@article{ito_uv_2020,
	title = {The {UV} {Luminosity} {Function} of {Protocluster} {Galaxies} at \$z{\textbackslash}sim4\$: the {Bright}-end {Excess} and the {Enhanced} {Star} {Formation} {Rate} {Density}},
	volume = {2007},
	shorttitle = {The {UV} {Luminosity} {Function} of {Protocluster} {Galaxies} at \$z{\textbackslash}sim4\$},
	url = {http://adsabs.harvard.edu/abs/2020arXiv200702961I},
	abstract = {We report the rest-frame ultraviolet luminosity function of \$g\$-dropout 
galaxies in 177 protocluster candidates (PC UVLF) at \$z{\textbackslash}sim4\$ selected
in the Hyper Suprime-Cam Subaru Strategic Program. Comparing with the
UVLF of field galaxies at the same redshift, we find that the PC UVLF
shows a significant excess towards the bright-end. This excess can not
be explained by the contribution of only active galactic nuclei, and we
also find that this is more significant in higher dense regions.
Assuming that all protocluster members are located on the star formation
main sequence, the PC UVLF can be converted into a stellar mass
function. Consequently, our protocluster members are inferred to have a
2.8 times more massive characteristic stellar mass than that of the
field Lyman break galaxies at the same redshift. This study, for the
first time, clearly shows that the enhancement in star formation or
stellar mass in overdense regions can generally be seen as early as at
\$z{\textbackslash}sim4\$. We also estimate the star formation rate density (SFRD) in
protocluster regions as \${\textbackslash}simeq 6-20{\textbackslash}\%\$ of the cosmic SFRD, based on the
measured PC UVLF after correcting for the selection incompleteness in
our protocluster sample. This high value suggests that protoclusters
make a non-negligible contribution to the cosmic SFRD at \$z{\textbackslash}sim4\$, as
previously suggested by simulations. Our results suggest that
protoclusters are essential components for the galaxy evolution at
\$z{\textbackslash}sim4\$.},
	urldate = {2020-07-09},
	journal = {arXiv e-prints},
	author = {Ito, Kei and Kashikawa, Nobunari and Toshikawa, Jun and Overzier, Roderik and Kubo, Mariko and Uchiyama, Hisakazu and Liang, Yongming and Onoue, Masafusa and Tanaka, Masayuki and Komiyama, Yutaka and Lee, Chien-Hsiu and Lin, Yen-Ting and Marinello, Murilo and Martin, Crystal L. and Shibuya, Takatoshi},
	month = jul,
	year = {2020},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:2007.02961},
}

{"_id":"3nwxvqMZLkHpY7jhk","bibbaseid":"ito-kashikawa-toshikawa-overzier-kubo-uchiyama-liang-onoue-etal-theuvluminosityfunctionofprotoclustergalaxiesatztextbackslashsim4thebrightendexcessandtheenhancedstarformationratedensity-2020","author_short":["Ito, K.","Kashikawa, N.","Toshikawa, J.","Overzier, R.","Kubo, M.","Uchiyama, H.","Liang, Y.","Onoue, M.","Tanaka, M.","Komiyama, Y.","Lee, C.","Lin, Y.","Marinello, M.","Martin, C. L.","Shibuya, T."],"bibdata":{"bibtype":"article","type":"article","title":"The UV Luminosity Function of Protocluster Galaxies at \\$z{\\textbackslash}sim4\\$: the Bright-end Excess and the Enhanced Star Formation Rate Density","volume":"2007","shorttitle":"The UV Luminosity Function of Protocluster Galaxies at \\$z{\\textbackslash}sim4\\$","url":"http://adsabs.harvard.edu/abs/2020arXiv200702961I","abstract":"We report the rest-frame ultraviolet luminosity function of \\$g\\$-dropout galaxies in 177 protocluster candidates (PC UVLF) at \\$z{\\textbackslash}sim4\\$ selected in the Hyper Suprime-Cam Subaru Strategic Program. Comparing with the UVLF of field galaxies at the same redshift, we find that the PC UVLF shows a significant excess towards the bright-end. This excess can not be explained by the contribution of only active galactic nuclei, and we also find that this is more significant in higher dense regions. Assuming that all protocluster members are located on the star formation main sequence, the PC UVLF can be converted into a stellar mass function. Consequently, our protocluster members are inferred to have a 2.8 times more massive characteristic stellar mass than that of the field Lyman break galaxies at the same redshift. This study, for the first time, clearly shows that the enhancement in star formation or stellar mass in overdense regions can generally be seen as early as at \\$z{\\textbackslash}sim4\\$. We also estimate the star formation rate density (SFRD) in protocluster regions as \\${\\textbackslash}simeq 6-20{\\textbackslash}%\\$ of the cosmic SFRD, based on the measured PC UVLF after correcting for the selection incompleteness in our protocluster sample. This high value suggests that protoclusters make a non-negligible contribution to the cosmic SFRD at \\$z{\\textbackslash}sim4\\$, as previously suggested by simulations. Our results suggest that protoclusters are essential components for the galaxy evolution at \\$z{\\textbackslash}sim4\\$.","urldate":"2020-07-09","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Ito"],"firstnames":["Kei"],"suffixes":[]},{"propositions":[],"lastnames":["Kashikawa"],"firstnames":["Nobunari"],"suffixes":[]},{"propositions":[],"lastnames":["Toshikawa"],"firstnames":["Jun"],"suffixes":[]},{"propositions":[],"lastnames":["Overzier"],"firstnames":["Roderik"],"suffixes":[]},{"propositions":[],"lastnames":["Kubo"],"firstnames":["Mariko"],"suffixes":[]},{"propositions":[],"lastnames":["Uchiyama"],"firstnames":["Hisakazu"],"suffixes":[]},{"propositions":[],"lastnames":["Liang"],"firstnames":["Yongming"],"suffixes":[]},{"propositions":[],"lastnames":["Onoue"],"firstnames":["Masafusa"],"suffixes":[]},{"propositions":[],"lastnames":["Tanaka"],"firstnames":["Masayuki"],"suffixes":[]},{"propositions":[],"lastnames":["Komiyama"],"firstnames":["Yutaka"],"suffixes":[]},{"propositions":[],"lastnames":["Lee"],"firstnames":["Chien-Hsiu"],"suffixes":[]},{"propositions":[],"lastnames":["Lin"],"firstnames":["Yen-Ting"],"suffixes":[]},{"propositions":[],"lastnames":["Marinello"],"firstnames":["Murilo"],"suffixes":[]},{"propositions":[],"lastnames":["Martin"],"firstnames":["Crystal","L."],"suffixes":[]},{"propositions":[],"lastnames":["Shibuya"],"firstnames":["Takatoshi"],"suffixes":[]}],"month":"July","year":"2020","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2007.02961","bibtex":"@article{ito_uv_2020,\n\ttitle = {The {UV} {Luminosity} {Function} of {Protocluster} {Galaxies} at \\$z{\\textbackslash}sim4\\$: the {Bright}-end {Excess} and the {Enhanced} {Star} {Formation} {Rate} {Density}},\n\tvolume = {2007},\n\tshorttitle = {The {UV} {Luminosity} {Function} of {Protocluster} {Galaxies} at \\$z{\\textbackslash}sim4\\$},\n\turl = {http://adsabs.harvard.edu/abs/2020arXiv200702961I},\n\tabstract = {We report the rest-frame ultraviolet luminosity function of \\$g\\$-dropout \ngalaxies in 177 protocluster candidates (PC UVLF) at \\$z{\\textbackslash}sim4\\$ selected\nin the Hyper Suprime-Cam Subaru Strategic Program. Comparing with the\nUVLF of field galaxies at the same redshift, we find that the PC UVLF\nshows a significant excess towards the bright-end. This excess can not\nbe explained by the contribution of only active galactic nuclei, and we\nalso find that this is more significant in higher dense regions.\nAssuming that all protocluster members are located on the star formation\nmain sequence, the PC UVLF can be converted into a stellar mass\nfunction. Consequently, our protocluster members are inferred to have a\n2.8 times more massive characteristic stellar mass than that of the\nfield Lyman break galaxies at the same redshift. This study, for the\nfirst time, clearly shows that the enhancement in star formation or\nstellar mass in overdense regions can generally be seen as early as at\n\\$z{\\textbackslash}sim4\\$. We also estimate the star formation rate density (SFRD) in\nprotocluster regions as \\${\\textbackslash}simeq 6-20{\\textbackslash}\\%\\$ of the cosmic SFRD, based on the\nmeasured PC UVLF after correcting for the selection incompleteness in\nour protocluster sample. This high value suggests that protoclusters\nmake a non-negligible contribution to the cosmic SFRD at \\$z{\\textbackslash}sim4\\$, as\npreviously suggested by simulations. Our results suggest that\nprotoclusters are essential components for the galaxy evolution at\n\\$z{\\textbackslash}sim4\\$.},\n\turldate = {2020-07-09},\n\tjournal = {arXiv e-prints},\n\tauthor = {Ito, Kei and Kashikawa, Nobunari and Toshikawa, Jun and Overzier, Roderik and Kubo, Mariko and Uchiyama, Hisakazu and Liang, Yongming and Onoue, Masafusa and Tanaka, Masayuki and Komiyama, Yutaka and Lee, Chien-Hsiu and Lin, Yen-Ting and Marinello, Murilo and Martin, Crystal L. and Shibuya, Takatoshi},\n\tmonth = jul,\n\tyear = {2020},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:2007.02961},\n}\n\n","author_short":["Ito, K.","Kashikawa, N.","Toshikawa, J.","Overzier, R.","Kubo, M.","Uchiyama, H.","Liang, Y.","Onoue, M.","Tanaka, M.","Komiyama, Y.","Lee, C.","Lin, Y.","Marinello, M.","Martin, C. L.","Shibuya, T."],"key":"ito_uv_2020","id":"ito_uv_2020","bibbaseid":"ito-kashikawa-toshikawa-overzier-kubo-uchiyama-liang-onoue-etal-theuvluminosityfunctionofprotoclustergalaxiesatztextbackslashsim4thebrightendexcessandtheenhancedstarformationratedensity-2020","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2020arXiv200702961I"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["luminosity","function","protocluster","galaxies","textbackslash","sim4","bright","end","excess","enhanced","star","formation","rate","density","ito","kashikawa","toshikawa","overzier","kubo","uchiyama","liang","onoue","tanaka","komiyama","lee","lin","marinello","martin","shibuya"],"title":"The UV Luminosity Function of Protocluster Galaxies at \\$z{\\textbackslash}sim4\\$: the Bright-end Excess and the Enhanced Star Formation Rate Density","year":2020}