS (2013, methodology): “The original 90s depth IRAC Shallow Survey was repeated three more times as part of the Spitzer Deep, Wide-Field Survey (SDWFS; Ashby et al. 2009) in Spitzer Cycle 4 (PID 40839), leading to a factor of 2 increase in depth and a significantly more robust catalog in terms of resistance to cosmic rays…”
SEDS: THE SPITZER EXTENDED DEEP SURVEY. SURVEY DESIGN, PHOTOMETRY, AND DEEP IRAC SOURCE COUNTS (2013, methodology): “2.5.0; Bertin & Arnouts 1996), a standard tool for these purposes (e.g., Lonsdale et al. 2003; Ashby et al. 2009).”
A SUNYAEV–ZEL'DOVICH-SELECTED SAMPLE OF THE MOST MASSIVE GALAXY CLUSTERS IN THE 2500 deg2 SOUTH POLE TELESCOPE SURVEY (2011, methodology): “The data were reduced exactly as in Brodwin et al. (2010), following the method of Ashby et al. (2009).”
CHARACTERIZING THE MID-INFRARED EXTRAGALACTIC SKY WITH WISE AND SDSS (2012, methodology): “…of W1−W2 method, briefly discussed in Jarrett et al. (2011), is tested and discussed in detail in Stern et al. (2012) and Assef et al. (2012) (see also Ashby et al. 2009; Assef et al. 2010; Eckart et al. 2010; Edelson & Malkan 2012; Massaro et al. 2012; Wu et al. 2012; Mateos et al. 2012).”
HerMES: CANDIDATE GRAVITATIONALLY LENSED GALAXIES AND LENSING STATISTICS AT SUBMILLIMETER WAVELENGTHS (2012, methodology): “Multi-band photometry Spitzer/MIPS 24, 70 and 160µm flux densities of the candidate lensed SMGs are retrieved from archival data, including Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE) (Lonsdale et al. 2003) and the Spitzer Deep, Wide-Field Survey (SDWFS) (Ashby et al. 2009).”
Galaxy pairs in the Sloan Digital Sky Survey – IX. Merger-induced AGN activity as traced by the Wide-field Infrared Survey Explorer (2014, methodology): “We use data from theSpitzerDeep Wide-Field Survey (SDWFS; Ashby et al. (2009)), who performed deep observations with IRAC over 8 deg2 in the Boötes multiwavelength survey area.”
AN ATLAS OF GALAXY SPECTRAL ENERGY DISTRIBUTIONS FROM THE ULTRAVIOLET TO THE MID-INFRARED (2013, methodology): “For this comparison we used optical and mid-infrared colors of z ∼ 0.3 galaxies in the Boötes field (Jannuzi & Dey 1999; Ashby et al. 2009).”
THE PRISM MULTI-OBJECT SURVEY (PRIMUS). I. SURVEY OVERVIEW AND CHARACTERISTICS (2010, background): “…deep survey to K = 21, the Spitzer Wide-area Infrared Extragalactic Survey (SWIRE, Lonsdale et al. 2003), the Spitzer Deep, Wide-Field Survey (SDWFS Ashby et al. 2009) and Spitzer GTO shallow program (Eisenhardt et al. 2004), the GALEX Deep Imaging Survey (DIS), and companion deep optical imaging…”
A CORRELATION BETWEEN STAR FORMATION RATE AND AVERAGE BLACK HOLE ACCRETION IN STAR-FORMING GALAXIES (2013, methodology): “We also supplemented the AGES redshift measurements with photometric redshifts fromSpitzer Deep Wide Field Survey (SDWFS, Ashby et al. 2009) and the Spitzer IRAC (Infrared Array Camera) Shallow Survey (ISS, Brodwin et al. 2006).”
The WISE AGN Catalog (2017, methodology): “In addition to the original deep Bw, R, I and K broadband imaging from the NDWFS survey, we also use data from the NUV and FUV bands of GALEX (Martin et al. 2005), z-band from the zBoötes survey (Cool 2007), J , H and Ks bands of NEWFIRM (Gonzalez et al. 2010), the Spitzer/IRAC [3.6], [4.5], [5.8] ”