Dark Energy Survey Year 1 Results: Detection of Intracluster Light at Redshift ∼ 0.25
Using data collected by the Dark Energy Survey (DES), we report the detection of intracluster light (ICL) with ∼300 galaxy clusters in the redshift range of 0.2-0.3. We design methods to mask detected galaxies and stars in the images and stack the cluster light profiles, while accounting for several...
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| Veröffentlicht in: | The Astrophysical journal 2019-04, Vol.874 (2), p.165 |
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| creator | Zhang, Y. Yanny, B. Palmese, A. Gruen, D. To, C. Rykoff, E. S. Leung, Y. Collins, C. Hilton, M. Abbott, T. M. C. Annis, J. Avila, S. Bertin, E. Brooks, D. Burke, D. L. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Cunha, C. E. D'Andrea, C. B. Costa, L. N. da Vicente, J. De Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Drlica-Wagner, A. Eifler, T. F. Evrard, A. E. Flaugher, B. Fosalba, P. Frieman, J. García-Bellido, J. Gaztanaga, E. Gerdes, D. W. Gruendl, R. A. Gschwend, J. Gutierrez, G. Hartley, W. G. Hollowood, D. L. Honscheid, K. Hoyle, B. James, D. J. Jeltema, T. Kuehn, K. Kuropatkin, N. Li, T. S. Lima, M. Maia, M. A. G. March, M. Marshall, J. L. Melchior, P. Menanteau, F. Miller, C. J. Miquel, R. Mohr, J. J. Ogando, R. L. C. Plazas, A. A. Romer, A. K. Sanchez, E. Scarpine, V. Schubnell, M. Serrano, S. Sevilla-Noarbe, I. Smith, M. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Thomas, D. Wester, W. |
| description | Using data collected by the Dark Energy Survey (DES), we report the detection of intracluster light (ICL) with ∼300 galaxy clusters in the redshift range of 0.2-0.3. We design methods to mask detected galaxies and stars in the images and stack the cluster light profiles, while accounting for several systematic effects (sky subtraction, instrumental point-spread function, cluster selection effects, and residual light in the ICL raw detection from background and cluster galaxies). The methods allow us to acquire high signal-to-noise measurements of the ICL and central galaxies (CGs), which we separate with radial cuts. The ICL appears as faint and diffuse light extending to at least 1 Mpc from the cluster center, reaching a surface brightness level of 30 mag arcsec−2. The ICL and the cluster CG contribute 44% 17% of the total cluster stellar luminosity within 1 Mpc. The ICL color is overall consistent with that of the cluster red sequence galaxies, but displays the trend of becoming bluer with increasing radius. The ICL demonstrates an interesting self-similarity feature-for clusters in different richness ranges, their ICL radial profiles are similar after scaling with cluster R200m, and the ICL brightness appears to be a good tracer of the cluster radial mass distribution. These analyses are based on the DES redMaPPer cluster sample identified in the first year of observations. |
| doi_str_mv | 10.3847/1538-4357/ab0dfd |
| format | Article |
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S. ; Leung, Y. ; Collins, C. ; Hilton, M. ; Abbott, T. M. C. ; Annis, J. ; Avila, S. ; Bertin, E. ; Brooks, D. ; Burke, D. L. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; Cunha, C. E. ; D'Andrea, C. B. ; Costa, L. N. da ; Vicente, J. De ; Desai, S. ; Diehl, H. T. ; Dietrich, J. P. ; Doel, P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Evrard, A. E. ; Flaugher, B. ; Fosalba, P. ; Frieman, J. ; García-Bellido, J. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Hartley, W. G. ; Hollowood, D. L. ; Honscheid, K. ; Hoyle, B. ; James, D. J. ; Jeltema, T. ; Kuehn, K. ; Kuropatkin, N. ; Li, T. S. ; Lima, M. ; Maia, M. A. G. ; March, M. ; Marshall, J. L. ; Melchior, P. ; Menanteau, F. ; Miller, C. J. ; Miquel, R. ; Mohr, J. J. ; Ogando, R. L. C. ; Plazas, A. A. ; Romer, A. K. ; Sanchez, E. ; Scarpine, V. ; Schubnell, M. ; Serrano, S. ; Sevilla-Noarbe, I. ; Smith, M. ; Soares-Santos, M. