Author: "J. De Vicente" / Topic: astrophysics::cosmology and extragalactic astrophysics - Searchworks@Jio Institute Digital Library Search Results

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118 results on '"J. De Vicente"'

1. Consistent lensing and clustering in a low-S8 Universe with BOSS, DES Year 3, HSC Year 1, and KiDS-1000

Author: A Amon, N C Robertson, H Miyatake, C Heymans, M White, J DeRose, S Yuan, R H Wechsler, T N Varga, S Bocquet, A Dvornik, S More, A J Ross, H Hoekstra, A Alarcon, M Asgari, J Blazek, A Campos, R Chen, A Choi, M Crocce, H T Diehl, C Doux, K Eckert, J Elvin-Poole, S Everett, A Ferté, M Gatti, G Giannini, D Gruen, R A Gruendl, W G Hartley, K Herner, H Hildebrandt, S Huang, E M Huff, B Joachimi, S Lee, N MacCrann, J Myles, A Navarro-Alsina, T Nishimichi, J Prat, L F Secco, I Sevilla-Noarbe, E Sheldon, T Shin, T Tröster, M A Troxel, I Tutusaus, A H Wright, B Yin, M Aguena, S Allam, J Annis, D Bacon, M Bilicki, D Brooks, D L Burke, A Carnero Rosell, J Carretero, F J Castander, R Cawthon, M Costanzi, L N da Costa, M E S Pereira, J de Jong, J De Vicente, S Desai, J P Dietrich, P Doel, I Ferrero, J Frieman, J García-Bellido, D W Gerdes, J Gschwend, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D Huterer, A Kannawadi, K Kuehn, N Kuropatkin, O Lahav, M Lima, M A G Maia, J L Marshall, F Menanteau, R Miquel, J J Mohr, R Morgan, J Muir, F Paz-Chinchón, A Pieres, A A Plazas Malagón, A Porredon, M Rodriguez-Monroy, A Roodman, E Sanchez, S Serrano, H Shan, E Suchyta, M E C Swanson, G Tarle, D Thomas, C To, Y Zhang, Amon, A., Robertson, N. C., Miyatake, H., Heymans, C., White, M., Derose, J., Yuan, S., Wechsler, R. H., Varga, T. N., Bocquet, S., Dvornik, A., More, S., Ross, A. J., Hoekstra, H., Alarcon, A., Asgari, M., Blazek, J., Campos, A., Chen, R., Choi, A., Crocce, M., Diehl, H. T., Doux, C., Eckert, K., Elvin-Poole, J., Everett, S., Ferté, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Hartley, W. G., Herner, K., Hildebrandt, H., Huang, S., Huff, E. M., Joachimi, B., Lee, S., Maccrann, N., Myles, J., Navarro-Alsina, A., Nishimichi, T., Prat, J., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Tröster, T., Troxel, M. A., Tutusaus, I., Wright, A. H., Yin, B., Aguena, M., Allam, S., Annis, J., Bacon, D., Bilicki, M., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., de Jong, J., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Frieman, J., García-Bellido, J., Gerdes, D. W., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Kannawadi, A., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Porredon, A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Serrano, S., Shan, H., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Zhang, Y.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmology observations, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, gravitational lensing weak, large-scale structure of Universe, Cosmology and Nongalactic Astrophysics, Astrophysic, Space and Planetary Science, cosmology observation, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We evaluate the consistency between lensing and clustering probes of large-scale structure based on measurements of projected galaxy clustering from BOSS combined with overlapping galaxy-galaxy lensing from three surveys: DES Y3, HSC Y1, and KiDS-1000. An intra-lensing-survey study finds good agreement between these lensing data. We model the observations using the Dark Emulator and fit the data at two fixed cosmologies: Planck, with $S_8=0.83$, and a Lensing cosmology with $S_8=0.76$. For a joint analysis limited to scales with $R>5.25h^{-1}$Mpc, we find that both cosmologies provide an acceptable fit to the data. Full utilisation of the small-scale clustering and lensing measurements is hindered by uncertainty in the impact of baryon feedback and assembly bias, which we account for with a reasoned theoretical error budget. We incorporate a systematic scaling parameter for each redshift bin, $A$, that decouples the lensing and clustering to capture any inconsistency. When a wide range of scales ($0.15, Comment: 28 pages, 11 figures
Published: 2023

