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251. Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution?

Author

R. L. C. Ogando, Brian Yanny, Enrique Gaztanaga, Antonella Palmese, E. Suchyta, S. Everett, August E. Evrard, M. A. G. Maia, Matt Hilton, Tesla E. Jeltema, A. Choi, J. Carretero, Douglas L. Tucker, Kyler Kuehn, G. Tarle, K. Honscheid, M. Costanzi, Michel Aguena, J. Gschwend, David J. James, M. Carrasco Kind, Ofer Lahav, D. L. Burke, Pablo Fosalba, Scarpine, Markus Rau, Chang Chihway, B. Flaugher, S. Allam, Robert A. Gruendl, T. M. C. Abbott, D. L. Hollowood, David J. Brooks, A. A. Plazas, M. March, Basilio X. Santiago, Ben Hoyle, Josh Frieman, Jesse B. Golden-Marx, J. Annis, J. De Vicente, E. J. Sanchez, Mohr Joe, N. Kuropatkin, T. N. Varga, L. N. da Costa, Santiago Avila, Chihway Chang, Jennifer L. Marshall, F. Paz-Chinchón, Michael Schubnell, H. Sampaio-Santos, Pagul Amanda, Joe Zuntz, M. Smith, Daniel Gruen, T. Shin, D. W. Gerdes, M. Gatti, Samuel Hinton, G. Gutierrez, Risa H. Wechsler, Matt J. Jarvis, Yanxi Zhang, Ramon Miquel, E. Bertin, Peter Doel, K. Herner, H. T. Diehl, Juan Garcia-Bellido, Sampaio-Santos, H., Zhang, Y., Ogando, R. L. C., Shin, T., Golden-Marx, Jesse B., Yanny, B., Herner, K., Hilton, M., Choi, A., Gatti, M., Gruen, D., Hoyle, B., Rau, M. M., De Vicente, J., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Marshall, J. L., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Tucker, D. L., Varga, T. N., Wechsler, R. H., UAM. Departamento de Física Teórica, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
galaxies: clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Evolution, galaxies: photometry, dark matter, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Optical Light, Luminosity, Clusters, Photometry, Astrophysics - Astrophysics of Galaxie, Clusters: General [Galaxies], Stellar Haloes, 0103 physical sciences, Cluster (physics), Galaxy formation and evolution, Satellite galaxy, Galaxies: Photometry, Dark Matter, Surface brightness, General, 010303 astronomy & astrophysics, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Dark Energy Survey, Física, Astronomy and Astrophysics, Illustristng Simulations, Mass, Galaxies, Galaxy, Space and Planetary Science, cluster [galaxies], Astrophysics of Galaxies (astro-ph.GA), Calibration, photometry [galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: Clusters: General
Abstract

We explore the relation between diffuse intracluster light (central galaxy included) and the galaxy cluster (baryonic and dark) matter distribution using a sample of 528 clusters at $0.2\leq z \leq 0.35$ found in the Dark Energy Survey (DES) Year 1 data. The surface brightness of the diffuse light shows an increasing dependence on cluster total mass at larger radius, and appears to be self-similar with a universal radial dependence after scaling by cluster radius. We also compare the diffuse light radial profiles to the cluster (baryonic and dark) matter distribution measured through weak lensing and find them to be comparable. The IllustrisTNG galaxy formation simulation, TNG300, offers further insight into the connection between diffuse stellar mass and cluster matter distributions -- the simulation radial profile of the diffuse stellar component does not have a similar slope with the total cluster matter content, although that of the cluster satellite galaxies does. Regardless of the radial trends, the amount of diffuse stellar mass has a low-scatter scaling relation with cluster's total mass in the simulation, out-performing the total stellar mass of cluster satellite galaxies. We conclude that there is no consistent evidence yet on whether or not diffuse light is a faithful radial tracer of the cluster matter distribution. Nevertheless, both observational and simulation results reveal that diffuse light is an excellent indicator of the cluster's total mass., Comment: Accepted on MNRAS

Published
2020
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252. Milky Way Satellite Census -- II. Galaxy-Halo Connection Constraints Including the Impact of the Large Magellanic Cloud

Author

Nadler, E.O., Wechsler, R.H., Bechtol, K., Mao, Y.-Y., Green, G., Drlica-Wagner, A., McNanna, M., Mau, S., Pace, A.B., Simon, J.D., Kravtsov, A., Dodelson, S., Li, T.S., Riley, A.H., Wang, M.Y., Abbott, T.M.C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G.M., Bertin, E., Brooks, D., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L.N., De Vicente, J., Desai, S., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W.G., Hinton, S.R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M.A.G., Marshall, J.L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A.A., Romer, A.K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T.N., Walker, A.R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Kavli Institute for Particle Astrophysics and Cosmology, National Aeronautics and Space Administration (US), Department of Energy (US), Ministerio de Ciencia e Innovación (España), Science and Technology Facilities Council (UK), University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Generalitat de Catalunya, Nadler, E. O., Wechsler, R. H., Bechtol, K., Mao, Y. -Y., Green, G., Drlica-Wagner, A., Mcnanna, M., Mau, S., Pace, A. B., Simon, J. D., Kravtsov, A., Dodelson, S., T. S., Li, Riley, A. H., Wang, M. Y., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T. N., and Walker, A. R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Virial theorem, Galactic halo, Galaxy abundances, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Milky Way dark matter halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, Physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The population of Milky Way (MW) satellites contains the faintest known galaxies and thus provides essential insight into galaxy formation and dark matter microphysics. Here we combine a model of the galaxy-halo connection with newly derived observational selection functions based on searches for satellites in photometric surveys over nearly the entire high Galactic latitude sky. In particular, we use cosmological zoom-in simulations of MW-like halos that include realistic Large Magellanic Cloud (LMC) analogs to fit the position-dependent MW satellite luminosity function. We report decisive evidence for the statistical impact of the LMC on the MW satellite population due to an estimated 6 ± 2 observed LMC-associated satellites, consistent with the number of LMC satellites inferred from Gaia proper-motion measurements, confirming the predictions of cold dark matter models for the existence of satellites within satellite halos. Moreover, we infer that the LMC fell into the MW within the last 2 Gyr at high confidence. Based on our detailed full-sky modeling, we find that the faintest observed satellites inhabit halos with peak virial masses below 3.2× 10 M· at 95% confidence, and we place the first robust constraints on the fraction of halos that host galaxies in this regime. We predict that the faintest detectable satellites occupy halos with peak virial masses above 10 M·, highlighting the potential for powerful galaxy formation and dark matter constraints from future dwarf galaxy searches., This research received support from the National Science Foundation (NSF) under grant No. NSF AST-1517422, grant No. NSF PHY17-48958 through the Kavli Institute for Theoretical Physics program “The Small-Scale Structure of Cold(?) Dark Matter,” and grant No. NSF DGE-1656518 through the NSF Graduate Research Fellowship received by E.O.N. Support for Y.-Y.M. was provided by the Pittsburgh Particle Physics, Astrophysics and Cosmology Center through the Samuel P. Langley PITT PACC Postdoctoral Fellowship and NASA through NASA Hubble Fellowship grant No. HST-HF2-51441.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Part of this work was performed at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. This research made use of computational resources at SLAC National Accelerator Laboratory, a U.S. Department of Energy Office; the authors are thankful for the support of the SLAC computational team. This research made use of the Sherlock cluster at the Stanford Research Computing Center (SRCC); the authors are thankful for the support of the SRCC team. This research made use of https://arXiv.org and NASA’s Astrophysics Data System for bibliographic information. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the NSFʼs National Optical-Infrared Astronomy Laboratory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This work is based in part on observations at Cerro Tololo Inter-American Observatory, NSFʼs National Optical-Infrared Astronomy Laboratory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. The IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/ 2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by the Fermi Research Alliance, LLC, under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2019

