Subaru Deep Survey. VI. A Census of Lyman Break Galaxies at z ≃ 4 and 5 in the Subaru Deep Fields: Clustering Properties

By M. Ouchi, K. Shimasaku, S. Okamura, H. Furusawa, N. Kashikawa, K. Ota, M. Doi, M. Hamabe, M. Kimura, Y. Komiyama and 6 more. 2003

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We investigate the clustering properties of 2600 Lyman break galaxies (LBGs) at z = 3.5-5.2 in two large blank fields, the Subaru Deep Field and the Subaru/XMM-Newton Deep Field (600 arcmin2 each). The angular correlation functions of these LBGs show a clear clustering at both z ≃ 4 and 5. The correlation lengths are r0 = 4.1 and 5.9h Mpc (r0 = 5.1 and 5.9h Mpc) for all the detected LBGs (for L ≳ L* LBGs) at z ≃ 4 and 5, respectively. These correlation lengths correspond to galaxy-dark matter biases of bg = 2.9 and 4.6 (bg = 3.5 and 4.6) for all the detected LBGs (for L ≳ L* LBGs) at z ≃ 4 and 5, respectively. These results, combined with estimates for z ≃ 3 LBGs in the literature, show that the correlation length of L ≳ L* LBGs is almost constant, ~5 h Mpc, over z ≃ 3-5, while the bias monotonically increases with redshift at z ≳ 3. We also find that for LBGs at z ≃ 4 the clustering amplitude increases with UV-continuum luminosity and with the amount of dust extinction. We estimate the mass of dark halos hosting various kinds of high-z galaxies, including LBGs, with the analytic model given by Sheth & Tormen. We find that the typical mass of dark halos hosting L ≳ L* LBGs is about 1 × 1012 h M☉ over z ≃ 3-5, which is comparable to that of the Milky Way. A single dark halo with ~1012 h M☉ is found to host 0.1-0.3 LBGs on average but about four K-band-selected galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Probing the Coevolution of Supermassive Black Holes and Galaxies Using Gravitationally Lensed Quasar Hosts (2006, background): “The typical star formation in a Lyman break galaxy of φ & 2 (Reddy et al. 2006; Ouchi et al. 2004; Reddy, Steidel, & Erb 2005) is more than sufficient to eliminate the stellar mass deficit of the bulge hosting a 108M⊙ BH.”
Evolution of the Intergalactic Opacity: Implications for the Ionizing Background, Cosmic Star Formation, and Quasar Activity (2008, background): “For instance, Ouchi et al. (2004) find no evolution in dust extinction (based on E(B-V)) between LBGs at z = 3 and 4.”
HUBBLE FRONTIER FIELDS FIRST COMPLETE CLUSTER DATA: FAINT GALAXIES AT z ∼ 5–10 FOR UV LUMINOSITY FUNCTIONS AND COSMIC REIONIZATION (2014, methodology): “Here we estimate the expected number of such contaminants that meet our dropout selection criteria, basically following the method described in Section 3.3 of Schenker et al. (2013, see also Section 3.1 of Ouchi et al. 2004).”
ON THE STELLAR POPULATIONS AND EVOLUTION OF STAR-FORMING GALAXIES AT 6.3 < z ⩽ 8.6 (2009, background): “This is in contrast to studies of star–forming LBGs at lower redshifts, 2< z< 6 (e.g., Papovich et al. 2001; Ouchi et al. 2004; Reddy & Steidel 2009; Overzier et al. 2009; Bouwens et al. 2009a).”
Galaxies at z ~ 6: The UV Luminosity Function and Luminosity Density from 506 HUDF, HUDF Parallel ACS Field, and GOODS i-Dropouts (2005, background): “A similar evolution from bluer spectral slopes has already been noted in a number of other highredshift (z > 3) studies (Lehnert & Bremer 2003; Kneib et al. 2004; B06a; Bouwens et al. 2004c; Schaerer & Pelló 2005; Yan et al. 2005; cf. Ouchi et al. 2004).”
The luminosity function, halo masses and stellar masses of luminous Lyman-break galaxies at redshifts 5 < z < 6 (2008, methodology): “Thez ≃ 5 luminosity function has been investigated by several recent studies using both ground-based and HST imaging (e.g. Ouchi et al. 2004; Yoshida et al. 2006; Iwata et al. 2007; Oesch et al. 2007; Bouwens et al. 2007).”