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, D. ; Wester, W.</creator><creatorcontrib>Zhang, Y. ; Yanny, B. ; Palmese, A. ; Gruen, D. ; To, C. ; Rykoff, E. S. ; Leung, Y. ; Collins, C. ; Hilton, M. ; Abbott, T. M. C. ; Annis, J. ; Avila, S. ; Bertin, E. ; Brooks, D. ; Burke, D. L. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; Cunha, C. E. ; D'Andrea, C. B. ; Costa, L. N. da ; Vicente, J. De ; Desai, S. ; Diehl, H. T. ; Dietrich, J. P. ; Doel, P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Evrard, A. E. ; Flaugher, B. ; Fosalba, P. ; Frieman, J. ; García-Bellido, J. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Hartley, W. G. ; Hollowood, D. L. ; Honscheid, K. ; Hoyle, B. ; James, D. J. ; Jeltema, T. ; Kuehn, K. ; Kuropatkin, N. ; Li, T. S. ; Lima, M. ; Maia, M. A. G. ; March, M. ; Marshall, J. L. ; Melchior, P. ; Menanteau, F. ; Miller, C. J. ; Miquel, R. ; Mohr, J. J. ; Ogando, R. L. C. ; Plazas, A. A. ; Romer, A. K. ; Sanchez, E. ; Scarpine, V. ; Schubnell, M. ; Serrano, S. ; Sevilla-Noarbe, I. ; Smith, M. ; Soares-Santos, M. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, D. ; Wester, W. ; DES Collaboration ; SLAC National Accelerator Lab., Menlo Park, CA (United States) ; Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States) ; Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States) ; Univ. of Michigan, Ann Arbor, MI (United States)</creatorcontrib><description>Using data collected by the Dark Energy Survey (DES), we report the detection of intracluster light (ICL) with ∼300 galaxy clusters in the redshift range of 0.2-0.3. We design methods to mask detected galaxies and stars in the images and stack the cluster light profiles, while accounting for several systematic effects (sky subtraction, instrumental point-spread function, cluster selection effects, and residual light in the ICL raw detection from background and cluster galaxies). The methods allow us to acquire high signal-to-noise measurements of the ICL and central galaxies (CGs), which we separate with radial cuts. The ICL appears as faint and diffuse light extending to at least 1 Mpc from the cluster center, reaching a surface brightness level of 30 mag arcsec−2. The ICL and the cluster CG contribute 44% 17% of the total cluster stellar luminosity within 1 Mpc. The ICL color is overall consistent with that of the cluster red sequence galaxies, but displays the trend of becoming bluer with increasing radius. The ICL demonstrates an interesting self-similarity feature-for clusters in different richness ranges, their ICL radial profiles are similar after scaling with cluster R200m, and the ICL brightness appears to be a good tracer of the cluster radial mass distribution. These analyses are based on the DES redMaPPer cluster sample identified in the first year of observations.</description><identifier>ISSN: 0004-637X</identifier><identifier>ISSN: 1538-4357</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ab0dfd</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>ASTRONOMY AND ASTROPHYSICS ; Astrophysics ; Dark energy ; Galactic clusters ; Galaxies ; galaxies: clusters: general ; galaxies: evolution ; Image detection ; Luminosity ; Mass distribution ; Point spread functions ; Red shift ; Self-similarity ; Sky surveys (astronomy) ; Stellar luminosity ; Subtraction ; Surface brightness</subject><ispartof>The Astrophysical journal, 2019-04, Vol.874 (2), p.165</ispartof><rights>2019. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Apr 01, 2019</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c443t-6d8035bbf6d7f937f8937dfd658afb033bbd13dd1f7abd9f23c0bf44de1c9c033</citedby><cites>FETCH-LOGICAL-c443t-6d8035bbf6d7f937f8937dfd658afb033bbd13dd1f7abd9f23c0bf44de1c9c033</cites><orcidid>0000-0001-6942-2736 ; 0000-0001-5969-4631 ; 0000-0002-6610-4836 ; 0000-0002-8134-9591 ; 0000-0002-9541-2678 ; 0000-0002-6011-0530 ; 0000-0002-4588-6517 ; 0000-0001-8251-933X ; 0000-0001-6082-8529 ; 0000-0002-9369-4157 ; 0000-0003-1704-0781 ; 0000000159694631 ; 0000000266104836 ; 0000000260110530 ; 000000018251933X ; 0000000293694157 ; 0000000317040781 ; 0000000245886517 ; 0000000281349591 ; 0000000169422736 ; 0000000160828529 ; 0000000295412678</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ab0dfd/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/ab0dfd$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://www.osti.gov/servlets/purl/1489389$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Zhang, Y.</creatorcontrib><creatorcontrib>Yanny, B.</creatorcontrib><creatorcontrib>Palmese, A.</creatorcontrib><creatorcontrib>Gruen, D.</creatorcontrib><creatorcontrib>To, C.</creatorcontrib><creatorcontrib>Rykoff, E. 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F.</creatorcontrib><creatorcontrib>Evrard, A. E.</creatorcontrib><creatorcontrib>Flaugher, B.</creatorcontrib><creatorcontrib>Fosalba, P.</creatorcontrib><creatorcontrib>Frieman, J.</creatorcontrib><creatorcontrib>García-Bellido, J.</creatorcontrib><creatorcontrib>Gaztanaga, E.</creatorcontrib><creatorcontrib>Gerdes, D. W.</creatorcontrib><creatorcontrib>Gruendl, R. A.</creatorcontrib><creatorcontrib>Gschwend, J.</creatorcontrib><creatorcontrib>Gutierrez, G.</creatorcontrib><creatorcontrib>Hartley, W. G.</creatorcontrib><creatorcontrib>Hollowood, D. L.</creatorcontrib><creatorcontrib>Honscheid, K.</creatorcontrib><creatorcontrib>Hoyle, B.</creatorcontrib><creatorcontrib>James, D. J.</creatorcontrib><creatorcontrib>Jeltema, T.</creatorcontrib><creatorcontrib>Kuehn, K.</creatorcontrib><creatorcontrib>Kuropatkin, N.</creatorcontrib><creatorcontrib>Li, T. S.</creatorcontrib><creatorcontrib>Lima, M.</creatorcontrib><creatorcontrib>Maia, M. A. G.</creatorcontrib><creatorcontrib>March, M.</creatorcontrib><creatorcontrib>Marshall, J. L.</creatorcontrib><creatorcontrib>Melchior, P.</creatorcontrib><creatorcontrib>Menanteau, F.</creatorcontrib><creatorcontrib>Miller, C. J.</creatorcontrib><creatorcontrib>Miquel, R.</creatorcontrib><creatorcontrib>Mohr, J. J.</creatorcontrib><creatorcontrib>Ogando, R. L. C.</creatorcontrib><creatorcontrib>Plazas, A. A.</creatorcontrib><creatorcontrib>Romer, A. K.</creatorcontrib><creatorcontrib>Sanchez, E.</creatorcontrib><creatorcontrib>Scarpine, V.</creatorcontrib><creatorcontrib>Schubnell, M.</creatorcontrib><creatorcontrib>Serrano, S.</creatorcontrib><creatorcontrib>Sevilla-Noarbe, I.</creatorcontrib><creatorcontrib>Smith, M.</creatorcontrib><creatorcontrib>Soares-Santos, M.</creatorcontrib><creatorcontrib>Sobreira, F.</creatorcontrib><creatorcontrib>Suchyta, E.</creatorcontrib><creatorcontrib>Swanson, M. E. C.</creatorcontrib><creatorcontrib>Tarle, G.</creatorcontrib><creatorcontrib>Thomas, D.</creatorcontrib><creatorcontrib>Wester, W.