2. Dark energy survey year 3 results: Galaxy sample for BAO measurement

Author: Josh Frieman, R. L. C. Ogando, J. Calcino, David J. James, Pablo Fosalba, F. J. Castander, Ramon Miquel, O. Alves, Elisabeth Krause, J. Mena-Fernández, Will J. Percival, N. Weaverdyck, Karl Glazebrook, D Burke, A Roodman, C. Lidman, B. E. Tucker, A. Brandao-Souza, Erin Sheldon, A. Choi, T. M. C. Abbott, M. Carrasco Kind, F. Andrade-Oliveira, Jennifer L. Marshall, K. Honscheid, J. Carretero, Michael Schubnell, Jack Elvin-Poole, Tamara M. Davis, Anais Möller, E. Bertin, Chun-Hao To, Agnès Ferté, E. J. Sanchez, Ashley J. Ross, Martin Crocce, I. Sevilla-Noarbe, M. Soares-Santos, R. Cawthon, Daniel Thomas, A. G. Kim, E. Suchyta, J. Gschwend, August E. Evrard, Tommaso Giannantonio, A. A. Plazas Malagón, Geraint F. Lewis, G. Tarle, W. Riquelme, Rob Sharp, Santiago Avila, E. Buckley-Geer, S. A. Uddin, Ofer Lahav, Alex Drlica-Wagner, Dragan Huterer, A. Porredon, W. G. Hartley, M. Costanzi, Felipe Menanteau, A. Carnero Rosell, K. D. Eckert, T. N. Varga, Peter Doel, Douglas L. Tucker, V. Scarpine, Daniela Carollo, Robert Morgan, Juan Garcia-Bellido, S. Desai, Kyler Kuehn, D. L. Hollowood, J. Annis, H. T. Diehl, Christopher J. Conselice, S. Serrano, I. Ferrero, L. N. da Costa, Ben Hoyle, K. C. Chan, Rogerio Rosenfeld, Enrique Gaztanaga, B. Flaugher, David J. Brooks, Antonella Palmese, Marcos Lima, M. A. G. Maia, M. Rodriguez-Monroy, U. Malik, Adriano Pieres, F. Paz-Chinchón, Joseph J. Mohr, J. De Vicente, M.E. da Silva Pereira, M. Smith, S. Everett, Daniel Gruen, H. Camacho, J. Muir, Samuel Hinton, D. W. Gerdes, G. Gutierrez, M. E. C. Swanson, Jacobo Asorey, Michel Aguena, D. Sanchez Cid, S. Allam, Robert A. Gruendl, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), 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), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), DES, UAM. Departamento de Física Teórica, Rosell, A. C., Rodriguez-Monroy, M., Crocce, M., Elvin-Poole, J., Porredon, A., Ferrero, I., Mena-Fernandez, J., Cawthon, R., De Vicente, J., Gaztanaga, E., Ross, A. J., Sanchez, E., Sevilla-Noarbe, I., Alves, O., Andrade-Oliveira, F., Asorey, J., Avila, S., Brandao-Souza, A., Camacho, H., Chan, K. C., Ferte, A., Muir, J., Riquelme, W., Rosenfeld, R., Cid, D. S., Hartley, W. G., Weaverdyck, N., Abbott, T., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D., Calcino, J., Carollo, D., Kind, M. C., Carretero, J., Castander, F., Choi, A., Conselice, C., Costanzi, M., Da Costa, L., Da Silva Pereira, M. E., Davis, T., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Everett, S., Evrard, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D., Giannantonio, T., Glazebrook, K., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., Hoyle, B., Huterer, D., James, D., Kim, A., Krause, E., Kuehn, K., Lahav, O., Lewis, G., Lidman, C., Lima, M., Maia, M., Malik, U., Marshall, J., Menanteau, F., Miquel, R., Mohr, J., Moller, A., Morgan, R., Ogando, R., Palmese, A., Paz-Chinchon, F., Percival, W., Pieres, A., Malagon, A. P., Roodman, A., Scarpine, V., Schubnell, M., Serrano, S., Sharp, R., Sheldon, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., Tucker, B., Tucker, D., Uddin, S., Varga, T. N., Instituto de Astrofísica de Canarias, Dpto. Astrofísica, Laboratório Interinstitucional de E-Astronomia - LIneA, Medioambientales y Tecnológicas (CIEMAT), Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), The Ohio State University, University of Oslo, University of Wisconsin-Madison, University of Michigan, Universidade Estadual Paulista (UNESP), Universidad Autónoma de Madrid, Universidade Estadual de Campinas (UNICAMP), California Institute of Technology, Stanford University, University of Geneva, NSF's National Optical-Infrared Astronomy Research Laboratory, Fermi National Accelerator Laboratory, Institut d'Astrophysique de Paris, University College London, University of Chicago, SLAC National Accelerator Laboratory, University of Queensland, Astrophysical Observatory of Turin, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Manchester, School of Physics and Astronomy, University of Trieste, Observatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, University of Pennsylvania, Santa Cruz Institute for Particle Physics, University of Cambridge, Swinburne University of Technology, Ludwig-Maximilians-Universität, Center for Astrophysics | Harvard and Smithsonian, Lawrence Berkeley National Laboratory, University of Arizona, Macquarie University, Lowell Observatory, The University of Sydney, The Australian National University, Australian National University, Universidade de São Paulo (USP), Texas A&M University, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, LPC, University of Waterloo, Perimeter Institute for Theoretical Physics, Peyton Hall, Brookhaven National Laboratory, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, and The University of Texas at Austin
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology: observations, Large-Scale Structure of Universe [Cosmology], FOS: Physical sciences, Física, Astronomy and Astrophysics, observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Catalogues, Sample (graphics), Catalogue, Galaxy, Cosmology: large-scale structure of Universe, Observations [Cosmology], Space and Planetary Science, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Rosell, A., et al. (DES Collaboration), In this paper, we present and validate the galaxy sample used for the analysis of the baryon acoustic oscillation (BAO) signal in the Dark Energy Survey (DES) Y3 data. The definition is based on a colour and redshift-dependent magnitude cut optimized to select galaxies at redshifts higher than 0.5, while ensuring a high-quality determination. The sample covers ~4100 deg2 to a depth of i = 22.3 (AB) at 10s. It contains 7031 993 galaxies in the redshift range from z = 0.6 to 1.1, with a mean effective redshift of 0.835. Redshifts are estimated with the machine learning algorithm DNF, and are validated using the VIPERS PDR2 sample. We find a mean redshift bias of zbias~0.01 and a mean uncertainty, in units of 1 + z, of σ68~0.03. We evaluate the galaxy population of the sample, showing it is mostly built upon Elliptical to Sbc types. Furthermore, we find a low level of stellar contamination of ≤ 4 per cent. We present the method used to mitigate the effect of spurious clustering coming from observing conditions and other large-scale systematics.We apply it to the BAO sample and calculate weights that are used to get a robust estimate of the galaxy clustering signal. This paper is one of a series dedicated to the analysis of the BAO signal in DES Y3. In the companion papers, we present the galaxy mock catalogues used to calibrate the analysis and the angular diameter distance constraints obtained through the fitting to the BAO scale., 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 Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). ACR acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under grant AYA2017-84061-P, co-financed by FEDER (European Regional Development Funds) and by the Spanish Space Research Program ‘Participation in the NISP instrument and preparation for the science of EUCLID’ (ESP2017-84272-C2-1-R). SA was supported by the MICUES project, funded by the EU’s H2020 MSCA grant agreement no. 713366 (InterTalentum UAM).
Published: 2022

