Galaxies in the Hubble Ultra Deep Field. I. Detection, Multiband Photometry, Photometric Redshifts, and Morphology

By D. Coe, N. Benı́tez, S. Sánchez, M. Jee, R. Bouwens, H. C. Ford. 2006

373 citations recorded by the source corpus.

We present aperture-matched point-spread function (PSF)-corrected BVi′z′JH photometry and Bayesian photometric redshifts (BPZ) for objects detected in the Hubble Ultra Deep Field (UDF), 8042 of which are detected at the 10 σ level (e.g., i′ < 29.01 or z′ < 28.43). Most of our objects are defined identically to those in the public STScI catalogs, enabling a straightforward object-by-object comparison. We have combined detections from i′, z′, J + H, and B + V + i′ + z′ images into a single comprehensive segmentation map. Using a new program called SExSeg, we are able to force this segmentation map into SExtractor for photometric analysis. The resulting photometry is corrected for the wider NIC3 PSFs using our ColorPro software. We also correct for the ACS z′-band PSF halo. Offsets are applied to our NIC3 magnitudes, which are found to be too faint relative to the ACS fluxes. Based on BPZ spectral energy distribution (SED) fits to objects of known spectroscopic redshift, we derived corrections of -0.30 ± 0.03 mag in J and -0.18 ± 0.04 mag in H. Our offsets appear to be supported by a recent recalibration of the UDF NIC3 images combined with nonlinearity measured in NICMOS itself. The UDF reveals a large population of faint blue galaxies (presumably young starbursts), bluer than those observed in the original Hubble Deep Fields. To accommodate these galaxies, we have added two new starburst templates to the SED library used in previous BPZ papers. The resulting photometric redshifts are accurate to within 0.04(1 + zspec) out to z < 6. Our BPZ results include a full redshift probability distribution for each galaxy. By adding these distributions, we obtain the redshift probability histogram for galaxies in the UDF. Median redshifts are also provided for different magnitude-limited samples. Finally, we measure galaxy morphology, including Sérsic index and asymmetry. Simulations allow us to quantify the reliability of our morphological results. Our full catalog, along with our software packages SExSeg and ColorPro, is available from our ACS Web site.

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

View Paper: https://www.semanticscholar.org/paper/09585afb08d7c6b920ceda37d2377b2466e1df3d

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Citations in the corpus

The Zurich Extragalactic Bayesian Redshift Analyzer and its first application: COSMOS (2006, methodology): “…mode of ZEBRA offers the possibility of correcting for any such possible systematic calibration error before performing any correction to the shape of the individual templates (as done, e.g., in Beńıtez (2000) and Capak et al. (2004); see also Coe et al. (2006) for an application).”
Discovery of a Ringlike Dark Matter Structure in the Core of the Galaxy Cluster Cl 0024+17 (2007, methodology): “For these objects, we merged their segmentation map pixels by hand and performed photometry by running SExtractor via the SExSeg software (Coe et al. 2006).”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, methodology): “Photometric Redshifts We derive photometric redshift estimates using two independent packages: BPZ (Beńıtez 2000; Beńıtez et al. 2004; Coe et al. 2006) and LePHARE (Ilbert et al. 2006, hereafter LPZ).”
CFHTLenS: Improving the quality of photometric redshifts with precision photometry (2011, methodology): “Photo-z’s are estimated with the BPZ code (Beńıtez 2000; Coe et al. 2006) one of the most-widely used photo-z codes.”
The first and second data releases of the Kilo-Degree Survey (2015, methodology): “The colours and photometric redshifts are derived from the code (Benítez 2000; Coe et al. 2006) applied to the output from a PSF-homogenized photometry pipeline – again an evolution from the CFHTLenS analysis pipeline, see Hildebrandt et al. (2012) – which runs on the calibrated stacked images…”
The Frontier Fields lens modelling comparison project (2016, methodology): “Their spectral energy distributions were obtained as part of the photometric redshift measurements of these galaxies described in Coe et al. (2006); (iii) the deflection fields of the lensing clusters are used to trace a bundle of rays from a virtual CCD, resembling the properties of the Advanced…”
New Constraints on the Lyman Continuum Escape Fraction at z ~ 1.3 (2007, methodology): “The HUDF near-IR photometry was corrected by ∆J = 0.30 and ∆H = 0.18 as discussed in Coe et al. (2006).”
CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, methodology): “Our primary photometry analysis uses the Bayesian photometric redshift softwareBPZ (Benı́tez 2000; Coe et al. 2006) to estimate photometric redshifts after performing an extinction correction on the multi-colour magnitudes.”
CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, methodology): “Coe et al. (2006) published a photometric redshift z = 2.74± 0.44 for this object using BPZ, in good agreement with the true redshift.”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, methodology): “Photometric redshifts for the CFHTLenS source catalogue have been calculated by Hildebrandt et al. (2012) using the Bayesian photometric redshift software BPZ (Benı́tez 2000; Coe et al. 2006).”
Creation of cosmic structure in the complex galaxy cluster merger Abell 2744 (2011, methodology): “To select lensed background galaxies, we obtained photometric redshifts based on our three filters using Bayesian photometric redshifts (BPZ) (Beńıtez 2000; Coe et al. 2006).”
Observations of Thick Disks in the Hubble Space Telescope Ultra Deep Field (2006, methodology): “Here we measure the disk thicknesses, colors, and perpendicular color gradients of edge-on UDF galaxies using distances from photometric redshifts (Coe et al. 2006).”
Dark Energy Survey Year 1 results: weak lensing mass calibration of redMaPPer galaxy clusters (2018, methodology): “We use the DES Y1 photometric redshifts estimated and validated by Hoyle et al. (2018) using the template-based BPZ algorithm (Benı́tez 2000; Coe et al. 2006).”
CLASH: THE ENHANCED LENSING EFFICIENCY OF THE HIGHLY ELONGATED MERGING CLUSTER MACS J0416.1−2403 (2012, methodology): “The CLASH pipeline uses the 16-band observations to derive photometric redshifts for each arc, via the BPZ program (Beńıtez et al. 2004; Coe et al. 2006), used here to constrain the model.”
A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) (2015, background): “…to the automated and crowd-sourced classifications that are a common practice in astronomy today, especially for high redshift studies (e.g., Coe et al. 2006; Huertas-Company et al. 2008; Lee et al. 2013); and (7) the large number of images that are homogeneous in sensitivity, coverage, and…”
Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift (2007, methodology): “UDF simulations by Coe et al. (2006) reveal the accuracy to which the Sérsic index n can bemeasured.”
LINE-EMITTING GALAXIES BEYOND A REDSHIFT OF 7: AN IMPROVED METHOD FOR ESTIMATING THE EVOLVING NEUTRALITY OF THE INTERGALACTIC MEDIUM (2014, methodology): “PSF matching was implemented using the ColorPro program (Coe et al. 2006).”
UV Luminosity Functions at z~4, 5, and 6 from the Hubble Ultra Deep Field and Other Deep Hubble Space Telescope ACS Fields: Evolution and Star Formation History (2007, methodology): “We measured these corrections off the square root of the χ2 image to improve the S/N. Figure 5 of Coe et al. (2006) provides a graphic description of a similar procedure.”