The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging

By M. Giavalisco, H. Ferguson, A. Koekemoer, M. Dickinson, David B. Alexander, F. E. Bauer, J. Bergeron, C. Biagetti, W. N. Brandt, S. Casertano and 47 more. 2003

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This special issue of the Astrophysical Journal Letters is dedicated to presenting initial results from the Great Observatories Origins Deep Survey (GOODS) that are primarily, but not exclusively, based on multiband imaging data obtained with the Hubble Space Telescope and the Advanced Camera for Surveys (ACS). The survey covers roughly 320 arcmin2 in the ACS F435W, F606W, F814W, and F850LP bands, divided into two well-studied fields. Existing deep observations from the Chandra X-Ray Observatory and ground-based facilities are supplemented with new, deep imaging in the optical and near-infrared from the European Southern Observatory and from the Kitt Peak National Observatory. Deep observations with the Space Infrared Telescope Facility are scheduled. Reduced data from all facilities are being released worldwide within 3-6 months of acquisition. Together, this data set provides two deep reference fields for studies of distant normal and active galaxies, supernovae, and faint stars in our own Galaxy. This Letter serves to outline the survey strategy and describe the specific data that have been used in the accompanying letters, summarizing the reduction procedures and sensitivity limits.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/682e33dcb50ba277f466c457bee25ebdec303a6f

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Citations in the corpus

SEDS: THE SPITZER EXTENDED DEEP SURVEY. SURVEY DESIGN, PHOTOMETRY, AND DEEP IRAC SOURCE COUNTS (2013, methodology): “The HDFN was first observed by IRAC in Spitzer Cycle 1 by the GOODS team (Giavalisco et al. 2004), who used a narrow and deep configuration to cover the multiband data originally obtained with HST (Williams et al. 1996).”
A New Photometric Technique for the Joint Selection of Star-forming and Passive Galaxies at 1.4 ≲ z ≲ 2.5 (2004, methodology): “…photometry is available for this field, including groundbasedBVRIzJHK imaging with very good seeing (generally 0.4–0.7′′) obtained with FORS1, FORS2 and ISAAC at the VLT (the same imaging dataset used in D04), together with the HST+ACSbviz data released by the GOODS Team (Giavalisco et al. 2004).”
Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints (2005, background): “ACS imaging of GOODS fields (Giavalisco et al. 2004a) will potentially allow us to make these determinations, although high-resolution deep infrared imaging is needed to make definitive progress.”
THE EVOLUTION OF GALAXY NUMBER DENSITY AT z < 8 AND ITS IMPLICATIONS (2016, background): “This was later expanded to other deep fields such as the Hubble Deep Field South (Williams et al. 2000), the Great Observatories Origins Survey (Giavalisco et al. 2004), and the near-infrared CANDELS fields (Grogin et al. 2011; Koekemoer et al. 2011), and finally to the Hubble Ultra Deep Field…”
GALAXY STELLAR MASS ASSEMBLY BETWEEN 0.2 < z < 2 FROM THE S-COSMOS SURVEY (2009, methodology): “Bundy et al. (2005), Franceschini et al. (2006) and Pannella et al. (2006) have derived the MF by morphological type using respectively 2150, 1478 and 1645 galaxies at z < 1.4 in the two GOODS fields covering 160 arcmin2 each (Giavalisco et al. 2004).”
DEEP U BAND AND R IMAGING OF GOODS-SOUTH: OBSERVATIONS, DATA REDUCTION AND FIRST RESULTS, (2009, methodology): “A source catalog was also produced and matched against the same astrometric catalog originally used to provide an astrometric grid for the ACS mosaic (Giavalisco et al. 2004; see Appendix A for details).”
BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, methodology): “Additional data used for this work include pre-existing ACS imaging in the GOODS, EGS, and COSMOS fields (Giavalisco et al. 2004; Davis et al. 2007; Koekemoer et al. 2007), plus WFC3 imaging in ERS (Windhorst et al. 2011).”
PHAT: PHoto-z Accuracy Testing (2010, methodology): “The imaging data for this test are part of the Great Observatories Origins Deep Survey northern field (GOODS-N, Giavalisco et al. 2004).”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, methodology): “This is largely because many previous studies corrected the star formation rate density by factors of ∼ 5 − 8× (e.g., Giavalisco et al. 2004b) – which is the dust correction relevant for L∗ galaxies.”
THE SPITZER DEEP, WIDE-FIELD SURVEY (2009, background): “Much as the Great Observatory Origins Deep Survey (GOODS; Giavalisco et al. 2004) fields have become the fields of choice for ultradeep pencil-beam surveys across the electromagnetic spectrum, the 9 deg2 Boötes field has become the wide-area, deep survey field of choice and thus was chosen as the…”
The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei (2004, methodology): “In Figure 29, we show for the sources in the ACS GOODSNorth region of the CDF-N the host galaxy luminosities (excluding the nuclear contributions) computed at rest-frame 5000 8 versus redshift.”
The extragalactic background light revisited and the cosmic photon–photon opacity (Corrigendum) (2017, background): “…300 square arcminutes each, and the latter an area of approximately 2 sq.deg., all including a vast amount of complementary data in all e.m. bands (Giavalisco et al. 2004; Scoville et al. 2007; Sanders et al. 2007), optical spectroscopic surveys (Lilly et al. 2007) and highly precise photometric…”
Star formation and mass assembly in high-redshift galaxies (2009, methodology): “We present and use an updated version of the multicolour GOODS-MUSIC sample (GOODS MUlticolour Southern Infrared Catalog; Grazian et al. 2006), extracted from the public data of the GOODS-South survey (Giavalisco et al. 2004).”
THE PERSISTENCE OF COOL GALACTIC WINDS IN HIGH STELLAR MASS GALAXIES BETWEEN z ∼ 1.4 AND ∼1 (2009, methodology): “The limiting surface brightness at 1σ in a 1 arcsec2 aperture in the F850LP band is μAB = 27.3 mag arcsec−2 (Giavalisco et al. 2004, ver.”
Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies (2015, methodology): “We analyze the star-formation and structural properties of massive galaxies in the CANDELS/GOODS-S field to study the relation between stellar mass and structural growth, and the role of the latter in the quenching of star-formation since z ∼ 3.”
The Large-Scale and Small-Scale Clustering of Lyman Break Galaxies at 3.5 ⩽ z ⩽ 5.5 from the GOODS Survey (2005, methodology): “They are also described in Giavalisco et al. (2004a), and we refer the reader to that publication for details.”