3. Dark Energy Survey Year 3 results: cosmology with moments of weak lensing mass maps – validation on simulations

Author: M. Smith, Daniel Gruen, D. W. Gerdes, F. Paz-Chinchón, D. J. James, J. Carretero, G. Tarle, Ian Harrison, J. Gschwend, Shantanu Desai, Marcos Lima, Kyler Kuehn, M. Carrasco Kind, Ramon Miquel, E. Suchyta, Juan Garcia-Bellido, August E. Evrard, Felipe Menanteau, Daniel Thomas, E. Buckley-Geer, Jennifer L. Marshall, L. Whiteway, Peter Doel, Juan Estrada, M. March, J. DeRose, L. F. Secco, Josh Frieman, V. Scarpine, Oliver Friedrich, Michael Schubnell, H. T. Diehl, Enrique Gaztanaga, Michael Troxel, T. M. C. Abbott, David Bacon, Martin Crocce, Pablo Fosalba, A. Carnero Rosell, Marcelle Soares-Santos, Niall MacCrann, S. Everett, Peter Melchior, David J. Brooks, R. Cawthon, Elisabeth Krause, E. J. Sanchez, Antonella Palmese, M. A. G. Maia, M. E. C. Swanson, A. A. Plazas, D. L. Burke, S. Santiago, J. Annis, I. Sevilla-Noarbe, T. McClintock, S. Allam, Robert A. Gruendl, J. De Vicente, L. N. da Costa, Santiago Avila, Carlos Solans Sanchez, Chihway Chang, Bhuvnesh Jain, M. D. Johnson, Joe Zuntz, Niall Jeffrey, I. Ferrero, Tim Eifler, G. Gutierrez, M. Gatti, Henry Luce Foundation, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, 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 de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Generalitat de Catalunya, and Fermilab
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Higher education, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Gravitational lensing: weak, Observatory, 0103 physical sciences, media_common.cataloged_instance, MECÂNICA ESTATÍSTICA, European union, Astronomy observatory, 010303 astronomy & astrophysics, media_common, Physics, 010308 nuclear & particles physics, business.industry, European research, Cosmology: observations, Astronomy and Astrophysics, 13. Climate action, Space and Planetary Science, Fundamental physics, Christian ministry, business, National laboratory, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a simulated cosmology analysis using the second and third moments of the weak lensing mass (convergence) maps. The second moment, or variances, of the convergence as a function of smoothing scale contains information similar to standard shear two-point statistics. The third moment, or the skewness, contains additional non-Gaussian information. The analysis is geared towards the third year (Y3) data from the Dark Energy Survey (DES), but the methodology can be applied to other weak lensing data sets. We present the formalism for obtaining the convergence maps from the measured shear and for obtaining the second and third moments of these maps given partial sky coverage. We estimate the covariance matrix from a large suite of numerical simulations. We test our pipeline through a simulated likelihood analyses varying 5 cosmological parameters and 10 nuisance parameters and identify the scales where systematic or modelling uncertainties are not expected to affect the cosmological analysis. Our simulated likelihood analysis shows that the combination of second and third moments provides a 1.5 per cent constraint on S8 σ8(ωm/0.3)0.5 for DES Year 3 data. This is 20 per cent better than an analysis using a simulated DES Y3 shear two-point statistics, owing to the non-Gaussian information captured by the inclusion of higher order statistics. This paper validates our methodology for constraining cosmology with DES Year 3 data, which will be presented in a subsequent paper., 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, Fundac¸ao Carlos Chagas Filho de Amparo ˜ a Pesquisa do ` Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient´ıfico e Tecnologico and the Minist ´ erio da Ci ´ encia, Tecnologia ˆ e Inovac¸ao, the Deutsche Forschungsgemeinschaft and the Collabo- ˜ rating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California, Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y ´ Tecnologicas-Madrid, the University of Chicago, University College ´ London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Z ¨ urich, Fermi ¨ National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the ` Institut de F´ısica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat M¨ unchen, 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 Inter-American 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 Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, 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 7th Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant ˆ 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: 2020

4. Modelling the Milky Way – I. Method and first results fitting the thick disc and halo with DES-Y3 data

Author: Erin Sheldon, M. E. C. Swanson, Alex Drlica-Wagner, R. L. C. Ogando, Enrique Gaztanaga, Andrew B. Pace, L. Girardi, M. Carrasco Kind, David J. Brooks, E. Balbinot, G. Tarle, G. Gutierrez, K. Bechtol, Adriano Pieres, Jennifer L. Marshall, B. Flaugher, Vinu Vikram, Marcelle Soares-Santos, E. Suchyta, A. Carnero Rosell, Juan Garcia-Bellido, E. Bertin, A. A. Plazas, Tenglin Li, Santiago Avila, Daniel Thomas, I. Sevilla-Noarbe, M. dal Ponte, K. Honscheid, J. Gschwend, N. Kuropatkin, Flavia Sobreira, Ramon Miquel, L. N. da Costa, Martin Groenewegen, S. Desai, H. T. Diehl, D. L. Burke, David J. James, Basilio X. Santiago, A. R. Walker, Pablo Fosalba, E. J. Sanchez, Robert A. Gruendl, J. De Vicente, Adam Amara, Kyler Kuehn, Tim Eifler, M. Smith, Daniel Gruen, D. W. Gerdes, D. L. Hollowood, S. Serrano, J. Carretero, Josh Frieman, M. A. G. Maia, 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, Astronomy, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, 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 de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), and German Research Foundation
Subjects: astro-ph.SR, astro-ph.GA, Milky Way, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star count, 01 natural sciences, 7. Clean energy, Galactic halo, 0103 physical sciences, halo [Galaxy], stellar content [Galaxy], Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Galaxy: structure, 010303 astronomy & astrophysics, Stellar density, Solar and Stellar Astrophysics (astro-ph.SR), STFC, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, Galaxy: stellar content, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Galaxy: halo, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Globular cluster, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], structure [Galaxy]
Abstract: Full author list: A Pieres, L Girardi, E Balbinot, B Santiago, L N da Costa, A Carnero Rosell, A B Pace, K Bechtol, M A T Groenewegen, A Drlica-Wagner, T S Li, M A G Maia, R L C Ogando, M dal Ponte, H T Diehl, A Amara, S Avila, E Bertin, D Brooks, D L Burke, M Carrasco Kind, J Carretero, J De Vicente, S Desai, T F Eifler, B Flaugher, P Fosalba, J Frieman, J García-Bellido, E Gaztanaga, D W Gerdes, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, D L Hollowood, K Honscheid, D J James, K Kuehn, N Kuropatkin, J L Marshall, R Miquel, A A Plazas, E Sanchez, S Serrano, I Sevilla-Noarbe, E Sheldon, M Smith, M Soares-Santos, F Sobreira, E Suchyta, M E C Swanson, G Tarle, D Thomas, V Vikram, A R Walker, We present a technique to fit the stellar components of the Galaxy by comparing Hess Diagrams (HDs) generated from TRILEGAL models to real data. We apply this technique, which we call MWFITTING, to photometric data from the first 3 yr of the Dark Energy Survey (DES). After removing regions containing known resolved stellar systems such as globular clusters, dwarf galaxies, nearby galaxies, the Large Magellanic Cloud, and the Sagittarius Stream, our main sample spans a total area of ~2300 deg2. We further explore a smaller subset (~1300 deg2) that excludes all regions with known stellar streams and stellar overdensities. Validation tests on synthetic data possessing similar properties to the DES data show that the method is able to recover input parameters with a precision better than 3 per cent. We fit the DES data with an exponential thick disc model and an oblate double power-law halo model. We find that the best-fitting thick disc model has radial and vertical scale heights of 2.67 ± 0.09 kpc and 925 ± 40 pc, respectively. The stellar halo is fit with a broken power-law density profile with an oblateness of 0.75 ± 0.01, an inner index of 1.82 ± 0.08, an outer index of 4.14 ± 0.05, and a break at 18.52 ± 0.27 kpc from the Galactic centre. Several previously discovered stellar overdensities are recovered in the residual stellar density map, showing the reliability of MWFITTING in determining the Galactic components. Simulations made with the best-fitting parameters are a promising way to predict Milky Way star counts for surveys such as the LSST and Euclid., The DESDM is supported by the National Science Foundation under grants AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, 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 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ci?ncia e Tecnologia (INCT) do e-Universe (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. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. 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 Centre for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Centre for Cosmology and AstroParticle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ão 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 Inovac¸ão, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the DES.
Published: 2020

5. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z ∼ 1

Author: Nikhel Gupta, Tesla E. Jeltema, X. Shao, C. Lidman, Santiago Avila, Vinu Vikram, Michael McDonald, E. Buckley-Geer, David J. Brooks, R. L. C. Ogando, Joseph J. Mohr, M. E. C. Swanson, D. L. Hollowood, V. Scarpine, Shantanu Desai, Maurilio Pannella, Peter Doel, S. Serrano, V. Strazzullo, I-Non Chiu, Matthias Klein, John P. Stott, Enrique Gaztanaga, Robert A. Gruendl, Michael Schubnell, Basilio X. Santiago, J. P. Dietrich, Juan Garcia-Bellido, E. Suchyta, Ramon Miquel, E. J. Sanchez, August E. Evrard, Marcos Lima, Rafe Schindler, J. Annis, Kyler Kuehn, Federico Bianchini, M. Costanzi, J. Gschwend, G. Gutierrez, Christian L. Reichardt, David J. James, A. Saro, Antonella Palmese, A. A. Plazas, L. N. da Costa, M. Smith, I. Sevilla-Noarbe, Daniel Gruen, M. A. G. Maia, S. Everett, F. Paz-Chinchón, J. de Vicente, Jennifer L. Marshall, Esra Bulbul, M. Carrasco Kind, Alfredo Zenteno, J. Carretero, Eli S. Rykoff, A. Carnero Rosell, K. Honscheid, Felipe Menanteau, Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chiu, I., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Mcdonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., and Zenteno, A.
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, galaxies [submillimeter], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, Intracluster medium, 0103 physical sciences, clusters: general [galaxies], 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Luminosity function (astronomy), Physics, Astronomy and Astrophysics, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies: luminosity function, galaxies: clusters: general, mass function, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], galaxies: luminosity function, mass function, High Energy Physics::Experiment, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843~MHz radio AGN population in galaxy clusters from two large catalogs created using the Dark Energy Survey (DES): $\sim$11,800 optically selected RM-Y3 and $\sim$1,000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGN are highly concentrated around cluster centers to $z\sim1$. We measure the halo occupation number for cluster radio AGN above a threshold luminosity, finding that the number of radio AGN per cluster increases with cluster halo mass as $N\propto M^{1.2\pm0.1}$ ($N\propto M^{0.68\pm0.34}$) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad band colors and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGN luminosity function (LF). The LF exhibits a redshift trend of the form $(1+z)^\gamma$ in density and luminosity, respectively, of $\gamma_{\rm D}=3.0\pm0.4$ and $\gamma_{\rm P}=0.21\pm0.15$ in the RM-Y3 sample, and $\gamma_{\rm D}=2.6\pm0.7$ and $\gamma_{\rm P}=0.31\pm0.15$ in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGN, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core ($, Comment: 20 pages, 15 figures Replaced with published version
Published: 2020

