The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles
Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The clustercentric radius at which this process occurs, rsp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid de...
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| Veröffentlicht in: | Astrophys.J 2018-09, Vol.864 (1), p.83 |
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| creator | Chang, C. Baxter, E. Jain, B. Sánchez, C. Adhikari, S. Varga, T. N. Fang, Y. Rozo, E. Rykoff, E. S. Kravtsov, A. Gruen, D. Hartley, W. Huff, E. M. Jarvis, M. Kim, A. G. Prat, J. MacCrann, N. McClintock, T. Palmese, A. Rapetti, D. Rollins, R. P. Samuroff, S. Sheldon, E. Troxel, M. A. Wechsler, R. H. Zhang, Y. Zuntz, J. Abbott, T. M. C. Abdalla, F. B. Allam, S. Annis, J. Bechtol, K. Benoit-Lévy, A. Bernstein, G. M. Brooks, D. Buckley-Geer, E. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. D'Andrea, C. B. Costa, L. N. da Davis, C. Desai, S. Diehl, H. T. Dietrich, J. P. Drlica-Wagner, A. Eifler, T. F. Flaugher, B. Fosalba, P. Frieman, J. García-Bellido, J. Gaztanaga, E. Gerdes, D. W. Gruendl, R. A. Gschwend, J. Gutierrez, G. Honscheid, K. James, D. J. Jeltema, T. Krause, E. Kuehn, K. Lahav, O. Lima, M. March, M. Marshall, J. L. Martini, P. Melchior, P. Menanteau, F. Miquel, R. Mohr, J. J. Nord, B. Ogando, R. L. C. Plazas, A. A. Sanchez, E. Scarpine, V. Schindler, R. Schubnell, M. Sevilla-Noarbe, I. Smith, M. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Swanson, M. E. C. Tarle, G. Weller, J. |
| description | Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The clustercentric radius at which this process occurs, rsp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near rsp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first-year Dark Energy Survey (DES) data. For a cluster sample with mean M200m mass 2.5 × 1014 M , we find strong evidence of a splashback-like steepening of the galaxy density profile and measure rsp = 1.13 0.07 h−1 Mpc, consistent with the earlier Sloan Digital Sky Survey measurements of More et al. and Baxter et al. Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure rsp = 1.34 0.21 h−1 Mpc from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that, consistent with ΛCDM simulations, rsp scales with R200m and does not evolve with redshift over the redshift range of 0.3-0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of rsp. We discuss the progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples. |
| doi_str_mv | 10.3847/1538-4357/aad5e7 |
| format | Article |
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N. ; Fang, Y. ; Rozo, E. ; Rykoff, E. S. ; Kravtsov, A. ; Gruen, D. ; Hartley, W. ; Huff, E. M. ; Jarvis, M. ; Kim, A. G. ; Prat, J. ; MacCrann, N. ; McClintock, T. ; Palmese, A. ; Rapetti, D. ; Rollins, R. P. ; Samuroff, S. ; Sheldon, E. ; Troxel, M. A. ; Wechsler, R. H. ; Zhang, Y. ; Zuntz, J. ; Abbott, T. M. C. ; Abdalla, F. B. ; Allam, S. ; Annis, J. ; Bechtol, K. ; Benoit-Lévy, A. ; Bernstein, G. M. ; Brooks, D. ; Buckley-Geer, E. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; D'Andrea, C. B. ; Costa, L. N. da ; Davis, C. ; Desai, S. ; Diehl, H. T. ; Dietrich, J. P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Flaugher, B. ; Fosalba, P. ; Frieman, J. ; García-Bellido, J. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Honscheid, K. ; James, D. J. ; Jeltema, T. ; Krause, E. ; Kuehn, K. ; Lahav, O. ; Lima, M. ; March, M. ; Marshall, J. L. ; Martini, P. ; Melchior, P. ; Menanteau, F. ; Miquel, R. ; Mohr, J. J. ; Nord, B. ; Ogando, R. L. C. ; Plazas, A. A. ; Sanchez, E. ; Scarpine, V. ; Schindler, R. ; Schubnell, M. ; Sevilla-Noarbe, I. ; Smith, M. ; Smith, R. C. ; Soares-Santos, M. