Luminous Quasars Do Not Live in the Most Overdense Regions of Galaxies at z\textasciitilde4. Uchiyama, H., Toshikawa, J., Kashikawa, N., Overzier, R., Chiang, Y., Tanaka, M., Niino, Y., Ishikawa, S., Onoue, M., Ichikawa, K., Akiyama, M., Coupon, J., Harikane, Y., Imanishi, M., Kodama, T., Komiyama, Y., Lee, C., Lin, Y., Miyazaki, S., Nagao, T., Nishizawa, A. J., Ono, Y., Ouchi, M., Strauss, M., & Wang, S. arXiv:1704.06050 [astro-ph], April, 2017. arXiv: 1704.06050![Luminous Quasars Do Not Live in the Most Overdense Regions of Galaxies at z\textasciitilde4 [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We present the cross-correlation between 151 luminous quasars (\$M_\{ {\textbackslash}mathrm\{UV\}\} {\textless} -26\$) and 179 protocluster candidates at \$z {\textbackslash}sim 3.8\$, extracted from the Wide imaging survey (\$ {\textbackslash}sim 121{\textasciitilde} \$deg\${\textasciicircum}2\$) performed with a part of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We find that only two out of 151 quasars reside in regions that are more overdense compared to the average field at \$ {\textgreater} 4 {\textbackslash}sigma \$. The distributions of the distance between quasars and the nearest protoclusters and the significance of the overdensity at the position of quasars are statistically identical to those found for \$g\$-dropout galaxies, suggesting that quasars tend to reside in almost the same environment as star-forming galaxies at this redshift. Using stacking analysis, we find that the average density of \$g\$-dropout galaxies around quasars is slightly higher than that around \$g\$-dropout galaxies on \$1.0 - 2.5\$ pMpc scales, while at \$ {\textless} 0.5\$ pMpc that around quasars tends to be lower. We also find that quasars with higher UV-luminosity or with more massive black holes tend to avoid the most overdense regions, and that the quasar near zone sizes are anti-correlated with overdensity. These findings are consistent with a scenario in which the luminous quasar at \$z {\textbackslash}sim4 \$ resides in structures that are less massive than those expected for the progenitors of today's rich clusters of galaxies, and possibly that luminous quasars may be suppressing star formation in their close vicinity.
@article{uchiyama_luminous_2017,
title = {Luminous {Quasars} {Do} {Not} {Live} in the {Most} {Overdense} {Regions} of {Galaxies} at z{\textasciitilde}4},
url = {http://arxiv.org/abs/1704.06050},
abstract = {We present the cross-correlation between 151 luminous quasars (\$M\_\{ {\textbackslash}mathrm\{UV\}\} {\textless} -26\$) and 179 protocluster candidates at \$z {\textbackslash}sim 3.8\$, extracted from the Wide imaging survey (\$ {\textbackslash}sim 121{\textasciitilde} \$deg\${\textasciicircum}2\$) performed with a part of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We find that only two out of 151 quasars reside in regions that are more overdense compared to the average field at \$ {\textgreater} 4 {\textbackslash}sigma \$. The distributions of the distance between quasars and the nearest protoclusters and the significance of the overdensity at the position of quasars are statistically identical to those found for \$g\$-dropout galaxies, suggesting that quasars tend to reside in almost the same environment as star-forming galaxies at this redshift. Using stacking analysis, we find that the average density of \$g\$-dropout galaxies around quasars is slightly higher than that around \$g\$-dropout galaxies on \$1.0 - 2.5\$ pMpc scales, while at \$ {\textless} 0.5\$ pMpc that around quasars tends to be lower. We also find that quasars with higher UV-luminosity or with more massive black holes tend to avoid the most overdense regions, and that the quasar near zone sizes are anti-correlated with overdensity. These findings are consistent with a scenario in which the luminous quasar at \$z {\textbackslash}sim4 \$ resides in structures that are less massive than those expected for the progenitors of today's rich clusters of galaxies, and possibly that luminous quasars may be suppressing star formation in their close vicinity.},
