Color-selected Galaxies at z ≈ 6 in the Great Observatories Origins Deep Survey

By Mark Dickinson, Daniel Stern, M. Giavalisco, H. Ferguson, Z. Tsvetanov, Ryan Chornock, S. Cristiani, S. Dawson, A. Dey, A. Filippenko and 15 more. 2003

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We report early results on galaxies at z ~ 6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Lyα at z = 5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z = 6 had the same luminosity function as those at z = 3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z = 6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z = 3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.

Subfields: Astronomy and Astrophysics, Instrumentation

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A CRITICAL ASSESSMENT OF PHOTOMETRIC REDSHIFT METHODS: A CANDELS INVESTIGATION (2013, methodology): “…spectroscopic sample is compiled from a set of publicly available data including Cristiani et al. (2000), Croom et al. (2001), Bunker et al. (2003), Dickinson et al. (2004), LeFèvre et al. (2004), Stanway et al. (2004), Strolger et al. (2004), Szokoly et al. (2004), van der Wel et al. (2004),…”
The Hubble Deep Field North SCUBA Super-map - III. Optical and near-infrared properties of submillimetre galaxies (2005, methodology): “The GOODS survey includes the addition of deepz850-band data (toz850 ≃ 27), which extends object selection out to a redshift of∼ 6 using the Lyman-break technique (Dickinson et al. 2004).”
The luminosity function, halo masses and stellar masses of luminous Lyman-break galaxies at redshifts 5 < z < 6 (2008, methodology): “…function have been based, virtually exclusively, on the deep HST imaging availble in the two GOODS regions, the Hubble Ultra-Deep Field (HUDF) and the HUDF parallel fields (e.g. Bunker et al. 2004; Dickinson et al. 2004; Yan & Windhorst 2004; Malhotra et al. 2005; Bouwens et al. 2006, 2007).”
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, background): “…frontier has been extended to z ∼ 4-5 (e.g., Madau et al. 1996; Steidel et al. 1999), z ∼ 6 (e.g., Stanway et al. 2003; Bouwens et al. 2003; Dickinson et al. 2004), z ∼ 7 (e.g., Bouwens et al. 2004; Yan & Windhorst 2004; Bouwens & Illingworth 2006b; Iye et al. 2006; Fontana et al.…”
UV LUMINOSITY FUNCTIONS AT REDSHIFTS z ∼ 4 TO z ∼ 10: 10,000 GALAXIES FROM HST LEGACY FIELDS (2014, methodology): “Importantly, the HST ACS instrument enabled astronomers to obtain deep, wide-area imaging in the z850 band, allowing for the efficient selection of galaxies at z ∼ 6 (Stanway et al. 2003; Bouwens et al. 2003b; Dickinson et al. 2004).”
z ~ 7-10 Galaxies in the HUDF and GOODS Fields: UV Luminosity Functions (2008, methodology): “While some studies have argued that the evolution primarily occurs at the bright end (i.e., Dickinson et al. 2004; Shimasaku et al. 2005; Ouchi et al. 2004a; Bouwens et al. 2006; Yoshida et al. 2006; Bouwens et al. 2007), there have been other efforts which have argued that the evolution occurs…”
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): “Already, there have been quite a significant number of LF determinations at z ∼ 6 (e.g., Dickinson et al. 2004; Bouwens et al. 2004a; Yan & Windhorst 2004; Bunker et al. 2004; Malhotra et al. 2005; B06; Beckwith et al. 2006).”
Lyα Emitters at z = 5.7 in the Subaru Deep Field (2006, result): “We compare the far UV LF of our LAEs with that of z ∼ 6 LBGs. Determinations of the far UV LF of z ∼ 6 LBGs have been recently accumulating (e.g., Dickinson et al. 2004; Yan & Windhorst 2004; Bunker et al. 2004; Bouwens et al. 2005; Shimasaku et al. 2005); see a compilation given in Bouwens et al.…”
The End of the Reionization Epoch Probed by Lyα Emitters at z = 6.5 in the Subaru Deep Field (2006, background): “…advances over the past three years in detecting distant galaxies at the edge of the cosmic reionization era beyond z = 6 in both dropout searches (Dickinson et al. 2004; Bouwens et al. 2003, 2005; Kneib et al. 2004; Pelló et al. 2004; Stanway et al. 2005) to find their strong Lyman breaks and…”
The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, background): “…and ECDFS area a collection of more than 5000 spectroscopic redshifts are available (Cristiani et al. 2000; Croom et al. 2001; Bunker et al. 2003; Dickinson et al. 2004; Stanway et al. 2004; Strolger et al. 2004; Szokoly et al. 2004; van der Wel et al. 2004; Doherty et al. 2005; Le Fèvre et al.…”
THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3 EARLY RELEASE SCIENCE DATA: PANCHROMATIC FAINT OBJECT COUNTS FOR 0.2–2 μm WAVELENGTH (2010, methodology): “Besides the deep, four-color ACS BViz imaging (Giavalisco et al. 2004; Dickinson et al. 2004), there are low resolution (R∼100) ACS slitless G800L grism spectra covering the wavelength range ∼0.55–0.95 µm (cf. Pirzkal et al. 2004; Malhotra et al. 2005; Ferreras et al. 2009; Rhoads et al. 2009;…”
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Galaxies at z ~ 6: The UV Luminosity Function and Luminosity Density from 506 HUDF, HUDF Parallel ACS Field, and GOODS i-Dropouts (2005, methodology): “This works out to a 75% contamination rate, which is much higher than the ∼45% estimated in the Giavalisco et al. (2004b) and Dickinson et al. (2004) studies.”
The K20 survey. VII. The spectroscopic catalogue: spectral properties and evolution of the galaxy population ⋆, ⋆⋆ (2005, background): “The K20 32.2 arcmin2 field in the CDFS is also located within the 150 arcmin2 southern field of the GOODS project, where several multi-wavelength public data are or will be available (Dickinson et al. 2004; Giavalisco et al. 2004).”
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