</creatorcontrib><creatorcontrib>DES Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Univ. of Michigan, Ann Arbor, MI (United States)</creatorcontrib><title>Dark Energy Survey Year 1 Results: Detection of Intracluster Light at Redshift ∼ 0.25</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>Using data collected by the Dark Energy Survey (DES), we report the detection of intracluster light (ICL) with ∼300 galaxy clusters in the redshift range of 0.2-0.3. We design methods to mask detected galaxies and stars in the images and stack the cluster light profiles, while accounting for several systematic effects (sky subtraction, instrumental point-spread function, cluster selection effects, and residual light in the ICL raw detection from background and cluster galaxies). The methods allow us to acquire high signal-to-noise measurements of the ICL and central galaxies (CGs), which we separate with radial cuts. The ICL appears as faint and diffuse light extending to at least 1 Mpc from the cluster center, reaching a surface brightness level of 30 mag arcsec−2. The ICL and the cluster CG contribute 44% 17% of the total cluster stellar luminosity within 1 Mpc. The ICL color is overall consistent with that of the cluster red sequence galaxies, but displays the trend of becoming bluer with increasing radius. The ICL demonstrates an interesting self-similarity feature-for clusters in different richness ranges, their ICL radial profiles are similar after scaling with cluster R200m, and the ICL brightness appears to be a good tracer of the cluster radial mass distribution. These analyses are based on the DES redMaPPer cluster sample identified in the first year of observations.</description><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Astrophysics</subject><subject>Dark energy</subject><subject>Galactic clusters</subject><subject>Galaxies</subject><subject>galaxies: clusters: general</subject><subject>galaxies: evolution</subject><subject>Image detection</subject><subject>Luminosity</subject><subject>Mass distribution</subject><subject>Point spread functions</subject><subject>Red shift</subject><subject>Self-similarity</subject><subject>Sky surveys (astronomy)</subject><subject>Stellar luminosity</subject><subject>Subtraction</subject><subject>Surface brightness</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNp1kMtKAzEUhoMoWKt7l0G3TptMMjd30lYtFAQvqKuQazu1TmqSEfoGPpRP45OYMqIrISSck-_85-cH4BijASlpMcQZKRNKsmLIBVJG7YDeb2sX9BBCNMlJ8bQPDrxfbsu0qnrgcczdC5w02s038K5173oDnzV3EMNb7dtV8OdwrIOWobYNtAZOm-C4XLU-aAdn9XwRIA-RVX5RmwC_Pj4hGqTZIdgzfOX10c_bBw-Xk_vRdTK7uZqOLmaJpJSEJFclIpkQJleFqUhhynhF93lWciMQIUIoTJTCpuBCVSYlEglDqdJYVjL-98FJp2t9qJmXdbS6kLZpomOGaZSLpw9OO2jt7FurfWBL27om-mIpiauKkuA8UqijpLPeO23Y2tWv3G0YRmybMdsGyraBsi7jOHLWjdR2_af5L_4NpmF-Eg</recordid><startdate>20190401</startdate><enddate>20190401</enddate><creator>Zhang, Y.</creator><creator>Yanny, B.</creator><creator>Palmese, A.</creator><creator>Gruen, D.</creator><creator>To, C.</creator><creator>Rykoff, E. 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C.</creator><creator>Tarle, G.</creator><creator>Thomas, D.</creator><creator>Wester, W.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><general>Institute of Physics (IOP)</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>OIOZB</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0001-6942-2736</orcidid><orcidid>https://orcid.org/0000-0001-5969-4631</orcidid><orcidid>https://orcid.org/0000-0002-6610-4836</orcidid><orcidid>https://orcid.org/0000-0002-8134-9591</orcidid><orcidid>https://orcid.org/0000-0002-9541-2678</orcidid><orcidid>https://orcid.org/0000-0002-6011-0530</orcidid><orcidid>https://orcid.org/0000-0002-4588-6517</orcidid><orcidid>https://orcid.org/0000-0001-8251-933X</orcidid><orcidid>https://orcid.org/0000-0001-6082-8529</orcidid><orcidid>https://orcid.org/0000-0002-9369-4157</orcidid><orcidid>https://orcid.org/0000-0003-1704-0781</orcidid><orcidid>https://orcid.org/0000000159694631</orcidid><orcidid>https://orcid.org/0000000266104836</orcidid><orcidid>https://orcid.org/0000000260110530</orcidid><orcidid>https://orcid.org/000000018251933X</orcidid><orcidid>https://orcid.org/0000000293694157</orcidid><orcidid>https://orcid.org/0000000317040781</orcidid><orcidid>https://orcid.org/0000000245886517</orcidid><orcidid>https://orcid.org/0000000281349591</orcidid><orcidid>https://orcid.org/0000000169422736</orcidid><orcidid>https://orcid.org/0000000160828529</orcidid><orcidid>https://orcid.org/0000000295412678</orcidid></search><sort><creationdate>20190401</creationdate><title>Dark