253. Reducing Ground-based Astrometric Errors with Gaia and Gaussian Processes

Author

J. Frieman, I. Sevilla-Noarbe, A. E. Evrard, S. Bhargava, J. De Vicente, E. Suchyta, G. Tarle, Maria E. S. Pereira, J. Carretero, Pedro H. Bernardinelli, M. Costanzi, Jochen Weller, David James, A. Roodman, William Wester, Kyler Kuehn, Basilio X. Santiago, P. Doel, Chun-Hao To, L. N. da Costa, Keith Bechtol, A. R. Walker, M. S. Schubnell, V. Scarpine, William G. Hartley, N. P. Kuropatkin, S. Desai, M. Smith, A. A. Plazas, M. Aguena, Alex Drlica-Wagner, Enrique Gaztanaga, J. L. Marshall, M. A. G. Maia, Ricardo L. C. Ogando, M. Jarvis, Ami Choi, I. Ferrero, David Bacon, Tim Eifler, Sahar S. Allam, Stephen M. Kent, D. W. Gerdes, Antonella Palmese, Douglas L. Tucker, T. N. Varga, Robert Morgan, J. Gschwend, K. Eckert, Gary Bernstein, Robert A. Gruendl, Devon L. Hollowood, W. F. Fortino, F. Paz-Chinchón, D. Brooks, Juan Garcia-Bellido, Santiago Serrano, K. Honscheid, Eli S. Rykoff, D. L. Burke, James Annis, G. Gutierrez, Ramon Miquel, J. Myles, Felipe Menanteau, E. J. Sanchez, Samuel Hinton, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Fortino, W. F., Bernstein, G. M., Bernardinelli, P. H., Aguena, M., Allam, S., Annis, J., Bacon, D., Bechtol, K., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Choi, A., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Evrard, A. E., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Kent, S., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Varga, T. N., Walker, A. R., Weller, J., and Wester, W.

Subjects
Field (physics), FOS: Physical sciences, Astrometry, Sky noise, Astronomy data analysis, 80, 1463, 1858, Astrophysics - Instrumentation and Methods for Astrophysics, 01 natural sciences, Physics::Geophysics, symbols.namesake, Kriging, Distortion, 0103 physical sciences, Astronometry, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Gaussian process, Astrophysics::Galaxy Astrophysics, Physics, 05 social sciences, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy data analysi, 050301 education, Astronomy and Astrophysics, Geodesy, Stars, Space and Planetary Science, Ground-penetrating radar, Orbit (dynamics), symbols, Astrophysics::Earth and Planetary Astrophysics, 0503 education
Abstract

Fortino, W. F., et al. DES Collaboration, Stochastic field distortions caused by atmospheric turbulence are a fundamental limitation to the astrometric accuracy of ground-based imaging. This distortion field is measurable at the locations of stars with accurate positions provided by the Gaia DR2 catalog; we develop the use of Gaussian process regression (GPR) to interpolate the distortion field to arbitrary locations in each exposure. We introduce an extension to standard GPR techniques that exploits the knowledge that the 2D distortion field is curl-free. Applied to several hundred 90 s exposures from the Dark Energy Survey as a test bed, we find that the GPR correction reduces the variance of the turbulent astrometric distortions ≈12× , on average, with better performance in denser regions of the Gaia catalog. The rms per-coordinate distortion in the riz bands is typically ≈7 mas before any correction and ≈2 mas after application of the GPR model. The GPR astrometric corrections are validated by the observation that their use reduces, from 10 to 5 mas rms, the residuals to an orbit fit to riz-band observations over 5 yr of the r = 18.5 trans-Neptunian object Eris. We also propose a GPR method, not yet implemented, for simultaneously estimating the turbulence fields and the 5D stellar solutions in a stack of overlapping exposures, which should yield further turbulence reductions in future deep surveys., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018- 094773, PGC2018-102021, SEV-2016-0588, SEV-2016- 0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciˆencia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02- 07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2021

