The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view
Abstract We present a weak-lensing and dynamical study of the complex cluster Abell 1758 (A1758, $\bar{z} = 0.278$ ) supported by hydrodynamical simulations. This cluster is composed of two main structures called A1758N and A1758S. The northern structure is composed of A1758NW and A1758NE, with lens...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2017-04, Vol.466 (3), p.2614-2632 |
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| container_title | Monthly notices of the Royal Astronomical Society |
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| creator | Monteiro-Oliveira, R. Cypriano, E. S. Machado, R. E. G. Lima Neto, G. B. Ribeiro, A. L. B. Sodré, L. Dupke, R. |
| description | Abstract
We present a weak-lensing and dynamical study of the complex cluster Abell 1758 (A1758,
$\bar{z} = 0.278$
) supported by hydrodynamical simulations. This cluster is composed of two main structures called A1758N and A1758S. The northern structure is composed of A1758NW and A1758NE, with lensing determined masses of
$7.90_{-1.55}^{+1.89}$
× 1014 M⊙ and
$5.49_{-1.33}^{+1.67}$
× 1014 M⊙, respectively. They show a remarkable feature: while in A1758NW, there is a spatial agreement among weak-lensing mass distribution, intracluster medium and its brightest cluster galaxy (BCG), in A1758NE, the X-ray peak is located
$96_{-15}^{+14}$
arcsec away from the mass peak and BCG positions. Given the detachment between gas and mass, we could use the local surface mass density to estimate an upper limit for the dark matter self-interaction cross-section: σ/m |
| doi_str_mv | 10.1093/mnras/stw3238 |
| format | Article |
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We present a weak-lensing and dynamical study of the complex cluster Abell 1758 (A1758,
$\bar{z} = 0.278$
) supported by hydrodynamical simulations. This cluster is composed of two main structures called A1758N and A1758S. The northern structure is composed of A1758NW and A1758NE, with lensing determined masses of
$7.90_{-1.55}^{+1.89}$
× 1014 M⊙ and
$5.49_{-1.33}^{+1.67}$
× 1014 M⊙, respectively. They show a remarkable feature: while in A1758NW, there is a spatial agreement among weak-lensing mass distribution, intracluster medium and its brightest cluster galaxy (BCG), in A1758NE, the X-ray peak is located
$96_{-15}^{+14}$
arcsec away from the mass peak and BCG positions. Given the detachment between gas and mass, we could use the local surface mass density to estimate an upper limit for the dark matter self-interaction cross-section: σ/m < 5.83 cm2 g−1. Combining our velocity data with hydrodynamical simulations, we have shown that A1758 NW and NE had their closest approach 0.27 Gyr ago and their merger axis is 21° ± 12° from the plane of the sky. In the A1758S system, we have measured a total mass of
$4.96_{-1.19}^{+1.08} \times 10^{14}$
M⊙ and, using radial velocity data, we found that the main merger axis is located at 70° ± 4° from the plane of the sky, therefore closest to the line of sight.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stw3238</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Astronomy ; Clusters ; Cross sections ; Dark matter ; Fluid mechanics ; Galaxies ; Line of sight ; Mass distribution ; Planes ; Simulation ; Star & galaxy formation</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2017-04, Vol.466 (3), p.2614-2632</ispartof><rights>2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2016</rights><rights>Copyright Oxford University Press, UK Apr 21, 2017</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c469t-dcd249b3502f4946bd785de8a482f738b394e63e9f96eafe4d3fdfb3109bad0b3</citedby><cites>FETCH-LOGICAL-c469t-dcd249b3502f4946bd785de8a482f738b394e63e9f96eafe4d3fdfb3109bad0b3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stw3238$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Monteiro-Oliveira, R.</creatorcontrib><creatorcontrib>Cypriano, E. S.</creatorcontrib><creatorcontrib>Machado, R. E. G.</creatorcontrib><creatorcontrib>Lima Neto, G. B.</creatorcontrib><creatorcontrib>Ribeiro, A. L. B.</creatorcontrib><creatorcontrib>Sodré, L.</creatorcontrib><creatorcontrib>Dupke, R.</creatorcontrib><title>The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view</title><title>Monthly notices of the Royal Astronomical Society</title><description>Abstract
We present a weak-lensing and dynamical study of the complex cluster Abell 1758 (A1758,
$\bar{z} = 0.278$
) supported by hydrodynamical simulations. This cluster is composed of two main structures called A1758N and A1758S. The northern structure is composed of A1758NW and A1758NE, with lensing determined masses of
$7.90_{-1.55}^{+1.89}$
× 1014 M⊙ and
$5.49_{-1.33}^{+1.67}$
× 1014 M⊙, respectively. They show a remarkable feature: while in A1758NW, there is a spatial agreement among weak-lensing mass distribution, intracluster medium and its brightest cluster galaxy (BCG), in A1758NE, the X-ray peak is located
$96_{-15}^{+14}$
