The Hubble Ultra Deep Field

By S. Beckwith, M. Stiavelli, A. Koekemoer, J. Caldwell, H. Ferguson, R. Hook, R. Lucas, L. Bergeron, M. Corbin, S. Jogee and 5 more. 2003

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This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million s exposure of an 11 arcmin2 region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i 775), and F850LP (z850), to give approximately uniform limiting magnitudes mAB ∼ 29 for point sources. The image contains at least 10,000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ∼4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density. Examination of the catalog for dropout sources yields 504 B435 dropouts, 204 V 606 dropouts, and 54 i775 dropouts. The i775 dropouts are most likely galaxies at redshifts between 6 and 7. Using these samples, which are at different redshifts but derived from the same data, we find no evidence for a change in the characteristic luminosity of galaxies but some evidence for a decrease in their number densities between redshifts of 4 and 7. Assessing the factors needed to derive the luminosity function from the data suggests that there is considerable uncertainty in parameters from samples discovered with different instruments and derived using independent assumptions about the source populations. This assessment calls into question some of the strong conclusions of recently published work on distant galaxies. The ultraviolet luminosity density of these samples is dominated by galaxies fainter than the characteristic luminosity, and the HUDF reveals considerably more luminosity than shallower surveys. The apparent ultraviolet luminosity density of galaxies appears to decrease from redshifts of a few to redshifts greater than 6, although this decrease may be the result of faint-end incompleteness in the most distant samples. The highest redshift samples show that star formation was already vigorous at the earliest epochs at which galaxies have been observed, less than 1 billion years after the big bang.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/0013b6e4f52895c4f9d8735fd2e2ab8bc25dd96f

