MORPHOLOGIES OF ∼190,000 GALAXIES AT z = 0–10 REVEALED WITH HST LEGACY DATA. I. SIZE EVOLUTION

By T. Shibuya, M. Ouchi, Y. Harikane. 2015

316 citations recorded by the source corpus.

We present the redshift evolution of the galaxy effective radius re obtained from the Hubble Space Telescope (HST) samples of ∼190,000 galaxies at z = 0–10. Our HST samples consist of 176,152 photo-z galaxies at z = 0–6 from the 3D-HST+CANDELS catalog and 10,454 Lyman break galaxies (LBGs) at z = 4–10 identified in the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS), HUDF 09/12, and HFF parallel fields, providing the largest data set to date for galaxy size evolution studies. We derive re with the same technique over the wide redshift range of z = 0–10, evaluating the optical-to-UV morphological K correction and the selection bias of photo-z galaxies+LBGs as well as the cosmological surface-brightness dimming effect. We find that re values at a given luminosity significantly decrease toward high z, regardless of statistics choices (e.g., r e ∝ ( 1 + z ) − 1.10 ± 0.06 ?> for median). For star-forming galaxies, there is no evolution of the power-law slope of the size–luminosity relation and the median Sérsic index ( n ∼ 1.5 ?> ). Moreover, the re distribution is well represented by log-normal functions whose standard deviation &sgr; ln r e ?> does not show significant evolution within the range of &sgr; ln r e ∼ 0.45 − 0.75 ?> . We calculate the stellar-to-halo size ratio from our re measurements and the dark-matter halo masses estimated from the abundance-matching study, and we obtain a nearly constant value of r e / r vir = 1.0 % − 3.5 % ?> at z = 0–8. The combination of the re-distribution shape+standard deviation, the constant r e / r vir ?> , and n ∼ 1.5 ?> suggests a picture in which typical high-z star-forming galaxies have disk-like stellar components in a sense of dynamics and morphology over cosmic time of z ∼ 0 − 6 ?> . If high-z star-forming galaxies are truly dominated by disks, the r e / r vir ?> value and the disk-formation model indicate that the specific angular momentum of the disk normalized by the host halo is j d / m d ≃ 0.5 − 1 ?> . These are statistical results for major stellar components of galaxies, and the detailed study of clumpy subcomponents is presented in the paper II.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/20418f5e45d3a3399f4dba2d9b5417846fd33c54

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In Astronomy and Astrophysics

1. P. V. van Dokkum
2. P. Hopkins
3. C. Conroy
4. L. Hernquist
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In Instrumentation

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3. Richard S. Ellis
4. M. Franx
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6. P. Hopkins
7. A. Dekel
8. P. Oesch

Citations in the corpus

• UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, background): “As galaxy sizes scale approximately with the virial halo radius (van der Wel et al. 2014; Shibuya et al. 2015), we set the maximum threshold distance for merging with the host halo’s galaxy at fmerge ·Rvir,host, with fmerge a free parameter.”
• The MUSE Hubble Ultra Deep Field Survey - VIII. Extended Lyman-α haloes around high-z star-forming galaxies (2017, background): “The upper panel of Figure 12 shows the expected correlation (ρs=0.35, p0∼10−6) between the UV sizes and UV magnitudes of galaxies (Shibuya et al. 2015).”
• Extended Lyman α haloes around individual high-redshift galaxies revealed by MUSE (2015, background): “However, the observed trend could be mainly a by-product of the general size evolution of galaxies (e.g. Shibuya et al. 2015).”
• Inferences on the timeline of reionization at z ∼ 8 from the KMOS Lens-Amplified Spectroscopic Survey (2019, background): “′′8 wide IFUs cover ∼ 14 proper kpc at z ∼ 8, while the UV effective radii of galaxies at these redshifts is only ∼< 1 proper kpc (Shibuya et al. 2015).”
• SILVERRUSH. IV. Lyα luminosity functions at z = 5.7 and 6.6 studied with ∼1300 Lyα emitters on the 14–21 deg2 sky (2017, unknown): “(Shibuya et al. 2015).”
• The extreme faint end of the UV luminosity function at z ∼ 6 through gravitational telescopes: a comprehensive assessment of strong lensing uncertainties (2018, methodology): “Stacking very faint high-redshift galaxies in HFF observations, Bouwens et al. (2016) find that they do not show the apparent size expected for the calculated shear at their location if one assumes the common sizes used in the literature (e.g. the size-luminosity relation of Shibuya et al. 2015).”
• The z ∼ 6 Luminosity Function Fainter than −15 mag from the Hubble Frontier Fields: The Impact of Magnification Uncertainties (2016, background): “27: e.g., Shibuya et al. 2015), i.e., L/R2 ∝ L/(L0.”
• ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, background): “We remark that one might naturally expect an evolution in dust temperature given the observed evolution in the SFR surface densities observed in galaxies with cosmic time (e.g., Shibuya et al. 2015) and the correlation of dust temperature with SFR surface density (e.g., Elbaz et al. 2011).”
• Dark matter cores all the way down (2015, result): “We find that the relationship between R1/2 and M200 for our simulations agrees within a factor of two with that found in Kravtsov (2013); Shibuya et al. (2015); Agertz & Kravtsov (2015b), namely: R1/2 ∼ r1/2 ∼ 0.015r200 (28) where r200 is related to the virial mass M200 via equation 4.”
• A Comprehensive Study of Galaxies at z ∼ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch (2022, methodology): “The mock highredshift galaxies follow the size–MUV redshift distribution revealed with the HST legacy data sets for galaxies at z∼ 0–10 (Shibuya et al. 2015), which is extrapolated to our redshift ranges, where the size–MUV distribution is a log-normal distribution.”
• The MUSE Hubble Ultra Deep Field Survey: I. Survey description, data reduction and source detection (2017, background): “…González et al. 2011; Grazian et al. 2015; Song et al. 2016), galaxy sizes (e.g., Oesch et al. 2010; Ono et al. 2013; van der Wel et al. 2014; Shibuya et al. 2015; Curtis-Lake et al. 2016) and dust and molecular gas content (e.g., Aravena et al. 2016b,a; Decarli et al. 2016b,a), along with…”
• Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies (2015, background): “…11 Shenyang Normal University 12 Centro de Astrobiologia, CSIC-INTA 13 Colby College mic time (Bouwens et al. 2010; Finkelstein et al. 2013; Oesch et al. 2014), and have made a pivotal contribution to the study of galaxy sizes and morphologies (e.g., van der Wel et al. 2012; Shibuya et al. 2015).”
• THE POPULATION OF GALAXY–GALAXY STRONG LENSES IN FORTHCOMING OPTICAL IMAGING SURVEYS (2015, methodology): “Shibuya et al. (2015) recently analyzed the median sizes of galaxies in HST from redshift 0-10, finding that it is proportional to (1 + z)−1.12; if we use this result rather than the rs ∝ (1+z)−1.2 assumed in Equation 5, we find that this makes sources somewhat larger at high redshift (9 per cent…”
• Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST (2022, background): “The resulting sizes of 0.5 and 0.7 kpc are typical for luminous L∗ galaxies at z ∼ 6− 9, where measurements have been possible to date (e.g., Holwerda et al. 2015; Shibuya et al. 2015; Bowler et al. 2017; Kawamata et al. 2018; Yang et al. 2022).”
• Rapid Reionization by the Oligarchs: The Case for Massive, UV-bright, Star-forming Galaxies with High Escape Fractions (2019, methodology): “The SFRs are all calculated from the UV because the average ΣSFR versus z relation we calibrate our model against is derived from the UV (Shibuya et al. 2015).”