6. From the fire: a deeper look at the Phoenix stream

Author: K. Tavangar, P. Ferguson, N. Shipp, A. Drlica-Wagner, S. Koposov, D. Erkal, E. Balbinot, J. García-Bellido, K. Kuehn, G. F. Lewis, T. S. Li, S. Mau, A. B. Pace, A. H. Riley, T. M. C. Abbott, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, H. T. Diehl, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, E. Gaztanaga, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, N. Kuropatkin, M. A. G. Maia, J. L. Marshall, F. Menanteau, R. Miquel, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, M. Rodriguez-Monroy, E. Sanchez, V. Scarpine, S. Serrano, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, T. N. Varga, A. R. Walker, UAM. Departamento de Física Teórica, Tavangar, K [0000-0001-6584-6144], Ferguson, P [0000-0001-6957-1627], Shipp, N [0000-0003-2497-091X], Drlica-Wagner, A [0000-0001-8251-933X], Koposov, S [0000-0003-2644-135X], Erkal, D [0000-0002-8448-5505], Balbinot, E [0000-0002-1322-3153], García-Bellido, J [0000-0002-9370-8360], Kuehn, K [0000-0003-0120-0808], Lewis, GF [0000-0003-3081-9319], Li, TS [0000-0002-9110-6163], Mau, S [0000-0003-3519-4004], Pace, AB [0000-0002-6021-8760], Riley, AH [0000-0001-5805-5766], Aguena, M [0000-0001-5679-6747], Allam, S [0000-0002-7069-7857], Annis, J [0000-0002-0609-3987], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], De Vicente, J [0000-0001-8318-6813], Diehl, HT [0000-0002-8357-7467], Flaugher, B [0000-0002-2367-5049], Frieman, J [0000-0003-4079-3263], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Gruen, D [0000-0003-3270-7644], Gschwend, J [0000-0003-3023-8362], Gutierrez, G [0000-0003-0825-0517], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Kuropatkin, N [0000-0003-2511-0946], Maia, MAG [0000-0001-9856-9307], Marshall, JL [0000-0003-0710-9474], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Ogando, RLC [0000-0003-2120-1154], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Plazas Malagón, AA [0000-0002-2598-0514], Sanchez, E [0000-0002-9646-8198], Sevilla-Noarbe, I [0000-0002-1831-1953], Smith, M [0000-0002-3321-1432], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Walker, AR [0000-0002-7123-8943], Apollo - University of Cambridge Repository, Astronomy, University of Chicago, University of Wisconsin-Madison, Texas AandM University, MIT Kavli Institute for Astrophysics and Space Research, Fermi National Accelerator Laboratory, Royal Observatory, University of Cambridge, University of Surrey, University of Groningen, Universidad Autonoma de Madrid, Lowell Observatory, Macquarie University, The University of Sydney, University of Toronto, Observatories of the Carnegie Institution for Science, Princeton University, Stanford University, Carnegie Mellon University, NSF's National Optical-Infrared Astronomy Research Laboratory, Laboratório Interinstitucional de E-Astronomia-LIneA, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, University College London, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Trieste, Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Universität Hamburg, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Ludwig-Maximilians-Universität, University of Queensland, The Ohio State University, Center for Astrophysics | Harvard and Smithsonian, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, National Science Foundation (US), Department of Energy (US), German Research Foundation, Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Generalitat de Catalunya, Tavangar, K., Ferguson, P., Shipp, N., Drlica-Wagner, A., Koposov, S., Erkal, D., Balbinot, E., García-Bellido, J., Kuehn, K., Lewis, G. F., T. S., Li, Mau, S., Pace, A. B., Riley, A. H., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., and Walker, A. R.
Subjects: Galaxy structure, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar stream, Stellar streams, FOS: Physical sciences, Física, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxies and Cosmology, Cosmology, Dark matter, Astronomy data modeling, Milky Way dynamics, Milky way dynamics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Tavangar et al., We use 6 yr of data from the Dark Energy Survey to perform a detailed photometric characterization of the Phoenix stellar stream, a 15° long, thin, dynamically cold, low-metallicity stellar system in the Southern Hemisphere. We use natural splines, a nonparametric modeling technique, to simultaneously fit the stream track, width, and linear density. This updated stream model allows us to improve measurements of the heliocentric distance (17.4 ± 0.1 (stat.) ±0.8 (sys.) kpc) and distance gradient (−0.009 ± 0.006 kpc deg−1) of Phoenix, which corresponds to a small change of 0.13 ± 0.09 kpc in heliocentric distance along the length of the stream. We measure linear intensity variations on degree scales, as well as deviations in the stream track on ∼2° scales, suggesting that the stream may have been disturbed during its formation and/or evolution. We recover three peaks and one gap in linear intensity along with fluctuations in the stream track. Compared to other thin streams, the Phoenix stream shows more fluctuations and, consequently, the study of Phoenix offers a unique perspective on gravitational perturbations of stellar streams. We discuss possible sources of perturbations to Phoenix, including baryonic structures in the Galaxy and dark matter subhalos., 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 LudwigMaximilians 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. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-20160597, 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 No. CE110001020, and the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2022

7. Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. I. Evidence for Thermal Energy Anisotropy Using Oriented Stacking

