SEDS: THE SPITZER EXTENDED DEEP SURVEY. SURVEY DESIGN, PHOTOMETRY, AND DEEP IRAC SOURCE COUNTS

By M. Ashby, S. Willner, G. Fazio, J.-S. Huang, R. Arendt, Pauline Barmby, G. Barro, Eric F. Bell, R. Bouwens, A. Cattaneo and 35 more. 2013

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The Spitzer Extended Deep Survey (SEDS) is a very deep infrared survey within five well-known extragalactic science fields: the UKIDSS Ultra-Deep Survey, the Extended Chandra Deep Field South, COSMOS, the Hubble Deep Field North, and the Extended Groth Strip. SEDS covers a total area of 1.46 deg2 to a depth of 26 AB mag (3σ) in both of the warm Infrared Array Camera (IRAC) bands at 3.6 and 4.5 μm. Because of its uniform depth of coverage in so many widely-separated fields, SEDS is subject to roughly 25% smaller errors due to cosmic variance than a single-field survey of the same size. SEDS was designed to detect and characterize galaxies from intermediate to high redshifts (z = 2–7) with a built-in means of assessing the impact of cosmic variance on the individual fields. Because the full SEDS depth was accumulated in at least three separate visits to each field, typically with six-month intervals between visits, SEDS also furnishes an opportunity to assess the infrared variability of faint objects. This paper describes the SEDS survey design, processing, and publicly-available data products. Deep IRAC counts for the more than 300,000 galaxies detected by SEDS are consistent with models based on known galaxy populations. Discrete IRAC sources contribute 5.6 ± 1.0 and 4.4 ± 0.8 nW m−2 sr−1 at 3.6 and 4.5 μm to the diffuse cosmic infrared background (CIB). IRAC sources cannot contribute more than half of the total CIB flux estimated from DIRBE data. Barring an unexpected error in the DIRBE flux estimates, half the CIB flux must therefore come from a diffuse component.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0b7ae053740ebf58106f321cc5fab4a7f02e23ed

