The Size Evolution of High-Redshift Galaxies

Ferguson, Henry C.; Dickinson, Mark; Giavalisco, Mauro; Kretchmer, C.; Ravindranath, Swara; Idzi, R.; Taylor, Edward N.; Conselice, Christopher J.; Fall, S. Michael; Gardner, Jonathan P.; Livio, Mario; Madau, Piero; Moustakas, Leonidas A.; Papovich, C.; Somerville, Rachel S.; Spinrad, Hyron; Stern, Daniel

doi:10.1086/378578

Cited by 393 publications

(506 citation statements)

References 31 publications

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“…The half light radius of these LAEs at z = 2, however, is not correlated to the EW in Lyman-α. The stellar massradius relation evolves in redshift as (1 + z) −1 , in a manner consistent with the size evolution found by Bouwens et al (2004) and Ferguson et al (2004) for LBGs at z ≥ 2-5 and by Hathi et al (2008) at z ∼ 5-6.…”

Section: Introductionsupporting

confidence: 87%

“…A more reliable distribution for the axial ratio parameter b/a, following Ferguson et al (2004) can be adopted in our simulations, but we must stress that, in their work, this functional form is measured on a sample of photometrically selected candidate galaxies at z ∼ 4, and it is not clear whether this should be applied also to our z ∼ 7 sample. A more detailed approach, like that adopted in Law et al (2012) work, is more appropriate but very complex and goes beyond the aims of this paper.…”

Section: Is This Picture Conclusive?mentioning

confidence: 99%

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The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

Grazian

Castellano

Fontana

et al. 2012

A&A

103

157

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Context. The exploration of the relation between galaxy sizes and other physical parameters (luminosity, mass, star formation rate) has provided important clues for understanding galaxy formation, but such exploration has until recently been limited to intermediate redshift objects. Aims. We use the currently available CANDELS Deep+Wide surveys in the GOODS-South, UDS and EGS fields, complemented by data from the HUDF09 program, to address the relation between size and luminosity at z ∼ 7. Methods. The six different fields used for this study are characterized by a wide combination of depth and areal coverage, well suited for reducing the biases on the observed size-magnitude plane. From these fields, we select 153 z-band dropout galaxies. Detailed simulations have been carried out for each of these six fields, inserting simulated galaxies at different magnitudes and half light radius in the two dimensional images for all the Hubble Space Telescope (HST) bands available and recovering them as carried out for the real galaxies. These simulations allow us to derive precisely the completeness as a function of size and magnitude and to quantify measurements errors/biases, under the assumption that the 2D profile of z = 7 galaxies is well represented by an exponential disk function. Results. We find in a rather robust way that the half light radius distribution function of z ∼ 7 galaxies fainter than J = 26.6 is peaked at ≤0.1 arcsec (or equivalently 0.5 kpc proper), while at brighter magnitudes high-z galaxies are typically larger than ∼0.15 arcsec. We also find a well defined size-luminosity relation, Rh ∝ L 1/2 . We compute the luminosity function (LF) in the HUDF and P12HUDF fields, finding large spatial variation on the number density of faint galaxies. Adopting the size distribution and the size-luminosity relation found for faint galaxies at z = 7, we derive a mean slope of −1.7 ± 0.1 for the LF of LBGs at this redshift. Conclusions. Using this LF, we find that the number of ionizing photons emitted from galaxies at z ∼ 7 cannot keep the Universe re-ionized if the IGM is clumpy (C HII ≥ 3) and the Lyman continuum escape fraction of high-z LBGs is relatively low ( f esc ≤ 0.3). If these results are confirmed and strengthened by future CANDELS data, in particular by the forthcoming deep observations in GOODS-South and North and the wide field COSMOS, we can put severe limits to the role of galaxies in the reionization of the Universe.