urldate = {2017-04-25},
journal = {arXiv:1704.06050 [astro-ph]},
author = {Uchiyama, Hisakazu and Toshikawa, Jun and Kashikawa, Nobunari and Overzier, Roderik and Chiang, Yi-Kuan and Tanaka, Masayuki and Niino, Yuu and Ishikawa, Shogo and Onoue, Masafusa and Ichikawa, Kohei and Akiyama, Masayuki and Coupon, Jean and Harikane, Yuichi and Imanishi, Masatoshi and Kodama, Tadayuki and Komiyama, Yutaka and Lee, Chien-Hsiu and Lin, Yen-Ting and Miyazaki, Satoshi and Nagao, Tohru and Nishizawa, Atushi J. and Ono, Yoshiaki and Ouchi, Masami and Strauss, Michael and Wang, Shiang-Yu},
month = apr,
year = {2017},
note = {arXiv: 1704.06050},
keywords = {Astrophysics - Astrophysics of Galaxies},
}
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J.","Ono, Y.","Ouchi, M.","Strauss, M.","Wang, S."],"bibdata":{"bibtype":"article","type":"article","title":"Luminous Quasars Do Not Live in the Most Overdense Regions of Galaxies at z\\textasciitilde4","url":"http://arxiv.org/abs/1704.06050","abstract":"We present the cross-correlation between 151 luminous quasars (\\$M_\\{ {\\textbackslash}mathrm\\{UV\\}\\} {\\textless} -26\\$) and 179 protocluster candidates at \\$z {\\textbackslash}sim 3.8\\$, extracted from the Wide imaging survey (\\$ {\\textbackslash}sim 121{\\textasciitilde} \\$deg\\${\\textasciicircum}2\\$) performed with a part of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We find that only two out of 151 quasars reside in regions that are more overdense compared to the average field at \\$ {\\textgreater} 4 {\\textbackslash}sigma \\$. The distributions of the distance between quasars and the nearest protoclusters and the significance of the overdensity at the position of quasars are statistically identical to those found for \\$g\\$-dropout galaxies, suggesting that quasars tend to reside in almost the same environment as star-forming galaxies at this redshift. Using stacking analysis, we find that the average density of \\$g\\$-dropout galaxies around quasars is slightly higher than that around \\$g\\$-dropout galaxies on \\$1.0 - 2.5\\$ pMpc scales, while at \\$ {\\textless} 0.5\\$ pMpc that around quasars tends to be lower. We also find that quasars with higher UV-luminosity or with more massive black holes tend to avoid the most overdense regions, and that the quasar near zone sizes are anti-correlated with overdensity. These findings are consistent with a scenario in which the luminous quasar at \\$z {\\textbackslash}sim4 \\$ resides in structures that are less massive than those expected for the progenitors of today's rich clusters of galaxies, and possibly that luminous quasars may be suppressing star formation in their close vicinity.","urldate":"2017-04-25","journal":"arXiv:1704.06050 [astro-ph]","author":[{"propositions":[],"lastnames":["Uchiyama"],"firstnames":["Hisakazu"],"suffixes":[]},{"propositions":[],"lastnames":["Toshikawa"],"firstnames":["Jun"],"suffixes":[]},{"propositions":[],"lastnames":["Kashikawa"],"firstnames":["Nobunari"],"suffixes":[]},{"propositions":[],"lastnames":["Overzier"],"firstnames":["Roderik"],"suffixes":[]},{"propositions":[],"lastnames":["Chiang"],"firstnames":["Yi-Kuan"],"suffixes":[]},{"propositions":[],"lastnames":["Tanaka"],"firstnames":["Masayuki"],"suffixes":[]},{"propositions":[],"lastnames":["Niino"],"firstnames":["Yuu"],"suffixes":[]},{"propositions":[],"lastnames":["Ishikawa"],"firstnames":["Shogo"],"suffixes":[]},{"propositions":[],"lastnames":["Onoue"],"firstnames":["Masafusa"],"suffixes":[]},{"propositions":[],"lastnames":["Ichikawa"],"firstnames":["Kohei"],"suffixes":[]},{"propositions":[],"lastnames":["Akiyama"],"firstnames":["Masayuki"],"suffixes":[]},{"propositions":[],"lastnames":["Coupon"],"firstnames":["Jean"],"suffixes":[]},{"propositions":[],"lastnames":["Harikane"],"firstnames":["Yuichi"],"suffixes":[]},{"propositions":[],"lastnames":["Imanishi"],"firstnames":["Masatoshi"],