@article{mostoghiu_three_2021,
	title = {The {Three} {Hundred} {Project}: {The} stellar angular momentum evolution of cluster galaxies},
	volume = {2105},
	shorttitle = {The {Three} {Hundred} {Project}},
	url = {http://adsabs.harvard.edu/abs/2021arXiv210501676M},
	abstract = {Using 324 numerically modelled galaxy clusters as provided by THE THREE 
HUNDRED project, we study the evolution of the kinematic properties of
the stellar component of haloes on first infall. We select objects with
M\$\_\{{\textbackslash}textrm\{star\}\}{\textgreater}5{\textbackslash}times10{\textasciicircum}\{10\} h{\textasciicircum}\{-1\}M\_\{{\textbackslash}odot\}\$ within \$3R\_\{200\}\$
of the main cluster halo at \$z=0\$ and follow their progenitors. We find
that although haloes are stripped of their dark matter and gas after
entering the main cluster halo, there is practically no change in their
stellar kinematics. For the vast majority of our `galaxies' -- defined
as the central stellar component found within the haloes that form our
sample -- their kinematic properties, as described by the fraction of
ordered rotation, and their position in the specific stellar angular
momentum\$-\$stellar mass plane \$j\_\{{\textbackslash}rm star\}\$ -- M\$\_\{{\textbackslash}rm star\}\$, are
mostly unchanged by the influence of the central host cluster. However,
for a small number of infalling galaxies, stellar mergers and encounters
with remnant stellar cores close to the centre of the main cluster,
particularly during pericentre passage, are able to spin-up their
stellar component by \$z=0\$.},
	urldate = {2021-05-11},
	journal = {arXiv e-prints},
	author = {Mostoghiu, Robert and Knebe, Alexander and Pearce, Frazer R. and Power, Chris and Lagos, Claudia D. P. and Cui, Weiguang and Borgani, Stefano and Dolag, Klaus and Murante, Giuseppe and Yepes, Gustavo},
	month = may,
	year = {2021},
	keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
	pages = {arXiv:2105.01676},
}

{"_id":"ojPYeb6FWoRc4qWPh","bibbaseid":"mostoghiu-knebe-pearce-power-lagos-cui-borgani-dolag-etal-thethreehundredprojectthestellarangularmomentumevolutionofclustergalaxies-2021","author_short":["Mostoghiu, R.","Knebe, A.","Pearce, F. R.","Power, C.","Lagos, C. D. P.","Cui, W.","Borgani, S.","Dolag, K.","Murante, G.","Yepes, G."],"bibdata":{"bibtype":"article","type":"article","title":"The Three Hundred Project: The stellar angular momentum evolution of cluster galaxies","volume":"2105","shorttitle":"The Three Hundred Project","url":"http://adsabs.harvard.edu/abs/2021arXiv210501676M","abstract":"Using 324 numerically modelled galaxy clusters as provided by THE THREE HUNDRED project, we study the evolution of the kinematic properties of the stellar component of haloes on first infall. We select objects with M\\$_\\{{\\textbackslash}textrm\\{star\\}\\}{\\textgreater}5{\\textbackslash}times10{\\textasciicircum}\\{10\\} h{\\textasciicircum}\\{-1\\}M_\\{{\\textbackslash}odot\\}\\$ within \\$3R_\\{200\\}\\$ of the main cluster halo at \\$z=0\\$ and follow their progenitors. We find that although haloes are stripped of their dark matter and gas after entering the main cluster halo, there is practically no change in their stellar kinematics. For the vast majority of our `galaxies' – defined as the central stellar component found within the haloes that form our sample – their kinematic properties, as described by the fraction of ordered rotation, and their position in the specific stellar angular momentum\\$-\\$stellar mass plane \\$j_\\{{\\textbackslash}rm star\\}\\$ – M\\$_\\{{\\textbackslash}rm star\\}\\$, are mostly unchanged by the influence of the central host cluster. However, for a small number of infalling galaxies, stellar mergers and encounters with remnant stellar cores close to the centre of the main cluster, particularly during pericentre passage, are able to spin-up their stellar component by \\$z=0\\$.","urldate":"2021-05-11","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Mostoghiu"],"firstnames":["Robert"],"suffixes":[]},{"propositions":[],"lastnames":["Knebe"],"firstnames":["Alexander"],"suffixes":[]},{"propositions":[],"lastnames":["Pearce"],"firstnames":["Frazer","R."],"suffixes":[]},{"propositions":[],"lastnames":["Power"],"firstnames":["Chris"],"suffixes":[]},{"propositions":[],"lastnames":["Lagos"],"firstnames":["Claudia","D.","P."],"suffixes":[]},{"propositions":[],"lastnames":["Cui"],"firstnames":["Weiguang"],"suffixes":[]},{"propositions":[],"lastnames":["Borgani"],"firstnames":["Stefano"],"suffixes":[]},{"propositions":[],"lastnames":["Dolag"],"firstnames":["Klaus"],"suffixes":[]},{"propositions":[],"lastnames":["Murante"],"firstnames":["Giuseppe"],"suffixes":[]},{"propositions":[],"lastnames":["Yepes"],"firstnames":["Gustavo"],"suffixes":[]}],"month":"May","year":"2021","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics","pages":"arXiv:2105.01676","bibtex":"@article{mostoghiu_three_2021,\n\ttitle = {The {Three} {Hundred} {Project}: {The} stellar angular momentum evolution of cluster galaxies},\n\tvolume = {2105},\n\tshorttitle = {The {Three} {Hundred} {Project}},\n\turl = {http://adsabs.harvard.edu/abs/2021arXiv210501676M},\n\tabstract = {Using 324 numerically modelled galaxy clusters as provided by THE THREE \nHUNDRED project, we study the evolution of the kinematic properties of\nthe stellar component of haloes on first infall. We select objects with\nM\\$\\_\\{{\\textbackslash}textrm\\{star\\}\\}{\\textgreater}5{\\textbackslash}times10{\\textasciicircum}\\{10\\} h{\\textasciicircum}\\{-1\\}M\\_\\{{\\textbackslash}odot\\}\\$ within \\$3R\\_\\{200\\}\\$\nof the main cluster halo at \\$z=0\\$ and follow their progenitors. We find\nthat although haloes are stripped of their dark matter and gas after\nentering the main cluster halo, there is practically no change in their\nstellar kinematics. For the vast majority of our `galaxies' -- defined\nas the central stellar component found within the haloes that form our\nsample -- their kinematic properties, as described by the fraction of\nordered rotation, and their position in the specific stellar angular\nmomentum\\$-\\$stellar mass plane \\$j\\_\\{{\\textbackslash}rm star\\}\\$ -- M\\$\\_\\{{\\textbackslash}rm star\\}\\$, are\nmostly unchanged by the influence of the central host cluster. However,\nfor a small number of infalling galaxies, stellar mergers and encounters\nwith remnant stellar cores close to the centre of the main cluster,\nparticularly during pericentre passage, are able to spin-up their\nstellar component by \\$z=0\\$.},\n\turldate = {2021-05-11},\n\tjournal = {arXiv e-prints},\n\tauthor = {Mostoghiu, Robert and Knebe, Alexander and Pearce, Frazer R. and Power, Chris and Lagos, Claudia D. P. and Cui, Weiguang and Borgani, Stefano and Dolag, Klaus and Murante, Giuseppe and Yepes, Gustavo},\n\tmonth = may,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},\n\tpages = {arXiv:2105.01676},\n}\n\n","author_short":["Mostoghiu, R.","Knebe, A.","Pearce, F. R.","Power, C.","Lagos, C. D. P.","Cui, W.","Borgani, S.","Dolag, K.","Murante, G.","Yepes, G."],"key":"mostoghiu_three_2021","id":"mostoghiu_three_2021","bibbaseid":"mostoghiu-knebe-pearce-power-lagos-cui-borgani-dolag-etal-thethreehundredprojectthestellarangularmomentumevolutionofclustergalaxies-2021","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2021arXiv210501676M"},"keyword":["Astrophysics - Astrophysics of Galaxies","Astrophysics - Cosmology and Nongalactic Astrophysics"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies","astrophysics - cosmology and nongalactic astrophysics"],"search_terms":["three","hundred","project","stellar","angular","momentum","evolution","cluster","galaxies","mostoghiu","knebe","pearce","power","lagos","cui","borgani","dolag","murante","yepes"],"title":"The Three Hundred Project: The stellar angular momentum evolution of cluster galaxies","year":2021}