ESO imaging survey - Deep public survey: Multi-color optical data for the Chandra Deep Field South

By Stéphane Arnouts, B. Vandame, C. Benoist, M. Groenewegen, L. D. Costa, M. Schirmer, R. Mignani, R. Slijkhuis, E. Hatziminaoglou, R. N. Hook and 3 more. 2001

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This paper presents multi-passband optical data obtained from observations of the Chandra Deep Field South (CDF-S), located at 3 h 32 m , 2748 0 . The observations were conducted at the ESO/MPG 2.2 m telescope at La Silla using the 8k 8k Wide-Field Imager (WFI). This data set, taken over a period of one year, represents the rst eld to be completed by the ongoing Deep Public Survey (DPS) being carried out as a part of the ESO Imaging Survey (EIS) project. This paper describes the optical observations, the techniques employed for un-supervised pipeline processing and the general characteristics of the nal data set. Image processing has been performed using multi-resolution image decomposition techniques adapted to the EIS pipeline. The automatic processing steps include standard de-bias and flat-eld, automatic removal of satellite tracks, de-fringing/sky-subtraction, image stacking/mosaicking and astrometry. Stacking of dithered images is carried out using pixel-based astrometry which enables the ecient removal of cosmic rays and image defects, yielding remarkably clean nal images. The nal astrometric calibration is based on a pre-release of the GSC-II catalog and has an estimated intrinsic accuracy of <0.10 arcsec, with all passbands sharing the same solution. The paper includes data taken in six dierent lters (U 0 UBVRI). The data cover an area of about 0.25 square degrees reaching 5 limiting magnitudes of U 0 AB =2 6:0, UAB =2 5:7, BAB =2 6:4, VAB =2 5:4;RAB =2 5: 5a nd IAB = 24.7 mag, as measured within a 2FWHM aperture. The optical data covers an area of 0.1 square degrees for which moderately deep observations in two near-infrared bands are also available, reaching 5 limiting magnitudes of JAB 23: 4a ndKAB 22:6. The current optical/infrared data also fully encompass the region of the deep X-ray observations recently completed by the Chandra telescope. The optical data presented here, as well as the infrared data released earlier, are publicly available world-wide in the form of fully calibrated pixel and associated weight maps and source lists extracted in each passband. These data can be requested through the URL \http://www.eso.org/eis".

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d413d76f2197d9242f886bd7795e3a53d504bac8