Author: M. Lokken, R. Hložek, A. van Engelen, M. Madhavacheril, E. Baxter, J. DeRose, C. Doux, S. Pandey, E. S. Rykoff, G. Stein, C. To, T. M. C. Abbott, S. Adhikari, M. Aguena, S. Allam, F. Andrade-Oliveira, J. Annis, N. Battaglia, G. M. Bernstein, E. Bertin, J. R. Bond, D. Brooks, E. Calabrese, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, R. Cawthon, A. Choi, M. Costanzi, M. Crocce, L. N. da Costa, M. E. da Silva Pereira, J. De Vicente, S. Desai, J. P. Dietrich, P. Doel, J. Dunkley, S. Everett, A. E. Evrard, S. Ferraro, B. Flaugher, P. Fosalba, J. Frieman, P. A. Gallardo, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, T. Giannantonio, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, J. C. Hill, M. Hilton, A. D. Hincks, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, Z. Huang, J. P. Hughes, D. Huterer, B. Jain, D. J. James, T. Jeltema, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, J. McMahon, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, K. Moodley, R. Morgan, F. Nati, L. Page, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas Malagón, A. Pieres, A. K. Romer, E. Rozo, E. Sanchez, V. Scarpine, A. Schillaci, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, E. Sheldon, T. Shin, C. Sifón, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, D. L. Tucker, T. N. Varga, J. Weller, R. H. Wechsler, R. D. Wilkinson, E. J. Wollack, Z. Xu, Lokken, M., Hlozek, R., Engelen, A. V., Madhavacheril, M., Baxter, E., Derose, J., Doux, C., Pandey, S., Rykoff, E. S., Stein, G., To, C., Abbott, T. M. C., Adhikari, S., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Battaglia, N., Bernstein, G. M., Bertin, E., Bond, J. R., Brooks, D., Calabrese, E., Rosell, A. C., Kind, M. C., Carretero, J., Cawthon, R., Choi, A., Costanzi, M., Crocce, M., Costa, L. N. D., Pereira, M. E. D. S., Vicente, J. D., Desai, S., Dietrich, J. P., Doel, P., Dunkley, J., Everett, S., Evrard, A. E., Ferraro, S., Flaugher, B., Fosalba, P., Frieman, J., Gallardo, P. A., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hill, J. C., Hilton, M., Hincks, A. D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huang, Z., Hughes, J. P., Huterer, D., Jain, B., James, D. J., Jeltema, T., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Mcmahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Nati, F., Page, L., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Malagon, A. A. P., Pieres, A., Romer, A. K., Rozo, E., Sanchez, E., Scarpine, V., Schillaci, A., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Sifon, C., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Weller, J., Wechsler, R. H., Wilkinson, R. D., Wollack, E. J., Xu, Z., Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Generalitat de Catalunya, European Research Council, Ministerio de Economía y Competitividad (España), Lokken, M, Hlozek, R, Engelen, A, Madhavacheril, M, Baxter, E, Derose, J, Doux, C, Pandey, S, Rykoff, E, Stein, G, To, C, Abbott, T, Adhikari, S, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Battaglia, N, Bernstein, G, Bertin, E, Bond, J, Brooks, D, Calabrese, E, Rosell, A, Kind, M, Carretero, J, Cawthon, R, Choi, A, Costanzi, M, Crocce, M, Costa, L, Pereira, M, Vicente, J, Desai, S, Dietrich, J, Doel, P, Dunkley, J, Everett, S, Evrard, A, Ferraro, S, Flaugher, B, Fosalba, P, Frieman, J, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Gerdes, D, Giannantonio, T, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hill, J, Hilton, M, Hincks, A, Hinton, S, Hollowood, D, Honscheid, K, Hoyle, B, Huang, Z, Hughes, J, Huterer, D, Jain, B, James, D, Jeltema, T, Kuehn, K, Lima, M, Maia, M, Marshall, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Nati, F, Page, L, Ogando, R, Palmese, A, Paz-Chinchon, F, Malagon, A, Pieres, A, Romer, A, Rozo, E, Sanchez, E, Scarpine, V, Schillaci, A, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Sifon, C, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, Tucker, D, Varga, T, Weller, J, Wechsler, R, Wilkinson, R, Wollack, E, and Xu, Z
Subjects: cosmic web, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ENERGIA TÉRMICA, Space and Planetary Science, cluster of galaxies, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmic web, CMB, SZ effect, cosmology, cluster of galaxie, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Lokken et al., The cosmic web contains filamentary structure on a wide range of scales. On the largest scales, superclustering aligns multiple galaxy clusters along intercluster bridges, visible through their thermal Sunyaev–Zel'dovich signal in the cosmic microwave background. We demonstrate a new, flexible method to analyze the hot gas signal from multiscale extended structures. We use a Compton y-map from the Atacama Cosmology Telescope (ACT) stacked on redMaPPer cluster positions from the optical Dark Energy Survey (DES). Cutout images from the y-map are oriented with large-scale structure information from DES galaxy data such that the superclustering signal is aligned before being overlaid. We find evidence of an extended quadrupole moment of the stacked y signal at the 3.5σ level, demonstrating that the large-scale thermal energy surrounding galaxy clusters is anisotropically distributed. We compare our ACT × DES results with the Buzzard simulations, finding broad agreement. Using simulations, we highlight the promise of this novel technique for constraining the evolution of anisotropic, non-Gaussian structure using future combinations of microwave and optical surveys., J.R.B. was funded by the Natural Sciences and Engineering Research Council of Canada Discovery Grant Program and a fellowship from the Canadian Institute for Advanced Research (CIFAR) Gravity and Extreme Universe program. A.D.H. acknowledges support from the Sutton Family Chair in Science, Christianity and Cultures. R.H. is a CIFAR Azrieli Global Scholar, Gravity and the Extreme Universe Program, 2019, and a 2020 Alfred P. Sloan Research Fellow. R.H. is supported by the Natural Sciences and Engineering Research Council of Canada Discovery Grant Program and the Connaught Fund. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. J.P.H. acknowledges funding for SZ cluster studies from NSF AAG No. AST-1615657. M.L. acknowledges the support of the National Sciences and Engineering Research Council of Canada (NSERC) [PGSD - 559296 - 2021] and the Queen Elizabeth II / Graduate Scholarships in Science and Technology (QEII-GSST). K.M. acknowledges support from the National Research Foundation of South Africa. This work was supported by the U.S. National Science Foundation through awards AST-0408698, AST-0965625, and AST-1440226 for the ACT project, as well as awards PHY-0355328, PHY-0855887, and PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronómico Atacama in northern Chile under the auspices of the Comisión Nacional de Investigación (CONICYT). The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. Detector research at NIST was supported by the NIST Innovations in Measurement Science program. 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' 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 Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grant Nos. 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 Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). We thank the anonymous referee for providing valuable comments which improved the quality of the manuscript. 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. This work received support from the U.S. Department of Energy under contract No. DE-AC02-76SF00515 at SLAC National Accelerator Laboratory. This research used computing resources at SLAC National Accelerator Laboratory and at the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility located at Lawrence Berkeley National Laboratory, operated under contract No. DE-AC02-05CH11231.
Published: 2022