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Citations in the corpus

Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, background): “This consists of (up to) 11 bands at ultraviolet to near-infrared wavelengths for 9927 galaxies in the Hubble Ultra Deep Field (Beckwith et al. 2006).”
Lensing and x-ray mass estimates of clusters (simulations) (2012, methodology): “In the current version of the simulator, the shapelet database contains ∼ 3000 galaxies in the z-band from the GOODS/ACS archive (Giavalisco et al. 2004) and ∼ 10000 galaxies in the B,V, i,z bands from the Hubble-Ultra-Deep-Field ( HUDF) archive (Beckwith et al. 2006).”
The James Webb Space Telescope Mission (2023, background): “An example that uses this mode can be found in Program 1963, which is a medium-band survey of the Hubble Ultra-Deep Field.”
A Keck Survey for Gravitationally Lensed Lyα Emitters in the Redshift Range 8.5 < z < 10.4: New Constraints on the Contribution of Low-Luminosity Sources to Cosmic Reionization (2007, background): “…(Ellis et al. 2001; Kneib et al. 2004; Santos et al. 2004; Egami et al. 2005), stellar continuum slopes, Lyman-α profiles and star formation rates have been determined for sources whose intrinsic flux is close to the faintest direct imaging limits so far reached, IAB ≃ 30 (Beckwith et al. 2006).”
The z ∼ 6 Luminosity Function Fainter than −15 mag from the Hubble Frontier Fields: The Impact of Magnification Uncertainties (2016, background): “…(e.g., Siana et al. 2010, 2015; Vanzella et al. 2012, 2016; Nestor et al. 2013), and what the total emissivity is in the rest-frame UV in faint galaxies beyond the limits of current surveys in the Hubble Ultra Deep Field (HUDF: Beckwith et al. 2006; Ellis et al. 2013; Illingworth et al. 2013).”
UVUDF: ULTRAVIOLET THROUGH NEAR-INFRARED CATALOG AND PHOTOMETRIC REDSHIFTS OF GALAXIES IN THE HUBBLE ULTRA DEEP FIELD (2015, methodology): “We make use of the source positions measured in the F435W ACS mosaics of the UDF (Beckwith et al. 2006) as our absolute astrometric reference frame.”
The COSMOS Survey: Hubble Space Telescope Advanced Camera for Surveys Observations and Data Processing (2007, methodology): “Subsequent surveys included the Hubble Ultra Deep Field (UDF: Beckwith et al. 2006) which went deeper over a somewhat larger 11 arcminute2 area; the Great Observatories Origins Deep Survey (GOODS: Giavalisco et al. 2004) which was shallower but covered a larger 360 arcminute2 area; and two larger…”
VERY BLUE UV-CONTINUUM SLOPE β OF LOW LUMINOSITY z ∼ 7 GALAXIES FROM WFC3/IR: EVIDENCE FOR EXTREMELY LOW METALLICITIES? (2009, methodology): “0 reductions of the HUDF ACS data (Beckwith et al. 2006) rebinned on a 0.06′′-pixel scale, and our own reduction of the HUDF09 WFC3/IR data over the HUDF (Bouwens et al. 2009b; Oesch et al. 2009b).”
COSMIC REIONIZATION AND EARLY STAR-FORMING GALAXIES: A JOINT ANALYSIS OF NEW CONSTRAINTS FROM PLANCK AND THE HUBBLE SPACE TELESCOPE (2015, background): “…University of California, Los Angeles CA 90095 4 Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UK of their abundance over 8 < z < 10 from Hubble Space Telescope (HST) Ultra Deep Field (UDF) observations (Beckwith et al. 2006; Koekemoer et al. 2013; Illingworth et al. 2013).”
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: SURVEY DESCRIPTION (2016, background): “In a sense, spectral line scans follow the spirit of the original HST deep fields (e.g., Williams et al. 1996; Beckwith et al. 2006), as essentially no prior knowledge/selection based on galaxy properties enters the choice of field.”
MORPHOLOGIES OF ∼190,000 GALAXIES AT z = 0–10 REVEALED WITH HST LEGACY DATA. I. SIZE EVOLUTION (2015, background): “…sample consists of 10, 454 LBGs at z = 4−10 made by Y. Harikane et al. (in preparation) in the CANDELS, the Hubble Ultra Deep Field 09+12 (HUDF 09+12; Beckwith et al. 2006; Bouwens et al. 2011; Illingworth et al. 2013; Ellis et al. 2013) fields6, and the parallel fields of Abell 2744 and MACS0416…”
A deep ALMA image of the Hubble Ultra Deep Field (2016, background): “These unparalleled near-infrared data, covering an area ' 4.5 arcmin2, are complemented by what remains the deepest ever optical imaging obtained with ACS on HST (Beckwith et al. 2006).”
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): “Among the surveys carried out in areas included in the CDF-S are K20 (Cimatti et al. 2002), GMASS (Cimatti et al. 2008), VVDS (Le Fèvre et al. 2004), and the Hubble Ultra Deep Field (Beckwith et al. 2006).”
The MUSE 3D view of the Hubble Deep Field South (2014, methodology): “The Hubble deep fields North and South (see e.g. Williams et al. 1996; Ferguson et al. 2000; Beckwith et al. 2006) are still among the deepest images ever obtained in the optical/infrared, providing broad band photometry for sources up to V∼30 .”
THE MOST LUMINOUS z ∼ 9–10 GALAXY CANDIDATES YET FOUND: THE LUMINOSITY FUNCTION, COSMIC STAR-FORMATION RATE, AND THE FIRST MASS DENSITY ESTIMATE AT 500 Myr (2013, methodology): “Despite extremely deep imaging over the Hubble Ultra-Deep Field (HUDF; Beckwith et al. 2006; Illingworth et al. 2013; Ellis et al. 2013), only one reliable z ∼ 10 galaxy candidate could be identified over this small field and over additional wider area blank field data in the Chandra Deep Field…”
The Evolution of Galaxy Structure Over Cosmic Time (2014, background): “24 Christopher J. Conselice Similar to Figure 9, showing massive galaxies in the Hubble Ultra Deep Field (UDF) as imaged through the ACS camera ordered by the value of their asymmetries from most symmetric to asymmetric.”