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## MC2: galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301

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MC2 : galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301. / Dawson, William A.; Jee, M. James; Stroe, Andra; Ng, Y. Karen; Golovich, Nathan; Wittman, David; Sobral, David; Brüggen, M.; Röttgering, H. J A; Weeren, R. J Van.

In: The Astrophysical Journal, Vol. 805, No. 2, 143, 01.06.2015.

Research output: Contribution to journalJournal articlepeer-review

### Harvard

Dawson, WA, Jee, MJ, Stroe, A, Ng, YK, Golovich, N, Wittman, D, Sobral, D, Brüggen, M, Röttgering, HJA & Weeren, RJV 2015, 'MC2: galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301', The Astrophysical Journal, vol. 805, no. 2, 143. https://doi.org/10.1088/0004-637X/805/2/143

### APA

Dawson, W. A., Jee, M. J., Stroe, A., Ng, Y. K., Golovich, N., Wittman, D., Sobral, D., Brüggen, M., Röttgering, H. J. A., & Weeren, R. J. V. (2015). MC2: galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301. The Astrophysical Journal, 805(2), [143]. https://doi.org/10.1088/0004-637X/805/2/143

### Vancouver

Dawson WA, Jee MJ, Stroe A, Ng YK, Golovich N, Wittman D et al. MC2: galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301. The Astrophysical Journal. 2015 Jun 1;805(2). 143. https://doi.org/10.1088/0004-637X/805/2/143

### Author

Dawson, William A. ; Jee, M. James ; Stroe, Andra ; Ng, Y. Karen ; Golovich, Nathan ; Wittman, David ; Sobral, David ; Brüggen, M. ; Röttgering, H. J A ; Weeren, R. J Van. / MC2 : galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301. In: The Astrophysical Journal. 2015 ; Vol. 805, No. 2.

### Bibtex

@article{e03af3ce159f4218aceef0780495087a,
title = "MC2: galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301",
abstract = "X-ray and radio observations of CIZA J2242.8+5301 suggest that it is a major cluster merger. Despite being well studied in the X-ray and radio, little has been presented on the cluster structure and dynamics inferred from its galaxy population. We carried out a deep ($i\lt 25$) broadband imaging survey of the system with Subaru SuprimeCam (g and i bands) and the Canada–France–Hawaii Telescope (r band), as well as a comprehensive spectroscopic survey of the cluster area (505 redshifts) using Keck DEep Imaging Multi-Object Spectrograph. We use these data to perform a comprehensive galaxy/redshift analysis of the system, which is the first step to a proper understanding of the geometry and dynamics of the merger, as well as using the merger to constrain self-interacting dark matter. We find that the system is dominated by two subclusters of comparable richness with a projected separation of $6\buildrel{\,\prime}\over{.} 9_{-0.5}^{+0.7}$ (1.3$_{-0.10}^{+0.13}\;{\rm Mpc}$). We find that the north and south subclusters have similar redshifts of $z\approx 0.188$ with a relative line-of-sight (LOS) velocity difference of 69 ± 190 ${\rm km}\;{{{\rm s}}^{-1}}$. We also find that north and south subclusters have velocity dispersions of $1160_{-90}^{+100}$ and $1080_{-70}^{+100}\;{\rm km}\;{{{\rm s}}^{-1}}$, respectively. These correspond to masses of $16.1_{-3.3}^{+4.6}\times {{10}^{14}}$ and $13.0_{-2.5}^{+4.0}\times {{10}^{14}}$ ${{M}_{\odot }}$, respectively. While velocity dispersion measurements of merging clusters can be biased, we believe the bias in this system to be minor due to the large projected separation and nearly plane-of-sky merger configuration. We also find that the cDs of the north and south subclusters are very near their subcluster centers, in both projection (55 and 85 kpc, respectively) and normalized LOS velocity ($|{\Delta }v|/{{\sigma }_{v}}=0.43\pm 0.13$ and 0.21 ± 0.12 for the north and south, respectively). CIZA J2242.8+5301 is a relatively clean dissociative cluster merger with near 1:1 mass ratio, which makes it an ideal merger for studying merger-associated physical phenomena.",
author = "Dawson, {William A.} and Jee, {M. James} and Andra Stroe and Ng, {Y. Karen} and Nathan Golovich and David Wittman and David Sobral and M. Br{\"u}ggen and R{\"o}ttgering, {H. J A} and Weeren, {R. J Van}",
year = "2015",
month = jun,
day = "1",
doi = "10.1088/0004-637X/805/2/143",
language = "English",
volume = "805",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "2",

}

### RIS

TY - JOUR

T1 - MC2

T2 - galaxy imaging and redshift analysis of the merging cluster CIZA J2242.8+5301

AU - Dawson, William A.