254. A Detection of CMB-Cluster Lensing using Polarization Data from SPTpol

Author

Benjamin Saliwanchik, C. L. Chang, V. G. Yefremenko, Sebastian Bocquet, C. Corbett Moran, Devon L. Hollowood, J. A. Beall, N. Huang, Jessica Avva, A. E. Lowitz, Adrian T. Lee, Lloyd Knox, Peter A. R. Ade, Nikhel Gupta, J. E. Ruhl, Yanxi Zhang, Pablo Fosalba, Stephen Padin, Marcelle Soares-Santos, J. D. Hrubes, G. Gutierrez, Elizabeth George, Tesla E. Jeltema, Joseph J. Mohr, K. Vanderlinde, Gene C. Hilton, A. Roodman, Tommaso Giannantonio, K. T. Story, Valentine Novosad, Srinivasan Raghunathan, David Brooks, M. E. C. Swanson, H. C. Chiang, Robert I. Citron, Bradford Benson, Gensheng Wang, Jason Gallicchio, N. W. Halverson, Antony A. Stark, Chang Feng, T. Natoli, G. P. Holder, T. Veach, A. A. Plazas, M. Costanzi, C. Sievers, Shantanu Desai, Michael Schubnell, Jason W. Henning, D. L. Burke, Dale Li, Carole Tucker, Mathew Smith, Christian L. Reichardt, B. Flaugher, Jason E. Austermann, Ramon Miquel, S. S. Meyer, M. A. G. Maia, N. L. Harrington, John E. Carlstrom, Matt Dobbs, Peter Melchior, S. Allam, Robert A. Gruendl, L. M. Mocanu, G. I. Noble, Joaquin Vieira, Federico Bianchini, Graeme Smecher, J. P. Dietrich, Nathan Whitehorn, I. Sevilla-Noarbe, Juan Garcia-Bellido, T. McClintock, N. Kuropatkin, Eduardo Rozo, J. De Vicente, T. M. Crawford, Peter Doel, J. T. Sayre, T. N. Varga, E. Suchyta, August E. Evrard, Amy N. Bender, L. N. da Costa, A. K. Romer, H. T. Diehl, Felipe Menanteau, David Bacon, W. L. K. Wu, J. Carretero, K. K. Schaffer, Jennifer L. Marshall, M. Carrasco Kind, Joshua Montgomery, Johannes Hubmayr, Gregory Tarle, J. Gschwend, Joshua A. Frieman, David Rapetti, A. J. Gilbert, S. Serrano, Adam Anderson, Enrique Gaztanaga, Jeff McMahon, K. Honscheid, Eli S. Rykoff, Eric J. Baxter, Vinu Vikram, R. L. C. Ogando, Marcos Lima, T. de Haan, V. Scarpine, S. Patil, John P. Nibarger, Andrew Nadolski, A. Carnero Rosell, Kent D. Irwin, W. L. Holzapfel, Ofer Lahav, S. Everett, C. Pryke, Lindsey Bleem, F. J. Castander, E. J. Sanchez, Santiago Avila, A. T. Crites, Raghunathan, S., Patil, S., Baxter, E., Benson, B. A., Bleem, L. E., Crawford, T. M., Holder, G. P., Mcclintock, T., Reichardt, C. L., Varga, T. N., Whitehorn, N., Ade, P. A. R., Allam, S., Anderson, A. J., Austermann, J. E., Avila, S., Avva, J. S., Bacon, D., Beall, J. A., Bender, A. N., Bianchini, F., Bocquet, S., Brooks, D., Burke, D. L., Carlstrom, J. E., Carretero, J., Castander, F. J., Chang, C. L., Chiang, H. C., Citron, R., Costanzi, M., Crites, A. T., Da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Doel, P., Everett, S., Evrard, A. E., Feng, C., Flaugher, B., Fosalba, P., Frieman, J., Gallicchio, J., Garcia-Bellido, J., Gaztanaga, E., George, E. M., Giannantonio, T., Gilbert, A., Gruendl, R. A., Gschwend, J., Gupta, N., Gutierrez, G., De Haan, T., Halverson, N. W., Harrington, N., Henning, J. W., Hilton, G. C., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hrubes, J. D., Huang, N., Hubmayr, J., Irwin, K. D., Jeltema, T., Kind, M. C., Knox, L., Kuropatkin, N., Lahav, O., Lee, A. T., Li, D., Lima, M., Lowitz, A., Maia, M. A. G., Marshall, J. L., Mcmahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Montgomery, J., Moran, C. C., Nadolski, A., Natoli, T., Nibarger, J. P., Noble, G., Novosad, V., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Rapetti, D., Romer, A. K., Roodman, A., Rosell, A. C., Rozo, E., Ruhl, J. E., Rykoff, E. S., Saliwanchik, B. R., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sievers, C., Smecher, G., Smith, M., Soares-Santos, M., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, C., Vanderlinde, K., Veach, T., De Vicente, J., Vieira, J. D., Vikram, V., Wang, G., W. L. K., Wu, Yefremenko, V., and Zhang, Y.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Cosmic microwave background Gravitational lenses Galaxy Clusters, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, RCUK, General Physics and Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, Cosmology, Gravitational lens, 0103 physical sciences, astro-ph.CO, Dark energy, Cluster (physics), 010306 general physics, STFC, Galaxy cluster, Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the first detection of gravitational lensing due to galaxy clusters using only the polarization of the cosmic microwave background (CMB). The lensing signal is obtained using a new estimator that extracts the lensing dipole signature from stacked images formed by rotating the cluster-centered Stokes $Q/U$ map cutouts along the direction of the locally measured background CMB polarization gradient. Using data from the SPTpol 500 deg$^{2}$ survey at the locations of roughly 18,000 clusters with richness $\lambda \ge 10$ from the Dark Energy Survey (DES) Year-3 full galaxy cluster catalog, we detect lensing at $4.8\sigma$. The mean stacked mass of the selected sample is found to be $(1.43 \pm 0.4)\ \times 10^{14}\ {\rm M_{\odot}}$ which is in good agreement with optical weak lensing based estimates using DES data and CMB-lensing based estimates using SPTpol temperature data. This measurement is a key first step for cluster cosmology with future low-noise CMB surveys, like CMB-S4, for which CMB polarization will be the primary channel for cluster lensing measurements., Comment: 10 pages, 3 figures, 1 table; typos fixed; accepted for publication in PRL

Published
2019

255. Dark Energy Survey Year 1 results: Validation of weak lensing cluster member contamination estimates from P(z) decomposition

Author

M. Carrasco Kind, Marcos Lima, Enrique Gaztanaga, Joshua A. Frieman, Douglas L. Tucker, J. DeRose, Kyler Kuehn, D. L. Burke, Peter Doel, A. Carnero Rosell, I. Sevilla-Noarbe, H. T. Diehl, N. Kuropatkin, Daniel Thomas, E. Buckley-Geer, Robert A. Gruendl, Michael Schubnell, Melanie Simet, T. N. Varga, L. N. da Costa, A. K. Romer, David Brooks, M. E. C. Swanson, A. A. Plazas, K. Honscheid, J. Carretero, E. J. Sanchez, J. P. Dietrich, Juan Garcia-Bellido, David J. James, B. Flaugher, Pablo Fosalba, G. Gutierrez, Eli S. Rykoff, Eduardo Rozo, J. Annis, Thomas McClintock, Stella Seitz, Daniel Gruen, A. von der Linden, Tesla E. Jeltema, W. G. Hartley, J. De Vicente, V. Scarpine, Devon L. Hollowood, S. Serrano, E. Suchyta, August E. Evrard, Jennifer L. Marshall, C. B. D'Andrea, Shantanu Desai, D. W. Gerdes, Mathew Smith, Felipe Menanteau, Gregory Tarle, Christopher J. Miller, Yanxi Zhang, M. Costanzi, Ramon Miquel, Santiago Avila, Carlos E. Cunha, M. A. G. Maia, Risa H. Wechsler, Niall MacCrann, E. Bertin, J. Gschwend, Flavia Sobreira, M. March, R. L. C. Ogando, Peter Melchior, Ben Hoyle, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Varga, T. N., Derose, J., Gruen, D., Mcclintock, T., Seitz, S., Rozo, E., Costanzi, M., Hoyle, B., Maccrann, N., Plazas, A. A., Rykoff, E. S., Simet, M., Von Der Linden, A., Wechsler, R. H., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., D'Andrea, C. B., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., and Zhang, Y.

