The luminosity function, halo masses and stellar masses of luminous Lyman-break galaxies at redshifts 5 < z < 6

By R. McLure, M. Cirasuolo, J. Dunlop, S. Foucaud, O. Almaini. 2008

142 citations recorded by the source corpus.

We present the results of a study of a large sample of luminous (z 0 A B < 26) Lyman break galaxies (LBGs) in the redshift interval 4:7 < z < 6:3, selected from a contiguous 0.63 square degree area covered by the UKIDSS Ultra Deep Survey (UDS) and the Subaru XMMNewton Survey (SXDS). Utilising the large area coverage and the excellent available optical+nearIR data, we use a photometric redshift analysis to derive a new, robust, measurement

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/43c4d337204d4aa06d23eac8570e3fbbaffd2123

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In Astronomy and Astrophysics

1. Richard S. Ellis
2. J. Dunlop
3. R. Bouwens
4. P. Oesch
5. P. V. van Dokkum
6. M. Franx
7. G. Illingworth
8. I. Labbé

In Instrumentation

1. Richard S. Ellis
2. M. Franx
3. R. Bouwens
4. P. V. van Dokkum
5. J. Dunlop
6. P. Oesch
7. I. Labbé
8. G. Illingworth

Citations in the corpus

• The VISTA deep extragalactic observations (VIDEO) survey (2012, background): “In addition to probing the sub-L population up to z ∼ 4, VIDEO will be uniquely placed to quantify the density and spatial clustering of the most massive galaxies at the earliest epochs (e.g. McLure et al. 2009; Hickey et al. 2010).”
• The galaxy luminosity function at z ≃ 6 and evidence for rapid evolution in the bright end from z ≃ 7 to 5 (2014, methodology): “The lack of luminosity evolution in the restframe UV LF at high redshift from these recent studies contrasts starkly with the majority of previous studies which have overwhelmingly favoured pure luminosityevolution (Bouwens et al. 2007, 2008, 2011; McLure et al. 2009).”
• STATISTICS OF 207 Lyα EMITTERS AT A REDSHIFT NEAR 7: CONSTRAINTS ON REIONIZATION AND GALAXY FORMATION MODELS (2010, background): “Thus, a typical halo mass of LBG is estimated to be ∼ 1012±1M⊙, about one order of magnitude larger than that of LAEs (Hamana et al. 2004; Ouchi et al. 2004b, 2005b; Lee et al. 2006, 2009; McLure et al. 2009; Hildebrandt et al. 2009).”
• z ∼ 7 GALAXIES IN THE HUDF: FIRST EPOCH WFC3/IR RESULTS (2009, background): “The luminosity function (LF) brightens significantly from z ∼ 6 to z ∼ 4 (e.g McLure et al. 2009a; Bouwens et al. 2007; Bouwens & Illingworth 2006; Oesch et al. 2007; Yoshida et al. 2006; Ouchi et al. 2004; Steidel et al. 1999), following M∗(z) = −21.02 + 0.36∗ (z−3.8) (Bouwens et al. 2008), and…”
• A new multifield determination of the galaxy luminosity function at z = 7-9 incorporating the 2012 Hubble Ultra-Deep Field imaging (2012, methodology): “7 http://pono.ucsd.edu/ adam/browndwarfs/spexprism/ Following the methodology of McLure et al. (2009), we adopt a parametric model of the evolving high-redshift galaxy luminosity function in order to generate a realistic synthetic population of high-redshift galaxies.”
• CANDELS: THE CONTRIBUTION OF THE OBSERVED GALAXY POPULATION TO COSMIC REIONIZATION (2012, background): “Atz ∼ 5– 6, where the samples are larger, there is no strong evidence for deviation from this function (e.g., Bouwens et al. 2007; McLure et al. 2009).”
• The mass evolution of the first galaxies: stellar mass functions and star formation rates at 4 < z < 7 in the CANDELS GOODS-South field (2014, methodology): “Previous work using photometric redshifts has dealt with this problem by making use of the full redshift PDF when calculating LF (Dahlen et al. 2005; McLure et al. 2009, 2013), thereby incorporating the uncertainty in the analysis.”