Energy Survey Year 1 Results: Detection of Intracluster Light at Redshift ∼ 0.25</title><author>Zhang, Y. ; Yanny, B. ; Palmese, A. ; Gruen, D. ; To, C. ; Rykoff, E. S. ; Leung, Y. ; Collins, C. ; Hilton, M. ; Abbott, T. M. C. ; Annis, J. ; Avila, S. ; Bertin, E. ; Brooks, D. ; Burke, D. L. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; Cunha, C. E. ; D'Andrea, C. B. ; Costa, L. N. da ; Vicente, J. De ; Desai, S. ; Diehl, H. T. ; Dietrich, J. P. ; Doel, P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Evrard, A. E. ; Flaugher, B. ; Fosalba, P. ; Frieman, J. ; García-Bellido, J. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Hartley, W. G. ; Hollowood, D. L. ; Honscheid, K. ; Hoyle, B. ; James, D. J. ; Jeltema, T. ; Kuehn, K. ; Kuropatkin, N. ; Li, T. S. ; Lima, M. ; Maia, M. A. G. ; March, M. ; Marshall, J. L. ; Melchior, P. ; Menanteau, F. ; Miller, C. J. ; Miquel, R. ; Mohr, J. J. ; Ogando, R. L. C. ; Plazas, A. A. ; Romer, A. K. ; Sanchez, E. ; Scarpine, V. ; Schubnell, M. ; Serrano, S. ; Sevilla-Noarbe, I. ; Smith, M. ; Soares-Santos, M. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Thomas, D. ; Wester, W.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c443t-6d8035bbf6d7f937f8937dfd658afb033bbd13dd1f7abd9f23c0bf44de1c9c033</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Astrophysics</topic><topic>Dark energy</topic><topic>Galactic clusters</topic><topic>Galaxies</topic><topic>galaxies: clusters: general</topic><topic>galaxies: evolution</topic><topic>Image detection</topic><topic>Luminosity</topic><topic>Mass distribution</topic><topic>Point spread functions</topic><topic>Red shift</topic><topic>Self-similarity</topic><topic>Sky surveys (astronomy)</topic><topic>Stellar luminosity</topic><topic>Subtraction</topic><topic>Surface brightness</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Zhang, Y.</creatorcontrib><creatorcontrib>Yanny, B.</creatorcontrib><creatorcontrib>Palmese, A.</creatorcontrib><creatorcontrib>Gruen, D.</creatorcontrib><creatorcontrib>To, C.</creatorcontrib><creatorcontrib>Rykoff, E. S.</creatorcontrib><creatorcontrib>Leung, Y.</creatorcontrib><creatorcontrib>Collins, C.</creatorcontrib><creatorcontrib>Hilton, M.</creatorcontrib><creatorcontrib>Abbott, T. M. C.</creatorcontrib><creatorcontrib>Annis, J.</creatorcontrib><creatorcontrib>Avila, S.</creatorcontrib><creatorcontrib>Bertin, E.</creatorcontrib><creatorcontrib>Brooks, D.</creatorcontrib><creatorcontrib>Burke, D. L.</creatorcontrib><creatorcontrib>Rosell, A. Carnero</creatorcontrib><creatorcontrib>Kind, M. Carrasco</creatorcontrib><creatorcontrib>Carretero, J.</creatorcontrib><creatorcontrib>Cunha, C. E.</creatorcontrib><creatorcontrib>D'Andrea, C. B.</creatorcontrib><creatorcontrib>Costa, L. N. da</creatorcontrib><creatorcontrib>Vicente, J. De</creatorcontrib><creatorcontrib>Desai, S.</creatorcontrib><creatorcontrib>Diehl, H. T.</creatorcontrib><creatorcontrib>Dietrich, J. P.</creatorcontrib><creatorcontrib>Doel, P.</creatorcontrib><creatorcontrib>Drlica-Wagner, A.</creatorcontrib><creatorcontrib>Eifler, T. F.</creatorcontrib><creatorcontrib>Evrard, A. E.</creatorcontrib><creatorcontrib>Flaugher, B.</creatorcontrib><creatorcontrib>Fosalba, P.</creatorcontrib><creatorcontrib>Frieman, J.</creatorcontrib><creatorcontrib>García-Bellido, J.</creatorcontrib><creatorcontrib>Gaztanaga, E.</creatorcontrib><creatorcontrib>Gerdes, D. W.</creatorcontrib><creatorcontrib>Gruendl, R. A.