@article{ando_systematic_2020,
	title = {A {Systematic} {Search} for {Galaxy} {Proto}-{Cluster} {Cores} at \$z{\textbackslash}sim 2\$},
	volume = {2002},
	url = {http://adsabs.harvard.edu/abs/2020arXiv200210511A},
	abstract = {A proto-cluster core is the most massive dark matter halo (DMH) in a given proto-cluster. To reveal the galaxy formation in core regions, we search for proto-cluster cores at \$z{\textbackslash}sim 2\$ in \${\textbackslash}sim 1.5{\textbackslash},
{\textbackslash}mathrm\{deg\}{\textasciicircum}\{2\}\$ of the COSMOS field. Using pairs of massive galaxies (\${\textbackslash}log(M\_\{*\}/M\_\{{\textbackslash}odot\}){\textbackslash}geq11\$) as tracers of cores, we find 75
candidate cores, among which 54{\textbackslash}\% are estimated to be real. A clustering analysis finds that these cores have an average DMH mass of
\$2.6\_\{-0.8\}{\textasciicircum}\{+0.9\}{\textbackslash}times 10{\textasciicircum}\{13\}{\textbackslash}, M\_\{{\textbackslash}odot\}\$, or \$4.0\_\{-1.5\}{\textasciicircum}\{+1.8\}{\textbackslash}, {\textbackslash}times 10{\textasciicircum}\{13\} M\_\{{\textbackslash}odot\}\$ after contamination correction. The extended Press-Schechter model shows that their descendant mass at \$z=0\$ is consistent with Fornax-like or Virgo-like clusters. Moreover, using the IllustrisTNG simulation, we confirm that pairs of massive galaxies are good tracers of DMHs massive enough to be regarded as proto-cluster cores. We then derive the stellar mass function (SMF) and the quiescent fraction for member galaxies of the 75 candidate cores. We find that the core galaxies have a more top-heavy SMF than field galaxies at the same redshift, showing an excess at \${\textbackslash}log(M\_\{*\}/M\_\{{\textbackslash}odot\}){\textbackslash}gtrsim 10.5\$. The quiescent fraction, \$0.17\_\{-0.04\}{\textasciicircum}\{+0.04\}\$ in the mass range \$9.0{\textbackslash}leq {\textbackslash}log(M\_\{*\}/M\_\{{\textbackslash}odot\}){\textbackslash}leq 11.0\$, is about three times higher than that of field counterparts, giving an environmental quenching efficiency of \$0.13\_\{-0.04\}{\textasciicircum}\{+0.04\}\$. These results suggest that stellar mass assembly and quenching are accelerated as early as at \$z{\textbackslash}sim 2\$ in proto-cluster cores.},
	urldate = {2020-02-28},
	journal = {arXiv e-prints},
	author = {Ando, Makoto and Shimasaku, Kazuhiro and Momose, Rieko},
	month = feb,
	year = {2020},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:2002.10511},
}

{"_id":"4ez3QHhxPbi6K9JqB","bibbaseid":"ando-shimasaku-momose-asystematicsearchforgalaxyprotoclustercoresatztextbackslashsim2-2020","author_short":["Ando, M.","Shimasaku, K.","Momose, R."],"bibdata":{"bibtype":"article","type":"article","title":"A Systematic Search for Galaxy Proto-Cluster Cores at \\$z{\\textbackslash}sim 2\\$","volume":"2002","url":"http://adsabs.harvard.edu/abs/2020arXiv200210511A","abstract":"A proto-cluster core is the most massive dark matter halo (DMH) in a given proto-cluster. To reveal the galaxy formation in core regions, we search for proto-cluster cores at \\$z{\\textbackslash}sim 2\\$ in \\${\\textbackslash}sim 1.5{\\textbackslash}, {\\textbackslash}mathrm\\{deg\\}{\\textasciicircum}\\{2\\}\\$ of the COSMOS field. Using pairs of massive galaxies (\\${\\textbackslash}log(M_\\{*\\}/M_\\{{\\textbackslash}odot\\}){\\textbackslash}geq11\\$) as tracers of cores, we find 75 candidate cores, among which 54\\textbackslash% are estimated to be real. A clustering analysis finds that these cores have an average DMH mass of \\$2.6_\\{-0.8\\}{\\textasciicircum}\\{+0.9\\}{\\textbackslash}times 10{\\textasciicircum}\\{13\\}{\\textbackslash}, M_\\{{\\textbackslash}odot\\}\\$, or \\$4.0_\\{-1.5\\}{\\textasciicircum}\\{+1.8\\}{\\textbackslash}, {\\textbackslash}times 10{\\textasciicircum}\\{13\\} M_\\{{\\textbackslash}odot\\}\\$ after contamination correction. The extended Press-Schechter model shows that their descendant mass at \\$z=0\\$ is consistent with Fornax-like or Virgo-like clusters. Moreover, using the IllustrisTNG simulation, we confirm that pairs of massive galaxies are good tracers of DMHs massive enough to be regarded as proto-cluster cores. We then derive the stellar mass function (SMF) and the quiescent fraction for member galaxies of the 75 candidate cores. We find