"suffixes":[]},{"propositions":[],"lastnames":["Kodama"],"firstnames":["Tadayuki"],"suffixes":[]},{"propositions":[],"lastnames":["Komiyama"],"firstnames":["Yutaka"],"suffixes":[]},{"propositions":[],"lastnames":["Lee"],"firstnames":["Chien-Hsiu"],"suffixes":[]},{"propositions":[],"lastnames":["Lin"],"firstnames":["Yen-Ting"],"suffixes":[]},{"propositions":[],"lastnames":["Miyazaki"],"firstnames":["Satoshi"],"suffixes":[]},{"propositions":[],"lastnames":["Nagao"],"firstnames":["Tohru"],"suffixes":[]},{"propositions":[],"lastnames":["Nishizawa"],"firstnames":["Atushi","J."],"suffixes":[]},{"propositions":[],"lastnames":["Ono"],"firstnames":["Yoshiaki"],"suffixes":[]},{"propositions":[],"lastnames":["Ouchi"],"firstnames":["Masami"],"suffixes":[]},{"propositions":[],"lastnames":["Strauss"],"firstnames":["Michael"],"suffixes":[]},{"propositions":[],"lastnames":["Wang"],"firstnames":["Shiang-Yu"],"suffixes":[]}],"month":"April","year":"2017","note":"arXiv: 1704.06050","keywords":"Astrophysics - Astrophysics of Galaxies","bibtex":"@article{uchiyama_luminous_2017,\n\ttitle = {Luminous {Quasars} {Do} {Not} {Live} in the {Most} {Overdense} {Regions} of {Galaxies} at z{\\textasciitilde}4},\n\turl = {http://arxiv.org/abs/1704.06050},\n\tabstract = {We present the cross-correlation between 151 luminous quasars (\\$M\\_\\{ {\\textbackslash}mathrm\\{UV\\}\\} {\\textless} -26\\$) and 179 protocluster candidates at \\$z {\\textbackslash}sim 3.8\\$, extracted from the Wide imaging survey (\\$ {\\textbackslash}sim 121{\\textasciitilde} \\$deg\\${\\textasciicircum}2\\$) performed with a part of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We find that only two out of 151 quasars reside in regions that are more overdense compared to the average field at \\$ {\\textgreater} 4 {\\textbackslash}sigma \\$. The distributions of the distance between quasars and the nearest protoclusters and the significance of the overdensity at the position of quasars are statistically identical to those found for \\$g\\$-dropout galaxies, suggesting that quasars tend to reside in almost the same environment as star-forming galaxies at this redshift. Using stacking analysis, we find that the average density of \\$g\\$-dropout galaxies around quasars is slightly higher than that around \\$g\\$-dropout galaxies on \\$1.0 - 2.5\\$ pMpc scales, while at \\$ {\\textless} 0.5\\$ pMpc that around quasars tends to be lower. We also find that quasars with higher UV-luminosity or with more massive black holes tend to avoid the most overdense regions, and that the quasar near zone sizes are anti-correlated with overdensity. These findings are consistent with a scenario in which the luminous quasar at \\$z {\\textbackslash}sim4 \\$ resides in structures that are less massive than those expected for the progenitors of today's rich clusters of galaxies, and possibly that luminous quasars may be suppressing star formation in their close vicinity.},\n\turldate = {2017-04-25},\n\tjournal = {arXiv:1704.06050 [astro-ph]},\n\tauthor = {Uchiyama, Hisakazu and Toshikawa, Jun and Kashikawa, Nobunari and Overzier, Roderik and Chiang, Yi-Kuan and Tanaka, Masayuki and Niino, Yuu and Ishikawa, Shogo and Onoue, Masafusa and Ichikawa, Kohei and Akiyama, Masayuki and Coupon, Jean and Harikane, Yuichi and Imanishi, Masatoshi and Kodama, Tadayuki and Komiyama, Yutaka and Lee, Chien-Hsiu and Lin, Yen-Ting and Miyazaki, Satoshi and Nagao, Tohru and Nishizawa, Atushi J. and Ono, Yoshiaki and Ouchi, Masami and Strauss, Michael and Wang, Shiang-Yu},\n\tmonth = apr,\n\tyear = {2017},\n\tnote = {arXiv: 1704.06050},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n","author_short":["Uchiyama, H.","Toshikawa, J.","Kashikawa, N.","Overzier, R.","Chiang, Y.","Tanaka, M.","Niino, Y.","Ishikawa, S.","Onoue, M.","Ichikawa, K.","Akiyama, M.","Coupon, J.","Harikane, Y.","Imanishi, M.","Kodama, T.","Komiyama, Y.","Lee, C.","Lin, Y.","Miyazaki, S.","Nagao, T.","Nishizawa, A. 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