• The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching? (2013, methodology): “In particular, the number density at the bright end has been determined by McLure et al. (2009) who exploited the DR8 release of near-infrared imaging within the UDS field to select a sample of LBGs at z = 5 and z = 6.”
• LARGE AREA SURVEY FOR z = 7 GALAXIES IN SDF AND GOODS-N: IMPLICATIONS FOR GALAXY FORMATION AND COSMIC REIONIZATION (2009, methodology): “We calculate Ṅion at z = 4 − 6 from the best-fit Schechter parameters of UV LFs obtained by Yoshida et al. (2006), Bouwens et al. (2008), and McLure et al. (2009a).”
• The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, background): “…published by EDP Sciences A70, page 1 of 27 To get a continuous view of galaxies’ history, one has to combine low-z estimates (e.g. Fontana et al. 2004, 2006; Pozzetti et al. 2010; Ilbert et al. 2010) with SMFs derived at z > 3 (e.g. McLure et al. 2009; Caputi et al. 2011; Santini et al. 2012).”
• Galaxies at z = 6 - 9 from the WFC3/IR imaging of the HUDF (2009, methodology): “…either strong Lyman breaks and/or strong Lyman-α emission at observed wavelengthsλobs > 8500Å (e.g. Bouwens et al. 2004; Yan c© 0000 RAS & Windhorst 2004; Stark et al., 2007; Bouwens et al. 2008; Richard et al. 2008; McLure et al. 2009; Oesch et al. 2009a; Zheng et al. 2009; Ouchi et al. 2009).”
• UltraVISTA: a new ultra-deep near-infrared survey in COSMOS (2012, background): “This has led to a number of breakthroughs in extra-galactic astronomy, including, for example, the study of the bright end of the galaxy luminosity function from z = 0 out to z 6 (McLure et al. 2009; Cirasuolo et al. 2010), and the discovery of the most distant known quasar (Mortlock et al. 2011).”
• ULTRAVIOLET LUMINOSITY FUNCTIONS FROM 132 z ∼ 7 AND z ∼ 8 LYMAN-BREAK GALAXIES IN THE ULTRA-DEEP HUDF09 AND WIDE-AREA EARLY RELEASE SCIENCE WFC3/IR OBSERVATIONS (2010, background): “This figure provides further support to the suggestion that the primary mode of evolution in the LF from z ∼ 7 to z ∼ 4 is in the characteristic luminosity (see also Bouwens et al. 2006; Yoshida et al. 2006; Bouwens et al. 2007; McLure et al. 2009).”
• THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION OVER THE FIRST TWO BILLION YEARS (2014, methodology): “Specifically, Bouwens et al. (2007) found M* = -20.29 ± 0.19, and McLure et al. (2009) found M* = -20.04 ± 0.12.”
• THE EVOLUTION OF GALAXY NUMBER DENSITY AT z < 8 AND ITS IMPLICATIONS (2016, methodology): “For this we use the luminosity functions published in Bouwens et al. (2011), McLure et al. (2009), McLure et al. (2013), Bouwens et al. (2015) and Finkelstein et al. (2015).”
• THE UV LUMINOSITY FUNCTION OF STAR-FORMING GALAXIES VIA DROPOUT SELECTION AT REDSHIFTS z ∼ 7 AND 8 FROM THE 2012 ULTRA DEEP FIELD CAMPAIGN (2012, background): “Previous studies at redshifts 2 < z < 6 find a remarkably consistent value of α ∼ −1.7 across this range (e.g., Oesch et al. 2007; Bouwens et al. 2007; Reddy & Steidel 2009; McLure et al. 2009).”
• DISCOVERY OF z ∼ 8 GALAXIES IN THE HUBBLE ULTRA DEEP FIELD FROM ULTRA-DEEP WFC3/IR OBSERVATIONS (2009, methodology): “Adopting the z ∼ 6 i-dropout LF from Bouwens et al. (2007: see also McLure et al. 2009) and assuming no evolution to higher redshift, we predict 20±6 Y105-dropouts in our WFC3/IR field.”
• ARE ULTRA-FAINT GALAXIES AT z = 6–8 RESPONSIBLE FOR COSMIC REIONIZATION? COMBINED CONSTRAINTS FROM THE HUBBLE FRONTIER FIELDS CLUSTERS AND PARALLELS (2015, methodology): “…to our data, which has been extensively used to describe the galaxy UV LF across a wide redshift range (e.g. Bunker et al. 2004; Beckwith et al. 2006; Reddy & Steidel 2009; Bouwens et al. 2006; McLure et al. 2009; Ouchi et al. 2009; Wilkins et al. 2010; Oesch et al. 2012; Willott et al. 2013).”