Subjects
High energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gravitational lensing: weak, Clusters: General [Galaxies], 0103 physical sciences, media_common.cataloged_instance, European union, Observation [Cosmology], 010303 astronomy & astrophysics, STFC, QC, media_common, Physics, 010308 nuclear & particles physics, business.industry, European research, RCUK, Astronomy and Astrophysics, observations [cosmology], Cosmology: Observations, Galaxies: Clusters: General, Gravitational lensing: weak, 13. Climate action, Space and Planetary Science, Research council, galaxies: clusters: general, cosmology: observations, Fundamental physics, Christian ministry, CLUSTERS, weak [Gravitational lensing], business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Weak lensing source galaxy catalogs used in estimating the masses of galaxy clusters can be heavily contaminated by cluster members, prohibiting accurate mass calibration. In this study we test the performance of an estimator for the extent of cluster member contamination based on decomposing the photometric redshift $P(z)$ of source galaxies into contaminating and background components. We perform a full scale mock analysis on a simulated sky survey approximately mirroring the observational properties of the Dark Energy Survey Year One observations (DES Y1), and find excellent agreement between the true number profile of contaminating cluster member galaxies in the simulation and the estimated one. We further apply the method to estimate the cluster member contamination for the DES Y1 redMaPPer cluster mass calibration analysis, and compare the results to an alternative approach based on the angular correlation of weak lensing source galaxies. We find indications that the correlation based estimates are biased by the selection of the weak lensing sources in the cluster vicinity, which does not strongly impact the $P(z)$ decomposition method. Collectively, these benchmarks demonstrate the strength of the $P(z)$ decomposition method in alleviating membership contamination and enabling highly accurate cluster weak lensing studies without broad exclusion of source galaxies, thereby improving the total constraining power of cluster mass calibration via weak lensing., Comment: 14 pages, 8 figures; submitted to MNNRAS

Published
2019

256. Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release

Author

G. Gutierrez, Melanie Simet, Marcos Lima, Xi Chen, A. Roodman, David J. James, Sunayana Bhargava, Tommaso Giannantonio, Pablo Fosalba, K. Bechtol, Eli S. Rykoff, M. Smith, Jennifer L. Marshall, A. A. Plazas, Christopher J. Miller, Daniel Gruen, A. Bermeo-Hernandez, Yanxi Zhang, M. E. C. Swanson, Tim Eifler, Arya Farahi, Huan Lin, Martin Crocce, J. Carretero, Santiago Avila, Filipe B. Abdalla, J. De Vicente, Marcelle Soares-Santos, Carlos E. Cunha, Peter Doel, Elisabeth Krause, J. P. Dietrich, Juan Garcia-Bellido, A. von der Linden, A. Carnero Rosell, J. DeRose, Flavia Sobreira, H. T. Diehl, Rafe Schindler, David J. Brooks, Joshua A. Frieman, Tesla E. Jeltema, D. W. Gerdes, Eduardo Rozo, I. Sevilla-Noarbe, R. L. C. Ogando, Ramon Miquel, V. Scarpine, W. G. Hartley, T. McClintock, C. Davis, N. Kuropatkin, T. N. Varga, J. Gschwend, M. March, Devon L. Hollowood, S. Serrano, Adam Mantz, L. N. da Costa, Daniel Thomas, E. Buckley-Geer, Enrique Gaztanaga, E. Suchyta, S. W. Allen, Risa H. Wechsler, D. L. Burke, Jochen Weller, M. Carrasco Kind, Kyler Kuehn, T. M. C. Abbott, Robert A. Gruendl, E. J. Sanchez, Ben Hoyle, Paul Giles, M. A. G. Maia, M. Costanzi, B. Flaugher, A. K. Romer, Paul Martini, Joseph J. Mohr, Juan Estrada, Michael Schubnell, K. Honscheid, Erin Sheldon, Felipe Menanteau, G. Tarle, August E. Evrard, Costanzi, M., Rozo, E., Simet, M., Zhang, Y., Evrard, A. E., Mantz, A., Rykoff, E. S., Jeltema, T., Gruen, D., Allen, S., Mcclintock, T., Romer, A. K., von der Linden, A., Farahi, A., Derose, J., Varga, T. N., Weller, J., Giles, P., Hollowood, D. L., Bhargava, S., Bermeo-Hernandez, A., Chen, X., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., de Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., Hoyle, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Wechsler, R. H.

Subjects
Cosmological parameter, Large-scale structure of Universe, Cosmological parameters, Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, clusters: general [Galaxies], 01 natural sciences, 7. Clean energy, Cosmology, symbols.namesake, Nucleosynthesis, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, QC, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies: clusters: general, Redshift, Baryon, 13. Climate action, Space and Planetary Science, symbols, Dark energy, Neutrino, CLUSTERS
Abstract

We perform the first blind analysis of cluster abundance data. Specifically, we derive cosmological constraints from the abundance and weak-lensing signal of \redmapper\ clusters of richness $\lambda\geq 20$ in the redshift range $z\in[0.1,0.3]$ as measured in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness--mass relation of the clusters. For a flat $\Lambda$CDM cosmological model with massive neutrinos, we find $S_8 \equiv \sigma_{8}(\Omega_m/0.3)^{0.5}=0.79^{+0.05}_{-0.04}$. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES) and the Kilo-Degree Survey (KiDS), and with the Cosmic Microwave Background (CMB) anisotropies as measured by \planck. We demonstrate that the cosmological posteriors are robust against variation of the richness--mass relation model and to systematics associated with the calibration of the selection function. In combination with Baryon Acoustic Oscillation (BAO) data and Big-Bang Nucleosynthesis (BBN) data, we constrain the Hubble rate to be $h=0.66\pm 0.02$, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness--mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.

