The Spatial Clustering of Star-forming Galaxies at Redshifts 1.4 ≲ z ≲ 3.5

By K. Adelberger, C. Steidel, M. Pettini, A. Shapley, Naveen A. Reddy, D. Erb. 2004

281 citations recorded by the source corpus.

We analyzed the spatial distribution of 28,500 photometrically selected galaxies with magnitude 23.5 < ℛAB < 25.5 and redshift 1.4 < z < 3.5 in 21 fields with a total area of 0.81 deg2. The galaxies were divided into three subsamples, with mean redshifts = 1.7, 2.2, and 2.9, according to their UnGℛ colors. Combining the galaxies' measured angular clustering with redshift distributions inferred from 1600 spectroscopic redshifts, we find comoving correlation lengths at the three redshifts of r0 = 4.5 ± 0.6, 4.2 ± 0.5, and 4.0 ± 0.6 h-1 Mpc, respectively, and infer a roughly constant correlation function slope of γ = 1.6 ± 0.1. We derive similar numbers from the 1600 object spectroscopic sample itself with a new statistic, K, that is insensitive to many possible systematics. Galaxies that are bright in ℛ (λrest ~ 1500-2500 Å) cluster more strongly than fainter galaxies at z = 2.9 and 2.2 but not, apparently, at z = 1.7. Comparison to a numerical simulation that is consistent with recent WMAP observations suggests that galaxies in our samples are associated with dark matter halos of mass 1011.2-1011.8 (z = 2.9), 1011.8-1012.2 (z = 2.2), and 1011.9-1012.3 M☉ (z = 1.7) and that a small fraction of the halos contain more than one galaxy that satisfies our selection criteria. Adding recent observations of galaxy clustering at z ~ 0 and ~1 to the simulation results, we conclude that the typical object in our samples will evolve into an elliptical galaxy by redshift z = 0 and will already have an early-type spectrum by redshift z = 1. We comment briefly on the implied relationship between galaxies in our survey and those selected with other techniques.

Subfields: Astronomy and Astrophysics, Ecology, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/1b0e43ce6269991a81a9bc9c2792bd36626fa720

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. Volker Springel
6. C. Conroy
7. A. Dekel
8. P. V. van Dokkum

In Ecology

1. F. V. D. Bosch
2. H. Mo
3. M. Blanton
4. Xiaohu Yang
5. J. Brinkmann
6. D. Schneider
7. Idit Zehavi
8. Risa Wechsler

In Global and Planetary Change

1. P. Hopkins
2. J. Brinkmann
3. Naveen A. Reddy
4. C. Faucher-Giguére
5. M. Blanton
6. M. Franx
7. C. Conroy
8. C. Steidel

