The rotational profiles of cluster galaxies

Bilton, Lawrence E.; Hunt, Matthew P.; Pimbblet, Kevin A.; Röediger, E.

doi:10.1093/mnras/stz2927

Cited by 4 publications

(11 citation statements)

References 99 publications

(108 reference statements)

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“…We briefly outline the methods involved in the procurement and handling of the data used in order to conduct the aims of this work, which follows the same procedures-as well as providing the same cluster sample-used in Bilton et al (2019). This process involves utilising the X-ray Galaxy Clusters Database (BAX; Sadat et al 2004) to collate a list of X-ray clusters that is constrained through parameters defined by the authors.…”

Section: The Datamentioning

confidence: 99%

“…Where the value of is computed from the frequency, MC , in which the condition Δ obs < Δ MC is met to give = MC / MC . This results in two sub-samples of clusters, that are originally defined within Bilton et al (2019), that represent our merging and non-merging dynamical states that hold 8 and 25 clusters respectively. These clusters and their basic properties, including their Δ-test -values, can be found categorised by their dynamical states within Table 1.…”

Section: Delineating Between Merging and Non-merging Galaxy Clustersmentioning

confidence: 99%

“…Indeed, any angular momentum possessed within a galaxy cluster should influence the average motion of the galaxy cluster membership via these very dynamics, which would be imprinted onto the radial velocities of the individual cluster galaxies in -space. Thus, following the combined methodologies detailed within Manolopoulou & Plionis (2017) and Bilton et al (2019), we determine the relative rotational profiles of our aforementioned cluster galaxy sub-populations from the 2D plane of sky through the employment of a geometric 'perspective rotation' technique (Feast et al 1961).…”

Section: Cluster Galaxy Agn Rotational Profilesmentioning

confidence: 99%

“…Tests for determining the degree of sub-structuring, such as that of Dressler & Shectman (1988), can be used as proxies for delineating between 'merging' and 'non-merging' cluster environments. Analysing the cluster galaxy kinematics of these opposing cluster dynamical states via velocity dispersion profiles (VDPs) and rotational profiles can provide an insight into how cluster galaxies, and their sub-populations, respond kinematically to their environment as a function of radius (Hou et al 2009(Hou et al , 2012Bilton & Pimbblet 2018;Bilton et al 2019;Morell et al 2020). In addition, VDPs themselves can independently act as proxies for determining a merging environment if they depict a rising profile as one increases the clustocentric radius within the virial regions, vice versa for nonmerging environments (see Menci & Fusco-Femiano 1996;Hou et al 2009;Bilton & Pimbblet 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Within this work we seek to test the kinematic response of AGN-hosting cluster galaxies between the aforesaid two galaxy cluster dynamical states via VDPs, which are determined utilising a weighted Gaussian smoothing kernel as outlined by Hou et al (2009), and via rotational profiles based upon the work by Manolopoulou & Plionis (2017) and expanded on in Bilton et al (2019). Thereby allowing for the exploration into whether or not the AGN-hosting cluster galaxy kinematics provide results that correspond to prior studies; AGN activity is predominantly found in infalling galaxies while being encompassed by a merging cluster environment.…”

Section: Introductionmentioning

confidence: 99%

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The impact of disturbed galaxy clusters on the kinematics of active galactic nuclei

Bilton

Pimbblet

Gordon

2020

Monthly Notices of the Royal Astronomical Society

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We produce a kinematic analysis of AGN-hosting cluster galaxies from a sample 33 galaxy clusters selected using the X-ray Clusters Database (BAX) and populated with galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8). The 33 galaxy clusters are delimited by their relative intensity of member galaxy substructuring as a proxy to core merging to derive two smaller sub-samples of 8 dynamically active (merging) and 25 dynamically relaxed (non-merging) states. The AGN were selected for each cluster sub-sample by employing the WHAN diagram to the strict criteria of log10([N ii]/Hα) ≥ −0.32 and EWHα ≥ 6Å, providing pools of 70 merging and 225 non-merging AGN sub-populations. By co-adding the clusters to their respective dynamical states to improve the signal-to-noise of our AGN sub-populations we find that merging galaxy clusters on average host kinematically active AGN between 0-1.5 r200 as r200 → 0, where their velocity dispersion profile (VDP) presents a significant deviation from the non-AGN sub-population VDP by ≳ 3σ. This result is indicative that the AGN-hosting cluster galaxies have recently coalesced onto a common potential. Further analysis of the composite distributions illustrate non-merging AGN-hosting sub-populations have, on average, already been accreted and predominantly lie within backsplash regions of the projected phase-space. This suggests merging cluster dynamical states hold relatively younger AGN sub-populations kinematically compared with those found in non-merging cluster dynamical states.