Published
2019

257. Supernova Siblings: Assessing the Consistency of Properties of Type Ia Supernovae that Share the Same Parent Galaxies

Author

W. G. Hartley, V. Scarpine, N. E. Sommer, I. Sevilla-Noarbe, David J. Brooks, David J. James, G. Tarle, N. Kuropatkin, A. A. Plazas, Jennifer L. Marshall, Ramon Miquel, K. D. Eckert, Ryan J. Foley, T. N. Varga, L. N. da Costa, L. Kelsey, K. Kuehn, Karl Glazebrook, Lluís Galbany, C. Lidman, Samuel Hinton, Robert Morgan, Anais Möller, E. Bertin, E. Suchyta, Marcus Lima, G. Gutierrez, Edward Macaulay, P. Doel, Geraint F. Lewis, Alex Drlica-Wagner, M. Costanzi, J. Gschwend, D. J. Brout, Daniela Carollo, Salcedo Romero de Ávila, A. Massiah, T. F. Eifler, Tianjun Li, Michael Schubnell, P. Wiseman, J. Annis, Brodie Popovic, Joshua A. Frieman, T. M. C. Abbott, P. Fosalba, R. D. Wilkinson, M. Pursiainen, S. Everett, E. J. Sanchez, H. T. Diehl, K. Honscheid, M. Carrasco Kind, M. Sako, Robert C. Nichol, D. L. Hollowood, M. E. C. Swanson, B. Flaugher, S. Serrano, Richard Kessler, S. Desai, Enrique Gaztanaga, M. N. K. Smith, Mark Sullivan, Felipe Menanteau, K. Bechtol, Juan Garcia-Bellido, A. Carnero Rosell, A. R. Walker, J. De Vicente, Antonella Palmese, Daniel Gruen, D. L. Burke, M. A. G. Maia, Daniel Scolnic, B. P. Thomas, D. W. Gerdes, S. Allam, Robert A. Gruendl, B. E. Tucker, Michel Aguena, J. Carretero, R. Hounsell, Tamara M. Davis, F. Paz-Chinchón, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), National Aeronautics and Space Administration (US), European Commission, European Research Council, Department of Energy (US), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Scolnic, D., Smith, M., Massiah, A., Wiseman, P., Brout, D., Kessler, R., Davis, T. M., Foley, R. J., Galbany, L., Hinton, S. R., Hounsell, R., Kelsey, L., Lidman, C., Macaulay, E., Morgan, R., Nichol, R. C., Moller, A., Popovic, B., Sako, M., Sullivan, M., Thomas, B. P., Tucker, B. E., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. C., Carollo, D., Kind, M. C., Carretero, J., Costanzi Alunno Cerbolini, M., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lewis, G. F., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Pursiainen, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Walker, A. R., and Wilkinson, R.

Subjects
Observational cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Type (model theory), 01 natural sciences, 7. Clean energy, Consistency (statistics), 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation), Physics, Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Distance modulus, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DES Collaboration: et al. arXiv:2002.00974v2, While many studies have shown a correlation between properties of the light curves of SNe Ia and properties of their host galaxies, it remains unclear what is driving these correlations. We introduce a new direct method to study these correlations by analyzing "parent" galaxies that host multiple SNe Ia "siblings." Here, we search the Dark Energy Survey SN sample, one of the largest samples of discovered SNe, and find eight galaxies that hosted two likely SNe Ia. Comparing the light-curve properties of these SNe and recovered distances from the light curves, we find no better agreement between properties of SNe in the same galaxy as any random pair of galaxies, with the exception of the SN light-curve stretch. We show at 2.8σ significance that at least one-half of the intrinsic scatter of SNe Ia distance modulus residuals is not from common host properties. We also discuss the robustness with which we could make this evaluation with LSST, which will find 100× more pairs of galaxies, and pave a new line of study on the consistency of SNe Ia in the same parent galaxies. Finally, we argue that it is unlikely that some of these SNe are actually single, lensed SN with multiple images., D.S. is supported by DOE grant DE-SC0010007, the David and Lucile Packard Foundation. D.S. and R.K. are supported in part by NASA under Contract No. NNG17PX03C issued through the WFIRST Science Investigation Teams Programme. D.B. and M.S. were supported by DOE grant DE-FOA0001358 and NSF grant AST-1517742. L.G. was funded by the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 839090. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. We are grateful for the support of the University of Chicago Research Computing Center for assistance with the calculations carried out in this work. R.F. is supported in part by NSF grants AST-1518052 and AST1815935, the Gordon & Betty Moore Foundation, the HeisingSimons Foundation, and by fellowships from the David and Lucile Packard Foundation, as well as the NASA contract above. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo InterAmerican Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). We acknowledge support from EU/FP7-ERC grant No. 615929. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2020