arcsec away from the mass peak and BCG positions. Given the detachment between gas and mass, we could use the local surface mass density to estimate an upper limit for the dark matter self-interaction cross-section: σ/m < 5.83 cm2 g−1. Combining our velocity data with hydrodynamical simulations, we have shown that A1758 NW and NE had their closest approach 0.27 Gyr ago and their merger axis is 21° ± 12° from the plane of the sky. In the A1758S system, we have measured a total mass of
$4.96_{-1.19}^{+1.08} \times 10^{14}$
M⊙ and, using radial velocity data, we found that the main merger axis is located at 70° ± 4° from the plane of the sky, therefore closest to the line of sight.</description><subject>Astronomy</subject><subject>Clusters</subject><subject>Cross sections</subject><subject>Dark matter</subject><subject>Fluid mechanics</subject><subject>Galaxies</subject><subject>Line of sight</subject><subject>Mass distribution</subject><subject>Planes</subject><subject>Simulation</subject><subject>Star & galaxy formation</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNqNkc1LxDAQxYMouK4evQe8eKkmTZqm3hbxCxa8rOeSJpPdrm1Tk9bV_96suyB40bkMzPsxvMdD6JySK0oKdt12XoXrMGxYyuQBmlAmsiQthDhEE0JYlsic0mN0EsKaEMJZKibILFaAW_BL8HhVh8H5T-wsHuJVu7Zv4APrZgxDlGcVNA2meSZvsNqqVd2BwRtQr7iBLtTdEqvO4NCDHrwL2vW1xu81bE7RkVVNgLP9nqKX-7vF7WMyf354up3NE81FMSRGm5QXFctIannBRWVymRmQisvU5kxWrOAgGBS2EKAscMOssRWL4StlSMWm6HL3t_fubYQwlG0ddHStOnBjKKmUnFIiKP8HmueSpkRu0Ytf6NqNvotBIiVkllIWZ4qSHaVj9ODBlr2vW-U_S0rKbT3ldz3lvp4fA27s_0C_AKwRkl4</recordid><startdate>20170421</startdate><enddate>20170421</enddate><creator>Monteiro-Oliveira, R.</creator><creator>Cypriano, E. S.</creator><creator>Machado, R. E. G.</creator><creator>Lima Neto, G. B.</creator><creator>Ribeiro, A. L. B.</creator><creator>Sodré, L.</creator><creator>Dupke, R.</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7TG</scope><scope>KL.</scope></search><sort><creationdate>20170421</creationdate><title>The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view</title><author>Monteiro-Oliveira, R. ; Cypriano, E. S. ; Machado, R. E. G. ; Lima Neto, G. B. ; Ribeiro, A. L. B. ; Sodré, L. ; Dupke, R.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c469t-dcd249b3502f4946bd785de8a482f738b394e63e9f96eafe4d3fdfb3109bad0b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Astronomy</topic><topic>Clusters</topic><topic>Cross sections</topic><topic>Dark matter</topic><topic>Fluid mechanics</topic><topic>Galaxies</topic><topic>Line of sight</topic><topic>Mass distribution</topic><topic>Planes</topic><topic>Simulation</topic><topic>Star & galaxy formation</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Monteiro-Oliveira, R.</creatorcontrib><creatorcontrib>Cypriano, E. S.</creatorcontrib><creatorcontrib>Machado, R. E. G.</creatorcontrib><creatorcontrib>Lima Neto, G. B.</creatorcontrib><creatorcontrib>Ribeiro, A. L. B.</creatorcontrib><creatorcontrib>Sodré, L.</creatorcontrib><creatorcontrib>Dupke, R.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Monteiro-Oliveira, R.</au><au>Cypriano, E. S.</au><au>Machado, R. E. G.</au><au>Lima Neto, G. B.</au><au>Ribeiro, A. L. B.</au><au>Sodré, L.</au><au>Dupke, R.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2017-04-21</date><risdate>2017</risdate><volume>466</volume><issue>3</issue><spage>2614</spage><epage>2632</epage><pages>2614-2632</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>Abstract
We present a weak-lensing and dynamical study of the complex cluster Abell 1758 (A1758,
$\bar{z} = 0.278$
) supported by hydrodynamical simulations. This cluster is composed of two main structures called A1758N and A1758S. The northern structure is composed of A1758NW and A1758NE, with lensing determined masses of
$7.90_{-1.55}^{+1.89}$
× 1014 M⊙ and
$5.49_{-1.33}^{+1.67}$
× 1014 M⊙, respectively. They show a remarkable feature: while in A1758NW, there is a spatial agreement among weak-lensing mass distribution, intracluster medium and its brightest cluster galaxy (BCG), in A1758NE, the X-ray peak is located
$96_{-15}^{+14}$
arcsec away from the mass peak and BCG positions. Given the detachment between gas and mass, we could use the local surface mass density to estimate an upper limit for the dark matter self-interaction cross-section: σ/m < 5.83 cm2 g−1. Combining our velocity data with hydrodynamical simulations, we have shown that A1758 NW and NE had their closest approach 0.27 Gyr ago and their merger axis is 21° ± 12° from the plane of the sky. In the A1758S system, we have measured a total mass of
$4.96_{-1.19}^{+1.08} \times 10^{14}$
M⊙ and, using radial velocity data, we found that the main merger axis is located at 70° ± 4° from the plane of the sky, therefore closest to the line of sight.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/stw3238</doi><tpages>19</tpages><oa>free_for_read</oa></addata></record> |
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| language | eng |
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| source | Oxford Journals Open Access Collection |
| subjects | Astronomy Clusters Cross sections Dark matter Fluid mechanics Galaxies Line of sight Mass distribution Planes Simulation Star & galaxy formation |
| title | The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view |
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