8. Dark Energy Survey Y3 results: blending shear and redshift biases in image simulations

Author: Matthew R. Becker, J. Carretero, F. Paz-Chinchón, F. Tarsitano, Brian Yanny, Josh Frieman, David J. Brooks, M. March, Erin Sheldon, Martin Crocce, R. D. Wilkinson, Antonella Palmese, Carlos Solans Sanchez, M. Smith, M Rodriguez-Monroy, Peter Doel, R. L. C. Ogando, M. A. G. Maia, W. G. Hartley, Adriano Pieres, Daniel Gruen, J. Myles, D. L. Burke, V. Scarpine, B. Flaugher, H. T. Diehl, J. P. Dietrich, Juan Garcia-Bellido, D. W. Gerdes, David J. James, David Bacon, Alexandra Amon, G. Tarle, I. Harrison, Pablo Fosalba, Niall MacCrann, Agnès Ferté, J. Annis, E. Suchyta, I. Sevilla-Noarbe, S. Allam, Robert A. Gruendl, M. Soares-Santos, Peter Melchior, Maria E. S. Pereira, J. McCullough, K. D. Eckert, Daniel Thomas, K. Herner, T. N. Varga, Felipe Menanteau, M. Costanzi, E. Bertin, M. Gatti, M. Carrasco Kind, T. M. C. Abbott, Ramon Miquel, Michael Troxel, Paul Martini, Jennifer L. Marshall, J. Muir, Enrique Gaztanaga, J. Gschwend, A. Choi, D. L. Hollowood, A. Alarcon, Gary Bernstein, M. E. C. Swanson, Ofer Lahav, E. M. Huff, Chun-Hao To, K. Honscheid, A. Roodman, Tommaso Giannantonio, Samuel Hinton, E. J. Sanchez, Michel Aguena, S. Serrano, Robert Morgan, G. Gutierrez, Joe Zuntz, R. P. Rollins, A. Carnero Rosell, I. Ferrero, Matt J. Jarvis, Marcos Lima, Sarah Bridle, Scott Dodelson, Tim Eifler, S. Desai, Joseph J. Mohr, S. Everett, S. Samuroff, A. A. Plazas, L. F. Secco, J. de Vicente, Maccrann, N, Becker, M R, Mccullough, J, Amon, A, Gruen, D, Jarvis, M, Choi, A, Troxel, M A, Sheldon, E, Yanny, B, Herner, K, Dodelson, S, Zuntz, J, Eckert, K, Rollins, R P, Varga, T N, Bernstein, G M, Gruendl, R A, Harrison, I, Hartley, W G, Sevilla-Noarbe, I, Pieres, A, Bridle, S L, Myles, J, Alarcon, A, Everett, S, Sánchez, C, Huff, E M, Tarsitano, F, Gatti, M, Secco, L F, Abbott, T M C, Aguena, M, Allam, S, Annis, J, Bacon, D, Bertin, E, Brooks, D, Burke, D L, Carnero&nbsp, Rosell, A, Carrasco&nbsp, Kind, M, Carretero, J, Costanzi, M, Crocce, M, Pereira, M E S, De&nbsp, Vicente, J, Desai, S, Diehl, H&nbsp, T, Dietrich, J P, Doel, P, Eifler, T F, Ferrero, I, Ferté, A, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Giannantonio, T, Gschwend, J, Gutierrez, G, Hinton, S R, Hollowood, D L, Honscheid, K, James, D J, Lahav, O, Lima, M, Maia, M A G, March, M, Marshall, J L, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Mohr, J J, Morgan, R, Muir, J, Ogando, R L C, Palmese, A, Paz-Chinchón, F, Plazas, A A, Rodriguez-Monroy, M, Roodman, A, Samuroff, S, Sanchez, E, Scarpine, V, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, To, C, Wilkinson, R D, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), European Research Council, Department of Energy (US), National Aeronautics and Space Administration (US), and Fondo Nacional de Desarrollo Científico y Tecnológico (Chile)
Subjects: Physics, Large-scale structure of Universe, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Image (mathematics), gravitational lensing: weak, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Shear (sheet metal), Space and Planetary Science, Gravitational lensing: weak, weak [gravitational lensing], 0103 physical sciences, Dark energy, 010303 astronomy & astrophysics
Abstract: DES Collaboration: N. MacCrann et al., As the statistical power of galaxy weak lensing reaches per cent level precision, large, realistic, and robust simulations are required to calibrate observational systematics, especially given the increased importance of object blending as survey depths increase. To capture the coupled effects of blending in both shear and photometric redshift calibration, we define the effective redshift distribution for lensing, nγ(z), and describe how to estimate it using image simulations. We use an extensive suite of tailored image simulations to characterize the performance of the shear estimation pipeline applied to the Dark Energy Survey (DES) Year 3 data set. We describe the multiband, multi-epoch simulations, and demonstrate their high level of realism through comparisons to the real DES data. We isolate the effects that generate shear calibration biases by running variations on our fiducial simulation, and find that blending-related effects are the dominant contribution to the mean multiplicative bias of approximately −2 per cent ⁠. By generating simulations with input shear signals that vary with redshift, we calibrate biases in our estimation of the effective redshift distribution, and demonstrate the importance of this approach when blending is present. We provide corrected effective redshift distributions that incorporate statistical and systematic uncertainties, ready for use in DES Year 3 weak lensing analyses., 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 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) 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. NM acknowledges support from a European Research Council (ERC) Starting Grant under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 851274). MRB is supported by DOE grant DE-AC02-06CH11357. This work was supported by the Department of Energy, Laboratory Directed Research and Development program at SLAC National Accelerator Laboratory, under contract DE-AC02-76SF00515 and as part of the Panofsky Fellowship awarded to DG. MJ is partially supported by the U.S. Department of Energy grant DE-SC0007901 and funds from the University of Pennsylvania. AC acknowledges support from NASA grant 15-WFIRST15-0008. RR, IH, and SB acknowledge support from the European Research Council in the form of a Consolidator Grant with number 681431. IH also acknowledges support from the Beecroft Trust. We gratefully acknowledge the computing resources provided on Bebop, a high-performance computing cluster operated by the Laboratory Computing Resource Center at Argonne National Laboratory, and the RHIC Atlas Computing Facility, operated by Brookhaven National Laboratory. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231.
Published: 2022

9. Cosmic shear in harmonic space from the Dark Energy Survey Year 1 Data: compatibility with configuration space results

Author: H Camacho, F Andrade-Oliveira, A Troja, R Rosenfeld, L Faga, R Gomes, C Doux, X Fang, M Lima, V Miranda, T F Eifler, O Friedrich, M Gatti, G M Bernstein, J Blazek, S L Bridle, A Choi, C Davis, J DeRose, E Gaztanaga, D Gruen, W G Hartley, B Hoyle, M Jarvis, N MacCrann, J Prat, M M Rau, S Samuroff, C Sánchez, E Sheldon, M A Troxel, P Vielzeuf, J Zuntz, T M C Abbott, M Aguena, S Allam, J Annis, D Bacon, E Bertin, D Brooks, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, R Cawthon, M Costanzi, L N da Costa, M E S Pereira, J De Vicente, S Desai, H T Diehl, P Doel, S Everett, A E Evrard, I Ferrero, B Flaugher, P Fosalba, D Friedel, J Frieman, J García-Bellido, D W Gerdes, R A Gruendl, J Gschwend, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D Huterer, D J James, K Kuehn, N Kuropatkin, O Lahav, M A G Maia, J L Marshall, P Melchior, F Menanteau, R Miquel, R Morgan, F Paz-Chinchón, D Petravick, A Pieres, A A Plazas Malagón, K Reil, M Rodriguez-Monroy, E Sanchez, V Scarpine, M Schubnell, S Serrano, I Sevilla-Noarbe, M Smith, M Soares-Santos, E Suchyta, G Tarle, D Thomas, C To, T N Varga, J Weller, R D Wilkinson, (D E S Collaboration), Camacho, H., Andrade-Oliveira, F., Troja, A., Rosenfeld, R., Faga, L., Gomes, R., Doux, C., Fang, X., Lima, M., Miranda, V., Eifler, T. F., Friedrich, O., Gatti, M., Bernstein, G. M., Blazek, J., Bridle, S. L., Choi, A., Davis, C., Derose, J., Gaztanaga, E., Gruen, D., Hartley, W. G., Hoyle, B., Jarvis, M., Maccrann, N., Prat, J., Rau, M. M., Samuroff, S., Sánchez, C., Sheldon, E., Troxel, M. A., Vielzeuf, P., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plaza, Reil, K., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., and Des, Collaboration
Subjects: observation, model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), consistency, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, gravitational lensing: weak, weak [gravitational lensing], Space and Planetary Science, cosmology: observations, impact, astro-ph.CO, precision, LENTES GRAVITACIONAIS, (cosmology:) large-scale structure of Universe, large-scale structure of Universe, cosmology, physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a cosmic shear analysis in harmonic space using the first year of data collected by the Dark Energy Survey (DES-Y1). We measure the cosmic weak lensing shear power spectra using the Metacalibration catalogue and perform a likelihood analysis within the framework of CosmoSIS. We set scale cuts based on baryonic effects contamination and model redshift and shear calibration uncertainties as well as intrinsic alignments. We adopt as fiducial covariance matrix an analytical computation accounting for the mask geometry in the Gaussian term, including non-Gaussian contributions. A suite of 1200 lognormal simulations is used to validate the harmonic space pipeline and the covariance matrix. We perform a series of stress tests to gauge the robustness of the harmonic space analysis. Finally, we use the DES-Y1 pipeline in configuration space to perform a similar likelihood analysis and compare both results, demonstrating their compatibility in estimating the cosmological parameters $S_8$, $\sigma_8$ and $\Omega_m$. The methods implemented and validated in this paper will allow us to perform a consistent harmonic space analysis in the upcoming DES data., Comment: 16 pages, 11 figures. This version matches the published one
Published: 2022

