WFPC2 Observations of the Hubble Deep Field South

By S. Casertano, D. D. de Mello, Mark Dickinson, H. Ferguson, A. Fruchter, R. A. González-Lópezlira, I. Heyer, R. Hook, Z. Levay, R. Lucas and 7 more. 2000

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The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z > 2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z ∼ 2.7, and a factor of 1.3 higher at z ∼ 4.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/166d607a4115aef09bfef27d8344675640434557

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Citations in the corpus

The Luminosity, Stellar Mass, and Number Density Evolution of Field Galaxies of Known Morphology from z = 0.5 to 3 (2004, background): “…data are the Hubble Deep Field North WFPC2 (Williams et al. 1996) and NICMOS fields (Dickinson et al. 2000, 2003) (hereafter HDF-N) as well as the Hubble Deep Field South WFPC2 images (hereafter HDF-S) (Casertano et al. 2000) and the VLT near infrared ISAAC images of the HDF-S (Labbé et al. 2003).”
THE 2012 HUBBLE ULTRA DEEP FIELD (UDF12): OBSERVATIONAL OVERVIEW (2012, background): “…HST have yielded a wealth of scientific results to date, from the original Hubble Deep Field (Williams et al. 1996) and Hubble Deep Field South (Casertano et al. 2000; Williams et al. 2000; Lucas et al. 2003), together with the 2004 Ultra Deep Field (UDF: Beckwith et al. 2006; Thompson et al.…”
Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies (2014, methodology): “…correlations introduced by the drizzling process between neighbouring pixels, which artificially reduce the noise level of co-added drizzled images, we apply the remedy used by L07: simply scaling up the noise level in each pixel by the same constant FA ≈ 0.316, defined by Casertano et al. (2000).”
Clustering Segregation with Ultraviolet Luminosity in Lyman Break Galaxies at z~3 and Its Implications (2000, background): “The fainter one comes from the HDF surveys, both the North and South (Williams et al. 1996, 1998 ; Casertano et al. 2000).”
The First Release COSMOS Optical and Near-IR Data and Catalog (2007, background): “M. Iye & A. F. M. Moorwood, 72–81 Brott, I. & Hauschildt, P. H. 2005, in ESA SP-576, 565–+ Capak et al., 2004, AJ, 127, 180 Casertano et al., 2000, AJ, 120, 2747 Cowie, L. L., Songaila, A., & Barger, A. J. 1999, AJ, 118, 603 Daddi et al., 2004, ApJ, 617, 746 Dahlen et al., 2005, ApJ, 631, 126…”
Measuring the Redshift Evolution of Clustering: the Hubble Deep Field South (2001, background): “The data more recently obtained in the HDF-South (Casertano et al. 2000) offer a unique opportunity to test the robustness of HDF-North results, because of their mutual independence.”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, methodology): “At z ∼ 2.5, we use the deep U -band coverage available over the WFPC2 Hubble Deep Field (HDF) North (Williams et al. 1996) and HDF South (Casertano et al. 2000) to select z ∼ 2.5 U -dropouts.”
The GOODS-MUSIC sample: a multicolour catalog of near-IR selected galaxies in the GOODS-South field , (2006, background): “Therefore, the apparent rms background noise that one measures in the image is smaller than the actual rms, due to the effects of these correlations (for a more detailed discussion of weight map conventions and noise correlation in drizzling, please see Casertano et al. 2000, especially Sect.”
A CENSUS OF STAR-FORMING GALAXIES IN THE Z ∼ 9–10 UNIVERSE BASED ON HST+SPITZER OBSERVATIONS OVER 19 CLASH CLUSTERS: THREE CANDIDATE Z ∼ 9–10 GALAXIES AND IMPROVED CONSTRAINTS ON THE STAR FORMATION RATE DENSITY AT Z ∼ 9.2 (2012, methodology): “…z ∼ 1.3-2 galaxy case, we calibrate our priors based on the LF results of Giallongo et al. (2005) for red galaxies using deep near-IR observations available over the HDF-North and HDF-South fields (Williams et al. 1996; Casertano et al. 2000) and the K20 spectroscopic sample (Cimatti et al. 2002).”
Extended Lyman α haloes around individual high-redshift galaxies revealed by MUSE (2015, methodology): “Notice that the HST/WFPC2 F814W magnitudes are not identical to those from B2015 (taken in turn from Casertano et al. 2000), but were redetermined by us using GALFIT modelling as described in Sect.”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “Corrections to account for the effects of correlated noise have been made to address correlated noise in photometry measurements (Casertano et al. 2000; Masci 2009) and in shape measurements (Schrabback et al. 2007).”
The MUSE 3D view of the Hubble Deep Field South (2014, methodology): “Interestingly, 26 of the discovered Lyα emitters are below the HST detection limit, i.e V606> 29.6 and I814> 29 (3σ depth in a 0.2 arcsec2 aperture, Casertano et al. 2000).”
IRAC Mid-Infrared Imaging of the Hubble Deep Field-South: Star Formation Histories and Stellar Masses of Red Galaxies at z > 2 (2005, unknown): “In addition, we selected isolated LBGs in the same field to the sameKs-band limit and in the same redshift range, using theU-dropout criteria of Madau et al. (1996) on the WFPC2 imaging (Casertano et al. 2000).”
3D-HST: A WIDE-FIELD GRISM SPECTROSCOPIC SURVEY WITH THE HUBBLE SPACE TELESCOPE (2012, methodology): “…account for the effects of drizzling, which tends to smooth out some of the apparent noise because the pixel errors tend to be correlated (e.g., Casertano et al. 2000). are extracted using the technique described in Section 4.2 and uncertainties on the line fluxes are determined with an MCMC…”
Ultradeep Near-Infrared ISAAC Observations of the Hubble Deep Field South: Observations, Reduction, Multicolor Catalog, and Photometric Redshifts (2002, methodology): “The combined ISAAC images are aligned with the HST version 2 images (Casertano et al. 2000) with north up and are normalized to instrumental counts per second.”
CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results (2022, methodology): “In this case, the noise in the resampled science images and variance maps is reduced by the cor- relations, and so photometric uncertainties will by underestimated (e.g., Casertano et al. 2000; Labbé et al. 2003; Blanc et al. 2008; Whitaker et al. 2011; Papovich et al. 2016).”
The Rise of Faint, Red Active Galactic Nuclei at z > 4: A Sample of Little Red Dots in the JWST Extragalactic Legacy Fields (2025, unknown): “2; Gaia Collaboration et al. 2016 ) and combined into a single mosaic for each ﬁ eld using the drizzle algorithm with an inverse variance map weighting ( S. Casertano et al. 2000; A. S. Fruchter & R. N. Hook 2002 ) via the Resample step in the pipeline.”