JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES
We present a study of multiwavelength X-ray and weak lensing scaling relations for a sample of 50 clusters of galaxies. Our analysis combines Chandra and XMM-Newton data using an energy-dependent cross-calibration. After considering a number of scaling relations, we find that gas mass is the most ro...
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| Veröffentlicht in: | The Astrophysical journal 2013-04, Vol.767 (2), p.116 |
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| creator | Mahdavi, Andisheh Hoekstra, Henk Babul, Arif Bildfell, Chris Jeltema, Tesla Henry, J. Patrick |
| description | We present a study of multiwavelength X-ray and weak lensing scaling relations for a sample of 50 clusters of galaxies. Our analysis combines Chandra and XMM-Newton data using an energy-dependent cross-calibration. After considering a number of scaling relations, we find that gas mass is the most robust estimator of weak lensing mass, yielding 15% {+-} 6% intrinsic scatter at r{sub 500}{sup WL} (the pseudo-pressure Y{sub X} yields a consistent scatter of 22% {+-} 5%). The scatter does not change when measured within a fixed physical radius of 1 Mpc. Clusters with small brightest cluster galaxy (BCG) to X-ray peak offsets constitute a very regular population whose members have the same gas mass fractions and whose even smaller ( |
| doi_str_mv | 10.1088/0004-637X/767/2/116 |
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II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES</title><source>IOP Publishing Free Content</source><source>EZB-FREE-00999 freely available EZB journals</source><source>Alma/SFX Local Collection</source><creator>Mahdavi, Andisheh ; Hoekstra, Henk ; Babul, Arif ; Bildfell, Chris ; Jeltema, Tesla ; Henry, J. Patrick</creator><creatorcontrib>Mahdavi, Andisheh ; Hoekstra, Henk ; Babul, Arif ; Bildfell, Chris ; Jeltema, Tesla ; Henry, J. Patrick</creatorcontrib><description>We present a study of multiwavelength X-ray and weak lensing scaling relations for a sample of 50 clusters of galaxies. Our analysis combines Chandra and XMM-Newton data using an energy-dependent cross-calibration. After considering a number of scaling relations, we find that gas mass is the most robust estimator of weak lensing mass, yielding 15% {+-} 6% intrinsic scatter at r{sub 500}{sup WL} (the pseudo-pressure Y{sub X} yields a consistent scatter of 22% {+-} 5%). The scatter does not change when measured within a fixed physical radius of 1 Mpc. Clusters with small brightest cluster galaxy (BCG) to X-ray peak offsets constitute a very regular population whose members have the same gas mass fractions and whose even smaller (<10%) deviations from regularity can be ascribed to line of sight geometrical effects alone. Cool-core clusters, while a somewhat different population, also show the same (<10%) scatter in the gas mass-lensing mass relation. There is a good correlation and a hint of bimodality in the plane defined by BCG offset and central entropy (or central cooling time). The pseudo-pressure Y{sub X} does not discriminate between the more relaxed and less relaxed populations, making it perhaps the more even-handed mass proxy for surveys. Overall, hydrostatic masses underestimate weak lensing masses by 10% on the average at r{sub 500}{sup WL}; but cool-core clusters are consistent with no bias, while non-cool-core clusters have a large and constant 15%-20% bias between r{sub 2500}{sup WL} and r{sub 500}{sup WL}, in agreement with N-body simulations incorporating unthermalized gas. For non-cool-core clusters, the bias correlates well with BCG ellipticity. We also examine centroid shift variance and power ratios to quantify substructure; these quantities do not correlate with residuals in the scaling relations. Individual clusters have for the most part forgotten the source of their departures from self-similarity.