Revealing impacts of stellar mass and environment on galaxy quenching

Mao, Z.; Kodama, Tadayuki; Pérez-Martínez, J. M.; Suzuki, Tomoko L.; Yamamoto, Naoaki; Adachi, K.

doi:10.1051/0004-6361/202243733

Cited by 11 publications

(2 citation statements)

References 141 publications

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“…From the location of these galaxies in the UVJ diagram, which is also supported by their location below the star-forming main sequence (Figure 1), we interpret these galaxies as dusty post-starburst galaxies that have recently quenched their star-forming activities, which makes them detectable in F770W. Of the UVJ-quiescent galaxies in our sample, one galaxy satisfies the post-starburst classification according to Belli et al (2019), while all the UVJquiescent galaxies fall within the modified post-starburst region defined in Mao et al (2022).…”

Section: Investigating the Correlation Between Dust Morphology And Ph...supporting

confidence: 75%

A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging

Liu,

Morishita,

Kodama

2023

ApJ

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We study the morphological properties of mid-infrared selected galaxies at 1.0 < z < 1.7 in the SMACS J0723.3-7327 cluster field to investigate the mechanisms of galaxy mass assembly and structural formation at cosmic noon. We develop a new algorithm to decompose the dust and stellar components of individual galaxies by using high-resolution images in the MIRI F770W and NIRCam F200W bands. Our analysis reveals that a significant number of galaxies with stellar masses between 109.5 < M */M ⊙ < 1010.5 exhibit dust cores that are relatively more compact than their stellar cores. Specifically, within this mass range, the nonparametric method indicates that the dust cores are 1.23 (±0.05) times more compact than the stellar cores on average when evaluated with flux concentration of the two components within a fixed radius. Similarly, the parametric method yields an average compactness ratio of 1.27 (±0.06). Notably, the most massive galaxy (M * ∼ 1010.9 M ⊙) in our sample demonstrates a comparable level of compactness between its stellar core and dust, with a dust-to-stellar ratio of 0.86 (0.89) as derived from nonparametric (parametric) method. The observed compactness of the dust component is potentially attributed to the presence of a (rapidly growing) massive bulge that in some cases is associated with elevated star formation. Expanding the sample size through a joint analysis of multiple Cycle 1 deep-imaging programs can help to confirm the inferred picture. Our pilot study highlights that MIRI offers an efficient approach to studying the structural formation of galaxies from cosmic noon to the modern Universe.

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Section: Investigating the Correlation Between Dust Morphology And Ph...supporting

confidence: 75%

A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging

Liu,

Morishita,

Kodama

2023

ApJ

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“…Galaxy groups and clusters host galaxies with different morphologies that mainly depend on their histories and for how long they have been experiencing the two most important quenching mechanisms, i.e., mass and environmental quenching (Peng et al 2012;Contini et al 2017a;Kawinwanichakij et al 2017;Davies et al 2019;Rhee et al 2020;Mao et al 2022). These objects, not only host galaxies with different properties, but a large part of the stellar content within them, is made by a diffuse light from stars that are not bound to any galaxy, and feel only the potential well of the dark matter halo.…”

Section: Introductionmentioning

confidence: 99%

The Intracluster Light and Its Link with the Dynamical State of the Host Group/Cluster: The Role of the Halo Concentration

