Galaxy Structure, Stellar Populations, and Star Formation Quenching at 0.6 ≲ z ≲ 1.2

Kim, Keun-Ho; Malhotra, Sangeeta; Rhoads, James E.; Joshi, Bhavin; Fererras, Ignacio; Pasquali, A.

doi:10.3847/1538-4357/aae488

Cited by 23 publications

(28 citation statements)

References 134 publications

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“…A natural consequence of this is that the B/T (and also more generally the Sérsic index and light concentration which measures similar properties) ratio of galaxies is correlated with f Q , as we show in Fig. 8 (see also Kim et al 2018).…”

Section: Structural Dependence Predicted From the Quiescent Fractionsupporting

confidence: 62%

“…Overall we find quiescent galaxies to have higher values of B/T than star-forming galaxies at stellar masses greater than 10 10 M , which is expected given the more bulge-dominated nature of quiescent galaxies (e.g. Wuyts et al 2011;Kim et al 2018;Morselli et al 2019). Regarding the trend with stellar mass, we find that both quiescent and star-forming systems show an increase of B/T with increasing stellar mass (weak, non-negligible correlation -<1% -likely of being an uncorrelated distribution).…”

Section: Prominence Of Galactic Bulgessupporting

confidence: 56%

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VIS³COS

Paulino-Afonso

Sobral

Darvish

et al. 2019

A&A

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We study the impact of local density and stellar mass on the structure and morphology of approximately 500 quiescent and star-forming galaxies from the VIMOS Spectroscopic Survey of a Superstructure in COSMOS (VIS3COS). We perform bulge-to-disc decomposition of the surface brightness profiles and find ∼41 ± 3% of > 1010 M⊙ galaxies to be best fitted with two components. We complement our analysis with non-parametric morphological measurements and qualitative visual classifications. We find that both galaxy structure and morphology depend on stellar mass and environment for our sample as a whole. We only find an impact of the environment on galaxy size for galaxies more massive than 1011 M⊙. We find higher Sérsic indices (n) and bulge-to-total ratios (B/T) in high-density regions when compared to low-density counterparts at similar stellar masses. We also find that galaxies with higher stellar mass have steeper light profiles (high n, B/T) compared to galaxies with lower stellar mass. Using visual classifications, we find a morphology–density relation at z ∼ 0.84 for galaxies more massive than 1010 M⊙, with elliptical galaxies being dominant at high-density regions and disc galaxies more common in low-density regions. However, when splitting the sample into colour–colour-selected star-forming and quiescent sub-populations, there are no statistically significant differences between low- and high-density regions. We find that quiescent galaxies are smaller, have higher Sérsic indices (for single profiles, around n ∼ 4), and higher bulge-to-total light ratios (for decomposed profiles, around B/T ∼ 0.5) when compared to star-forming counterparts (n ∼ 1 and B/T ∼ 0.3, for single and double profiles, respectively). We confirm these trends with non-parametric quantities, finding quiescent galaxies to be smoother (lower asymmetry, lower M20) and to have most of their light over smaller areas (higher concentration and Gini coefficient) than star-forming galaxies. Overall, we find a stronger dependence of structure and morphology on stellar mass than on local density and these relations are strongly correlated with the quenching fraction. The change in average structure or morphology corresponds to a change in the relative fractions of blue disc-like galaxies and red elliptical galaxies with stellar mass and environment. We hypothesise that the processes responsible for the quenching of star formation must also affect the galaxy morphology on similar timescales.

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Section: Structural Dependence Predicted From the Quiescent Fractionsupporting

confidence: 62%

Section: Prominence Of Galactic Bulgessupporting

confidence: 56%

VIS³COS

Paulino-Afonso

Sobral

Darvish

et al. 2019

A&A

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“…The specific star formation rate (sSFR), defined as star formation rate normalized by stellar mass, is a powerful summary statistic for the level of star formation in galaxies (e,g., Whitaker et al 2012;Kim et al 2018). Since the power available to drive galactic winds increases with increasing star formation, while the escape velocity for such winds increases with stellar mass, it is reasonable to expect galactic scale outflows to be more common and stronger where sSFR is high.…”

Section: Examining Specific Star Formation Intensitymentioning

confidence: 99%

The Importance of Star Formation Intensity in Lyα Escape from Green Pea Galaxies and Lyman Break Galaxy Analogs