Modeling Luminosity-dependent Galaxy Clustering through Cosmic Time (2005, background): “…biased with respect to the matter distribution at high redshifts (Steidel et al. 1998; Giavalisco et al. 1998; Adelberger et al. 2003, 2005; Ouchi et al. 2004b, 2005; Lee et al. 2005; Hamana et al. 2005), and in which the bias decreases with time in such a way that the amplitude of galaxy…”
Keck spectroscopy of faint 3 < z < 7 Lyman break galaxies – I. New constraints on cosmic reionization from the luminosity and redshift-dependent fraction of Lyman α emission (2010, background): “…rest-frame UV luminosities, declines monotonically with redshift (e.g. Stanway, Bunker & McMahon 2003; Bunker et al. 2004) largely as a result of a corresponding fading of the characteristic UV luminosity (e.g. Ouchi et al. 2004; Yoshida et al. 2006; Bouwens et al. 2006, 2007; McLure et al. 2010).”
Subaru Weak Lensing Study of Seven Merging Clusters: Distributions of Mass and Baryons (2007, methodology): “Each Subaru data set was reduced using the software SDFRED (Yagi et al. 2002; Ouchi et al. 2004).”
Lyα Emitters at z = 5.7 in the Subaru Deep Field (2006, background): “The correction not only will strengthen the recent finding that the number density of bright LBGs drops from z ∼ 3 to z ∼ 6 (e.g., Ouchi et al. 2004; Shimasaku et al. 2005; Bouwens et al. 2005), but also might find a new trend that faint LBGs also decrease in number toward z ∼ 6.”
Star formation at z=1.47 from HiZELS: an Hα+[O ii] double-blind study* (2011, methodology): “The raw NB921 data were downloaded from the archive and reduced with the Suprime-Cam Deep field Reduction (SDFRED) package (Yagi et al. 2002; Ouchi et al. 2004) and IRAF.”
The Subaru/XMM-Newton Deep Survey (SXDS). II. Optical Imaging and Photometric Catalogs (2008, methodology): “First, we compare our observation with the earlier calibrated observations for the same overlapping field, which were made by the Suprime-Cam instrument development team (Ouchi et al. 2001, 2004).”
ON THE REDSHIFT EVOLUTION OF THE Lyα ESCAPE FRACTION AND THE DUST CONTENT OF GALAXIES (2010, methodology): “We also use the z = 4.5 and 4.86 Lyα LF points from Dawson et al. (2007) and Shioya et al. (2009), which we normalize by the dust-corrected UV point at z = 4.7 from Ouchi et al. (2004).”
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): “…amount of very deep, wide-area optical data available from ground and space to select large dropout samples at z ∼ 4 − 6 (e.g., Giavalisco et al. 2004b; Bunker et al. 2004; Dickinson et al. 2004; Yan & Windhorst 2004; Ouchi et al. 2004; Bouwens et al. 2006, hereinafter, B06; Yoshida et al. 2006).”
The SUBARU Deep Field Project: Lymanα Emitters at a Redshift of 6.6 (2004, background): “Several pilot papers related to the SDF project have already been published (Maihara et al. 2001; Totani et al. 2001a, 2001b, 2001c; Ouchi et al. 2001, 2003, 2004a, 2004b; Shimasaku et al. 2003; Kashikawa et al. 2003).”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, methodology): “Other groups (Lehnert & Bremer 2003; Ouchi et al. 2004; Stanway et al. 2005; Yan et al. 2005; Bouwens et al. 2006) have looked at these slopes at higher redshifts (z ∼ 4 − 6), again on a dropout selection.”
UV-CONTINUUM SLOPES AT z ∼ 4–7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR–MAGNITUDE RELATIONSHIP FOR z ⩾ 4 STAR-FORMING GALAXIES (2011, methodology): “Figure 9 shows different β determinations as a function of luminosity at z ∼ 4-5 (Ouchi et al. 2004; Overzier et al. 2008; Bouwens et al. 2009; Lee et al. 2011; Wilkins et al. 2011; Dunlop et al. 2012).10 Despite some dispersion in the precise values of the β measurements and some small variance in…”