Citations in the corpus

• GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, background): “…has also been made in recent years in measuring galaxy clustering at intermediate and high redshifts (e.g., Brown et al. 2003; Daddi et al. 2003; Adelberger et al. 2005; Ouchi et al. 2005; Lee et al. 2006; Phleps et al. 2006; Coil et al. 2006b, 2008; Meneux et al. 2008, 2009; Abbas et al. 2010).”
• SINFONI Integral Field Spectroscopy of z ~ 2 UV-selected Galaxies: Rotation Curves and Dynamical Evolution (2006, methodology): “This is in good agreement with estimates based on the clustering and comoving space density of the BM/BX population (Adelberger et al. 2005a).”
• THE CIRCUMGALACTIC MEDIUM OF MASSIVE GALAXIES AT z ∼ 3: A TEST FOR STELLAR FEEDBACK, GALACTIC OUTFLOWS, AND COLD STREAMS (2012, background): “…UV-color selected objects, provides a robust map of cool circumgalactic gas at galactocentric impact parameters b = 3− 125 kpc. Objects in this sample have been well-characterized in terms of their spatial clustering and stellar population parameters (Adelberger et al. 2005a; Erb et al. 2006b).”
• Constraining the Evolution of the Ionizing Background and the Epoch of Reionization with z ∼ 6 Quasars. II. A Sample of 19 Quasars (2005, methodology): “In comoving units, this is comparable to the correlation length of galaxy clustering at z ∼ 0, (r0 ∼ 5 h −1 Mpc, Zehavi et al. 2005), and of Lyman break galaxies at z ∼ 2 − 4 (r0 ∼ 4 h −1 Mpc, Adelberger et al. 2005), and at z = 4− 5 (r0 ∼ 4− 8 h −1 Mpc, Kashikawa et al. 2006).”
• SPECTROSCOPIC OBSERVATIONS OF LYMAN BREAK GALAXIES AT REDSHIFTS ∼4, 5, AND 6 IN THE GOODS-SOUTH FIELD (2009, background): “…et al. 2007; van Dokkum et al. 2006) are in overall quantitative agreement with the expected dependence of clustering with both mass and time, when compared to the less strongly clustered and less massive (in stellar content) UV–only selected galaxies at z ∼ 3 and ∼ 4 (Adelberger et al. 2005).”
• Dynamical Properties of z ~ 2 Star-forming Galaxies and a Universal Star Formation Relation (2007, unknown): “…converted to spheroids by mergers or secular evolution (van den Bosch 2002; Immeli et al. 2004; Förster Schreiber et al. 2006; Genzel et al. 2006, Governato et al. 2006), in agreement with the cosmic volume density of BX/s-BzK and their clustering (Adelberger et al. 2004, 2005; Kong et al. 2006).”
• Modeling Luminosity-dependent Galaxy Clustering through Cosmic Time (2005, methodology): “…in which bright galaxies are strongly 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…”
• Clustering of High-Redshift (z ≥ 2.9) Quasars from the Sloan Digital Sky Survey (2007, background): “The correlation length of Lyman-break galaxies at these redshifts is∼ 5h−1Mpc (Adelberger et al. 2005a), but the clustering strength appears to increase (alb it at z∼ 2) with increasing observed K-band luminosity (Adelberger et al. 2005b; Allen et al. 2005) and/or color (Quadri et al. 2006).”
• The Direct Detection of Lyman Continuum Emission from Star-forming Galaxies at z~3 (2006, background): “Since our sample is contained within an area of 9 × 13 comoving Mpc2 on the sky, ∼ 50% of the resulting set of galaxy sightline pairs are separated by less than 5.7 comoving Mpc, the auto-correlation length of z ∼ 3 LBGs (Adelberger et al. 2005).”
• The DEEP2 galaxy redshift survey: evolution of the colour–density relation at 0.4 < z < 1.35 (2006, background): “Studies of UV– selected galaxies and red, near–IR bright galaxies have found significant differences in clustering strengths depending on the sample selection, with the latter being more strongly clustered (e.g., Daddi et al. 2003; Adelberger et al. 2005b; Foucaud 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): “Given that the clustering 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…”
• Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, methodology): “Similar galaxy populations were studied following merger trees of DM-only simulations in combination with simple assumptions on how haloes are populated by galaxies (Adelberger et al. 2005; Conroy et al. 2008; Genel et al. 2008).”
• Lyα-EMITTING GALAXIES AT z = 2.1 IN ECDF-S: BUILDING BLOCKS OF TYPICAL PRESENT-DAY GALAXIES? (2009, unknown): “It is also consistent with the value calculated for the subset of “BX” galaxies dimmest in K-band (KV ega > 21.5, Adelberger et al. 2005b); that is low mass galaxies.”
• Lyα blobs as an observational signature of cold accretion streams into galaxies (2009, background): “LBGs populate dark matter halos of mass m = 1011.8M⊙ (Adelberger et al. 2005), which are biased tracers of the overall mass density field.”
• Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, background): “Recently, Adelberger et al. (2005) show that the 3D correlation length (r◦) of LBGs is such to match that of local lesser spheroids (M<∼1011M⊙) when the secular increase of r◦ is taken into account.”