The Large-Scale and Small-Scale Clustering of Lyman Break Galaxies at 3.5 ⩽ z ⩽ 5.5 from the GOODS Survey

By Kyoung-soo Lee, M. Giavalisco, O. Gnedin, R. Somerville, H. Ferguson, Mark Dickinson, M. Ouchi. 2005

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We report on the angular correlation function of Lyman break galaxies (LBGs) at z ~ 4 and 5 from deep samples obtained from the Great Observatories Deep Origins Survey (GOODS). As for LBGs at z ~ 3, the shape of w(θ) of the GOODS LBGs is well approximated by a power law with a slope β ≈ 0.6 at angular separation θ ≥ 10''. The clustering strength of the z ~ 4 and 5 LBGs depends on the rest-frame UV luminosity similar to that of z ~ 3 LBGs, with brighter galaxies more strongly clustered than fainter ones. At smaller separations, w(θ) significantly exceeds the extrapolation of the large-scale power-law fit, implying enhanced spatial clustering on comoving scales r ≤ 1 Mpc. We also find that bright LBGs statistically have more faint companions on scales θ ≲ 20'' than fainter ones. The enhanced small-scale clustering is very likely due to substructure, reflecting multiple galaxies within the same massive halos. A simple model for the halo occupation distribution along with the halo mass function in a ΛCDM cosmology reproduces well the observed w(θ). The scaling relationship of the clustering strength with volume density and redshift is quantitatively consistent with that of CDM halos. If we associate LBGs with dark matter halos that have the same clustering strength, this luminosity dependence of w(θ) implies a close correlation between the halo mass and the star formation rate. A comparison of the clustering strength of three samples of equal luminosity limit at z ~ 3, 4, and 5 shows that the LBGs at z ~ 5 are hosted in halos about 5-10 times less massive than those at z ~ 3-4, suggesting that star formation was more efficient at z ~ 5.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “Galaxy clustering statistics such as two-point correlation functions can provide strong constraints on the masses of the dark matter halos that harbor a given observed population (Conroy et al. 2006; Lee et al. 2006, 2009).”
THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, background): “First, it could mean gas accretion is low such that galaxies undergo recurrent and stochastic starformation that leads to a range of M1500 at a fixed stellar mass (Lee et al. 2006, 2011).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY—THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS, AND MOSAICS (2011, background): “…generations of stars (Cooray et al. 2004, Fernandez et al. 2010), as well as enabling the use of clustering statistics to constrain the properties of dark matter halos (Conroy et al. 2006, Lee et al. 2006, 2009), which drives the need to produce contiguous mosaics across each of the CANDELS fields.”
The rising star formation histories of distant galaxies and implications for gas accretion with time (2010, background): “Moreover, this assumption is justified by observations that find a tight relationship between UV luminosity and halo mass (e.g., Giavalisco & Dickinson 2001; Adelberger et al. 2005; Lee et al. 2006, 2009).”
Towards a concordant model of halo occupation statistics (2006, methodology): “The HOD modelling has also been applied to various galaxy populations at medium to high redshifts (e.g. Bullock, Wechsler & Somerville 2002; Zheng 2004a; Lee et al. 2006; Phleps et al. 2006) as well as to quasars (Porciani, Magliocchetti & Norberg 2004).”
STATISTICS OF 207 Lyα EMITTERS AT A REDSHIFT NEAR 7: CONSTRAINTS ON REIONIZATION AND GALAXY FORMATION MODELS (2010, background): “The lower limit of the fitting range, θ = 10′′, is placed, because 1-halo term of high-z galaxies is dominant at this small scale (Ouchi et al. 2005b; Lee et al. 2006; Hildebrandt et al. 2007, 2009).”
z ~ 7-10 Galaxies in the HUDF and GOODS Fields: UV Luminosity Functions (2008, background): “The chosen parameters yield similar, albeit slightly lower, halo masses to those inferred from clustering analyses of star-forming galaxies at z ∼ 4 (e.g., Ouchi et al. 2004b; Lee et al. 2006).”
GALAXY CLUSTERING IN THE NEWFIRM MEDIUM BAND SURVEY: THE RELATIONSHIP BETWEEN STELLAR MASS AND DARK MATTER HALO MASS AT 1 < z < 2 (2010, background): “These galaxies show strong clustering strengths which depends on their luminosity (Adelberger et al. 2005a,b; Ouchi et al. 2005; Lee et al. 2006, 2009; Hildebrandt et al. 2009; Bielby et al. 2010).”