258. Weak-lensing mass calibration of redMaPPer galaxy clusters in Dark Energy Survey Science Verification data

Author

G. Gutierrez, Ricardo L. C. Ogando, M. Jarvis, Niall MacCrann, Ofer Lahav, Joseph J. Mohr, A. Saro, E. Bertin, F. B. Abdalla, Enrique Gaztanaga, Peter Melchior, Daniel Gruen, David Brooks, Eli S. Rykoff, A. K. Romer, M. E. C. Swanson, E. Suchyta, Bhuvnesh Jain, J. Gschwend, Juan Garcia-Bellido, C. Bonnett, A. A. Plazas, Gary Bernstein, Matthew R. Becker, Flavia Sobreira, D. W. Gerdes, Eduardo Rozo, Daniel Thomas, E. Buckley-Geer, V. Scarpine, Shantanu Desai, Tesla E. Jeltema, M. A. G. Maia, W. G. Hartley, D. L. Hollowood, J. Carretero, C. J. Miller, Donnacha Kirk, M. Carrasco Kind, Robert C. Nichol, Elisabeth Krause, A. Carnero Rosell, Alistair R. Walker, Bradford Benson, Marcelle Soares-Santos, B. Flaugher, P. Martini, E. Sheldon, J. P. Dietrich, M. March, David J. James, Ramon Miquel, A. Bermeo, Pablo Fosalba, K. Honscheid, Joseph Clampitt, Marcos Lima, A. Benoit-Lévy, Yanxi Zhang, Robert A. Gruendl, Adam Amara, Tim Eifler, J. Annis, Felipe Menanteau, Gregory Tarle, Sarah Bridle, I. Sevilla-Noarbe, T. McClintock, Carlos E. Cunha, N. Kuropatkin, T. N. Varga, L. N. da Costa, Jochen Weller, T. M. C. Abbott, E. J. Sanchez, Joe Zuntz, Kyler Kuehn, Michael Troxel, R. C. Smith, C. B. D'Andrea, T. Kacprzak, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), DES, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Melchior, P., Gruen, D., Mcclintock, T., Varga, T. N., Sheldon, E., Rozo, E., Amara, A., Becker, M. R., Benson, B. A., Bermeo, A., Bridle, S. L., Clampitt, J., Dietrich, J. P., Hartley, W. G., Hollowood, D., Jain, B., Jarvis, M., Jeltema, T., Kacprzak, T., Maccrann, N., Rykoff, E., S., Saro, A., Suchyta, E., Troxel, M. A., Zuntz, J., Bonnett, C., Plazas, A. A., Abbott, T. M. C., Abdalla, F. B., Annis, J., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Eifler, T. F., Flaugher, B., Fosalba, P., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kirk, D., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Ogando, R., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., Weller, J., and Zhang, Y.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, gravitational lensing: weak, 0103 physical sciences, media_common.cataloged_instance, European union, Astronomy observatory, 010303 astronomy & astrophysics, STFC, Observations, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, QB, media_common, Physics, 010308 nuclear & particles physics, European research, RCUK, Astronomy and Astrophysics, Engineering physics, Cosmology, Red shift, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Fundamental physics, astro-ph.CO, Christian ministry, High Energy Physics::Experiment, weak [Gravitational lensing], National laboratory, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], observation [cosmology]
Abstract

Monthly Notices of the Royal Astronomical Society, 469 (4), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

Published
2017

259. Dark Energy Survey Year 1 Results: Weak Lensing Mass Calibration of redMaPPer Galaxy Clusters

Author

Eli S. Rykoff, Thomas McClintock, I. Sevilla-Noarbe, David J. James, Stella Seitz, Michael Troxel, A. Carnero Rosell, E. Suchyta, August E. Evrard, Pablo Fosalba, T. N. Varga, Joe Zuntz, Risa H. Wechsler, Adam Mantz, L. N. da Costa, Tesla E. Jeltema, A. Roodman, Tommaso Giannantonio, J. Carretero, Melanie Simet, Alex Drlica-Wagner, A. A. Plazas, C. B. D'Andrea, Scarpine, Markus Rau, P Li, Felipe Menanteau, Elisabeth Krause, Antonella Palmese, J. Annis, Steven W. Allen, G. Pollina, David J. Brooks, Juan Garcia-Bellido, J. P. Dietrich, Vikram, A. von der Linden, Matthew R. Becker, Flavia Sobreira, Eduardo Rozo, R. C. Smith, Filipe B. Abdalla, Tenglin Li, Sarah Bridle, D. L. Hollowood, Santiago Avila, Ramon Miquel, Joshua A. Frieman, G. Gutierrez, J. DeRose, Carlos E. Cunha, A. Bermeo, Mathew Smith, Nico Hamaus, K. Honscheid, Sunayana Bhargava, Douglas L. Tucker, Kyler Kuehn, Martin Crocce, Donnacha Kirk, Alistair R. Walker, Jochen Weller, F. J. Castander, W. G. Hartley, D. L. Burke, Joseph J. Mohr, Marcelle Soares-Santos, Jennifer L. Marshall, Peter Melchior, T. M. C. Abbott, A. K. Romer, Rafe Schindler, M. March, M. E. C. Swanson, T. Shin, Ofer Lahav, Daniel Gruen, E. J. Sanchez, S. Everett, S. Allam, Robert A. Gruendl, Ricardo L. C. Ogando, C. Vergara Cervantes, Marcos Lima, Ben Hoyle, D. W. Gerdes, G Morris, J. De Vicente, Brian Nord, C. Davis, Peter Doel, Yanxi Zhang, H. T. Diehl, Arya Farahi, Niall MacCrann, Erin Sheldon, G. Tarle, M. Costanzi, H. Israel, M. Carrasco Kind, Enrique Gaztanaga, B. Flaugher, Mcclintock, T., Varga, T. N., Gruen, D., Rozo, E., Rykoff, E. S., Shin, T., Melchior, P., Derose, J., Seitz, S., Dietrich, J. P., Sheldon, E., Zhang, Y., von der Linden, A., Jeltema, T., Mantz, A. B., Romer, A. K., Allen, S., Becker, M. R., Bermeo, A., Bhargava, S., Costanzi, M., Everett, S., Farahi, A., Hamaus, N., Hartley, W. G., Hollowood, D. L., Hoyle, B., Israel, H., Li, P., Maccrann, N., Morris, G., Palmese, A., Plazas, A. A., Pollina, G., Rau, M. M., Simet, M., Soares-Santos, M., Troxel, M. A., Vergara Cervantes, C., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Bridle, S. L., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Doel, P., Drlica-Wagner, A., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kirk, D., Krause, E., Kuehn, K., Lahav, O., T. S., Li, Lima, M., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Nord, B., Ogando, R. L. C., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), ST/N504452/1, FOS: Physical sciences, observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, Cosmology, Gravitational lensing: weak, ST/P000252/1, 0103 physical sciences, observations [Cosmology], 010303 astronomy & astrophysics, Scaling, Weak gravitational lensing, Galaxy cluster, Astrophysics::Galaxy Astrophysics, STFC, QC, Photometric redshift, Physics, 010308 nuclear & particles physics, Cosmology: observations, RCUK, Astronomy and Astrophysics, Galaxy, Redshift, Space and Planetary Science, Dark energy, astro-ph.CO, Galaxies: clusters: general, weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We constrain the mass--richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing. We split clusters into $4\times3$ bins of richness $\lambda$ and redshift $z$ for $\lambda\geq20$ and $0.2 \leq z \leq 0.65$ and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as $\langle M_{\rm 200m}|\lambda,z\rangle = M_0 (\lambda/40)^F ((1+z)/1.35)^G$, we constrain the normalization of the scaling relation at the 5.0 per cent level as $M_0 = [3.081 \pm 0.075 ({\rm stat}) \pm 0.133 ({\rm sys})] \cdot 10^{14}\ {\rm M}_\odot$ at $\lambda=40$ and $z=0.35$. The richness scaling index is constrained to be $F=1.356 \pm 0.051\ ({\rm stat})\pm 0.008\ ({\rm sys})$ and the redshift scaling index $G=-0.30\pm 0.30\ ({\rm stat})\pm 0.06\ ({\rm sys})$. These are the tightest measurements of the normalization and richness scaling index made to date. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentering, cluster member dilution of the source sample, systematic uncertainties in the modeling of the halo--mass correlation function, halo triaxiality, and projection effects. We discuss prospects for reducing this systematic error budget, which dominates the uncertainty on $M_0$. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid and WFIRST., Comment: 28 pages, 15 figures; matches MNRAS referee response version