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Weller, J.</creator><creatorcontrib>Chang, C. ; Baxter, E. ; Jain, B. ; Sánchez, C. ; Adhikari, S. ; Varga, T. N. ; Fang, Y. ; Rozo, E. ; Rykoff, E. S. ; Kravtsov, A. ; Gruen, D. ; Hartley, W. ; Huff, E. M. ; Jarvis, M. ; Kim, A. G. ; Prat, J. ; MacCrann, N. ; McClintock, T. ; Palmese, A. ; Rapetti, D. ; Rollins, R. P. ; Samuroff, S. ; Sheldon, E. ; Troxel, M. A. ; Wechsler, R. H. ; Zhang, Y. ; Zuntz, J. ; Abbott, T. M. C. ; Abdalla, F. B. ; Allam, S. ; Annis, J. ; Bechtol, K. ; Benoit-Lévy, A. ; Bernstein, G. M. ; Brooks, D. ; Buckley-Geer, E. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; D'Andrea, C. B. ; Costa, L. N. da ; Davis, C. ; Desai, S. ; Diehl, H. T. ; Dietrich, J. P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Flaugher, B. ; Fosalba, P. ; Frieman, J. ; García-Bellido, J. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Honscheid, K. ; James, D. J. ; Jeltema, T. ; Krause, E. ; Kuehn, K. ; Lahav, O. ; Lima, M. ; March, M. ; Marshall, J. L. ; Martini, P. ; Melchior, P. ; Menanteau, F. ; Miquel, R. ; Mohr, J. J. ; Nord, B. ; Ogando, R. L. C. ; Plazas, A. A. ; Sanchez, E. ; Scarpine, V. ; Schindler, R. ; Schubnell, M. ; Sevilla-Noarbe, I. ; Smith, M. ; Smith, R. C. ; Soares-Santos, M. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Weller, J. ; DES Collaboration ; SLAC National Accelerator Lab., Menlo Park, CA (United States) ; Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States) ; Brookhaven National Lab. (BNL), Upton, NY (United States) ; Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States) ; Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><description>Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The clustercentric radius at which this process occurs, rsp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near rsp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first-year Dark Energy Survey (DES) data. For a cluster sample with mean M200m mass 2.5 × 1014 M , we find strong evidence of a splashback-like steepening of the galaxy density profile and measure rsp = 1.13 0.07 h−1 Mpc, consistent with the earlier Sloan Digital Sky Survey measurements of More et al. and Baxter et al. Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure rsp = 1.34 0.21 h−1 Mpc from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that, consistent with ΛCDM simulations, rsp scales with R200m and does not evolve with redshift over the redshift range of 0.3-0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of rsp. We discuss the progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples.</description><identifier>ISSN: 0004-637X</identifier><identifier>ISSN: 1538-4357</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aad5e7</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Algorithms ; ASTRONOMY AND ASTROPHYSICS ; Astrophysics ; Computer simulation ; cosmology: observations ; Dark energy ; Dark matter ; Density ; Deposition ; Galactic clusters ; Galaxies ; galaxies: clusters: general ; galaxies: halos ; gravitational lensing: weak ; Milky Way ; Physics ; Red shift ; Sky surveys (astronomy) ; Stars & galaxies</subject><ispartof>Astrophys.J, 2018-09, Vol.864 (1), p.83</ispartof><rights>2018. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Sep 01, 2018</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c477t-91f016e2ea75f1363b7972b850fefac33b12ca9e065f5daa4deab0f888cdd9ec3</citedby><cites>FETCH-LOGICAL-c477t-91f016e2ea75f1363b7972b850fefac33b12ca9e065f5daa4deab0f888cdd9ec3</cites><orcidid>0000-0002-8873-5065 ; 0000-0002-4588-6517 ; 0000-0003-3270-7644 ; 0000-0002-7887-0896 ; 0000-0002-9378-3424 ; 0000-0003-1704-0781 ; 0000-0001-5303-6830 ; 0000-0003-2229-011X ; 0000-0002-6610-4836 ; 0000-0001-8251-933X ; 0000-0002-6011-0530 ; 0000-0003-3044-5150 ; 0000-0002-6836-3196 ; 0000-0002-0609-3987 ; 0000-0003-4307-634X ; 0000-0003-2196-6675 ; 0000-0001-6706-8972 ; 0000-0001-6942-2736 ; 0000-0001-9376-3135 ; 0000-0002-4279-4182 ; 0000-0001-6082-8529 ; 0000-0001-7039-9078 ; 0000-0002-1510-5214 ; 0000000193763135 ; 0000000167068972 ; 0000000332707644 ; 0000000160828529 ; 0000000169422736 ; 000000018251933X ; 0000000288735065 ; 0000000260110530 ; 000000034307634X ; 0000000242794182 ; 0000000317040781 ; 0000000330445150 ; 0000000153036830 ; 0000000245886517 ; 0000000266104836 ; 0000000278870896 ; 0000000268363196 ; 000000032229011X ; 0000000206093987 ; 0000000293783424 ; 0000000321966675</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/aad5e7/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,776,780,881,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aad5e7$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://hal.science/hal-01872309$$DView record in HAL$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/servlets/purl/1409347$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Chang, C.</creatorcontrib><creatorcontrib>Baxter, E.</creatorcontrib><creatorcontrib>Jain, B.</creatorcontrib><creatorcontrib>Sánchez, C.</creatorcontrib><creatorcontrib>Adhikari, S.</creatorcontrib><creatorcontrib>Varga, T. 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C.</creatorcontrib><creatorcontrib>Tarle, G.</creatorcontrib><creatorcontrib>Weller, J.</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>Brookhaven National Lab. (BNL), Upton, NY (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</creatorcontrib><title>The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles</title><title>Astrophys.J</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The clustercentric radius at which this process occurs, rsp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near rsp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first-year Dark Energy Survey (DES) data. For a cluster sample with mean M200m mass 2.5 × 1014 M , we find strong evidence of a splashback-like steepening of the galaxy density profile and measure rsp = 1.13 0.07 h−1 Mpc, consistent with the earlier Sloan Digital Sky Survey measurements of More et al. and Baxter et al. Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure rsp = 1.34 0.21 h−1 Mpc from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that, consistent with ΛCDM simulations, rsp scales with R200m and does not evolve with redshift over the redshift range of 0.3-0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of rsp. We discuss the progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples.</description><subject>Algorithms</subject><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>Astrophysics</subject><subject>Computer simulation</subject><subject>cosmology: observations</subject><subject>Dark energy</subject><subject>Dark matter</subject><subject>Density</subject><subject>Deposition</subject><subject>Galactic clusters</subject><subject>Galaxies</subject><subject>galaxies: clusters: general</subject><subject>galaxies: halos</subject><subject>gravitational lensing: weak</subject><subject>Milky Way</subject><subject>Physics</subject><subject>Red shift</subject><subject>Sky surveys (astronomy)</subject><subject>Stars & galaxies</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kU1LxDAQhoMouH7cPQY9CVaTpm0ab7J-woKCioKHME0nbrU2a9KK--9tqR8nT8O8PPPC8BCyw9mhyBN5xFORR4lI5RFAmaJcIZPfaJVMGGNJlAn5uE42QngZ1lipCXm6myO9XdQQ5gWYV3qO0HYeKXjXNSU9PbulF1DD55JO6y606MPxT3CKTajaJYWee0B4pbMhaJ7pjXe2qjFskTULdcDt77lJ7s_P7qaX0ez64mp6MotMImUbKW4ZzzBGkKnlIhOFVDIu8pRZtGCEKHhsQCHLUpuWAEmJUDCb57kpS4VGbJLdsdeFttLBVC2auXFNg6bVPGFKJLKH9kdoDrVe-OoN_FI7qPTlyUwPGeO5jAVTH7xn90Z24d17h6HVL67zTf-DjkWWKpFxMVBspIx3IXi0v7Wc6cGJHgToQYAenfQnB-NJ5RZ_nf_iX7CUjIY</recordid><startdate>20180901</startdate><enddate>20180901</enddate><creator>Chang, C.