AU - Jee, M. James

AU - Stroe, Andra

AU - Ng, Y. Karen

AU - Golovich, Nathan

AU - Wittman, David

AU - Sobral, David

AU - Brüggen, M.

AU - Röttgering, H. J A

AU - Weeren, R. J Van

PY - 2015/6/1

Y1 - 2015/6/1

N2 - X-ray and radio observations of CIZA J2242.8+5301 suggest that it is a major cluster merger. Despite being well studied in the X-ray and radio, little has been presented on the cluster structure and dynamics inferred from its galaxy population. We carried out a deep ($i\lt 25$) broadband imaging survey of the system with Subaru SuprimeCam (g and i bands) and the Canada–France–Hawaii Telescope (r band), as well as a comprehensive spectroscopic survey of the cluster area (505 redshifts) using Keck DEep Imaging Multi-Object Spectrograph. We use these data to perform a comprehensive galaxy/redshift analysis of the system, which is the first step to a proper understanding of the geometry and dynamics of the merger, as well as using the merger to constrain self-interacting dark matter. We find that the system is dominated by two subclusters of comparable richness with a projected separation of $6\buildrel{\,\prime}\over{.} 9_{-0.5}^{+0.7}$ (1.3$_{-0.10}^{+0.13}\;{\rm Mpc}$). We find that the north and south subclusters have similar redshifts of $z\approx 0.188$ with a relative line-of-sight (LOS) velocity difference of 69 ± 190 ${\rm km}\;{{{\rm s}}^{-1}}$. We also find that north and south subclusters have velocity dispersions of $1160_{-90}^{+100}$ and $1080_{-70}^{+100}\;{\rm km}\;{{{\rm s}}^{-1}}$, respectively. These correspond to masses of $16.1_{-3.3}^{+4.6}\times {{10}^{14}}$ and $13.0_{-2.5}^{+4.0}\times {{10}^{14}}$ ${{M}_{\odot }}$, respectively. While velocity dispersion measurements of merging clusters can be biased, we believe the bias in this system to be minor due to the large projected separation and nearly plane-of-sky merger configuration. We also find that the cDs of the north and south subclusters are very near their subcluster centers, in both projection (55 and 85 kpc, respectively) and normalized LOS velocity ($|{\Delta }v|/{{\sigma }_{v}}=0.43\pm 0.13$ and 0.21 ± 0.12 for the north and south, respectively). CIZA J2242.8+5301 is a relatively clean dissociative cluster merger with near 1:1 mass ratio, which makes it an ideal merger for studying merger-associated physical phenomena.

AB - X-ray and radio observations of CIZA J2242.8+5301 suggest that it is a major cluster merger. Despite being well studied in the X-ray and radio, little has been presented on the cluster structure and dynamics inferred from its galaxy population. We carried out a deep ($i\lt 25$) broadband imaging survey of the system with Subaru SuprimeCam (g and i bands) and the Canada–France–Hawaii Telescope (r band), as well as a comprehensive spectroscopic survey of the cluster area (505 redshifts) using Keck DEep Imaging Multi-Object Spectrograph. We use these data to perform a comprehensive galaxy/redshift analysis of the system, which is the first step to a proper understanding of the geometry and dynamics of the merger, as well as using the merger to constrain self-interacting dark matter. We find that the system is dominated by two subclusters of comparable richness with a projected separation of $6\buildrel{\,\prime}\over{.} 9_{-0.5}^{+0.7}$ (1.3$_{-0.10}^{+0.13}\;{\rm Mpc}$). We find that the north and south subclusters have similar redshifts of $z\approx 0.188$ with a relative line-of-sight (LOS) velocity difference of 69 ± 190 ${\rm km}\;{{{\rm s}}^{-1}}$. We also find that north and south subclusters have velocity dispersions of $1160_{-90}^{+100}$ and $1080_{-70}^{+100}\;{\rm km}\;{{{\rm s}}^{-1}}$, respectively. These correspond to masses of $16.1_{-3.3}^{+4.6}\times {{10}^{14}}$ and $13.0_{-2.5}^{+4.0}\times {{10}^{14}}$ ${{M}_{\odot }}$, respectively. While velocity dispersion measurements of merging clusters can be biased, we believe the bias in this system to be minor due to the large projected separation and nearly plane-of-sky merger configuration. We also find that the cDs of the north and south subclusters are very near their subcluster centers, in both projection (55 and 85 kpc, respectively) and normalized LOS velocity ($|{\Delta }v|/{{\sigma }_{v}}=0.43\pm 0.13$ and 0.21 ± 0.12 for the north and south, respectively). CIZA J2242.8+5301 is a relatively clean dissociative cluster merger with near 1:1 mass ratio, which makes it an ideal merger for studying merger-associated physical phenomena.

U2 - 10.1088/0004-637X/805/2/143

DO - 10.1088/0004-637X/805/2/143

M3 - Journal article

AN - SCOPUS:84930655615

VL - 805

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 143

ER -