MC2: Multiwavelength and Dynamical Analysis of the Merging Galaxy Cluster ZwCl 0008.8+5215: An Older and Less Massive Bullet Cluster
We present and analyze a rich data set including Subaru/SuprimeCam, HST/Advanced Camera for Surveys and Wide Field Camera 3, Keck/DEIMOS, Chandra/ACIS-I, and JVLA/C and D array for the merging cluster of galaxies ZwCl 0008.8+5215. With a joint Subaru+HST weak gravitational lensing analysis, we ident...
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| Veröffentlicht in: | The Astrophysical journal 2017-04, Vol.838 (2) |
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| creator | Golovich, Nathan Weeren, Reinout J. van Dawson, William A. Jee, M. James Wittman, David |
| description | We present and analyze a rich data set including Subaru/SuprimeCam, HST/Advanced Camera for Surveys and Wide Field Camera 3, Keck/DEIMOS, Chandra/ACIS-I, and JVLA/C and D array for the merging cluster of galaxies ZwCl 0008.8+5215. With a joint Subaru+HST weak gravitational lensing analysis, we identify two dominant subclusters and estimate the masses to be and . We estimate the projected separation between the two subclusters to be . We perform a clustering analysis of spectroscopically confirmed cluster member galaxies and estimate the line-of-sight velocity difference between the two subclusters to be . We further motivate, discuss, and analyze the merger scenario through an analysis of the 42 ks of Chandra/ACIS-I and JVLA/C and D array polarization data. The X-ray surface brightness profile reveals a merging gas-core reminiscent of the Bullet Cluster. The global X-ray luminosity in the 0.5-7.0 keV band is and the global X-ray temperature is 4.90 0.13 keV. The radio relics are polarized up to , and along with the masses, velocities, and positions of the two subclusters, we input these quantities into a Monte Carlo dynamical analysis and estimate the merger velocity at pericenter to be . This is a lower-mass version of the Bullet Cluster and therefore may prove useful in testing alternative models of dark matter (DM). We do not find significant offsets between DM and galaxies, but the uncertainties are large with the current lensing data. Furthermore, in the east, the BCG is offset from other luminous cluster galaxies, which poses a puzzle for defining DM-galaxy offsets. |
| doi_str_mv | 10.3847/1538-4357/aa667f |
| format | Article |
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James ; Wittman, David</creator><creatorcontrib>Golovich, Nathan ; Weeren, Reinout J. van ; Dawson, William A. ; Jee, M. James ; Wittman, David ; Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)</creatorcontrib><description>We present and analyze a rich data set including Subaru/SuprimeCam, HST/Advanced Camera for Surveys and Wide Field Camera 3, Keck/DEIMOS, Chandra/ACIS-I, and JVLA/C and D array for the merging cluster of galaxies ZwCl 0008.8+5215. With a joint Subaru+HST weak gravitational lensing analysis, we identify two dominant subclusters and estimate the masses to be and . We estimate the projected separation between the two subclusters to be . We perform a clustering analysis of spectroscopically confirmed cluster member galaxies and estimate the line-of-sight velocity difference between the two subclusters to be . We further motivate, discuss, and analyze the merger scenario through an analysis of the 42 ks of Chandra/ACIS-I and JVLA/C and D array polarization data. The X-ray surface brightness profile reveals a merging gas-core reminiscent of the Bullet Cluster. The global X-ray luminosity in the 0.5-7.0 keV band is and the global X-ray temperature is 4.90 0.13 keV. The radio relics are polarized up to , and along with the masses, velocities, and positions of the two subclusters, we input these quantities into a Monte Carlo dynamical analysis and estimate the merger velocity at pericenter to be . This is a lower-mass version of the Bullet Cluster and therefore may prove useful in testing alternative models of dark matter (DM). We do not find significant offsets between DM and galaxies, but the uncertainties are large with the current lensing data. 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James</creatorcontrib><creatorcontrib>Wittman, David</creatorcontrib><creatorcontrib>Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)</creatorcontrib><title>MC2: Multiwavelength and Dynamical Analysis of the Merging Galaxy Cluster ZwCl 0008.8+5215: An Older and Less Massive Bullet Cluster</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We present and analyze a rich data set including Subaru/SuprimeCam, HST/Advanced Camera for Surveys and Wide Field Camera 3, Keck/DEIMOS, Chandra/ACIS-I, and JVLA/C and D array for the merging cluster of galaxies ZwCl 0008.8+5215. With a joint Subaru+HST weak gravitational lensing analysis, we identify two dominant subclusters and estimate the masses to be and . We estimate the projected separation between the two subclusters to be . We perform a clustering analysis of spectroscopically confirmed cluster member galaxies and estimate the line-of-sight velocity difference between the two subclusters to be . We further motivate, discuss, and analyze the merger scenario through an analysis of the 42 ks of Chandra/ACIS-I and JVLA/C and D array polarization data. The X-ray surface brightness profile reveals a merging gas-core reminiscent of the Bullet Cluster. The global X-ray luminosity in the 0.5-7.0 keV band is and the global X-ray temperature is 4.90 0.13 keV. The radio relics are polarized up to , and along with the masses, velocities, and positions of the two subclusters, we input these quantities into a Monte Carlo dynamical analysis and estimate the merger velocity at pericenter to be . This is a lower-mass version of the Bullet Cluster and therefore may prove useful in testing alternative models of dark matter (DM). We do not find significant offsets between DM and galaxies, but the uncertainties are large with the current lensing data. Furthermore, in the east, the BCG is offset from other luminous cluster galaxies, which poses a puzzle for defining DM-galaxy offsets.