</creator><creator>Baxter, E.</creator><creator>Jain, B.</creator><creator>Sánchez, C.</creator><creator>Adhikari, S.</creator><creator>Varga, T. 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N. ; Fang, Y. ; Rozo, E. ; Rykoff, E. S. ; Kravtsov, A. ; Gruen, D. ; Hartley, W. ; Huff, E. M. ; Jarvis, M. ; Kim, A. G. ; Prat, J. ; MacCrann, N. ; McClintock, T. ; Palmese, A. ; Rapetti, D. ; Rollins, R. P. ; Samuroff, S. ; Sheldon, E. ; Troxel, M. A. ; Wechsler, R. H. ; Zhang, Y. ; Zuntz, J. ; Abbott, T. M. C. ; Abdalla, F. B. ; Allam, S. ; Annis, J. ; Bechtol, K. ; Benoit-Lévy, A. ; Bernstein, G. M. ; Brooks, D. ; Buckley-Geer, E. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; D'Andrea, C. B. ; Costa, L. N. da ; Davis, C. ; Desai, S. ; Diehl, H. T. ; Dietrich, J. P. ; Drlica-Wagner, A. ; Eifler, T. F. ; Flaugher, B. ; Fosalba, P. ; Frieman, J. ; García-Bellido, J. ; Gaztanaga, E. ; Gerdes, D. W. ; Gruendl, R. A. ; Gschwend, J. ; Gutierrez, G. ; Honscheid, K. ; James, D. J. ; Jeltema, T. ; Krause, E. ; Kuehn, K. ; Lahav, O. ; Lima, M. ; March, M. ; Marshall, J. L. ; Martini, P. ; Melchior, P. ; Menanteau, F. ; Miquel, R. ; Mohr, J. J. ; Nord, B. ; Ogando, R. L. C. ; Plazas, A. A. ; Sanchez, E. ; Scarpine, V. ; Schindler, R. ; Schubnell, M. ; Sevilla-Noarbe, I. ; Smith, M. ; Smith, R. C. ; Soares-Santos, M. ; Sobreira, F. ; Suchyta, E. ; Swanson, M. E. C. ; Tarle, G. ; Weller, J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c477t-91f016e2ea75f1363b7972b850fefac33b12ca9e065f5daa4deab0f888cdd9ec3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Algorithms</topic><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>Astrophysics</topic><topic>Computer simulation</topic><topic>cosmology: observations</topic><topic>Dark energy</topic><topic>Dark matter</topic><topic>Density</topic><topic>Deposition</topic><topic>Galactic clusters</topic><topic>Galaxies</topic><topic>galaxies: clusters: general</topic><topic>galaxies: halos</topic><topic>gravitational lensing: weak</topic><topic>Milky Way</topic><topic>Physics</topic><topic>Red shift</topic><topic>Sky surveys (astronomy)</topic><topic>Stars & galaxies</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Chang, C.</creatorcontrib><creatorcontrib>Baxter, E.</creatorcontrib><creatorcontrib>Jain, B.</creatorcontrib><creatorcontrib>Sánchez, C.</creatorcontrib><creatorcontrib>Adhikari, S.</creatorcontrib><creatorcontrib>Varga, T. 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C.</creatorcontrib><creatorcontrib>Abdalla, F. B.</creatorcontrib><creatorcontrib>Allam, S.</creatorcontrib><creatorcontrib>Annis, J.</creatorcontrib><creatorcontrib>Bechtol, K.</creatorcontrib><creatorcontrib>Benoit-Lévy, A.</creatorcontrib><creatorcontrib>Bernstein, G. M.</creatorcontrib><creatorcontrib>Brooks, D.</creatorcontrib><creatorcontrib>Buckley-Geer, E.</creatorcontrib><creatorcontrib>Rosell, A. Carnero</creatorcontrib><creatorcontrib>Kind, M. Carrasco</creatorcontrib><creatorcontrib>Carretero, J.</creatorcontrib><creatorcontrib>D'Andrea, C. B.</creatorcontrib><creatorcontrib>Costa, L. N. da</creatorcontrib><creatorcontrib>Davis, C.</creatorcontrib><creatorcontrib>Desai, S.</creatorcontrib><creatorcontrib>Diehl, H. T.</creatorcontrib><creatorcontrib>Dietrich, J. P.</creatorcontrib><creatorcontrib>Drlica-Wagner, A.</creatorcontrib><creatorcontrib>Eifler, T. 