The Rotational Profiles of Cluster Galaxies. (arXiv:1910.03453v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bilton_L/0/1/0/all/0/1">Lawrence E. Bilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hunt_M/0/1/0/all/0/1">Matthew Hunt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pimbblet_K/0/1/0/all/0/1">Kevin A. Pimbblet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roediger_E/0/1/0/all/0/1">Elke Roediger</a>
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 $lesssim 0.5 r_{200}$
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
$sim r_{200}$, indicative of an infalling blue galaxy sub-population with
interactive mixing between both sub-populations at $gtrsim r_{200}$. 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.
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 $lesssim 0.5 r_{200}$
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
$sim r_{200}$, indicative of an infalling blue galaxy sub-population with
interactive mixing between both sub-populations at $gtrsim r_{200}$. 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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