Identification of the progenitors of rich clusters and member galaxies in rapid formation at z\textgreater2. Shimakawa, R., Kodama, T., Tadaki, K., Tanaka, I., Hayashi, M., & Koyama, Y. Monthly Notices of the Royal Astronomical Society: Letters, 441(1):L1–L5, May, 2014. arXiv: 1402.3568![Identification of the progenitors of rich clusters and member galaxies in rapid formation at z\textgreater2 [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex We present the results of near-infrared spectroscopy of H\${\textbackslash}alpha\$ emitters (HAEs) associated with two protoclusters around radio galaxies (PKS1138-262 at \$z\$=2.2 and USS1558-003 at \$z\$=2.5) with Multi-Object Infrared Camera and Spectrograph (MOIRCS) on the Subaru telescope. Among the HAE candidates constructed from our narrow-band imaging, we have confirmed membership of 27 and 36 HAEs for the respective protoclusters, with a success rate of 70 per cent of our observed targets. The large number of spectroscopically confirmed members per cluster has enabled us for the first time to reveal the detailed kinematical structures of the protoclusters at \$z\$\${\textgreater}\$2. The clusters show prominent substructures such as clumps, filaments and velocity gradients, suggesting that they are still in the midst of rapid construction to grow to rich clusters at later times. We also estimate dynamical masses of the clusters and substructures assuming their local virialization. The inferred masses (\${\textbackslash}sim\$10\${\textasciicircum}\{14\}\$M\$_{\textbackslash}odot\$) of the protocluster cores are consistent with being typical progenitors of the present-day most massive class of galaxy clusters (\${\textbackslash}sim\$10\${\textasciicircum}\{15\}\$M\$_{\textbackslash}odot\$) if we take into account the typical mass growth history of clusters. We then calculated the integrated star formation rates of the protocluster cores normalized by the dynamical masses, and compare these with lower redshift descendants. We see a marked increase of star-forming activities in the cluster cores, by almost three orders of magnitude, as we go back in time to 11 billion years ago; this scales as (1\$+\$\$z\$)\${\textasciicircum}6\$.
@article{shimakawa_identification_2014,
title = {Identification of the progenitors of rich clusters and member galaxies in rapid formation at z{\textgreater}2},
volume = {441},
issn = {1745-3925, 1745-3933},
url = {http://arxiv.org/abs/1402.3568},
doi = {10.1093/mnrasl/slu029},
abstract = {We present the results of near-infrared spectroscopy of H\${\textbackslash}alpha\$ emitters (HAEs) associated with two protoclusters around radio galaxies (PKS1138-262 at \$z\$=2.2 and USS1558-003 at \$z\$=2.5) with Multi-Object Infrared Camera and Spectrograph (MOIRCS) on the Subaru telescope. Among the HAE candidates constructed from our narrow-band imaging, we have confirmed membership of 27 and 36 HAEs for the respective protoclusters, with a success rate of 70 per cent of our observed targets. The large number of spectroscopically confirmed members per cluster has enabled us for the first time to reveal the detailed kinematical structures of the protoclusters at \$z\$\${\textgreater}\$2. The clusters show prominent substructures such as clumps, filaments and velocity gradients, suggesting that they are still in the midst of rapid construction to grow to rich clusters at later times. We also estimate dynamical masses of the clusters and substructures assuming their local virialization. The inferred masses (\${\textbackslash}sim\$10\${\textasciicircum}\{14\}\$M\$\_{\textbackslash}odot\$) of the protocluster cores are consistent with being typical progenitors of the present-day most massive class of galaxy clusters (\${\textbackslash}sim\$10\${\textasciicircum}\{15\}\$M\$\_{\textbackslash}odot\$) if we take into account the typical mass growth history of clusters. We then calculated the integrated star formation rates of the protocluster cores normalized by the dynamical masses, and compare these with lower redshift descendants. We see a marked increase of star-forming activities in the cluster cores, by almost three orders of magnitude, as we go back in time to 11 billion years ago; this scales as (1\$+\$\$z\$)\${\textasciicircum}6\$.},
number = {1},
journal = {Monthly Notices of the Royal Astronomical Society: Letters},
author = {Shimakawa, Rhythm and Kodama, Tadayuki and Tadaki, Ken-ichi and Tanaka, Ichi and Hayashi, Masao and Koyama, Yusei},
month = may,
year = {2014},
note = {arXiv: 1402.3568},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {L1--L5},
}
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Among the HAE candidates constructed from our narrow-band imaging, we have confirmed membership of 27 and 36 HAEs for the respective protoclusters, with a success rate of 70 per cent of our observed targets. The large number of spectroscopically confirmed members per cluster has enabled us for the first time to reveal the detailed kinematical structures of the protoclusters at \\$z\\$\\${\\textgreater}\\$2. The clusters show prominent substructures such as clumps, filaments and velocity gradients, suggesting that they are still in the midst of rapid construction to grow to rich clusters at later times. We also estimate dynamical masses of the clusters and substructures assuming their local virialization. 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Among the HAE candidates constructed from our narrow-band imaging, we have confirmed membership of 27 and 36 HAEs for the respective protoclusters, with a success rate of 70 per cent of our observed targets. The large number of spectroscopically confirmed members per cluster has enabled us for the first time to reveal the detailed kinematical structures of the protoclusters at \\$z\\$\\${\\textgreater}\\$2. The clusters show prominent substructures such as clumps, filaments and velocity gradients, suggesting that they are still in the midst of rapid construction to grow to rich clusters at later times. We also estimate dynamical masses of the clusters and substructures assuming their local virialization. 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