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L.</creatorcontrib><creatorcontrib>Martini, P.</creatorcontrib><creatorcontrib>Melchior, P.</creatorcontrib><creatorcontrib>Menanteau, F.</creatorcontrib><creatorcontrib>Miquel, R.</creatorcontrib><creatorcontrib>Mohr, J. J.</creatorcontrib><creatorcontrib>Nord, B.</creatorcontrib><creatorcontrib>Ogando, R. L. C.</creatorcontrib><creatorcontrib>Plazas, A. A.</creatorcontrib><creatorcontrib>Sanchez, E.</creatorcontrib><creatorcontrib>Scarpine, V.</creatorcontrib><creatorcontrib>Schindler, R.</creatorcontrib><creatorcontrib>Schubnell, M.</creatorcontrib><creatorcontrib>Sevilla-Noarbe, I.</creatorcontrib><creatorcontrib>Smith, M.</creatorcontrib><creatorcontrib>Smith, R. C.</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>Weller, J.</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>Brookhaven National Lab. (BNL), Upton, NY (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (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>Hyper Article en Ligne (HAL)</collection><collection>OSTI.GOV - Hybrid</collection><collection>OSTI.GOV</collection><jtitle>Astrophys.J</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Chang, C.</au><au>Baxter, E.</au><au>Jain, B.</au><au>Sánchez, C.</au><au>Adhikari, S.</au><au>Varga, T. N.</au><au>Fang, Y.</au><au>Rozo, E.</au><au>Rykoff, E. S.</au><au>Kravtsov, A.</au><au>Gruen, D.</au><au>Hartley, W.</au><au>Huff, E. M.</au><au>Jarvis, M.</au><au>Kim, A. G.</au><au>Prat, J.</au><au>MacCrann, N.</au><au>McClintock, T.</au><au>Palmese, A.</au><au>Rapetti, D.</au><au>Rollins, R. P.</au><au>Samuroff, S.</au><au>Sheldon, E.</au><au>Troxel, M. A.</au><au>Wechsler, R. H.</au><au>Zhang, Y.</au><au>Zuntz, J.</au><au>Abbott, T. M. C.</au><au>Abdalla, F. B.</au><au>Allam, S.</au><au>Annis, J.</au><au>Bechtol, K.</au><au>Benoit-Lévy, A.</au><au>Bernstein, G. M.</au><au>Brooks, D.</au><au>Buckley-Geer, E.</au><au>Rosell, A. Carnero</au><au>Kind, M. Carrasco</au><au>Carretero, J.</au><au>D'Andrea, C. B.</au><au>Costa, L. N. da</au><au>Davis, C.</au><au>Desai, S.</au><au>Diehl, H. T.</au><au>Dietrich, J. P.</au><au>Drlica-Wagner, A.</au><au>Eifler, T. F.</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>Honscheid, K.</au><au>James, D. J.</au><au>Jeltema, T.</au><au>Krause, E.</au><au>Kuehn, K.</au><au>Lahav, O.</au><au>Lima, M.</au><au>March, M.</au><au>Marshall, J. L.</au><au>Martini, P.</au><au>Melchior, P.</au><au>Menanteau, F.</au><au>Miquel, R.</au><au>Mohr, J. J.</au><au>Nord, B.</au><au>Ogando, R. L. C.</au><au>Plazas, A. A.</au><au>Sanchez, E.</au><au>Scarpine, V.</au><au>Schindler, R.</au><au>Schubnell, M.</au><au>Sevilla-Noarbe, I.</au><au>Smith, M.</au><au>Smith, R. C.</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>Weller, J.</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>Brookhaven National Lab. (BNL), Upton, NY (United States)</aucorp><aucorp>Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)</aucorp><aucorp>Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles</atitle><jtitle>Astrophys.J</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2018-09-01</date><risdate>2018</risdate><volume>864</volume><issue>1</issue><spage>83</spage><pages>83-</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><abstract>Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The clustercentric radius at which this process occurs, rsp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near rsp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first-year Dark Energy Survey (DES) data. For a cluster sample with mean M200m mass 2.5 × 1014 M , we find strong evidence of a splashback-like steepening of the galaxy density profile and measure rsp = 1.13 0.07 h−1 Mpc, consistent with the earlier Sloan Digital Sky Survey measurements of More et al. and Baxter et al. Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure rsp = 1.34 0.21 h−1 Mpc from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that, consistent with ΛCDM simulations, rsp scales with R200m and does not evolve with redshift over the redshift range of 0.3-0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of rsp. We discuss the progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/aad5e7</doi><tpages>18</tpages><orcidid>https://orcid.org/0000-0002-8873-5065</orcidid><orcidid>https://orcid.org/0000-0002-4588-6517</orcidid><orcidid>https://orcid.org/0000-0003-3270-7644</orcidid><orcidid>https://orcid.org/0000-0002-7887-0896</orcidid><orcidid>https://orcid.org/0000-0002-9378-3424</orcidid><orcidid>https://orcid.org/0000-0003-1704-0781</orcidid><orcidid>https://orcid.org/0000-0001-5303-6830</orcidid><orcidid>https://orcid.org/0000-0003-2229-011X</orcidid><orcidid>https://orcid.org/0000-0002-6610-4836</orcidid><orcidid>https://orcid.org/0000-0001-8251-933X</orcidid><orcidid>https://orcid.org/0000-0002-6011-0530</orcidid><orcidid>https://orcid.org/0000-0003-3044-5150</orcidid><orcidid>https://orcid.org/0000-0002-6836-3196</orcidid><orcidid>https://orcid.org/0000-0002-0609-3987</orcidid><orcidid>https://orcid.org/0000-0003-4307-634X</orcidid><orcidid>https://orcid.org/0000-0003-2196-6675</orcidid><orcidid>https://orcid.org/0000-0001-6706-8972</orcidid><orcidid>https://orcid.org/0000-0001-6942-2736</orcidid><orcidid>https://orcid.org/0000-0001-9376-3135</orcidid><orcidid>https://orcid.org/0000-0002-4279-4182</orcidid><orcidid>https://orcid.org/0000-0001-6082-8529</orcidid><orcidid>https://orcid.org/0000-0001-7039-9078</orcidid><orcidid>https://orcid.org/0000-0002-1510-5214</orcidid><orcidid>https://orcid.org/0000000193763135</orcidid><orcidid>https://orcid.org/0000000167068972</orcidid><orcidid>https://orcid.org/0000000332707644</orcidid><orcidid>https://orcid.org/0000000160828529</orcidid><orcidid>https://orcid.org/0000000169422736</orcidid><orcidid>https://orcid.org/000000018251933X</orcidid><orcidid>https://orcid.org/0000000288735065</orcidid><orcidid>https://orcid.org/0000000260110530</orcidid><orcidid>https://orcid.org/000000034307634X</orcidid><orcidid>https://orcid.org/0000000242794182</orcidid><orcidid>https://orcid.org/0000000317040781</orcidid><orcidid>https://orcid.org/0000000330445150</orcidid><orcidid>https://orcid.org/0000000153036830</orcidid><orcidid>https://orcid.org/0000000245886517</orcidid><orcidid>https://orcid.org/0000000266104836</orcidid><orcidid>https://orcid.org/0000000278870896</orcidid><orcidid>https://orcid.org/0000000268363196</orcidid><orcidid>https://orcid.org/000000032229011X</orcidid><orcidid>https://orcid.org/0000000206093987</orcidid><orcidid>https://orcid.org/0000000293783424</orcidid><orcidid>https://orcid.org/0000000321966675</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | ISSN: 0004-637X |
| ispartof | Astrophys.J, 2018-09, Vol.864 (1), p.83 |
| issn | 0004-637X 1538-4357 1538-4357 |
| language | eng |
| recordid | cdi_proquest_journals_2365936131 |
| source | IOP Publishing Free Content |
| subjects | Algorithms ASTRONOMY AND ASTROPHYSICS Astrophysics Computer simulation cosmology: observations Dark energy Dark matter Density Deposition Galactic clusters Galaxies galaxies: clusters: general galaxies: halos gravitational lensing: weak Milky Way Physics Red shift Sky surveys (astronomy) Stars & galaxies |
| title | The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles |
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