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Citations in the corpus

Theoretical isochrones in several photometric systems I. Johnson-Cousins-Glass, HST/WFPC2, HST/NICMOS, Washington, and ESO Imaging Survey filter sets (2002, methodology): “It is evident from this plot that the normal Johnson-Cousins isochrones cannot be used to interpret WFI data that has been converted to VEGAmag or ABmag systems, as for most of EIS data (e.g. Arnouts et al. 2001; Groenewegen et al. 2002)6.”
The Chandra Deep Field-South: Optical Spectroscopy. I. (2003, background): “The ESO Imaging Survey (EIS) has covered this field to moderate depths (5 limiting AB magnitudes of 26.0, 25.7, 26.4, 25.4, 25.5, and 24.7 in U 0, U, B, V, R, and I, respectively) in several bands (Arnouts et al. 2001; Vandame et al. 2001).”
THE MULTIWAVELENGTH SURVEY BY YALE–CHILE (MUSYC): DEEP MEDIUM-BAND OPTICAL IMAGING AND HIGH-QUALITY 32-BAND PHOTOMETRIC REDSHIFTS IN THE ECDF-S (2010, unknown): “MUSYC Survey: Existing Optical and Near-Infrared Data The Extended Chandra Deep Field-South (ECDFS) has been targeted by a host of optical and infrared surveys (Arnouts et al. 2001; Moy et al. 2003; Wolf et al. 2004; Gawiser et al. 2006b; Hildebrandt et al. 2006; Damen et al 2010, submitted).”
The Extended Chandra Deep Field-South Survey: Chandra Point-Source Catalogs (2005, unknown): “Excellent ground-based imaging is also available (e.g., Arnouts et al. 2001; Renzini et al. 2003; Giavalisco et al. 2004; Wolf et al. 2004; Gawiser et al. 2005), and several spectroscopic campaigns are underway to identify sources in the E-CDF-S, most notably with the Very Large Telescope (VLT;…”
FIREWORKS U38-to-24 μm Photometry of the GOODS Chandra Deep Field-South: Multiwavelength Catalog and Total Infrared Properties of Distant Ks-selected Galaxies (2008, methodology): “In the case of the NIR ISAAC observations, the publicly released zero points were based onSOFI images of the EIS-DEEP andDPS infrared surveys conducted over the same region (Vandame et al. 2001), which themselves were photometrically calibrated using standard stars from Persson et al. (1998).”
Infrared Power-Law Galaxies in the Chandra Deep Field-South: Active Galactic Nuclei and Ultraluminous Infrared Galaxies (2006, methodology): “…been supplemented with optical and near-IR data sets available from the literature: (1) optical images (UUpBVRI ) from the ESO Imaging Survey (EIS; Arnouts et al. 2001 10), (2) optical fluxes from the COMBO-17 survey (Wolf et al. 2004), (3) RIz imaging obtained by the Las Campanas Infrared Survey…”
The evolution of the luminosity functions in the FORS Deep Field from low to high redshift: I. The blue bands (2004, background): “…deep Field (NDF; Arnouts et al. 1999), Hubble Deep Field South (HDFS; Williams et al. 2000; Casertano et al. 2000), Chandra Deep Field South (CDFS; Arnouts et al. 2001), William Herschel Deep Field (WHDF; McCracken et al. 2000; Metcalfe et al. 2001), Subaru Deep Field/Survey (SDF; Maihara et al.…”
The Fall of Active Galactic Nuclei and the Rise of Star-forming Galaxies: A Close Look at the Chandra Deep Field X-Ray Number Counts (2004, methodology): “Optical magnitudes for the CDF sources have been measured using Subaru observations in the CDF-N (Barger et al. 2003) and Wide-Field Imager (WFI) observations as part of an ESO deep public survey in the CDF-S (e.g., Arnouts et al. 2001).”
The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging (2003, methodology): “2 a The WFI U band is highly nonstandard (see Arnouts et al. 2001).”
Galaxies at z ~ 6: The UV Luminosity Function and Luminosity Density from 506 HUDF, HUDF Parallel ACS Field, and GOODS i-Dropouts (2005, methodology): “Zero points for the individual ISAAC frames were derived by matching photometry of ∼50 stars on each frame with the shallower SOFI (Arnouts et al. 2001) and Two Micron All Sky Survey (2MASS; Skrutskie et al. 1997) images.”
A New Photometric Technique for the Joint Selection of Star-forming and Passive Galaxies at 1.4 ≲ z ≲ 2.5 (2004, methodology): “ShallowerU-band imaging from Arnouts et al. (2001) was also used, obtained at the ESO 2.2m telescope.”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY—THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS, AND MOSAICS (2011, methodology): “For GOODS-South, we use an R-band mosaic from the ESO-MPI 2.2m / Wide Field Imager (WFI) obtained as part of the ESO Imaging Survey (EIS) of the field (Arnouts et al. 2001), registered to the GSC-2 (Lasker et al. 2008).”
The Chandra Deep Field North Survey. XIII. 2 Ms Point-Source Catalogs (2003, methodology): “The optical data used to create the optical source list was the R-band Wide-Field Imager (WFI) observations taken as part of the ESO Imaging Survey (Arnouts et al. 2001).”
Structure and Star Formation in Galaxies out to z = 3: Evidence for Surface Density Dependent Evolution and Upsizing (2008, methodology): “The optical imaging consisted of ACS GOODS imaging (Giavalisco et al 2004), and deep imaging with the ESO/MPG 2.2-m telescope (Arnouts et al. 2001, Wolf et al. 2004).”
The stellar masses of 25 000 galaxies at 0.2 ≤ z ≤ 1.0 estimated by the COMBO-17 survey (2006, methodology): “We have used deep, public, fully-reduced J, H, and K-band data on a 50 square arcminute sub-region of the CDFS taken with ISAAC at the VLT as a part of the ESO Imaging Survey EIS (Hatziminaoglou et al.2002).”
Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate (2005, methodology): “The Spitzer astrometry is aligned to the ESO Imaging Survey (Arnouts et al. 2001) with a typical accuracy 0B5.”
The 2dF Galaxy Redshift Survey: power-spectrum analysis of the final data set and cosmological implications (2005, methodology): “In the preliminary 100k release (Colless et al. 2001), the APM magnitudes were directly recalibrated using CCD data from the EIS (Prandoni et al. 1999; Arnouts et al. 2001) and 2MASS (Jarrett et al. 2000) (see Norberg et al. 2002b).”
EAZY: A Fast, Public Photometric Redshift Code (2008, methodology): “We use the CDFSGOODS catalog of Wuyts et al. (2008) which combines the deep HST GOODS photometry with ground-based UBVRI photometry from the ESO Deep Public Survey (Arnouts et al. 2001).”