TWO BRIGHT SUBMILLIMETER GALAXIES IN A z = 4.05 PROTOCLUSTER IN GOODS-NORTH, AND ACCURATE RADIO-INFRARED PHOTOMETRIC REDSHIFTS (2008, methodology): “Given that at these angular scales the angular correlation function ofB-band dropouts is non negligible (Lee et al. 2006), we account for the variance due to clustering to derive an expected r.m.s fluctuation in the counts in 25′′ radius apertures of about 1.8 galaxies.”
EVOLUTION OF THE GALAXY–DARK MATTER CONNECTION AND THE ASSEMBLY OF GALAXIES IN DARK MATTER HALOS (2011, background): “…connection and its evolution between z ∼ 1 and the present (e.g., Bullock et al. 2002; Moustakas & Somerville 2002; Yan et al. 2003; Zheng 2004; Lee et al. 2006; Hamana et al. 2006; Cooray 2005, 2006; Cooray & Ouchi 2006; Conroy et al. 2005, 2007; White et al. 2007; Zheng et al. 2007; Conroy…”
Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering (2007, background): “…explain the clustering properties of these high redshift galaxies (e.g., Bullock, Wechsler, & Somerville 2002; Moustakas & Somerville 2002; Yan, Madgwick, & White 2003; Zheng 2004; Lee et al. 2006; Hamana et al. 2006; Cooray 2005, 2006; Cooray & Ouchi 2006; Conroy et al. 2006; White et al. 2007).”
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, background): “Higher luminosity galaxies are consistently found to be more clustered than lower luminosity galaxies (e.g., Ouchi et al. 2004b; Lee et al. 2006).”
SPECTROSCOPIC CONFIRMATION OF THREE z-DROPOUT GALAXIES AT z = 6.844–7.213: DEMOGRAPHICS OF Lyα EMISSION IN z ∼ 7 GALAXIES (2011, background): “…strength of dropout galaxies increases with their UV luminosity (e.g., Giavalisco & Dickinson 2001; Ouchi et al. 2004; Adelberger et al. 2005; Lee et al. 2006), our results imply that the ionizing state of the IGM around galaxies hosted by less-massive dark matter halos changes later than…”
SPECTROSCOPIC OBSERVATIONS OF LYMAN BREAK GALAXIES AT REDSHIFTS ∼4, 5, AND 6 IN THE GOODS-SOUTH FIELD (2009, background): “…consistent with the observed spatial clustering properties and the stellar populations of LBGs at z ∼ 3 and ∼ 4 (Giavalisco et al. 1998; Giavalisco & Dickinson 2001; Lee et al. 2006, 2008; Ouchi et al. 2005) and those of the BzK and DRG galaxies at z ∼ 2−2.5 (Kong et al. 2006; Quadri et al. 2008).”
The DEEP2 Galaxy Redshift Survey: Color and Luminosity Dependence of Galaxy Clustering at z ∼ 1 (2007, background): “Significant deviations in the two-point correlation function from a power-law form have recently been detected on scales r < 10 h−1 Mpc for both local and high redshift populations (e.g., Zehavi et al. 2004; Lee et al. 2006; Ouchi et al. 2005; Coil et al. 2006a).”
CARS: the CFHTLS-Archive-Research Survey - II. Weighing dark matter halos of Lyman-break galaxies at z = 3–5 (2009, background): “Recently, several studies (Ouchi et al. 2005; Lee et al. 2006; Hildebrandt et al. 2007) have detected deviations from the large scale power-law behaviour on small scales in the correlation functions of Lyman-break galaxies (LBGs).”
DEEP U BAND AND R IMAGING OF GOODS-SOUTH: OBSERVATIONS, DATA REDUCTION AND FIRST RESULTS, (2009, background): “The uncertainties in the LF also affect the analysis of the clustering properties of LBG and their host dark matter halos (Giavalisco & Dickinson 2001; Lee et al. 2006, 2008).”
HALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES (2008, background): “…FROM A POWER LAW IN THE GALAXY TWO-POINT CORRELATION FUNCTION Departures of the galaxy two-point correlation function from a pure power law have been observed for both low- and highredshift galaxies (Hawkins et al. 2003; Zehavi et al. 2004; Ouchi et al. 2005; Coil et al. 2006; Lee et al. 2006).”