260. Dark Energy Survey Year 3 results: galaxy-halo connection from galaxy-galaxy lensing

Author

Martin Crocce, R. D. Wilkinson, Maria E. S. Pereira, Joe Zuntz, Alex Drlica-Wagner, K. Honscheid, J. Blazek, Elisabeth Krause, Scott Dodelson, Chihway Chang, Matthew R. Becker, S. Desai, F. J. Castander, T. M. C. Abbott, Marcos Lima, Antonella Palmese, C. Doux, Chun-Hao To, E. J. Sanchez, Stella Seitz, I. Tutusaus, E. Bertin, M. A. G. Maia, J. Annis, A. Alarcon, I. Ferrero, Matt J. Jarvis, Eli S. Rykoff, Peter Doel, Brian Yanny, Yanxi Zhang, P. F. Leget, Josh Frieman, David J. Brooks, W. G. Hartley, J. P. Dietrich, Juan Garcia-Bellido, Ramon Miquel, Bhuvnesh Jain, H. T. Diehl, David Bacon, A. Roodman, G. Zacharegkas, J. McCullough, M. Costanzi, E. M. Huff, R. Chen, M Gatti, Niall MacCrann, Jennifer L. Marshall, Carlos Solans Sanchez, Samuel Hinton, Michel Aguena, Adriano Pieres, C. Davis, G. Gutierrez, B. Yin, B. Flaugher, Alexandra Amon, R. P. Rollins, J. Myles, J. Gschwend, Gary Bernstein, K. Herner, A. Navarro-Alsina, Keith Bechtol, Enrique Gaztanaga, Ami Choi, Ben Hoyle, J. Carretero, G. Giannini, J. DeRose, E. Suchyta, August E. Evrard, Felipe Menanteau, David J. James, A. Carnero Rosell, S. Everett, Jack Elvin-Poole, A. Porredon, Youngsoo Park, Pablo Fosalba, Risa H. Wechsler, Daniel Thomas, Peter Melchior, R. Cawthon, Agnès Ferté, J. Cordero, D. L. Burke, D. L. Hollowood, R. L. C. Ogando, S. Serrano, A. Campos, F. Paz-Chinchón, I. Harrison, S. Allam, Robert A. Gruendl, M. Smith, Daniel Gruen, T. Shin, M. Carrasco Kind, F. Andrade-Oliveira, Marco Raveri, L. F. Secco, G. Tarle, Erin Sheldon, Ashley J. Ross, I. Sevilla-Noarbe, Kyler Kuehn, N. Kuropatkin, K. D. Eckert, T. N. Varga, L. N. da Costa, Michael Troxel, S. Pandey, J. Muir, J. Prat, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Zacharegkas, G., Chang, C., Prat, J., Pandey, S., Ferrero, I., Blazek, J., Jain, B., Crocce, M., Derose, J., Palmese, A., Seitz, S., Sheldon, E., Hartley, W. G., Wechsler, R. H., Dodelson, S., Fosalba, P., Krause, E., Park, Y., Sanchez, C., Alarcon, A., Amon, A., Bechtol, K., Becker, M. R., Bernstein, G. M., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Davis, C., Diehl, H. T., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Herner, K., Huff, E. M., Jarvis, M., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Myles, J., Navarro-Alsina, A., Porredon, A., Raveri, M., Rollins, R. P., Roodman, A., Ross, A. J., Rykoff, E. S., Secco, L. F., Sevilla-Noarbe, I., Shin, T., Troxel, M. A., Tutusaus, I., Varga, T. N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Muir, J., Ogando, R. L. C., Paz-Chinchon, F., Pieres, A., Sanchez, E., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Wilkinson, R. D., Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, National Aeronautics and Space Administration (US), University of Chicago, University of Pennsylvania, University of Oslo, Northeastern University, Observatoire de Sauverny, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Lawrence Berkeley National Laboratory, Fermi National Accelerator Laboratory, Giessenbachstrasse, Ludwig-Maximilians Universität München, Brookhaven National Laboratory, University of Geneva, Stanford University, Slac National Accelerator Laboratory, Carnegie Mellon University, University of Arizona, University of Tokyo, Argonne National Laboratory, University of Wisconsin-Madison, la Laguna, Laboratório Interinstitucional de E-Astronomia-LIneA, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, Ohio State University, University of Manchester, Santa Cruz Institute for Particle Physics, California Institute of Technology, Barcelona Institute of Science and Technology, Denys Wilkinson Building, University of Cambridge, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnológicas (CIEMAT), University of Edinburgh, Casilla, Universidade Estadual Paulista (UNESP), University of Portsmouth, Institut d'Astrophysique de Paris, University College London, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Iit Hyderabad, Ludwig-Maximilians-Universität, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, University of Sussex, and UAM. Departamento de Física Teórica

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo occupation distribution, Cosmology, matter haloes, Galactic halo, gravitational lensing: weak, dark matter [cosmology], weak [gravitational lensing], 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, large-scale structure of universe, occupation distribution, massive galaxies, model, 010308 nuclear & particles physics, 100 square degrees, Física, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, cosmology: dark matter, large-scale structure of Universe, Galaxy, Redshift, radial-distribution, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, cosmological constraints, cfhtlens, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DES Collaboration: G. Zacharegkas et al., Galaxy–galaxy lensing is a powerful probe of the connection between galaxies and their host dark matter haloes, which is important both for galaxy evolution and cosmology. We extend the measurement and modelling of the galaxy–galaxy lensing signal in the recent Dark Energy Survey Year 3 cosmology analysis to the highly non-linear scales (∼100 kpc). This extension enables us to study the galaxy–halo connection via a Halo Occupation Distribution (HOD) framework for the two lens samples used in the cosmology analysis: a luminous red galaxy sample (REDMAGIC) and a magnitude-limited galaxy sample (MAGLIM). We find that REDMAGIC (MAGLIM) galaxies typically live in dark matter haloes of mass log10(Mh/M⊙) ≈ 13.7 which is roughly constant over redshift (13.3−13.5 depending on redshift). We constrain these masses to ∼15 per cent ⁠, approximately 1.5 times improvement over the previous work. We also constrain the linear galaxy bias more than five times better than what is inferred by the cosmological scales only. We find the satellite fraction for REDMAGIC (MAGLIM) to be ∼0.1−0.2 (0.1−0.3) with no clear trend in redshift. Our constraints on these halo properties are broadly consistent with other available estimates from previous work, large-scale constraints, and simulations. The framework built in this paper will be used for future HOD studies with other galaxy samples and extensions for cosmological analyses., CC is supported by the Henry Luce Foundation. JP is supported by DOE grant DE-SC0021429. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773,PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

261. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations.