Contini,

Jeon,

Rhee

et al. 2023

ApJ

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We investigate the role of halo concentration in the formation of intracluster light (ICL) in galaxy groups and clusters, as predicted by a state-of-the-art semianalytic model of galaxy formation, coupled with a set of high-resolution dark-matter-only simulations. The analysis focuses on how the fraction of ICL correlates with halo mass, concentration, and fraction of early-type galaxies (ETGs) in a large sample of groups and clusters with 13.0 ≤ log M halo ≤ 15.0 . The fraction of ICL follows a normal distribution, a consequence of the stochastic nature of the physical processes responsible for the formation of the diffuse light. The fractional budget of ICL depends on both halo mass (very weakly) until group scales, and concentration (remarkably). More interestingly, the ICL fraction is higher in more concentrated objects, a result of the stronger tidal forces acting in the innermost regions of the halos where the concentration is the quantity playing the most relevant role. Our model predictions do not show any dependence between the ICL and ETGs fractions, and so we instead suggest the concentration rather than the mass, as recently claimed, to be the main driver of the ICL formation. The diffuse light starts to form in groups via stellar stripping and mergers and later assembled in more-massive objects. However, the formation and assembly keep going on group/cluster scales at lower redshift through the same processes, mainly via stellar stripping in the vicinity of the central regions where tidal forces are stronger.

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The VANDELS Survey: Star formation and quenching in two over-densities at 3 < z < 4

Espinoza Ortiz,

Guaita,

Demarco

et al. 2024

A&A

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Exploring galaxy evolution in dense environments, such as proto-clusters, is pivotal for understanding the mechanisms that drive star formation and the quenching of star formation. This study provides insights into how two over-densities could have impacted the physical properties, such as the star formation rate, stellar mass, morphology, and the evolution of their members, particularly members characterised by a quenching of star formation. We focus on the over-densities identified at $3<z<4$ in the Chandra Deep Field South (CDFS) and in the Ultra Deep Survey (UDS) regions of the VIMOS (VIsible MultiObject Spectrograph) Ultra Deep Survey (VANDELS). Our methodology involves the analysis of the spectral energy distribution of the members of the over-densities and of the galaxies in the field. We relied on Bayesian analysis techniques BEAGLE and BAGPIPES to study the best-fit physical parameters and the rest-frame U-V and V-J colours (UVJ). This approach allowed us to separate quenched and star-forming galaxies based on the UVJ diagram and by estimating their specific star formation rate (sSFR). We used the TNG300 simulation to interpret our results. We find that two out of 13 over-densities host quenched galaxies, with red rest-frame U-V colour and low sSFR. The physical properties of them are consistent with those of massive passive galaxies from the literature. The quenched members are redder, older, more massive, and show a more compact morphology than the other galaxy members. The two over-densities, with the highest-density peaks at $z and $z respectively, have dark matter halo masses consistent with being proto-clusters at $z and they each host an active galactic nucleus (AGN). We found five AGNs in the structure at $z and three AGNs in the one at $z In comparison to quenched galaxies in the field, our massive quenched members show a higher local density environment. By using the IllustrisTNG simulation (TNG300), we find that proto-cluster structures with quenched galaxies at high redshift are likely to evolve into a structure with a higher fraction of passive galaxies by $z = The two over-densities studied here host massive quenched galaxies in their highest-density peaks and AGNs. By following the evolution of the passive galaxies in the simulated proto-clusters at $z = 3$ from the TNG300 simulation, we find that the median of their sSFRs was larger than 10$^ $ yr$^ $ at $z=6$ and the median mass growth rate was 96<!PCT!> from $z=6$ to $z=3$. In 20<!PCT!> of the simulated proto-clusters, the passive galaxy had already accreted 10-20<!PCT!> of the mass at $z=6$, with SFRs $>100$ M$_ odot $ yr$^ $ at $z=8$. The conditions for this favorable mass assembly could be the galaxy interactions and the high gas accretion rate in the dense environment. As a consequence, the quenching of the star formation at $z=3$ could be driven by the black hole mass growth and AGN feedback. This scenario is consistent with the properties of the two quenched galaxies we find in our two over-densities at $z sim3$.

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Revealing impacts of stellar mass and environment on galaxy quenching

Abstract: Aims. Galaxy quenching is a critical step in galaxy evolution. In this work, we present a statistical study of galaxy quenching in 17 cluster candidates at 0.5 Show more

Cited by 11 publications

References 141 publications

A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging

A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging

The Intracluster Light and Its Link with the Dynamical State of the Host Group/Cluster: The Role of the Halo Concentration

The VANDELS Survey: Star formation and quenching in two over-densities at 3 < z < 4

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