CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY

By Norman Grogin, D. Kocevski, S. Faber, H. Ferguson, A. Koekemoer, A. Riess, V. Acquaviva, D. M. Alexander, O. Almaini, M. Ashby and 97 more. 2011

891 citations recorded by the source corpus.

The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) is designed to document the first third of galactic evolution, over the approximate redshift (z) range 8–1.5. It will image >250,000 distant galaxies using three separate cameras on the Hubble Space Telescope, from the mid-ultraviolet to the near-infrared, and will find and measure Type Ia supernovae at z > 1.5 to test their accuracy as standardizable candles for cosmology. Five premier multi-wavelength sky regions are selected, each with extensive ancillary data. The use of five widely separated fields mitigates cosmic variance and yields statistically robust and complete samples of galaxies down to a stellar mass of 109M☉ to z ≈ 2, reaching the knee of the ultraviolet luminosity function of galaxies to z ≈ 8. The survey covers approximately 800 arcmin2 and is divided into two parts. The CANDELS/Deep survey (5σ point-source limit H = 27.7 mag) covers ∼125 arcmin2 within Great Observatories Origins Deep Survey (GOODS)-N and GOODS-S. The CANDELS/Wide survey includes GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-deep Survey) and covers the full area to a 5σ point-source limit of H ≳ 27.0 mag. Together with the Hubble Ultra Deep Fields, the strategy creates a three-tiered “wedding-cake” approach that has proven efficient for extragalactic surveys. Data from the survey are nonproprietary and are useful for a wide variety of science investigations. In this paper, we describe the basic motivations for the survey, the CANDELS team science goals and the resulting observational requirements, the field selection and geometry, and the observing design. The Hubble data processing and products are described in a companion paper.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9502926fddd53fdaf9f82bbd022fcd823b2b8dad

