Faint Quasars Live in the Same Number Density Environments as Lyman Break Galaxies at z \textasciitilde 4

Faint Quasars Live in the Same Number Density Environments as Lyman Break Galaxies at z \textasciitilde 4. Uchiyama, H., Akiyama, M., Toshikawa, J., Kashikawa, N., Overzier, R., Nagao, T., Ichikawa, K., Marinello, M., Imanishi, M., Tanaka, M., Matsuoka, Y., Komiyama, Y., Ishikawa, S., Onoue, M., Kubo, M., Harikane, Y., Ito, K., Namiki, S., & Liang, Y. arXiv e-prints, 2011:arXiv:2011.10194, November, 2020.
$Faint Quasars Live in the Same Number Density Environments as Lyman Break Galaxies at z \textasciitilde 4 [link]$ Paper abstract bibtex

Characterizing high-z quasar environments is key to understanding the co-evolution of quasars and the surrounding galaxies. To restrict their global picture, we statistically examine the g-dropout galaxy overdensity distribution around 570 faint quasar candidates at z \textasciitilde 4, based on the Hyper Suprime-Cam Subaru Strategic Program survey. We compare the overdensity significances of g-dropout galaxies around the quasars with those around g-dropout galaxies, and find no significant difference between their distributions. A total of 4 (22) out of the 570 faint quasars, 0.7_\-0.4\\textasciicircum\+0.4\ (3.9_\-0.8\\textasciicircum\+0.8\) %, are found to be associated with the \textgreater 4 sigma overdense regions within an angular separation of 1.8 (3.0) arcmin, which is the typical size of protoclusters at this epoch. This is similar to the fraction of g-dropout galaxies associated with the \textgreater 4 sigma overdense regions. This result is consistent with our previous work that 1.3_\-0.9\\textasciicircum\+0.9\ % and 2.0_\-1.1\\textasciicircum\+1.1\ % of luminous quasars detected in the Sloan Digital Sky Survey exist in the \textgreater 4 sigma overdense regions within 1.8 and 3.0 arcmin separations, respectively. Therefore, we suggest that the galaxy number densities around quasars are independent of their luminosity, and most quasars do not preferentially appear in the richest protocluster regions at z \textasciitilde 4. The lack of an apparent positive correlation between the quasars and the protoclusters implies that: i) the gas-rich major merger rate is relatively low in the protocluster regions, ii) most high-z quasars may appear through secular processes, or iii) some dust-obscured quasars exist in the protocluster regions.

@article{uchiyama_faint_2020,
	title = {Faint {Quasars} {Live} in the {Same} {Number} {Density} {Environments} as {Lyman} {Break} {Galaxies} at z {\textasciitilde} 4},
	volume = {2011},
	url = {http://adsabs.harvard.edu/abs/2020arXiv201110194U},
	abstract = {Characterizing high-z quasar environments is key to understanding the 
co-evolution of quasars and the surrounding galaxies. To restrict their
global picture, we statistically examine the g-dropout galaxy
overdensity distribution around 570 faint quasar candidates at z {\textasciitilde} 4,
based on the Hyper Suprime-Cam Subaru Strategic Program survey. We
compare the overdensity significances of g-dropout galaxies around the
quasars with those around g-dropout galaxies, and find no significant
difference between their distributions. A total of 4 (22) out of the 570
faint quasars, 0.7\_\{-0.4\}{\textasciicircum}\{+0.4\} (3.9\_\{-0.8\}{\textasciicircum}\{+0.8\}) \%, are found to be
associated with the {\textgreater} 4 sigma overdense regions within an angular
separation of 1.8 (3.0) arcmin, which is the typical size of
protoclusters at this epoch. This is similar to the fraction of
g-dropout galaxies associated with the {\textgreater} 4 sigma overdense regions.
This result is consistent with our previous work that 1.3\_\{-0.9\}{\textasciicircum}\{+0.9\}
\% and 2.0\_\{-1.1\}{\textasciicircum}\{+1.1\} \% of luminous quasars detected in the Sloan
Digital Sky Survey exist in the {\textgreater} 4 sigma overdense regions within
1.8 and 3.0 arcmin separations, respectively. Therefore, we suggest that
the galaxy number densities around quasars are independent of their
luminosity, and most quasars do not preferentially appear in the richest
protocluster regions at z {\textasciitilde} 4. The lack of an apparent positive
correlation between the quasars and the protoclusters implies that: i)
the gas-rich major merger rate is relatively low in the protocluster
regions, ii) most high-z quasars may appear through secular processes,
or iii) some dust-obscured quasars exist in the protocluster regions.},
	urldate = {2020-12-02},
	journal = {arXiv e-prints},
	author = {Uchiyama, Hisakazu and Akiyama, Masayuki and Toshikawa, Jun and Kashikawa, Nobunari and Overzier, Roderik and Nagao, Tohru and Ichikawa, Kohei and Marinello, Murilo and Imanishi, Masatoshi and Tanaka, Masayuki and Matsuoka, Yoshiki and Komiyama, Yutaka and Ishikawa, Shogo and Onoue, Masafusa and Kubo, Mariko and Harikane, Yuichi and Ito, Kei and Namiki, Shigeru and Liang, Yongming},
	month = nov,
	year = {2020},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:2011.10194},
}