</description><subject>(cosmology:) large-scale structure of universe</subject><subject>Arrays</subject><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Astrophysics</subject><subject>Cameras</subject><subject>Cluster analysis</subject><subject>Clustering</subject><subject>Computer simulation</subject><subject>Dark matter</subject><subject>Deimos</subject><subject>Field cameras</subject><subject>Galactic clusters</subject><subject>Galaxies</subject><subject>galaxies: clusters: individual (ZwCl 0008.8+5215)</subject><subject>galaxies: clusters: intracluster medium</subject><subject>Galaxy mergers & collisions</subject><subject>Gravitational lenses</subject><subject>gravitational lensing</subject><subject>gravitational lensing: weak</subject><subject>large-scale structure of universe</subject><subject>Luminosity</subject><subject>Offsets</subject><subject>Space telescopes</subject><subject>Stars & galaxies</subject><subject>Surface brightness</subject><subject>Velocity</subject><subject>X-rays: galaxies: clusters</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNpFkTtPwzAUhS0EEqWwM1owQlo_EjvpBgEKUqsuICGWyPWjdWWSEjst3fnhJCqP6ere-50znAPAOUYDmsZ8iBOaRjFN-FAIxrg5AL2_0yHoIYTiiFH-egxOvF91K8myHvia5mQEp40Ldis22ulyEZZQlAre7UrxbqVw8KYUbueth5WBYanhVNcLWy7gWDjxuYO5a3zQNXzb5g62xukgvUoITkatEM6cal-d30R7D6fCe7vR8LZxTodf6Sk4MsJ5ffYz--Dl4f45f4wms_FTfjOJLMFZiOaSqJhyw7JUGaoylsZKzmkqMBYIC2MkyZTGc4OoZlIhZQyWjAtNGI95rGgfXOx9Kx9s4aUNWi5lVZZahgIzhhLMW-hyD63r6qPRPhSrqqnbCHxBKEsynBJOW-p6T9lq_Q9gVHRlFF3yRZd8sS-DfgN_WHuM</recordid><startdate>20170401</startdate><enddate>20170401</enddate><creator>Golovich, Nathan</creator><creator>Weeren, Reinout J. van</creator><creator>Dawson, William A.</creator><creator>Jee, M. 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James ; Wittman, David</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-i219t-bc2d437f698df3d9684dcb38a11a01affc29de1bf03e6cd0dff1c67ae267474d3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>(cosmology:) large-scale structure of universe</topic><topic>Arrays</topic><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Astrophysics</topic><topic>Cameras</topic><topic>Cluster analysis</topic><topic>Clustering</topic><topic>Computer simulation</topic><topic>Dark matter</topic><topic>Deimos</topic><topic>Field cameras</topic><topic>Galactic clusters</topic><topic>Galaxies</topic><topic>galaxies: clusters: individual (ZwCl 0008.8+5215)</topic><topic>galaxies: clusters: intracluster medium</topic><topic>Galaxy mergers & collisions</topic><topic>Gravitational lenses</topic><topic>gravitational lensing</topic><topic>gravitational lensing: weak</topic><topic>large-scale structure of universe</topic><topic>Luminosity</topic><topic>Offsets</topic><topic>Space telescopes</topic><topic>Stars & galaxies</topic><topic>Surface brightness</topic><topic>Velocity</topic><topic>X-rays: galaxies: clusters</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Golovich, Nathan</creatorcontrib><creatorcontrib>Weeren, Reinout J. van</creatorcontrib><creatorcontrib>Dawson, William A.</creatorcontrib><creatorcontrib>Jee, M. 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(LLNL), Livermore, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>MC2: Multiwavelength and Dynamical Analysis of the Merging Galaxy Cluster ZwCl 0008.8+5215: An Older and Less Massive Bullet Cluster</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2017-04-01</date><risdate>2017</risdate><volume>838</volume><issue>2</issue><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><abstract>We present and analyze a rich data set including Subaru/SuprimeCam, HST/Advanced Camera for Surveys and Wide Field Camera 3, Keck/DEIMOS, Chandra/ACIS-I, and JVLA/C and D array for the merging cluster of galaxies ZwCl 0008.8+5215. With a joint Subaru+HST weak gravitational lensing analysis, we identify two dominant subclusters and estimate the masses to be and . We estimate the projected separation between the two subclusters to be . We perform a clustering analysis of spectroscopically confirmed cluster member galaxies and estimate the line-of-sight velocity difference between the two subclusters to be . We further motivate, discuss, and analyze the merger scenario through an analysis of the 42 ks of Chandra/ACIS-I and JVLA/C and D array polarization data. The X-ray surface brightness profile reveals a merging gas-core reminiscent of the Bullet Cluster. The global X-ray luminosity in the 0.5-7.0 keV band is and the global X-ray temperature is 4.90 0.13 keV. The radio relics are polarized up to , and along with the masses, velocities, and positions of the two subclusters, we input these quantities into a Monte Carlo dynamical analysis and estimate the merger velocity at pericenter to be . This is a lower-mass version of the Bullet Cluster and therefore may prove useful in testing alternative models of dark matter (DM). 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| subjects | (cosmology:) large-scale structure of universe Arrays ASTRONOMY AND ASTROPHYSICS Astrophysics Cameras Cluster analysis Clustering Computer simulation Dark matter Deimos Field cameras Galactic clusters Galaxies galaxies: clusters: individual (ZwCl 0008.8+5215) galaxies: clusters: intracluster medium Galaxy mergers & collisions Gravitational lenses gravitational lensing gravitational lensing: weak large-scale structure of universe Luminosity Offsets Space telescopes Stars & galaxies Surface brightness Velocity X-rays: galaxies: clusters |
| title | MC2: Multiwavelength and Dynamical Analysis of the Merging Galaxy Cluster ZwCl 0008.8+5215: An Older and Less Massive Bullet Cluster |
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