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STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS (2014, methodology): “We also release the individual stellar mass estimates computed by each team, as their comparison may be useful especially when studying peculiar objects, as well as other physical parameters (such as age, SFR, metallicity, dust reddening, etc.) and rest-frame magnitudes associated with the SED fitti”
UVUDF: ULTRAVIOLET THROUGH NEAR-INFRARED CATALOG AND PHOTOMETRIC REDSHIFTS OF GALAXIES IN THE HUBBLE ULTRA DEEP FIELD (2015, methodology): “…observations of the UDF, such as ground-based imaging (e.g., Rafelski et al. 2009) or low-resolution spacebased imaging such as Spitzer IRAC (e.g., Ashby et al. 2013), to avoid source confusion, correlated photometry, and the added systematic uncertainties associated with more complex photometric…”
Faint AGNs at z > 4 in the CANDELS GOODS-S field: looking for contributors to the reionization of the Universe (2015, methodology): “The dataset also includes very deep imaging by the IRAC instrument on board the Spitzer Space Telescope coming from the Spitzer Extended Deep Survey (SEDS; Ashby et al. (2013)) and covering the CANDELS fields to 26 AB mag (3σ) at both 3.6 and 4.5 µm.”
X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue (2014, methodology): “For identification of counterparts, the J/K/H-band positions from the CANDELS (Koekemoer et al. 2011; Grogin et al. 2012) CDFS field (Guo et al. 2013; Hsieh et al. 2012) are used in combination with mid-infrared positions from IRAC (Damen et al. 2011; Ashby et al. 2013).”
THE EVOLUTION OF THE GALAXY STELLAR MASS FUNCTION AT z = 4–8: A STEEPENING LOW-MASS-END SLOPE WITH INCREASING REDSHIFT (2015, methodology): “Duncan et al. (2014) and Grazian et al. (2015) derived the GSMFs of galaxies at 4 < z < 7 in the GOODS-S field and GOODS-S/UDS fields, respectively, using the CANDELS HST data and the Spitzer Extended Deep Survey (SEDS; Ashby et al. 2013) IRAC data.”
GOODS-ALMA: 1.1 mm galaxy survey (2018, methodology): “These data have been supplemented by the Spitzer Extended Deep Survey (SEDS; PI: G. Fazio) at 3.6 and 4.5 µm (Ashby et al. 2013) as well as the Spitzer-Cosmic Assembly Near-Infrared Deep Extragalactic Survey (S-CANDELS; Ashby et al. 2015) and recently by the ultradeep IRAC imaging at 3.6 and 4.5 µm…”
THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION OVER THE FIRST TWO BILLION YEARS (2014, methodology): “Later, during Cycle 6 of the warm mission, broader regions encompassing the GOODS footprints were covered by the Spitzer Extended Deep Survey (SEDS Ashby et al. 2013) to 3σ depths of 26 AB mag at both 3.6 and 4.5 μm.”
THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, methodology): “In addition to CANDELS, this work includes the Early Release Science (ERS), Hubble Ultra Deep Field (HUDF), and deep IRAC imaging in all four IRAC channels (3.6–8.0 µm) from the Spitzer Extended Deep Survey (Ashby et al. 2013) programs.”
UV LUMINOSITY FUNCTIONS AT REDSHIFTS z ∼ 4 TO z ∼ 10: 10,000 GALAXIES FROM HST LEGACY FIELDS (2014, methodology): “A full consideration of the available Spitzer/IRAC (Ashby et al. 2013) and IRAC Ultra Deep Field 2010 (IUDF10: Labbé et al. 2013) observations over our fields are made in setting constraints on the LF at z ∼ 10 (see Oesch et al. 2014).”
A deep ALMA image of the Hubble Ultra Deep Field (2016, methodology): “Imaging longward of 2.2µm has been obtained with Spitzer, with new ultra-deep IRAC imaging of the HUDF at 3.6µm and 4.5µm being provided by our own stack of the available public data described by Labbé et al. (2015) (see also Ashby et al. 2013, 2015).”
THE EXTRAGALACTIC BACKGROUND LIGHT, THE HUBBLE CONSTANT, AND ANOMALIES: CONCLUSIONS FROM 20 YEARS OF TeV GAMMA-RAY OBSERVATIONS (2015, methodology): “In addition to constraints listed by Dwek & Krennrich (2013), we also include the lower limits at 3.6 and 4.5 mm from Ashby et al. (2013).”
THE 2 Ms CHANDRA DEEP FIELD-NORTH SURVEY AND THE 250 Ks EXTENDED CHANDRA DEEP FIELD-SOUTH SURVEY: IMPROVED POINT-SOURCE CATALOGS (2016, methodology): “As a comparison, Figure 22(c) presents the IRAC 3.6 μm magnitude versus the full-band flux for the new sources and old sources, since a larger fraction of 22 We note that the stacked averages only indicate the mean properties and cannot represent the full distribution of the stacked sample.”
THE MOST LUMINOUS z ∼ 9–10 GALAXY CANDIDATES YET FOUND: THE LUMINOSITY FUNCTION, COSMIC STAR-FORMATION RATE, AND THE FIRST MASS DENSITY ESTIMATE AT 500 Myr (2013, methodology): “Data in GOODS-N were obtained in two epochs in 2012 and combined with pre-existing IRAC data from SEDS (Ashby et al. 2013) and the original GOODS program (Dickinson et al. 2003).”
HYDROGEN-POOR SUPERLUMINOUS SUPERNOVAE AND LONG-DURATION GAMMA-RAY BURSTS HAVE SIMILAR HOST GALAXIES (2013, background): “Four of the lower-redshift PS1 host galaxies are detected in archival images from the Spitzer Extragalactic Representative Volume Survey (SERVS; Mauduit et al. 2012), the COSMOS Spitzer survey (S-COSMOS; Sanders et al. 2007), or the Spitzer Extended Deep Survey (SEDS; Ashby et al. 2013).”
AN INTENSELY STAR-FORMING GALAXY AT z ∼ 7 WITH LOW DUST AND METAL CONTENT REVEALED BY DEEP ALMA AND HST OBSERVATIONS (2013, methodology): “Spitzer Although Spitzer cannot match the resolution of the above morphological data, we use the very deep Spitzer/IRAC SEDS data reaching 26 mag at the 3σ level (Ashby et al. 2013) to investigate the counterpart of the overall Himiko system at 3.6µm and 4.5µm bands.”
The mass evolution of the first galaxies: stellar mass functions and star formation rates at 4 < z < 7 in the CANDELS GOODS-South field (2014, methodology): “The Spitzer/IRAC (Fazio et al. 2004) 3.6 and 4.5 µm images were taken from the Spitzer Extended Deep Survey (PI: G. Fazio, Ashby et al. 2013) incorporating the pre-existing cryogenic observations from the GOODS Spitzer Legacy project (PI: M. Dickinson).”
3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES (2014, methodology): “2 data release for the 3.6 and 4.5µm pass bands (Ashby et al. 2013).”
An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source (2015, methodology): “The Spitzer/IRAC 1 and 2 data are taken from the SCANDELS survey (Ashby et al. 2015), while the IRAC 3 and 4 are taken from Ashby et al. (2013).”
The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching? (2013, methodology): “Mid-infrared imaging over the COSMOS field by Spitzer/IRAC exists from two programmes; the Spitzer Extended Deep Survey (SEDS; Ashby et al. 2013) and the Spitzer Large Area Survey with Hyper-SuprimeCam (SPLASH, PI: Capak).”