Half-mass Radii of Quiescent and Star-forming Galaxies Evolve Slowly from 0 ≲ z ≤ 2.5: Implications for Galaxy Assembly Histories*

Suess, Katherine A.; Kriek, Mariska; Price, Sedona H.; Barro, Guillermo

doi:10.3847/2041-8213/ab4db3

Cited by 69 publications

(74 citation statements)

References 45 publications

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“…In the left panel of Figure 6 we reproduce the results reported in Suess et al (2019b) for quiescent galaxies with masses log(𝑀 ★ /M )>10.1, black dots with error bars. The strong 𝑅 50M /𝑅 50𝑟 evolution observed at 𝑧 1 appears to flatten at 𝑧 < 1.…”

Section: Comparison With Direct Observationssupporting

confidence: 65%

“…This is because the Υ ★ gradients became more negative with time. In Suess et al (2019b), the authors extended their analysis to 𝑧 ≈ 0.25 by adding ∼ 9000 CANDELS galaxies at 𝑧 ≤ 1.0 and found that the 𝑅 50M -to-𝑅 50L ratios decrease slower or remain constant at 𝑧 ∼ 1.…”

Section: Comparison With Direct Observationsmentioning

confidence: 99%

“…We measured the 𝑅 50M -to-𝑅 50𝑟 ratio of our CLE archaeological progenitors with masses log(𝑀 ★ (𝑧)/M )>10.1, where the masses are calculated at each 𝑧 as 𝑀 ★ (𝑧)=𝑀 ★ × (𝑀 P3D ★ (𝑧)/𝑀 P3D ★ (𝑧 obs )); recall that 𝑀 ★ is the mass of the observed galaxy from the NSA catalog. We plot the running medians of 𝑅 50M /𝑅 50L (orange solid line) in the same redshift bins as in Suess et al (2019b) and the associated quartiles (shaded area). Our fossil record inferences for the progenitors of local CLE galaxies show, on average, a similar trend but less evolution in the 𝑅 50M -to-𝑅 50L ratios than reported in Suess et al (2019b) for quiescent galaxies observed at different redshfits.…”

Section: Comparison With Direct Observationsmentioning

confidence: 99%

“…We plot the running medians of 𝑅 50M /𝑅 50L (orange solid line) in the same redshift bins as in Suess et al (2019b) and the associated quartiles (shaded area). Our fossil record inferences for the progenitors of local CLE galaxies show, on average, a similar trend but less evolution in the 𝑅 50M -to-𝑅 50L ratios than reported in Suess et al (2019b) for quiescent galaxies observed at different redshfits. Below we discuss some questions to consider regarding this comparison.…”

Section: Comparison With Direct Observationsmentioning

confidence: 99%

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The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

Ibarra-Medel,

Avila-Reese,

Lacerna

et al. 2021

Preprint

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We apply stellar population synthesis analysis to obtain spatially-resolved archaeological inferences for a large sample of "red and dead" Elliptical galaxies (Classical Ellipticals; CLEs) from the MaNGA/SDSS-IV DR15 survey. From their 2D stellar light and mass maps, we explore the differences between the radial mass and light distributions in the rest-frame bands 𝑔, 𝑟, and 𝑖 as functions of look-back time, 𝑡 lb , or redshift, 𝑧. We characterize these differences through the ratios between the following mass-and light-derived global properties: sizes, concentrations, and effective surface densities. We find that the mass-to-light ratios of these properties change with 𝑡 lb , more the more massive the galaxies are. The CLE galaxy archaeological progenitors are, on average, less compact, concentrated, and dense in light than in mass as 𝑧 decreases. However, at later times, when also the evolution of the progenitors becomes passive at all radii, there is an upturn in these trends and the differences between mass and light in compactness/concentration decrease towards 𝑧 ∼ 0. The trends in the ratios of mass to light sizes agree qualitatively with results from direct observations in galaxy surveys at different redshifts. We discuss the caveats and interpretations of our results, and speculate that the strong structural evolution found in some previous studies for early-type galaxies could be explained partially by photometric changes rather than by intrinsic structural changes.