Downloads: 0

{"_id":"HbuNy6QS2BnNnHt5a","bibbaseid":"uchiyama-akiyama-toshikawa-kashikawa-overzier-nagao-ichikawa-marinello-etal-faintquasarsliveinthesamenumberdensityenvironmentsaslymanbreakgalaxiesatztextasciitilde4-2020","author_short":["Uchiyama, H.","Akiyama, M.","Toshikawa, J.","Kashikawa, N.","Overzier, R.","Nagao, T.","Ichikawa, K.","Marinello, M.","Imanishi, M.","Tanaka, M.","Matsuoka, Y.","Komiyama, Y.","Ishikawa, S.","Onoue, M.","Kubo, M.","Harikane, Y.","Ito, K.","Namiki, S.","Liang, Y."],"bibdata":{"bibtype":"article","type":"article","title":"Faint Quasars Live in the Same Number Density Environments as Lyman Break Galaxies at z \\textasciitilde 4","volume":"2011","url":"http://adsabs.harvard.edu/abs/2020arXiv201110194U","abstract":"Characterizing high-z quasar environments is key to understanding the co-evolution of quasars and the surrounding galaxies. To restrict their global picture, we statistically examine the g-dropout galaxy overdensity distribution around 570 faint quasar candidates at z \\textasciitilde 4, based on the Hyper Suprime-Cam Subaru Strategic Program survey. We compare the overdensity significances of g-dropout galaxies around the quasars with those around g-dropout galaxies, and find no significant difference between their distributions. A total of 4 (22) out of the 570 faint quasars, 0.7_\\-0.4\\\\textasciicircum\\+0.4\\ (3.9_\\-0.8\\\\textasciicircum\\+0.8\\) %, are found to be associated with the \\textgreater 4 sigma overdense regions within an angular separation of 1.8 (3.0) arcmin, which is the typical size of protoclusters at this epoch. This is similar to the fraction of g-dropout galaxies associated with the \\textgreater 4 sigma overdense regions. This result is consistent with our previous work that 1.3_\\-0.9\\\\textasciicircum\\+0.9\\ % and 2.0_\\-1.1\\\\textasciicircum\\+1.1\\ % of luminous quasars detected in the Sloan Digital Sky Survey exist in the \\textgreater 4 sigma overdense regions within 1.8 and 3.0 arcmin separations, respectively. Therefore, we suggest that the galaxy number densities around quasars are independent of their luminosity, and most quasars do not preferentially appear in the richest protocluster regions at z \\textasciitilde 4. The lack of an apparent positive correlation between the quasars and the protoclusters implies that: i) the gas-rich major merger rate is relatively low in the protocluster regions, ii) most high-z quasars may appear through secular processes, or iii) some dust-obscured quasars exist in the protocluster regions.","urldate":"2020-12-02","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Uchiyama"],"firstnames":["Hisakazu"],"suffixes":[]},{"propositions":[],"lastnames":["Akiyama"],"firstnames":["Masayuki"],"suffixes":[]},{"propositions":[],"lastnames":["Toshikawa"],"firstnames":["Jun"],"suffixes":[]},{"propositions":[],"lastnames":["Kashikawa"],"firstnames":["Nobunari"],"suffixes":[]},{"propositions":[],"lastnames":["Overzier"],"firstnames":["Roderik"],"suffixes":[]},{"propositions":[],"lastnames":["Nagao"],"firstnames":["Tohru"],"suffixes":[]},{"propositions":[],"lastnames":["Ichikawa"],"firstnames":["Kohei"],"suffixes":[]},{"propositions":[],"lastnames":["Marinello"],"firstnames":["Murilo"],"suffixes":[]},{"propositions":[],"lastnames":["Imanishi"],"firstnames":["Masatoshi"],"suffixes":[]},{"propositions":[],"lastnames":["Tanaka"],"firstnames":["Masayuki"],"suffixes":[]},{"propositions":[],"lastnames":["Matsuoka"],"firstnames":["Yoshiki"],"suffixes":[]},{"propositions":[],"lastnames":["Komiyama"],"firstnames":["Yutaka"],"suffixes":[]},{"propositions":[],"lastnames":["Ishikawa"],"firstnames":["Shogo"],"suffixes":[]},{"propositions":[],"lastnames":["Onoue"],"firstnames":["Masafusa"],"suffixes":[]},{"propositions":[],"lastnames":["Kubo"],"firstnames":["Mariko"],"suffixes":[]},{"propositions":[],"lastnames":["Harikane"],"firstnames":["Yuichi"],"suffixes":[]},{"propositions":[],"lastnames":["Ito"],"firstnames":["Kei"],"suffixes":[]},{"propositions":[],"lastnames":["Namiki"],"firstnames":["Shigeru"],"suffixes":[]},{"propositions":[],"lastnames":["Liang"],"firstnames":["Yongming"],"suffixes":[]}],"month":"November","year":"2020","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2011.10194","bibtex":"@article{uchiyama_faint_2020,\n\ttitle = {Faint {Quasars} {Live} in the {Same} {Number} {Density} {Environments} as {Lyman} {Break} {Galaxies} at z {\\textasciitilde} 4},\n\tvolume = {2011},\n\turl = {http://adsabs.harvard.edu/abs/2020arXiv201110194U},\n\tabstract = {Characterizing high-z quasar environments is key to understanding the \nco-evolution of quasars and the surrounding galaxies. To restrict their\nglobal picture, we statistically examine the g-dropout galaxy\noverdensity distribution around 570 faint quasar candidates at z {\\textasciitilde} 4,\nbased on the Hyper Suprime-Cam Subaru Strategic Program survey. We\ncompare the overdensity significances of g-dropout galaxies around the\nquasars with those around g-dropout galaxies, and find no significant\ndifference between their distributions. A total of 4 (22) out of the 570\nfaint quasars, 0.7\\_\\{-0.4\\}{\\textasciicircum}\\{+0.4\\} (3.9\\_\\{-0.8\\}{\\textasciicircum}\\{+0.8\\}) \\%, are found to be\nassociated with the {\\textgreater} 4 sigma overdense regions within an angular\nseparation of 1.8 (3.0) arcmin, which is the typical size of\nprotoclusters at this epoch. This is similar to the fraction of\ng-dropout galaxies associated with the {\\textgreater} 4 sigma overdense regions.\nThis result is consistent with our previous work that 1.3\\_\\{-0.9\\}{\\textasciicircum}\\{+0.9\\}\n\\% and 2.0\\_\\{-1.1\\}{\\textasciicircum}\\{+1.1\\} \\% of luminous quasars detected in the Sloan\nDigital Sky Survey exist in the {\\textgreater} 4 sigma overdense regions within\n1.8 and 3.0 arcmin separations, respectively. Therefore, we suggest that\nthe galaxy number densities around quasars are independent of their\nluminosity, and most quasars do not preferentially appear in the richest\nprotocluster regions at z {\\textasciitilde} 4. The lack of an apparent positive\ncorrelation between the quasars and the protoclusters implies that: i)\nthe gas-rich major merger rate is relatively low in the protocluster\nregions, ii) most high-z quasars may appear through secular processes,\nor iii) some dust-obscured quasars exist in the protocluster regions.},\n\turldate = {2020-12-02},\n\tjournal = {arXiv e-prints},\n\tauthor = {Uchiyama, Hisakazu and Akiyama, Masayuki and Toshikawa, Jun and Kashikawa, Nobunari and Overzier, Roderik and Nagao, Tohru and Ichikawa, Kohei and Marinello, Murilo and Imanishi, Masatoshi and Tanaka, Masayuki and Matsuoka, Yoshiki and Komiyama, Yutaka and Ishikawa, Shogo and Onoue, Masafusa and Kubo, Mariko and Harikane, Yuichi and Ito, Kei and Namiki, Shigeru and Liang, Yongming},\n\tmonth = nov,\n\tyear = {2020},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:2011.10194},\n}\n\n","author_short":["Uchiyama, H.","Akiyama, M.","Toshikawa, J.","Kashikawa, N.","Overzier, R.","Nagao, T.","Ichikawa, K.","Marinello, M.","Imanishi, M.","Tanaka, M.","Matsuoka, Y.","Komiyama, Y.","Ishikawa, S.","Onoue, M.","Kubo, M.","Harikane, Y.","Ito, K.","Namiki, S.","Liang, Y."],"key":"uchiyama_faint_2020","id":"uchiyama_faint_2020","bibbaseid":"uchiyama-akiyama-toshikawa-kashikawa-overzier-nagao-ichikawa-marinello-etal-faintquasarsliveinthesamenumberdensityenvironmentsaslymanbreakgalaxiesatztextasciitilde4-2020","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2020arXiv201110194U"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["faint","quasars","live","same","number","density","environments","lyman","break","galaxies","textasciitilde","uchiyama","akiyama","toshikawa","kashikawa","overzier","nagao","ichikawa","marinello","imanishi","tanaka","matsuoka","komiyama","ishikawa","onoue","kubo","harikane","ito","namiki","liang"],"title":"Faint Quasars Live in the Same Number Density Environments as Lyman Break Galaxies at z \\textasciitilde 4","year":2020}