The influence of the dynamic state of galaxy clusters on segregation phenomena and velocity dispersion profiles

Nascimento, R. S.; Lopes, P. A. A.; Ribeiro, André; Costa, A P; Morell, D F

doi:10.1093/mnrasl/sly229

Cited by 8 publications

(8 citation statements)

References 49 publications

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“…Such a trend is found to be steeper in highmass clusters than in low-mass clusters (Brown et al 2017;Yoon & Rosenberg 2015;Hess & Wilcots 2013;Woo et al 2013), more significant for low-mass galaxies than for high-mass galaxies (Woo et al 2017;Zhang et al 2013;Woo et al 2013;Wetzel et al 2013), consistent with the way that RPS is predicted to work. Later, it was found that galaxy properties also vary as function of radial velocity offsets from the cluster center at a given projected distance (Nascimento et al 2019;Bayliss et al 2017;Barsanti et al 2016;Mahajan et al 2011;Pimbblet et al 2006). With the aid of cosmological simulations, it becomes clear that positions on the PSD are associated with galaxies at different infall stages, thus show correlation with the averaged galactic properties (Haines et al 2015;Boselli et al 2014b;Gill et al 2005).…”

Section: Radial Extension Of Rps In the Massive Clustersmentioning

confidence: 99%

Ram pressure stripping of HI-rich galaxies infalling into massive clusters

Wang,

Xu,

Lee

et al. 2020

Preprint

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We estimate the strength of ram pressure stripping (RPS) for Hi-rich galaxies in X-ray detected clusters. We find that galaxies under stronger RPS tend to show more significantly reduced total Hi mass and enhanced central SFR, compared to control galaxies in the field which have similar stellar mass, stellar surface density and integral star formation rate. Galaxies under strong or weak RPS account for ∼40% of the Hi-rich population at R 200 , and even beyond R 200 in the most massive clusters. Our results imply the important role of RPS as a channel of environmental processing far before the galaxies reach the core region of clusters.

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Section: Radial Extension Of Rps In the Massive Clustersmentioning

confidence: 99%

Ram pressure stripping of HI-rich galaxies infalling into massive clusters

Wang,

Xu,

Lee

et al. 2020

Preprint

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“…Menci & Fusco-Femiano 1996;Hou et al 2012;Pimbblet et al 2014;Bilton & Pimbblet 2018), presence of different spectral classes galaxies (Rood et al 1972) and cluster dynamical state (e.g. Hou et al 2009;Costa et al 2018;Nascimento et al 2019).…”

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

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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.

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“…interactions (de Carvalho et al 2017) either prior, or during, off-axial mergers between two sub-clusters; the pronounced population of late-type galaxies on infall in merging environments as inferred by the blue sub-populations of galaxies gaining angular momentum r200, chiefly thought to be the result of galaxies with spiral morphology that have survived pre-processing (e.g. Cava et al 2017;Costa et al 2018;Bilton & Pimbblet 2018;Nascimento et al 2019). The study of rotational profiles would have been aided by the addition of understanding how different morphological sub-populations of cluster galaxies contributed to each of the colour profiles.…”

Section: Discussion and Summarymentioning

confidence: 99%

The rotational profiles of cluster galaxies

Bilton

Hunt

Pimbblet

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We compile two samples of cluster galaxies with complimentary hydrodynamic and N-body analysis using FLASH code to ascertain how their differing populations drive their rotational profiles and to better understand their dynamical histories. We select our main cluster sample from the X-ray Galaxy Clusters Database (BAX), which are populated with Sloan Digital Sky Survey (SDSS) galaxies. The BAX clusters are tested for the presence of sub-structures, acting as proxies for core mergers, culminating in sub-samples of 8 merging and 25 non-merging galaxy clusters. An additional sample of 12 galaxy clusters with known dumbbell components is procured using galaxy data from the NASA/IPAC Extragalactic Database (NED) to compare against more extreme environments. BAX clusters of each sample are stacked onto a common RA-DEC space to produce rotational profiles within the range of 0.0 − 2.5 r 200 . Merging stacks possess stronger core rotation at 0.5r 200 primarily contributed by a red galaxy sub-population from relaxing core mergers, this is alongside high rotational velocities from blue galaxy sub-populations, until, they mix and homogenise with the red sub-populations at ∼ r 200 , indicative of an infalling blue galaxy sub-population with interactive mixing between both sub-populations at r 200 . FLASH code is utilised to simulate the merger phase between two originally independent clusters and test the evolution of their rotational profiles. Comparisons with the dumbbell clusters leads to the inference that the peculiar core rotations of some dumbbell clusters are the result of the linear motions of core galaxies relaxing onto the potential during post second infall.

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The influence of the dynamic state of galaxy clusters on segregation phenomena and velocity dispersion profiles

Cited by 8 publications

References 49 publications

Ram pressure stripping of HI-rich galaxies infalling into massive clusters

Ram pressure stripping of HI-rich galaxies infalling into massive clusters

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

The rotational profiles of cluster galaxies

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