Author

To C, Krause E, Rozo E, Wu H, Gruen D, Wechsler RH, Eifler TF, Rykoff ES, Costanzi M, Becker MR, Bernstein GM, Blazek J, Bocquet S, Bridle SL, Cawthon R, Choi A, Crocce M, Davis C, DeRose J, Drlica-Wagner A, Elvin-Poole J, Fang X, Farahi A, Friedrich O, Gatti M, Gaztanaga E, Giannantonio T, Hartley WG, Hoyle B, Jarvis M, MacCrann N, McClintock T, Miranda V, Pereira MES, Park Y, Porredon A, Prat J, Rau MM, Ross AJ, Samuroff S, Sánchez C, Sevilla-Noarbe I, Sheldon E, Troxel MA, Varga TN, Vielzeuf P, Zhang Y, Zuntz J, Abbott TMC, Aguena M, Amon A, Annis J, Avila S, Bertin E, Bhargava S, Brooks D, Burke DL, Carnero Rosell A, Carrasco Kind M, Carretero J, Chang C, Conselice C, da Costa LN, Davis TM, Desai S, Diehl HT, Dietrich JP, Everett S, Evrard AE, Ferrero I, Flaugher B, Fosalba P, Frieman J, García-Bellido J, Gruendl RA, Gutierrez G, Hinton SR, Hollowood DL, Honscheid K, Huterer D, James DJ, Jeltema T, Kron R, Kuehn K, Kuropatkin N, Lima M, Maia MAG, Marshall JL, Menanteau F, Miquel R, Morgan R, Muir J, Myles J, Palmese A, Paz-Chinchón F, Plazas AA, Romer AK, Roodman A, Sanchez E, Santiago B, Scarpine V, Serrano S, Smith M, Suchyta E, Swanson MEC, Tarle G, Thomas D, Tucker DL, Weller J, Wester W, and Wilkinson RD

Abstract

We present the first joint analysis of cluster abundances and auto or cross-correlations of three cosmic tracer fields: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis (4×2pt+N) of cluster abundances, three cluster cross-correlations, and the auto correlations of the galaxy density measured from the first year data of the Dark Energy Survey, we obtain Ω_{m}=0.305_{-0.038}^{+0.055} and σ_{8}=0.783_{-0.054}^{+0.064}. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat νΛCDM model. Consequently, we combine cluster abundances and all two-point correlations from across all three cosmic tracer fields (6×2pt+N) and find improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys.

Published
2021
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262. Detection of CMB-Cluster Lensing using Polarization Data from SPTpol.

Author

Raghunathan S, Patil S, Baxter E, Benson BA, Bleem LE, Crawford TM, Holder GP, McClintock T, Reichardt CL, Varga TN, Whitehorn N, Ade PAR, Allam S, Anderson AJ, Austermann JE, Avila S, Avva JS, Bacon D, Beall JA, Bender AN, Bianchini F, Bocquet S, Brooks D, Burke DL, Carlstrom JE, Carretero J, Castander FJ, Chang CL, Chiang HC, Citron R, Costanzi M, Crites AT, da Costa LN, Desai S, Diehl HT, Dietrich JP, Dobbs MA, Doel P, Everett S, Evrard AE, Feng C, Flaugher B, Fosalba P, Frieman J, Gallicchio J, García-Bellido J, Gaztanaga E, George EM, Giannantonio T, Gilbert A, Gruendl RA, Gschwend J, Gupta N, Gutierrez G, de Haan T, Halverson NW, Harrington N, Henning JW, Hilton GC, Hollowood DL, Holzapfel WL, Honscheid K, Hrubes JD, Huang N, Hubmayr J, Irwin KD, Jeltema T, Kind MC, Knox L, Kuropatkin N, Lahav O, Lee AT, Li D, Lima M, Lowitz A, Maia MAG, Marshall JL, McMahon JJ, Melchior P, Menanteau F, Meyer SS, Miquel R, Mocanu LM, Mohr JJ, Montgomery J, Moran CC, Nadolski A, Natoli T, Nibarger JP, Noble G, Novosad V, Ogando RLC, Padin S, Plazas AA, Pryke C, Rapetti D, Romer AK, Roodman A, Rosell AC, Rozo E, Ruhl JE, Rykoff ES, Saliwanchik BR, Sanchez E, Sayre JT, Scarpine V, Schaffer KK, Schubnell M, Serrano S, Sevilla-Noarbe I, Sievers C, Smecher G, Smith M, Soares-Santos M, Stark AA, Story KT, Suchyta E, Swanson MEC, Tarle G, Tucker C, Vanderlinde K, Veach T, De Vicente J, Vieira JD, Vikram V, Wang G, Wu WLK, Yefremenko V, and Zhang Y

Abstract

We report the first detection of gravitational lensing due to galaxy clusters using only the polarization of the cosmic microwave background (CMB). The lensing signal is obtained using a new estimator that extracts the lensing dipole signature from stacked images formed by rotating the cluster-centered Stokes QU map cutouts along the direction of the locally measured background CMB polarization gradient. Using data from the SPTpol 500  deg^{2} survey at the locations of roughly 18 000 clusters with richness λ≥10 from the Dark Energy Survey (DES) Year-3 full galaxy cluster catalog, we detect lensing at 4.8σ. The mean stacked mass of the selected sample is found to be (1.43±0.40)×10^{14}M_{⊙} which is in good agreement with optical weak lensing based estimates using DES data and CMB-lensing based estimates using SPTpol temperature data. This measurement is a key first step for cluster cosmology with future low-noise CMB surveys, like CMB-S4, for which CMB polarization will be the primary channel for cluster lensing measurements.

Published
2019
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