The Size Evolution of High-Redshift Galaxies

By H. Ferguson, Mark Dickinson, M. Giavalisco, C. Kretchmer, S. Ravindranath, R. Idzi, E. Taylor, Christopher J. Conselice, S. M. Fall, Jonathan P. Gardner and 7 more. 2003

333 citations recorded by the source corpus.

Hubble Space Telescope images of high-redshift galaxies selected via color and photometric redshifts are used to examine the size and axial ratio distribution of galaxies as a function of redshift at look-back times t > 8 Gyr. These parameters are measured at rest-frame UV wavelengths (1200 Å < λ < 2000 Å) on images with a rest-frame resolution of less than 0.8 kpc. Galaxy radii are found to scale with redshift approximately as the Hubble parameter H-1(z). This is in accord with the theoretical expectation that the typical sizes of the luminous parts of galaxies should track the expected evolution in the virial radius of dark matter halos. The mean ratio of the semimajor axis to the semiminor axis for a bright well-resolved sample of galaxies at z ~ 4 is b/a = 0.65, suggesting that these Lyman break galaxies are not drawn from a spheroidal population. However, the median concentration index of this sample is C = 3.5, which is closer to the typical concentration indices of nearby elliptical galaxies (C ~ 4) than to the values for local disk galaxies of type Sb and later (C < 2).

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c660509bd59928899e38357bb3f8cf4613b7ff17

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Citations in the corpus

THE ROLE OF COLD FLOWS IN THE ASSEMBLY OF GALAXY DISKS (2008, background): “…assembled prior to z = 1 (Vogt et al. 1996; Roche et al. 1998; Lilly et al. 1998; Simard et al. 1999; Labbé et al. 2003; Ravindranath et al. 2004; Ferguson et al. 2004; Trujillo & Aguerri 2004; Barden et al. 2005; Sargent et al. 2007; Melbourne et al. 2007; Kanwar et al. 2008), or even by z = 2…”
ARE ULTRA-FAINT GALAXIES AT z = 6–8 RESPONSIBLE FOR COSMIC REIONIZATION? COMBINED CONSTRAINTS FROM THE HUBBLE FRONTIER FIELDS CLUSTERS AND PARALLELS (2015, methodology): “We take the galaxy profile into account by creating two samples of exponential disks and de Vaucouleur shapes (Ferguson et al. 2004; Hathi et al. 2008).”
Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift (2007, background): “Other evidence for 2 times growth from z ¼ 4 to 1.5 was seen in a sample of galaxies of all types from theHDF-N and CDF-S fields (Ferguson et al. 2004) and for a sample of disk galaxies from the HDF-S (Tamm & Tenjes 2006).”
GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, background): “This can be understood through the fact that, on the one hand, galaxies are becoming slightly smaller in physical size (e.g., Ferguson et al. 2004, Elbaz et al. 2011, Pannella et al. in preparation) and at the same time their star formation rate density dramatically increases from the local…”
Properties of Lyα emitters around the radio galaxy MRC 0316 257 (2005, methodology): “The size of emitter #1518 measured with the same input parameter as Ferguson et al. (2004), is 0.”
THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION OVER THE FIRST TWO BILLION YEARS (2014, background): “The structures of these galaxies are resolvable, although they show small sizes with half-light radii 1 kpc, which is consistent with the evolution previously detected at lower redshifts (e.g., Ferguson et al. 2004; Oesch et al. 2010a; Ono et al. 2013).”
Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, result): “…at most weakly with redshift, in agreement with observations (Trujillo & Aguerri 2004; Trujillo et al. 2004, 2005; McIntosh et al. 2005b) (see also e.g. Ferguson et al. 2004; Bouwens et al. 2004; Papovich et al. 2005, although these authors do not separate the relation by morphological type).”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, methodology): “…simulations, we start with the pixelby-pixel profiles of the z ∼ 4 B-dropout sample from the HUDF (Bouwens et al. 2007) and scale their sizes as (1 + z)−1 (for fixed luminosity) to match the observed size-redshift trends (Bouwens et al. 2006; see also Ferguson et al. 2004 and Bouwens et al. 2004).”
The Rest-Frame Optical Properties of SCUBA Galaxies (2004, methodology): “We also measure the half-light radii of the SMGs in an analogous manner to that used by Ferguson et al. (2004), on the same HST data, and compare these with their distribution for the general optically selected population at z 2:3 (using the 15 galaxies in our sample with z ¼ 1:9 3, giving a…”
VERY BLUE UV-CONTINUUM SLOPE β OF LOW LUMINOSITY z ∼ 7 GALAXIES FROM WFC3/IR: EVIDENCE FOR EXTREMELY LOW METALLICITIES? (2009, methodology): “We modelled the pixel-by-pixel profiles of the sources using similar luminosity z ∼ 4 B-dropouts from the Bouwens et al. (2007) HUDF sample, but scaled in size (physical) as (1 + z)−1 to match the observed size-redshift relationship (Oesch et al. 2009c; Ferguson et al. 2004; Bouwens et al. 2004).”
MORPHOLOGIES OF ∼190,000 GALAXIES AT z = 0–10 REVEALED WITH HST LEGACY DATA. I. SIZE EVOLUTION (2015, background): “Assuming the constant SHSR, a number of studies discuss the evolution of host DM halos with the size growth rates (e.g., Ferguson et al. 2004; Hathi et al. 2008a).”
3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3 (2014, positive): “…for late-type galaxies is intermediate to the slow evolution of disk galaxies at z < 1 (Lilly et al. 1998; Ravindranath et al. 2004; Barden et al. 2005) and the fast evolution of UV-selected galaxies at z > 2 (Giavalisco et al. 1996; Ferguson et al. 2004; Oesch et al. 2010; Mosleh et al. 2012).”
Characterizing the Cluster Lens Population (2005, background): “However, high redshift galaxies are known to be 2 , zj+zj+1 2 ], which is represented by the bins of the histogram. compact with half light radii rh ∼ 0.3 ′′ (Ferguson et al. 2004) and thus giant arcs could be radially unresolved.”
The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation (2017, background): “…basic observational property that is found to significantly vary with galaxy mass, color or star-formation activity, and redshift (Shen et al. 2003; Ferguson et al. 2004; Trujillo et al. 2006; Elmegreen et al. 2007; Williams et al. 2010; Mosleh et al. 2012; Ono et al. 2013; van der Wel et al.…”
The Morphology-Density Relation in z ~ 1 Clusters (2005, background): “…rapidly becomes difficult and systematic errors increase both because galaxies are becoming smaller (e.g., Roche et al. 1998; Bouwens et al. 1998; Ferguson et al. 2004; Trujillo et al. 2004) and because there is insufficient area over which the integrated S/N is sufficient for accurate…”
Galaxies at z ~ 6: The UV Luminosity Function and Luminosity Density from 506 HUDF, HUDF Parallel ACS Field, and GOODS i-Dropouts (2005, methodology): “This scaling is derived in §3.7 using the current data sets and is in good agreement with previous measurements (Bouwens et al. 2004a,b; B06b; Ferguson et al. 2004).”
The Dramatic Size Evolution of Elliptical Galaxies and the Quasar Feedback (2008, background): “This scenario may appear to be contradicted by observations of Ferguson et al. (2004), who found an average size re ≃ 1.7kpc for luminous Lyman Break Galaxies (LBGs) at z ≃ 4, while we would expectre ∼ 0.5kpc, inserting the appropriate masses in eq.”