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Section: Comparison With Direct Observationssupporting

confidence: 65%

Section: Comparison With Direct Observationsmentioning

confidence: 99%

Section: Comparison With Direct Observationsmentioning

confidence: 99%

Section: Comparison With Direct Observationsmentioning

confidence: 99%

See 2 more Smart Citations

The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

Ibarra-Medel,

Avila-Reese,

Lacerna

et al. 2021

Preprint

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“…However, colors are not sensitive to IMF differences, so their methodology does not, in fact, it cannot account for IMF variations (or, for that matter, the age-metallicity degeneracy), which we showed may be the dominant driver of M * /L gradients at low-z. In this context, it is useful to compare our Figure 10 with the horizontal dashed line in the right hand panel of Figure 1 in Suess et al (2019b). Our analysis, which is sensitive to IMF-driven gradients, shows that Re, * /Re decreases from 0.8 to 0.5 as M * increases from 3 × 10 10 M to 5 × 10 11 M , whereas their analysis returns Re, * /Re ∼ 0.8 at all M * .…”

Section: Comparison With Quiescent Galaxies At High Redshiftmentioning

confidence: 99%

The half mass radius of MaNGA galaxies: Effect of IMF gradients

Bernardi¹,

Sheth²,

Sánchez³

et al. 2022

Preprint

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Gradients in the stellar populations of galaxies -e.g., in age, metallicity, IMF -can result in gradients in the stellar mass to light ratio, M * /L. Such gradients imply that the distribution of the stellar mass and light are different. For old stellar populations, such as those typical of early-type galaxies at z ∼ 0, the M * /L gradients are weak if driven by variations in age and metallicity. However, if they are driven by variations in the stellar Initial Mass Function (IMF), then they can be significantly larger. An IMF-driven gradient which has M * /L decreasing outwards from the center increases the estimated total stellar mass (M * ) and reduces the scale which contains half this mass (R e, * ), compared to the values of mass and size when the gradient is ignored. We estimate IMF-gradients from spatially resolved spectra of early-type galaxies in the final release of the MaNGA survey, showing that the fractional decrease in R e, * can be significantly larger than the fractional M * increase, especially when the light is more centrally concentrated. The R e, * −M * correlation which results from the IMF-driven M * /L gradients at z ∼ 0 is offset by almost 0.3 dex to smaller sizes compared to when these gradients are ignored. Comparison with higher redshift samples is not straightforward. If it is fair to compare z ∼ 0 'early-type' galaxies with 'quiescent' galaxies at higher-z, then one must be able to consistently account for evolution in stellar population gradients (especially age and IMF) as well as changes in the steepness of the light profile before drawing conclusions about the evolution of the R e, * − M * relation.

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The dark matter halo masses of elliptical galaxies as a function of observationally robust quantities

Sonnenfeld

Tortora

Hoekstra

et al. 2022

A&A

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Context. The assembly history of the stellar component of a massive elliptical galaxy is closely related to that of its dark matter halo. Measuring how the properties of galaxies correlate with their halo mass can therefore help to understand their evolution. Aims. We investigate how the dark matter halo mass of elliptical galaxies varies as a function of their properties, using weak gravitational lensing observations. To minimise the chances of biases, we focus on the following galaxy properties that can be determined robustly: the surface brightness profile and the colour. Methods. We selected 2409 central massive elliptical galaxies (log M*/M⊙ ≳ 11.4) from the Sloan Digital Sky Survey spectroscopic sample. We first measured their surface brightness profile and colours by fitting Sérsic models to photometric data from the Kilo-Degree Survey (KiDS). We fitted their halo mass distribution as a function of redshift, rest-frame r-band luminosity, half-light radius, and rest-frame u − g colour, using KiDS weak lensing measurements and a Bayesian hierarchical approach. For the sake of robustness with respect to assumptions on the large-radii behaviour of the surface brightness, we repeated the analysis replacing the total luminosity and half-light radius with the luminosity within a 10 kpc aperture, Lr, 10, and the light-weighted surface brightness slope, Γ10. Results. We did not detect any correlation between the halo mass and either the half-light radius or colour at fixed redshift and luminosity. Using the robust surface brightness parameterisation, we found that the halo mass correlates weakly with Lr, 10 and anti-correlates with Γ10. At fixed redshift, Lr, 10 and Γ10, the difference in the average halo mass between galaxies at the 84th percentile and 16th percentile of the colour distribution is 0.00 ± 0.11 dex. Conclusion. Our results indicate that the average star formation efficiency of massive elliptical galaxies has little dependence on their final size or colour. This suggests that the origin of the diversity in the size and colour distribution of these objects lies with properties other than the halo mass.

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Half-mass Radii of Quiescent and Star-forming Galaxies Evolve Slowly from 0 ≲ z ≤ 2.5: Implications for Galaxy Assembly Histories*

Cited by 69 publications

References 45 publications

The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

The half mass radius of MaNGA galaxies: Effect of IMF gradients

The dark matter halo masses of elliptical galaxies as a function of observationally robust quantities

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