Color-selected Galaxies at
                    <i>z</i>
                    6 in the Great Observatories Origins Deep Survey

Dickinson, Mark; Stern, Daniel; Giavalisco, Mauro; Ferguson, Henry C.; Tsvetanov, Z.; Chornock, R.; Cristiani, S.; Dawson, Steve; Dey, Arjun; Filippenko, A. V.; Moustakas, Leonidas A.; Nonino, M.; Papovich, Casey; Ravindranath, Swara; Riess, Adam G.; Rosati, P.; Spinrad, Hyron; Vanzella, E.

doi:10.1086/381119

Cited by 247 publications

(304 citation statements)

References 18 publications

(9 reference statements)

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“…A color selection similar to that in this paper and that of Bouwens et al (2003b) was performed by Dickinson et al (2004) in order to identify z % 6 candidates with a slightly bluer color cut criterion of (i 0 Àz 0 ) AB > 1:3, which may leave them susceptible to increased contamination from lower redshift galaxies. Rather than apply a strict magnitude limit, these authors have chosen to apply a cut based on object signal-tonoise ratio in their co-added images.…”

Section: Comparison With the Results Of The Goods Teammentioning

confidence: 99%

“…As a result, a large fraction of the z $ 6 candidates described in this paper and in Paper I do not form part of their survey. Dickinson et al (2004) identify only five candidate objects with signal-to-noise ratio greater than 10 in the combined GOODS-N and GOODS-S survey, of which three objects (in the GOODS-S field) were also selected in Paper I and the remaining GOODS-S object falls outside our color and magnitude cuts. The remaining candidate, NiD001, has colors that appear to vary significantly between epochs and averages across four epochs as too faint to appear in our selection.…”

Section: Comparison With the Results Of The Goods Teammentioning

confidence: 99%

“…Inspection of these spectra reveals no 7 This object has been independently confirmed as lying at z ¼ 5:8 by Dickinson et al (2004) and corresponds to their object SiD002. obvious Ly emission or continuum emission within the wavelength range sampled.…”

Section: Further Candidates In Goods-smentioning

confidence: 95%

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Hubble Space TelescopeImaging and Keck Spectroscopy ofz≈ 6i‐Band Dropout Galaxies in the Advanced Camera for Surveys GOODS Fields

Stanway

Bunker

McMahon

et al. 2004

ApJ

140

169

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We measure the surface density of i 0 -band dropout galaxies at z $ 6 through wide-field Hubble Space Telescope (HST ) Advanced Camera for Surveys (ACS) imaging and ultradeep Keck DEIMOS spectroscopy. Using deep HST ACS SDSS i 0 (F775W) and SDSS z 0 (F850LP) imaging from the Great Observatories Origins Deep Survey-North (GOODS-N; 200 arcmin 2 ), we identify nine i 0 -drops satisfying (i 0 Àz 0 ) AB > 1:5 to a depth of z 0 AB ¼ 25:6 (corresponding to L Ã UV at z $ 3). We use HK 0 imaging data to improve the fidelity of our sample, discriminating against lower redshift red galaxies and cool Galactic stars. Three i 0 -drops are consistent with M/L/T dwarf stars. We present ultradeep Keck DEIMOS spectroscopy of 10 objects from our combined GOODS-N and GOODS-S i 0 -drop sample. We detect Ly emission at z ¼ 5:83 from one object in the GOODS-S field, which lies only 8 0 (i.e., 3 h À1 70 Mpc) away from a previously confirmed z ¼ 5:78 object. One possible Ly emitter at z ¼ 6:24 is found in the GOODS-N field (although identification of this spatially offset emission line is ambiguous). Using the rest-frame UV continuum from our six candidate z $ 6 galaxies from the GOODS-N field, we determine a lower limit to the unobscured volume-averaged global star formation rate at z $ 6 of (5:4 AE 2:2) ; 10 À4 h 70 M yr À1 Mpc À3 . We find that the cosmic star formation density in Lyman break galaxies (LBGs) with unobscured star formation rates greater than 15 M yr À1 falls by a factor of 8 between z $ 3 and z $ 6. Hence, the luminosity function of LBGs must evolve in this redshift interval: a constant integrated star formation density at z > 3 requires a much steeper faint-end slope, or a brighter characteristic luminosity. This result is in agreement with our previous measurement from the GOODS-S field, indicating that cosmic variance is not a dominant source of uncertainty.