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Section: Introductionsupporting

confidence: 87%

Section: Is This Picture Conclusive?mentioning

confidence: 99%

The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

Grazian

Castellano

Fontana

et al. 2012

A&A

103

157

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“…Taking the BB paradigm for granted, Ferguson et al (2004) found the galaxy radii to scale with redshift approximately as the Hubble parameter H -1 (z), i.e., approximately ~ (1 + z) -1 . They say that "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."…”

Section: Angular Sizementioning

confidence: 99%

From magnitudes and redshifts of supernovae, their light-curves, and angular sizes of galaxies to a tenable cosmology

Traunmüller

2014

Astrophys Space Sci

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Early physical cosmologies were based on interpretations of the cosmic redshift for which there was insufficient evidence and on theories of gravitation that appear to be falsified by galactic dynamics. Eventually, the big bang paradigm came to be guarded against refutation by ad hoc hypotheses (dark matter, cosmic inflation, dark energy) and free parameters. Presently available data allow a more satisfactory phenomenological approach. Using data on magnitude and redshift from 892 type Ia supernovae, it is first shown that these suggest that the redshift factor (1 + z) is simply an exponential function of distance and that, for "standard candles", magnitude m = 5 log[(1 + z) ln(1 + z)] + const. While these functions are incompatible with a big bang, they characterize certain tired light models as well as exponential expansion models. However, the former are falsified by the stretched light curves of distant supernovae and the latter by the absence of a predicted 1+z increase in the angular sizes of galaxies. Instead, the observations suggest that physical processes speed up and objects contract uniformly as an exponential function of time, standards of measurement not excluded, and only free waves being excepted. Distant events proceed, then, more slowly, while angular sizes remain unaffected, approximately as observed. Since all objects contract in proportion, the Universe retains a static appearance. A corresponding physical theory, which should also explain galactic dynamics, remains yet to be derived from first principles. A way to do this, satisfying also Mach"s principle, is vaguely suggested.

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“…For the U-dropout galaxies, we have used the effective volume derived by Steidel et al (1999). For the B-dropout galaxies, we have simulated artificial LBGs in the GOODS data with a distribution of colors and sizes that match the observed B-dropout properties (see Ferguson et al 2004). We then measure photometry for the simulated galaxies and apply our color selection criteria to derive the probability that a LBG with given magnitude and redshift is detected in the data, .…”

Section: The Integrated Seds Of High-redshift Galaxiesmentioning

confidence: 99%

Evolution in the Colors of Lyman Break Galaxies from z ~ 4 to z ~ 3

Papovich

Dickinson

Ferguson

et al. 2004

ApJ

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The integrated colors of distant galaxies provide a means for interpreting the properties of their stellar content. Here we use rest-frame UV-to-optical colors to constrain the spectral energy distributions and stellar populations of color-selected, B-dropout galaxies at in the Great Observatories Origins Deep Survey (GOODS). We z ∼ 4 combine the Advanced Camera for Surveys data with ground-based near-infrared images, which extend the coverage of galaxies at to the rest-frame B band. We observe a color-magnitude trend in the rest-frame z ∼ 4 ϪB versus B diagram for the galaxies that has a fairly well-defined "blue envelope," and is strikingly m(UV) z ∼ 4 similar to that of color-selected, U-dropout galaxies at . We also find that although the co-moving luminosity z ∼ 3 density at rest-frame UV wavelengths (1600 ) is roughly comparable at and ∼4, the luminosity densitẙ A z ∼ 3 at rest-frame optical wavelengths increases by about one-third from to ∼3. Although the star formation z ∼ 4 histories of individual galaxies may involve complex and stochastic events, the evolution in the global luminosity density of the UV-bright galaxy population corresponds to an average star formation history with a star formation rate that is constant or increasing over these redshifts. This suggests that the evolution in the luminosity density corresponds to an increase in the stellar mass density of տ33%.

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The Size Evolution of High-Redshift Galaxies

Cited by 393 publications

References 31 publications

The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

From magnitudes and redshifts of supernovae, their light-curves, and angular sizes of galaxies to a tenable cosmology

Evolution in the Colors of Lyman Break Galaxies from z ~ 4 to z ~ 3

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