</creatorcontrib><creatorcontrib>Gschwend, J.</creatorcontrib><creatorcontrib>Gutierrez, G.</creatorcontrib><creatorcontrib>Hartley, W. G.</creatorcontrib><creatorcontrib>Hollowood, D. L.</creatorcontrib><creatorcontrib>Honscheid, K.</creatorcontrib><creatorcontrib>Hoyle, B.</creatorcontrib><creatorcontrib>James, D. J.</creatorcontrib><creatorcontrib>Jeltema, T.</creatorcontrib><creatorcontrib>Kuehn, K.</creatorcontrib><creatorcontrib>Kuropatkin, N.</creatorcontrib><creatorcontrib>Li, T. S.</creatorcontrib><creatorcontrib>Lima, M.</creatorcontrib><creatorcontrib>Maia, M. A. G.</creatorcontrib><creatorcontrib>March, M.</creatorcontrib><creatorcontrib>Marshall, J. L.</creatorcontrib><creatorcontrib>Melchior, P.</creatorcontrib><creatorcontrib>Menanteau, F.</creatorcontrib><creatorcontrib>Miller, C. J.</creatorcontrib><creatorcontrib>Miquel, R.</creatorcontrib><creatorcontrib>Mohr, J. J.</creatorcontrib><creatorcontrib>Ogando, R. L. C.</creatorcontrib><creatorcontrib>Plazas, A. A.</creatorcontrib><creatorcontrib>Romer, A. K.</creatorcontrib><creatorcontrib>Sanchez, E.</creatorcontrib><creatorcontrib>Scarpine, V.</creatorcontrib><creatorcontrib>Schubnell, M.</creatorcontrib><creatorcontrib>Serrano, S.</creatorcontrib><creatorcontrib>Sevilla-Noarbe, I.</creatorcontrib><creatorcontrib>Smith, M.</creatorcontrib><creatorcontrib>Soares-Santos, M.</creatorcontrib><creatorcontrib>Sobreira, F.</creatorcontrib><creatorcontrib>Suchyta, E.</creatorcontrib><creatorcontrib>Swanson, M. E. C.</creatorcontrib><creatorcontrib>Tarle, G.</creatorcontrib><creatorcontrib>Thomas, D.</creatorcontrib><creatorcontrib>Wester, W.</creatorcontrib><creatorcontrib>DES Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Lab., Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Univ. of Michigan, Ann Arbor, MI (United States)</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Zhang, Y.</au><au>Yanny, B.</au><au>Palmese, A.</au><au>Gruen, D.</au><au>To, C.</au><au>Rykoff, E. S.</au><au>Leung, Y.</au><au>Collins, C.</au><au>Hilton, M.</au><au>Abbott, T. M. C.</au><au>Annis, J.</au><au>Avila, S.</au><au>Bertin, E.</au><au>Brooks, D.</au><au>Burke, D. L.</au><au>Rosell, A. Carnero</au><au>Kind, M. Carrasco</au><au>Carretero, J.</au><au>Cunha, C. E.</au><au>D'Andrea, C. B.</au><au>Costa, L. N. da</au><au>Vicente, J. De</au><au>Desai, S.</au><au>Diehl, H. T.</au><au>Dietrich, J. P.</au><au>Doel, P.</au><au>Drlica-Wagner, A.</au><au>Eifler, T. F.</au><au>Evrard, A. E.</au><au>Flaugher, B.</au><au>Fosalba, P.</au><au>Frieman, J.</au><au>García-Bellido, J.</au><au>Gaztanaga, E.</au><au>Gerdes, D. W.</au><au>Gruendl, R. A.</au><au>Gschwend, J.</au><au>Gutierrez, G.</au><au>Hartley, W. G.</au><au>Hollowood, D. L.</au><au>Honscheid, K.</au><au>Hoyle, B.</au><au>James, D. J.</au><au>Jeltema, T.</au><au>Kuehn, K.</au><au>Kuropatkin, N.</au><au>Li, T. S.</au><au>Lima, M.</au><au>Maia, M. A. G.</au><au>March, M.</au><au>Marshall, J. L.</au><au>Melchior, P.</au><au>Menanteau, F.</au><au>Miller, C. J.</au><au>Miquel, R.</au><au>Mohr, J. J.</au><au>Ogando, R. L. C.</au><au>Plazas, A. A.</au><au>Romer, A. K.</au><au>Sanchez, E.</au><au>Scarpine, V.</au><au>Schubnell, M.</au><au>Serrano, S.</au><au>Sevilla-Noarbe, I.</au><au>Smith, M.</au><au>Soares-Santos, M.</au><au>Sobreira, F.</au><au>Suchyta, E.</au><au>Swanson, M. E. C.</au><au>Tarle, G.</au><au>Thomas, D.</au><au>Wester, W.