Environments of red nuggets at <i>z</i> ∼ 0.7 from the VIPERS survey

Siudek, M.; Lisiecki, Krzysztof; Krywult, J.; Donevski, Darko; Haines, C. P.; Karska, A.; Małek, K.; Moutard, T.; Pollo, A.

doi:10.1093/mnras/stad1685

Cited by 8 publications

(2 citation statements)

References 120 publications

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“…It is essential to acknowledge that these methodological differences may introduce systematic biases when making comparisons between the two studies. However, (Siudek et al 2023a) examined the field densities of red passive galaxies from VIPERS and COSMOS, revealing a general agreement. This implies that the biases introduced by different techniques may not significantly impact the ultimate conclusions.…”

Section: Comparison Of the Sfr Of Agn And Non-agn Galaxies As A Funct...mentioning

confidence: 89%

“…The VIPERS galaxy catalogue includes information on the local densities of the sources. Their calculation is described in Cucciati et al (2014Cucciati et al ( , 2017; Siudek et al (2022Siudek et al ( , 2023a. In brief, the local environment is characterized by the density contrast, δ, smoothed over a cylinder with a radius equal to the distance of the fifth nearest neighbour (Cucciati et al 2017), taking into account the local density and the mean density at each redshift.…”

Section: Local Densitiesmentioning

confidence: 99%

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Comparison of star formation histories of AGN and non-AGN galaxies

Mountrichas

Buat

Yang

et al. 2022

A&A

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We use AGN with X-ray luminosities, L X,2−10keV ∼ 10 42.5−44 erg s −1 , from the COSMOS-Legacy survey that lie within the UltraVISTA region and cross match them with the LEGA-C catalogue. The latter provides measurements of the calcium break, D n 4000, and H δ Balmer line that allow us to study the stellar populations of AGN and compare them with a galaxy reference catalogue. Our samples consist of 69 AGN and 2176 non-AGN systems, within 0.6 < z < 1.3, that satisfy the same photometric selection criteria. We construct the SEDs of both population and use the CIGALE code to investigate the effect of the two indices in the SED fitting process. Our analysis shows that the inclusion of D n 4000 and H δ allows CIGALE to constrain better the ages of the stellar populations. Furthermore, we find an increase of the estimated stellar masses by, on average, ∼ 0.2 dex, in particular for systems with young stars (D n 4000 < 1.5), when the two indices are included in the SED fitting. We then compare the D n 4000 and H δ of AGN with sources in the reference catalogue, accounting for the different stellar mass of the two populations. Our analysis reveals that low to moderate L X AGN tend to reside in galaxies with older stellar populations and are less likely to have experienced a recent star formation burst, compared to galaxies in the control sample. Finally, we compare the two populations as a function of their morphology (bulgedominated, BD, vs. non-BD) and compactness (mass-to-size ratio). A similar fraction of AGN and non-AGN systems are classified as non-BD (∼ 70%). Our analysis shows that BD AGN tend to have younger stellar populations compared to BD, non-AGN systems. On the other hand, non-BD AGN have, on average, older stellar populations and are less likely to have experienced a burst compared to non-BD sources in the reference sample. Furthermore, AGN tend to prefer more compact systems compared to non-AGN.

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Section: Comparison Of the Sfr Of Agn And Non-agn Galaxies As A Funct...mentioning

confidence: 89%

Section: Local Densitiesmentioning

confidence: 99%

Comparison of star formation histories of AGN and non-AGN galaxies

Mountrichas

Buat

Yang

et al. 2022

A&A

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Unsupervised Classification Reveals New Evolutionary Pathways

Siudek,

Lisiecki,

Mezcua

et al. 2023

Astrophysics and Space Science Proceedings

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The quiescent population at 0.5 ≤ z ≤ 0.9: Environmental impact on the mass–size relation

Figueira,

Siudek,

Pollo

et al. 2024

A&A

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How the quiescent galaxies evolve with redshift and the factors that impact their evolution are still debated. It is still unclear what the dominant mechanisms of passive galaxy growth are and what role is played by the environment in shaping their evolutionary paths over cosmic time. The population of quiescent galaxies is altered over time by several processes that can affect their mean properties. Our aim is to study the mass-size relation (MSR) of the quiescent population and to understand how the environment shapes the MSR at intermediate redshift. We used the VIMOS Public Extragalactic Redshift Survey (VIPERS), a large spectroscopic survey of sim 90 000 galaxies in the redshift range $0.5 z 1.2$. We selected a mass-complete sample of 4786 passive galaxies based on the NUVrK diagram and refined it using the $D_n4000$ spectral index to study the MSR of the passive population over $0.5 z 0.9$. The impact of the environment on the MSR and on the growth of the quiescent population is studied through the density contrast. The slope and the intercept of the MSR, $ 0.04$ and $ log (A)=0.52 0.01$, agree well with values from the literature at the same redshift. The intercept decreases with redshift, $R_e(z)=8.20 $, while the slope remains roughly constant, and the same trend is observed in the low-density (LD) and high-density (HD) environments. Thanks to the largest spectroscopic sample at $0.5 z 0.9$, these results are not prone to redshift uncertainties from photometric measurements. We find that the average size of the quiescent population in the LD and HD environments are identical within $3 and this result is robust against a change in the definition of the LD and HD environments or a change in the selection of quiescent galaxies. In the LD and HD environments, sim 30 and sim 40<!PCT!> of the population have experienced a minor merger process between $0.5 z 0.9$. However, minor mergers account only for 30 to 40<!PCT!> of the size evolution in this redshift range, the remaining evolution likely being due to the progenitor bias.

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Environments of red nuggets at z ∼ 0.7 from the VIPERS survey

Cited by 8 publications

References 120 publications

Comparison of star formation histories of AGN and non-AGN galaxies

Comparison of star formation histories of AGN and non-AGN galaxies

Unsupervised Classification Reveals New Evolutionary Pathways

The quiescent population at 0.5 ≤ z ≤ 0.9: Environmental impact on the mass–size relation

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