that the core galaxies have a more top-heavy SMF than field galaxies at the same redshift, showing an excess at \\${\\textbackslash}log(M_\\{*\\}/M_\\{{\\textbackslash}odot\\}){\\textbackslash}gtrsim 10.5\\$. The quiescent fraction, \\$0.17_\\{-0.04\\}{\\textasciicircum}\\{+0.04\\}\\$ in the mass range \\$9.0{\\textbackslash}leq {\\textbackslash}log(M_\\{*\\}/M_\\{{\\textbackslash}odot\\}){\\textbackslash}leq 11.0\\$, is about three times higher than that of field counterparts, giving an environmental quenching efficiency of \\$0.13_\\{-0.04\\}{\\textasciicircum}\\{+0.04\\}\\$. These results suggest that stellar mass assembly and quenching are accelerated as early as at \\$z{\\textbackslash}sim 2\\$ in proto-cluster cores.","urldate":"2020-02-28","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Ando"],"firstnames":["Makoto"],"suffixes":[]},{"propositions":[],"lastnames":["Shimasaku"],"firstnames":["Kazuhiro"],"suffixes":[]},{"propositions":[],"lastnames":["Momose"],"firstnames":["Rieko"],"suffixes":[]}],"month":"February","year":"2020","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2002.10511","bibtex":"@article{ando_systematic_2020,\n\ttitle = {A {Systematic} {Search} for {Galaxy} {Proto}-{Cluster} {Cores} at \\$z{\\textbackslash}sim 2\\$},\n\tvolume = {2002},\n\turl = {http://adsabs.harvard.edu/abs/2020arXiv200210511A},\n\tabstract = {A proto-cluster core is the most massive dark matter halo (DMH) in a given proto-cluster. To reveal the galaxy formation in core regions, we search for proto-cluster cores at \\$z{\\textbackslash}sim 2\\$ in \\${\\textbackslash}sim 1.5{\\textbackslash},\n{\\textbackslash}mathrm\\{deg\\}{\\textasciicircum}\\{2\\}\\$ of the COSMOS field. Using pairs of massive galaxies (\\${\\textbackslash}log(M\\_\\{*\\}/M\\_\\{{\\textbackslash}odot\\}){\\textbackslash}geq11\\$) as tracers of cores, we find 75\ncandidate cores, among which 54{\\textbackslash}\\% are estimated to be real. A clustering analysis finds that these cores have an average DMH mass of\n\\$2.6\\_\\{-0.8\\}{\\textasciicircum}\\{+0.9\\}{\\textbackslash}times 10{\\textasciicircum}\\{13\\}{\\textbackslash}, M\\_\\{{\\textbackslash}odot\\}\\$, or \\$4.0\\_\\{-1.5\\}{\\textasciicircum}\\{+1.8\\}{\\textbackslash}, {\\textbackslash}times 10{\\textasciicircum}\\{13\\} M\\_\\{{\\textbackslash}odot\\}\\$ after contamination correction. The extended Press-Schechter model shows that their descendant mass at \\$z=0\\$ is consistent with Fornax-like or Virgo-like clusters. Moreover, using the IllustrisTNG simulation, we confirm that pairs of massive galaxies are good tracers of DMHs massive enough to be regarded as proto-cluster cores. We then derive the stellar mass function (SMF) and the quiescent fraction for member galaxies of the 75 candidate cores. We find that the core galaxies have a more top-heavy SMF than field galaxies at the same redshift, showing an excess at \\${\\textbackslash}log(M\\_\\{*\\}/M\\_\\{{\\textbackslash}odot\\}){\\textbackslash}gtrsim 10.5\\$. The quiescent fraction, \\$0.17\\_\\{-0.04\\}{\\textasciicircum}\\{+0.04\\}\\$ in the mass range \\$9.0{\\textbackslash}leq {\\textbackslash}log(M\\_\\{*\\}/M\\_\\{{\\textbackslash}odot\\}){\\textbackslash}leq 11.0\\$, is about three times higher than that of field counterparts, giving an environmental quenching efficiency of \\$0.13\\_\\{-0.04\\}{\\textasciicircum}\\{+0.04\\}\\$. These results suggest that stellar mass assembly and quenching are accelerated as early as at \\$z{\\textbackslash}sim 2\\$ in proto-cluster cores.},\n\turldate = {2020-02-28},\n\tjournal = {arXiv e-prints},\n\tauthor = {Ando, Makoto and Shimasaku, Kazuhiro and Momose, Rieko},\n\tmonth = feb,\n\tyear = {2020},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:2002.10511},\n}\n\n","author_short":["Ando, M.","Shimasaku, K.","Momose, R."],"key":"ando_systematic_2020","id":"ando_systematic_2020","bibbaseid":"ando-shimasaku-momose-asystematicsearchforgalaxyprotoclustercoresatztextbackslashsim2-2020","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2020arXiv200210511A"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["systematic","search","galaxy","proto","cluster","cores","textbackslash","sim","ando","shimasaku","momose"],"title":"A Systematic Search for Galaxy Proto-Cluster Cores at \\$z{\\textbackslash}sim 2\\$","year":2020}