Kim

Malhotra

Rhoads

et al. 2020

ApJ

Self Cite

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We have studied ultraviolet images of 40 Green Pea galaxies and 15 local Lyman Break Galaxy Analogs to understand the relation between Lyα photon escape and central UV photometric properties. We measured star formation intensity (SFI, star formation rate per unit area) from the central 250 pc region (S 250pc ) using COS/NUV images from the Hubble Space Telescope. The measured S 250pc of our sample Green Peas ranges from 2.3-46 M ⊙ year −1 kpc −2 , with a geometric mean of 15M ⊙ year −1 kpc −2 and a standard deviation of 0.266 dex, forming a relatively narrow distribution. The Lyman Break Galaxy Analogs show a similarly narrow distribution of S 250pc (0.271 dex), though with a larger mean of 28 M ⊙ year −1 kpc −2 . We show that while the Lyα equivalent width (EW(Lyα)) and the Lyα escape fraction ( f Lyα esc ) are not significantly correlated with the central SFI (S 250pc ), both are positively correlated with the ratio of surface brightness to galaxy stellar mass (S 250pc /M star ), with correlation coefficients (p-values) of 0.702 (1 × 10 −8 ) and 0.529 (5 × 10 −4 ) with EW(Lyα) and f Lyα esc , respectively. These correlations suggest a scenario where intense central star formation can drive a galactic wind in galaxies with relatively shallow gravitational potential wells, thus clearing channels for the escape of Lyα photons.

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“…At 𝑧 < 1, many studies have reported a positive correlation between D n 4000 and stellar mass (e.g. Brinchmann et al 2004;Moresco et al 2010Moresco et al , 2011Moresco et al , 2016Haines et al 2017;Siudek et al 2017;Kim et al 2018;Wu et al 2018a). This has been widely associated with the "downsizing" trend, in which the stellar populations of more massive galaxies formed earlier in cosmic history, with present-day star formation concentrated in lower-mass galaxies (e.g.…”

Section: Introductionmentioning

confidence: 99%

A combined VANDELS and LEGA-C study: the evolution of quiescent galaxy size, stellar mass and age from $\mathbf{\textit{z} = 0.6}$ to $\mathbf{\textit{z} = 1.3}$

Hamadouche,

Carnall,

McLure

et al. 2022

Preprint

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We study the relationships between stellar mass, size and age within the quiescent population, using two mass-complete spectroscopic samples with log 10 (𝑀 ★ /M ) > 10.3, taken from VANDELS at 1.0 < 𝑧 < 1.3, and LEGA-C at 0.6 < 𝑧 < 0.8. Using robust D n 4000 values, we demonstrate that the well-known 'downsizing' signature is already in place by 𝑧 1.1, with D n 4000 increasing by 0.1 across a 1 dex mass interval for both VANDELS and LEGA-C. We then proceed to investigate the evolution of the quiescent galaxy stellar mass-size relation from 𝑧 1.1 to 𝑧 0.7. We find the median size increases by a factor of 1.9 ± 0.1 at log 10 (𝑀 ★ /M ) = 10.5, and see tentative evidence for flattening of the relation, finding slopes of 𝛼 = 0.72 ± 0.06 and 𝛼 = 0.56 ± 0.04 for VANDELS and LEGA-C respectively. We finally split our sample into galaxies above and below our fitted mass-size relations, to investigate how size and D n 4000 correlate. For LEGA-C, we see a clear difference, with larger galaxies found to have smaller D n 4000 at fixed stellar mass. Due to the faintness and smaller numbers of the VANDELS sample, we cannot confirm whether a similar relation exists at 𝑧 1.1. We consider whether differences in stellar age or metallicity are most likely to drive this size-D n 4000 relation, finding that any metallicity differences are unlikely to fully explain the observed offset, meaning smaller galaxies must be older than their larger counterparts. We find the observed evolution in size, mass and D n 4000 across the 2 Gyr from 𝑧 ∼ 1.1 to 𝑧 ∼ 0.7 can be explained by a simple toy model in which VANDELS galaxies evolve passively, whilst experiencing a series of minor mergers.

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Galaxy Structure, Stellar Populations, and Star Formation Quenching at 0.6 ≲ z ≲ 1.2

Cited by 23 publications

References 134 publications

VIS³COS

VIS³COS

The Importance of Star Formation Intensity in Lyα Escape from Green Pea Galaxies and Lyman Break Galaxy Analogs

A combined VANDELS and LEGA-C study: the evolution of quiescent galaxy size, stellar mass and age from $\mathbf{\textit{z} = 0.6}$ to $\mathbf{\textit{z} = 1.3}$

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