The mass density profile and star formation history of Gaussian and non-Gaussian clusters

Carvalho, R. R. de; Costa, A P; Moura, T. C.; Ribeiro, André

doi:10.1093/mnrasl/slz084

Cited by 7 publications

(6 citation statements)

References 41 publications

(58 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is the opposite of what happens with bright galaxies. This result may be related to the work of de Carvalho et al (2019) who find that faint spirals of NG groups are significantly different from their counterpart in the G groups, regarding their star formation history.…”

Section: The Intermediate Populationsupporting

confidence: 68%

“…Then, Costa et al (2018) find significant differences between the velocity dispersion profiles (VDP) of G and NG system, and also regarding bright and faint samples of galaxies. Finally, the study of de Carvalho et al (2019) on the Star Formation History (SFH) of cluster galaxies reveals that the SFH in faint spirals of NG groups is significantly different from their counterpart in the G groups, leading the authors to conclude that there is a higher infall rate of gas rich systems in NG groups.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Morell

Ribeiro

Carvalho

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We analyze the dependence of galaxy evolution on cluster dynamical state and galaxy luminosities for a sample of 146 galaxy clusters from the Yang SDSS catalog. Clusters were split according to their velocity distribution in Gaussians (G) and Non-Gaussians (NG), and further divided by luminosity regime. We performed a classification in the Age-SSFR plane providing three classes: star-forming (SF), passive (PAS), and intermediate (GV -green valley). We show that galaxies evolve in the same way in G and NG systems, but also suggest that their formation histories leads to different mixtures of galactic types and infall patterns. Separating the GV into star-forming and passive components, we find more bright galaxies in the passive mode of NG than in G systems. We also find more intermediate faint galaxies in the star-forming component of NG than in G systems. Our results suggest the GV as the stage where the transition from types Sab and Scd to S0 must be taking place, but the conversion between morphological types is independent of the dynamical stage of the clusters. Analyzing the velocity dispersion profiles, we find that objects recently infalling in clusters have a different composition between G and NG systems. While all galaxy types infall onto G systems, Sab and Scd dominate the infall onto NG systems. Finally, we find that faint Scd in the outskirts of NG systems present higher asymmetries relative to the mean asymmetry of field galaxies, suggesting environmental effects acting on these objects.

show abstract

Section: The Intermediate Populationsupporting

confidence: 68%

Section: Introductionmentioning

confidence: 99%

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Morell

Ribeiro

Carvalho

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…Also, faint galaxies in NG clusters show shallower color gradients than faint galaxies in G systems, indicating that galaxies entering NG clusters already started a transformation towards an elliptical morphology. Complementary to the results presented in this paper, de Carvalho et al (2019) show that faint spiral galaxies are the ones that suffer major environmental effects.…”

Section: Low Vs High Mass Galaxies Quenching In Dense Environmentssupporting

confidence: 85%

Investigating the Projected Phase Space of Gaussian and Non-Gaussian Clusters

Sampaio,

de Carvalho,

Ferreras

et al. 2021

Preprint

View full text Add to dashboard Cite

By way of the projected phase-space (PPS), we investigate the relation between galaxy properties and cluster environment in a subsample of groups from the Yang Catalog. The sample is split according to the gaussianity of the velocity distribution in the group into gaussian (G) and non-gaussian (NG). Our sample is limited to massive clusters with M 200 ≥ 10 14 M and 0.03 ≤ z ≤ 0.1. NG clusters are more massive, less concentrated and have an excess of faint galaxies compared to G clusters. NG clusters show mixed distributions of galaxy properties in the PPS compared to the G case. Using the relation between infall time and locus on the PPS, we find that, on average, NG clusters accreted ∼ 10 11 M more stellar mass in the last ∼ 5 Gyr than G clusters. The relation between galaxy properties and infall time is significantly different for galaxies in G and NG systems. The more mixed distribution in the PPS of NG clusters translates into shallower relations with infall time. Faint galaxies whose first crossing of the cluster virial radius happened 2-4 Gyr ago in NG clusters are older and more metal-rich than in G systems. All these results suggest that NG clusters experience a higher accretion of pre-processed galaxies, which characterizes G and NG clusters as different environments to study galaxy evolution.

show abstract

“…For instance, Roberts & Parker (2020) investigate the PPS of the Coma Cluster and find an excess of galaxies possibly suffering RPS in all projected radii within the virial radius at higher velocity offsets. Several works suggest differences between galaxy properties of clusters with different member velocity distributions, which translates to differences in the PPS (Ribeiro et al 2013;Roberts & Parker 2017;de Carvalho et al 2019;Sampaio et al 2021).…”

Section: Introductionmentioning

confidence: 99%

From blue cloud to red sequence: evidence of morphological transition prior to star formation quenching

Carvalho

Ferreras

Aragón-Salamanca

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present a study of a sample of 254 clusters from the SDSS-DR7 Yang Catalog and an auxiliary sample of field galaxies to perform a detailed investigation on how galaxy quenching depends on both environment and galaxy stellar mass. Our samples are restricted to 0.03≤z≤0.1 and we only consider clusters with $\rm log(M_{halo}/M_{\odot }) \ge 14$. Comparing properties of field and cluster galaxies in the Blue Cloud, Green Valley and Red Sequence, we find evidence that field galaxies in the red sequence hosted star formation events $\rm 2.1 \pm 0.7$ Gyr ago, on average, more recently than galaxies in cluster environments. Dissecting the star formation rate vs stellar mass diagram we show how morphology rapidly changes after reaching the green valley region, while the star formation rate keeps decreasing. In addition, we use the relation between location in the projected phase space and infall time to explore the time delay between morphological and specific Star Formation Rate variations. We estimate that the transition from late to early-type morphology happens in $\rm \Delta t_{inf} \sim$1 Gyr, whereas the quenching of star formation takes ∼3 Gyr. The time-scale we estimate for morphological transitions is similar to the expected for the delayed-then-rapid quenching model. Therefore, we suggest that the delay phase is characterized mostly by morphological transition, which then contributes morphological quenching as an additional ingredient in galaxy evolution.

show abstract

The mass density profile and star formation history of Gaussian and non-Gaussian clusters

Cited by 7 publications

References 41 publications

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Classification and evolution of galaxies according to the dynamical state of host clusters and galaxy luminosities

Investigating the Projected Phase Space of Gaussian and Non-Gaussian Clusters

From blue cloud to red sequence: evidence of morphological transition prior to star formation quenching

Contact Info

Product

Resources

About