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Section: The Datamentioning

confidence: 99%

Section: Delineating Between Merging and Non-merging Galaxy Clustersmentioning

confidence: 99%

Section: Cluster Galaxy Agn Rotational Profilesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The impact of disturbed galaxy clusters on the kinematics of active galactic nuclei

Bilton

Pimbblet

Gordon

2020

Monthly Notices of the Royal Astronomical Society

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The mass function dependence on the dynamical state of dark matter haloes

Seppi

Comparat

Nandra

et al. 2021

A&A

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Context. Galaxy clusters are luminous tracers of the most massive dark matter haloes in the Universe. To use them as a cosmological probe, a detailed description of the properties of dark matter haloes is required. Aims. We characterize how the dynamical state of haloes impacts the dark matter halo mass function at the high-mass end (i.e., for haloes hosting clusters of galaxies). Methods. We used the dark matter-only MultiDark suite of simulations and the high-mass objects M > 2.7 × 1013 M⊙ h−1 therein. We measured the mean relations of concentration, offset, and spin as a function of dark matter halo mass and redshift. We investigated the distributions around the mean relations. We measured the dark matter halo mass function as a function of offset, spin, and redshift. We formulated a generalized mass function framework that accounts for the dynamical state of the dark matter haloes. Results. We confirm the recent discovery of the concentration upturn at high masses and provide a model that predicts the concentration for different values of mass and redshift with one single equation. We model the distributions around the mean values of concentration, offset, and spin with modified Schechter functions. We find that the concentration of low-mass haloes shows a faster redshift evolution compared to high-mass haloes, especially in the high-concentration regime. We find that the offset parameter is systematically smaller at low redshift, in agreement with the relaxation of structures at recent times. The peak of its distribution shifts by a factor of ∼1.5 from z = 1.4 to z = 0. The individual models are combined into a comprehensive mass function model, which predicts the mass function as a function of spin and offset. Our model recovers the fiducial mass function with ∼3% accuracy at redshift 0 and accounts for redshift evolution up to z ∼ 1.5. Results. This new approach accounts for the dynamical state of the halo when measuring the halo mass function. It offers a connection with dynamical selection effects in galaxy cluster observations. This is key toward precision cosmology using cluster counts as a probe.

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The effect of cluster dynamical state on ram-pressure stripping

Lourenço,

Jaffé,

Vulcani

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Theoretical and observational studies have suggested that ram-pressure stripping by the intracluster medium can be enhanced during cluster interactions, boosting the formation of the ”jellyfish” galaxies. In this work, we study the incidence of galaxies undergoing ram-pressure stripping in 52 clusters of different dynamical states. We use optical data from the WINGS/OmegaWINGS surveys and archival X-ray data to characterise the dynamical state of our cluster sample, applying eight different proxies. We then compute the number of ram-pressure stripping candidates relative to the infalling population of blue late-type galaxies within a fixed circular aperture in each cluster. We find no clear correlation between the fractions of ram-pressure stripping candidates and the different cluster dynamical state proxies considered. These fractions also show no apparent correlation with cluster mass. To construct a dynamical state classification closer to a merging ”sequence”, we perform a visual classification of the dynamical states of the clusters, combining information available in optical, X-ray, and radio wavelengths. We find a mild increase in the RPS fraction in interacting clusters with respect to all other classes (including post-mergers). This mild enhancement could hint at a short-lived enhanced ram-pressure stripping in ongoing cluster mergers. However, our results are not statistically significant due to the low galaxy numbers. We note this is the first homogeneous attempt to quantify the effect of cluster dynamical state on ram-pressure stripping using a large cluster sample, but even larger (especially wider) multi-wavelength surveys are needed to confirm the results.

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The rotational profiles of cluster galaxies

Cited by 4 publications

References 99 publications

The impact of disturbed galaxy clusters on the kinematics of active galactic nuclei

The impact of disturbed galaxy clusters on the kinematics of active galactic nuclei

The mass function dependence on the dynamical state of dark matter haloes

The effect of cluster dynamical state on ram-pressure stripping

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