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Section: Comparison With the Results Of The Goods Teammentioning

confidence: 99%

Section: Comparison With the Results Of The Goods Teammentioning

confidence: 99%

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Hubble Space TelescopeImaging and Keck Spectroscopy ofz≈ 6i‐Band Dropout Galaxies in the Advanced Camera for Surveys GOODS Fields

Stanway

Bunker

McMahon

et al. 2004

ApJ

140

169

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“…Our first galaxy sample contains 2422 galaxies with secure spectroscopic redshifts (z spec ) from the ESO public compilation in the Chandra Deep Field South (CDFS; Cristiani et al 2000;Croom et al 2001;Bunker et al 2003;Dickinson et al 2004;Stanway et al 2004aStanway et al , 2004bStrolger et al 2004;Szokoly et al 2004;van der Wel et al 2004;Doherty et al 2005;Le Fèvre et al 2005;Mignoli et al 2005;Ravikumar et al 2007;Popesso et al 2009;Balestra et al 2010;Silverman et al 2010;Kurk et al 2013;Vanzella et al 2014) and from Morris et al (2015). In order to obtain multiwavelength photometry for these galaxies, we cross-matched this sample with the public Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al 2011;Koekemoer et al 2011) catalog for the Great Observatory Origins Deep Survey South field (GOODS-S) obtained by Guo et al (2013).…”

Section: Samplementioning

confidence: 99%

The Impact of JWST Broadband Filter Choice on Photometric Redshift Estimation

Bisigello

Caputi

Colina

et al. 2016

ApJS

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The determination of galaxy redshifts in the James Webb Space Telescope's (JWST) blank-field surveys will mostly rely on photometric estimates, based on the data provided by JWST's Near-Infrared Camera (NIRCam) at 0.6-5.0 μm and Mid Infrared Instrument (MIRI) at l m > 5.0 m. In this work we analyze the impact of choosing different combinations of NIRCam and MIRI broadband filters (F070W to F770W), as well as having ancillary data at l m < 0.6 m, on the derived photometric redshifts (z phot ) of a total of 5921 real and simulated galaxies, with known input redshifts z=0-10. We found that observations at l m < 0.6 m are necessary to control the contamination of high-z samples by low-z interlopers. Adding MIRI (F560W and F770W) photometry to the NIRCam data mitigates the absence of ancillary observations at l m < 0.6 m and improves the redshift estimation. At z=7-10, accurate z phot can be obtained with the NIRCam broadbands alone when  S N 10, but the z phot quality significantly degrades at  S N 5. Adding MIRI photometry with 1 mag brighter depth than the NIRCam depth allows for a redshift recovery of 83%-99%, depending on spectral energy distribution type, and its effect is particularly noteworthy for galaxies with nebular emission. The vast majority of NIRCam galaxies with [F150W]=29AB mag at z=7-10 will be detected with MIRI at [F560W, F770W] < 28 mag if these sources are at least mildly evolved or have spectra with emission lines boosting the mid-infrared fluxes.

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“…In Stanway, we searched 150 arcmin 2 of the GOODS-South field (the Chandra Deep FieldSouth) to select (i ′ − z ′ ) AB > 1.5 objects, of which six were probable z > 5.7 galaxies brighter than z AB < 25.6. Subsequent papers by the GOODS team (Dickinson et al 2004;Giavalisco et al 2004) reproduced many of these i ′ -drop candidates. To address potential cosmic variance issues, we performed a similar analysis in the GOODS-North field, which yielded a consistent estimate of the surface density of z ≃ 6 star forming sources (Stanway et al 2004b).…”

Section: Introductionmentioning

confidence: 98%