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/767/2/116</identifier><language>eng</language><publisher>United States</publisher><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; CALIBRATION ; GALAXY CLUSTERS ; GRAVITATIONAL LENSES ; MASS ; PEAKS ; SCALING ; SIMULATION ; X RADIATION ; X-RAY GALAXIES</subject><ispartof>The Astrophysical journal, 2013-04, Vol.767 (2), p.116</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c388t-42870bc9ebd5d7f44dbe9c4a4268520a031b6b7c26323f7ec31553d3d3e3146c3</citedby><cites>FETCH-LOGICAL-c388t-42870bc9ebd5d7f44dbe9c4a4268520a031b6b7c26323f7ec31553d3d3e3146c3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,27901,27902</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/22126928$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Mahdavi, Andisheh</creatorcontrib><creatorcontrib>Hoekstra, Henk</creatorcontrib><creatorcontrib>Babul, Arif</creatorcontrib><creatorcontrib>Bildfell, Chris</creatorcontrib><creatorcontrib>Jeltema, Tesla</creatorcontrib><creatorcontrib>Henry, J. Patrick</creatorcontrib><title>JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES</title><title>The Astrophysical journal</title><description>We present a study of multiwavelength X-ray and weak lensing scaling relations for a sample of 50 clusters of galaxies. Our analysis combines Chandra and XMM-Newton data using an energy-dependent cross-calibration. After considering a number of scaling relations, we find that gas mass is the most robust estimator of weak lensing mass, yielding 15% {+-} 6% intrinsic scatter at r{sub 500}{sup WL} (the pseudo-pressure Y{sub X} yields a consistent scatter of 22% {+-} 5%). The scatter does not change when measured within a fixed physical radius of 1 Mpc. Clusters with small brightest cluster galaxy (BCG) to X-ray peak offsets constitute a very regular population whose members have the same gas mass fractions and whose even smaller (<10%) deviations from regularity can be ascribed to line of sight geometrical effects alone. Cool-core clusters, while a somewhat different population, also show the same (<10%) scatter in the gas mass-lensing mass relation. There is a good correlation and a hint of bimodality in the plane defined by BCG offset and central entropy (or central cooling time). The pseudo-pressure Y{sub X} does not discriminate between the more relaxed and less relaxed populations, making it perhaps the more even-handed mass proxy for surveys. Overall, hydrostatic masses underestimate weak lensing masses by 10% on the average at r{sub 500}{sup WL}; but cool-core clusters are consistent with no bias, while non-cool-core clusters have a large and constant 15%-20% bias between r{sub 2500}{sup WL} and r{sub 500}{sup WL}, in agreement with N-body simulations incorporating unthermalized gas. For non-cool-core clusters, the bias correlates well with BCG ellipticity. We also examine centroid shift variance and power ratios to quantify substructure; these quantities do not correlate with residuals in the scaling relations. Individual clusters have for the most part forgotten the source of their departures from self-similarity.</description><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>CALIBRATION</subject><subject>GALAXY CLUSTERS</subject><subject>GRAVITATIONAL LENSES</subject><subject>MASS</subject><subject>PEAKS</subject><subject>SCALING</subject><subject>SIMULATION</subject><subject>X RADIATION</subject><subject>X-RAY GALAXIES</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNo9kMtOg0AUhidGE2v1CdxM4poyF67LkU7b0SkYhlq6msAAsUZbA2x8Dx9YsGrO4s9J_kvyAXCL0QyjILARQo7lUT-3fc-3iY2xdwYm2KWB5VDXPweTf8cluOq61_ElYTgBXw-JiDPIYiZ3SiiYLGAkNyrjKUzuFU-fWSaSWM2gEDMYrVg8T5mdr9dWzLdZEsPcStluiM_hlrNHKHmsRLyEKmJy1JTLUwFcJClkULH1k-TjiotgKqLV39rP8pJJlguursFFU7x19c2vTsFmwbNoZclkKYZmy9Ag6C2HBD4qTViXlVv5jeNUZR0ap3CIF7gEFYji0it9QzxKaOPXhmLXpdVwNcWOZ-gU3J16j12_153Z97V5McfDoTa9JgQTLyTB4KInl2mPXdfWjf5o9-9F-6kx0iN-PdLUI1w94NdED_jpN1Kva18</recordid><startdate>20130420</startdate><enddate>20130420</enddate><creator>Mahdavi, Andisheh</creator><creator>Hoekstra, Henk</creator><creator>Babul, Arif</creator><creator>Bildfell, Chris</creator><creator>Jeltema, Tesla</creator><creator>Henry, J. Patrick</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>OTOTI</scope></search><sort><creationdate>20130420</creationdate><title>JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES</title><author>Mahdavi, Andisheh ; Hoekstra, Henk ; Babul, Arif ; Bildfell, Chris ; Jeltema, Tesla ; Henry, J. Patrick</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c388t-42870bc9ebd5d7f44dbe9c4a4268520a031b6b7c26323f7ec31553d3d3e3146c3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>CALIBRATION</topic><topic>GALAXY CLUSTERS</topic><topic>GRAVITATIONAL LENSES</topic><topic>MASS</topic><topic>PEAKS</topic><topic>SCALING</topic><topic>SIMULATION</topic><topic>X RADIATION</topic><topic>X-RAY GALAXIES</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Mahdavi, Andisheh</creatorcontrib><creatorcontrib>Hoekstra, Henk</creatorcontrib><creatorcontrib>Babul, Arif</creatorcontrib><creatorcontrib>Bildfell, Chris</creatorcontrib><creatorcontrib>Jeltema, Tesla</creatorcontrib><creatorcontrib>Henry, J. Patrick</creatorcontrib><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Mahdavi, Andisheh</au><au>Hoekstra, Henk</au><au>Babul, Arif</au><au>Bildfell, Chris</au><au>Jeltema, Tesla</au><au>Henry, J. Patrick</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES</atitle><jtitle>The Astrophysical journal</jtitle><date>2013-04-20</date><risdate>2013</risdate><volume>767</volume><issue>2</issue><spage>116</spage><pages>116-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We present a study of multiwavelength X-ray and weak lensing scaling relations for a sample of 50 clusters of galaxies. Our analysis combines Chandra and XMM-Newton data using an energy-dependent cross-calibration. After considering a number of scaling relations, we find that gas mass is the most robust estimator of weak lensing mass, yielding 15% {+-} 6% intrinsic scatter at r{sub 500}{sup WL} (the pseudo-pressure Y{sub X} yields a consistent scatter of 22% {+-} 5%). The scatter does not change when measured within a fixed physical radius of 1 Mpc. Clusters with small brightest cluster galaxy (BCG) to X-ray peak offsets constitute a very regular population whose members have the same gas mass fractions and whose even smaller (<10%) deviations from regularity can be ascribed to line of sight geometrical effects alone. Cool-core clusters, while a somewhat different population, also show the same (<10%) scatter in the gas mass-lensing mass relation. There is a good correlation and a hint of bimodality in the plane defined by BCG offset and central entropy (or central cooling time). The pseudo-pressure Y{sub X} does not discriminate between the more relaxed and less relaxed populations, making it perhaps the more even-handed mass proxy for surveys. Overall, hydrostatic masses underestimate weak lensing masses by 10% on the average at r{sub 500}{sup WL}; but cool-core clusters are consistent with no bias, while non-cool-core clusters have a large and constant 15%-20% bias between r{sub 2500}{sup WL} and r{sub 500}{sup WL}, in agreement with N-body simulations incorporating unthermalized gas. For non-cool-core clusters, the bias correlates well with BCG ellipticity. We also examine centroid shift variance and power ratios to quantify substructure; these quantities do not correlate with residuals in the scaling relations. Individual clusters have for the most part forgotten the source of their departures from self-similarity.</abstract><cop>United States</cop><doi>10.1088/0004-637X/767/2/116</doi><oa>free_for_read</oa></addata></record> |
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| subjects | ASTROPHYSICS, COSMOLOGY AND ASTRONOMY CALIBRATION GALAXY CLUSTERS GRAVITATIONAL LENSES MASS PEAKS SCALING SIMULATION X RADIATION X-RAY GALAXIES |
| title | JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES |
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