</au><aucorp>DES Collaboration</aucorp><aucorp>SLAC National Accelerator Lab., Menlo Park, CA (United States)</aucorp><aucorp>Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)</aucorp><aucorp>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</aucorp><aucorp>Univ. of Michigan, Ann Arbor, MI (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Dark Energy Survey Year 1 Results: Detection of Intracluster Light at Redshift ∼ 0.25</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2019-04-01</date><risdate>2019</risdate><volume>874</volume><issue>2</issue><spage>165</spage><pages>165-</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><abstract>Using data collected by the Dark Energy Survey (DES), we report the detection of intracluster light (ICL) with ∼300 galaxy clusters in the redshift range of 0.2-0.3. We design methods to mask detected galaxies and stars in the images and stack the cluster light profiles, while accounting for several systematic effects (sky subtraction, instrumental point-spread function, cluster selection effects, and residual light in the ICL raw detection from background and cluster galaxies). The methods allow us to acquire high signal-to-noise measurements of the ICL and central galaxies (CGs), which we separate with radial cuts. The ICL appears as faint and diffuse light extending to at least 1 Mpc from the cluster center, reaching a surface brightness level of 30 mag arcsec−2. The ICL and the cluster CG contribute 44% 17% of the total cluster stellar luminosity within 1 Mpc. The ICL color is overall consistent with that of the cluster red sequence galaxies, but displays the trend of becoming bluer with increasing radius. The ICL demonstrates an interesting self-similarity feature-for clusters in different richness ranges, their ICL radial profiles are similar after scaling with cluster R200m, and the ICL brightness appears to be a good tracer of the cluster radial mass distribution. These analyses are based on the DES redMaPPer cluster sample identified in the first year of observations.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ab0dfd</doi><tpages>19</tpages><orcidid>https://orcid.org/0000-0001-6942-2736</orcidid><orcidid>https://orcid.org/0000-0001-5969-4631</orcidid><orcidid>https://orcid.org/0000-0002-6610-4836</orcidid><orcidid>https://orcid.org/0000-0002-8134-9591</orcidid><orcidid>https://orcid.org/0000-0002-9541-2678</orcidid><orcidid>https://orcid.org/0000-0002-6011-0530</orcidid><orcidid>https://orcid.org/0000-0002-4588-6517</orcidid><orcidid>https://orcid.org/0000-0001-8251-933X</orcidid><orcidid>https://orcid.org/0000-0001-6082-8529</orcidid><orcidid>https://orcid.org/0000-0002-9369-4157</orcidid><orcidid>https://orcid.org/0000-0003-1704-0781</orcidid><orcidid>https://orcid.org/0000000159694631</orcidid><orcidid>https://orcid.org/0000000266104836</orcidid><orcidid>https://orcid.org/0000000260110530</orcidid><orcidid>https://orcid.org/000000018251933X</orcidid><orcidid>https://orcid.org/0000000293694157</orcidid><orcidid>https://orcid.org/0000000317040781</orcidid><orcidid>https://orcid.org/0000000245886517</orcidid><orcidid>https://orcid.org/0000000281349591</orcidid><orcidid>https://orcid.org/0000000169422736</orcidid><orcidid>https://orcid.org/0000000160828529</orcidid><orcidid>https://orcid.org/0000000295412678</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 0004-637X |
| ispartof | The Astrophysical journal, 2019-04, Vol.874 (2), p.165 |
| issn | 0004-637X 1538-4357 1538-4357 |
| language | eng |
| recordid | cdi_crossref_primary_10_3847_1538_4357_ab0dfd |
| source | IOP Publishing Free Content |
| subjects | ASTRONOMY AND ASTROPHYSICS Astrophysics Dark energy Galactic clusters Galaxies galaxies: clusters: general galaxies: evolution Image detection Luminosity Mass distribution Point spread functions Red shift Self-similarity Sky surveys (astronomy) Stellar luminosity Subtraction Surface brightness |
| title | Dark Energy Survey Year 1 Results: Detection of Intracluster Light at Redshift ∼ 0.25 |
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