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Citations in the corpus

• JADES Initial Data Release for the Hubble Ultra Deep Field: Revealing the Faint Infrared Sky with Deep JWST NIRCam Imaging (2023, methodology): “We also report the fractional fl ux median offset between CANDELS and JADES for objects brighter than the 5 σ extended object depth reported by Grogin et al. ( 2011 ) for each CANDELS band ( blue dashed line ) .”
• Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, positive): “…(imaging in Beckwith et al. 2006), and the near-infrared ones in four WFC3 bands, F105W, F125W, F140W and F160W, from the UDF09, UDF12 (Oesch et al. 2010a,b; Bouwens et al. 2011; Ellis et al. 2013; Koekemoer et al. 2013) and CANDELS GOODS-S programs (Grogin et al. 2011; Koekemoer et al. 2011).”
• The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5 (2023, methodology): “For our astrometric alignment and analysis we make use of the archival Hubble Space Telescope ( HST ) imaging from the All-wavelength Extended Groth Strip International Survey ( AEGIS; Davis et al. 2007 ) , the Cosmic Assembly Deep Extragalactic Legacy Survey ( CANDELS; Grogin et al. 2011; Koekemoer”
• The Rise of Faint, Red Active Galactic Nuclei at z > 4: A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields (2025, positive): “…measured in all of the available NIRCam bands in each fi eld, as well as the F606W and F814W Hubble Space Telescope ( HST ) bands using public data from the CANDELS and 3D-HST surveys ( N. A. Grogin et al. 2011; A. M. Koekemoer et al. 2011; G. B. Brammer et al. 2012; I. G. Momcheva et al. 2016 ) .”
• EMERGE – an empirical model for the formation of galaxies since z ∼ 10 (2017, neutral): “A different option has emerged with the advent of data sets from large galaxy surveys (York et al. 2000; Colless et al. 2001; Lilly et al. 2007; Driver et al. 2011; Grogin et al. 2011; McCracken et al. 2012) and avoids explicitly modelling the baryonic physics.”
• 3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES (2014, positive): “The largest area WFC3 imaging survey done to date is the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS, Grogin et al. 2011; Koekemoer et al. 2011), a 912-orbit Multi-Cycle Treasury imaging program (PIs: S. Faber and H. Ferguson).”
• The ALPINE-ALMA [CII] survey (2020, positive): “The data that we use in the area of the ECDFS is from the CANDELS survey (Grogin et al. 2011; Koekemoer et al. 2011).”
• THE 3D-HST SURVEY: HUBBLE SPACE TELESCOPE WFC3/G141 GRISM SPECTRA, REDSHIFTS, AND EMISSION LINE MEASUREMENTS FOR ∼100,000 GALAXIES (2015, positive): “The survey fields were chosen to coincide with those of the CANDELS Multi-Cycle Treasury project (Grogin et al. 2011; Koekemoer et al. 2011).”
• The UV continua and inferred stellar populations of galaxies at z ~7-9 revealed by the Hubble Ultra-Deep Field 2012 campaign (2012, positive): “…et al. 2010), WFC3/IR has been used to conduct wider-area surveys for more luminous galaxies at z = 7–8, both through the CANDELS Treasury programme (Grogin et al. 2011; C© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society at U niversity of St A…”
• 3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3 (2014, positive): “To extend the dynamic range we analyze ACS/F814W imaging in the COSMOS field from CANDELS parallel observations.”
• The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, positive): “The reference SFG population is here taken from the CANDELS/3D-HST surveys (Grogin et al. 2011; Koekemoer et al. 2011; Skelton et al. 2014; Momcheva et al. 2016), which provide the largest sample with sizes measured in the near-IR from HST imaging (van der Wel et al. 2012, 2014b).”
• SUBMILLIMETER GALAXIES AS PROGENITORS OF COMPACT QUIESCENT GALAXIES (2014, positive): “The sample is also covered by high-resolution NIR imaging with HST / WFC3 from the CANDELS survey (Grogin et al. 2011; Koekemoer et al. 2011), yielding accurate constraints on the rest-frame optical surface brightness profiles and effective radii ( r e ).”
• THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, positive): “The 3D-HST survey overlaps with the imaging fields of the CANDELS survey, which contributes highresolution WFC3 near-IR imaging along with ACS imaging for all the KMOS3D targets (Grogin et al. 2011; Koekemoer et al. 2011).”
• THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION, AND REDSHIFTS (2012, positive): “Most recently, EGS has become one of five fields targeted by the CANDELS (Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey) Multi-Cycle Treasury program on HST (Grogin et al. 2011; Koekemoer et al. 2011); it is being imaged deeply with both the ACS and WFC3 instruments as part of this ”
• THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR ∼1500 H-SELECTED GALAXIES AT 1.37 ≤ z ≤ 3.8 ?> (2014, positive): “Within all fields we target the regions that are covered by the CANDELS (Grogin et al. 2011; Koekemoer et al. 2011) and 3D-HST (Brammer et al. 2012) surveys, as illustrated in Figure 2 for the three primary fields.”
• The birth of a galaxy – III. Propelling reionization with the faintest galaxies (2014, positive): “Deep galaxy surveys, such as the Hubble Ultra Deep Field (HUDF; Beckwith et al. 2006; Koekemoer et al. 2013) and CANDELS (Grogin et al. 2011; Koekemoer et al. 2011) can probe z 6 galaxies up to absolute UV magnitudes MUV < −18 or equivalently a stellar mass of M∗ 108 M .”
• HST/WFC3 CONFIRMATION OF THE INSIDE-OUT GROWTH OF MASSIVE GALAXIES AT 0 < z < 2 AND IDENTIFICATION OF THEIR STAR-FORMING PROGENITORS AT z ∼ 3 (2012, positive): “To measure structural parameters we utilize HST imaging in the UDS that was acquired as part of CANDELS9 (Grogin et al. 2011).”
• Type-Ia Supernova Rates and the Progenitor Problem: A Review (2011, neutral): “Two ongoing multi-cycle treasury (MCT) programs with HST, CLASH (Postman et al. 2011) and CANDELS (Grogin et al. 2011; Koekemoer et al. 2011) aim to measure the SN rate out to z = 2 and perhaps even somewhat beyond.”