10. The Evolution of AGN Activity in Brightest Cluster Galaxies

Author: T. Somboonpanyakul, M. McDonald, A. Noble, M. Aguena, S. Allam, A. Amon, F. Andrade-Oliveira, D. Bacon, M. B. Bayliss, E. Bertin, S. Bhargava, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Calzadilla, R. Canning, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, P. Doel, P. Eisenhardt, S. Everett, A. E. Evrard, I. Ferrero, B. Flaugher, B. Floyd, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, A. Gonzalez, D. Gruen, R. A. Gruendl, J. Gschwend, N. Gupta, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. J. James, T. Jeltema, G. Khullar, K. J. Kim, M. Klein, K. Kuehn, M. Lima, M. A. G. Maia, J. L. Marshall, P. Martini, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. Pieres, A. A. Plazas Malagón, K. Reil, A. K. Romer, F. Ruppin, E. Sanchez, A. Saro, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, P. Singh, M. Smith, M. Soares-Santos, V. Strazzullo, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, D. L. Tucker, R. D. Wilkinson, National Aeronautics and Space Administration (US), National Science Foundation (US), Department of Energy (US), Somboonpanyakul, T., Mcdonald, M., Noble, A., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Bacon, D., Bayliss, M. B., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Calzadilla, M., Canning, R., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Doel, P., Eisenhardt, P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Floyd, B., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gonzalez, A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, N., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Khullar, G., Kim, K. J., Klein, M., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Romer, A. K., Ruppin, F., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Singh, P., Smith, M., Soares-Santos, M., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Tucker, D. L., Wilkinson, R. D., UAM. Departamento de Física Teórica, Massachusetts Institute of Technology, Stanford University, Arizona State University, Laboratório Interinstitucional de E-Astronomia - LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), University of Portsmouth, University of Cincinnati, Institut d'Astrophysique de Paris, University of Sussex, University College London, University of Chicago, SLAC National Accelerator Laboratory, Instituto de Astrofisica de Canarias, Dpto. Astrofìsica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, University of Trieste, Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, IObservatório Nacional, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), California Institute of Technology, Santa Cruz Institute for Particle Physics, University of Oslo, University of Missouri-Kansas City, Universidad Autonoma de Madrid, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Florida, Ludwig-Maximilians-Universität, CSIRO Astronomy and Space Science, University of Queensland, The Ohio State University, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Max Planck Institute for Extraterrestrial Physics, University of Wisconsin-Madison, National Institute for Nuclear Physics, University of Southampton, Osservatorio Astronomico di Brera, and Oak Ridge National Laboratory
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Física, Active Galactic Nuclei, Astronomy and Astrophysics, GALÁXIAS, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, cluster fo galaxies, AGN, Radio Jets (Astronomy), cluster fo galaxie, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics
Abstract: Somboonpanyakul et al., We present the results of an analysis of Wide-field Infrared Survey Explorer (WISE) observations of the full 2500 deg2 South Pole Telescope (SPT)-Sunyaev–Zel'dovich cluster sample. We describe a process for identifying active galactic nuclei (AGN) in brightest cluster galaxies (BCGs) based on WISE mid-IR color and redshift. Applying this technique to the BCGs of the SPT-SZ sample, we calculate the AGN-hosting BCG fraction, which is defined as the fraction of BCGs hosting bright central AGNs over all possible BCGs. Assuming an evolving single-burst stellar population model, we find statistically significant evidence (>99.9%) for a mid-IR excess at high redshift compared to low redshift, suggesting that the fraction of AGN-hosting BCGs increases with redshift over the range of 0 < z < 1.3. The best-fit redshift trend of the AGN-hosting BCG fraction has the form (1 + z)4.1±1.0. These results are consistent with previous studies in galaxy clusters as well as as in field galaxies. One way to explain this result is that member galaxies at high redshift tend to have more cold gas. While BCGs in nearby galaxy clusters grow mostly by dry mergers with cluster members, leading to no increase in AGN activity, BCGs at high redshift could primarily merge with gas-rich satellites, providing fuel for feeding AGNs. If this observed increase in AGN activity is linked to gas-rich mergers rather than ICM cooling, we would expect to see an increase in scatter in the Pcav versus Lcool relation at z > 1. Last, this work confirms that the runaway cooling phase, as predicted by the classical cooling-flow model, in the Phoenix cluster is extremely rare and most BCGs have low (relative to Eddington) black hole accretion rates., T.S. and M.M. acknowledge support from the Kavli Research Investment Fund at MIT, and from NASA through Chandra grant GO5-16143. F.R. acknowledges financial support provided by NASA through SAO Award Number SV2-82023 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. 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 Cientìfico 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 Enérgeticas, 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 Fìsica 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 OzDES Membership Consortium, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.
Published: 2022

11. Galaxy–galaxy lensing with the DES-CMASS catalogue: measurement and constraints on the galaxy-matter cross-correlation

Author: J. De Vicente, A. A. Plazas Malagón, M. March, W. G. Hartley, J. P. Dietrich, David J. Brooks, Juan Garcia-Bellido, Christopher M. Hirata, Dragan Huterer, Joseph J. Mohr, Jochen Weller, J. Carretero, F. J. Castander, G. Tarle, Carlos Solans Sanchez, E. Bertin, Adriano Pieres, Jack Elvin-Poole, B. Flaugher, M. Carrasco Kind, A. Roodman, F. Andrade-Oliveira, Tommaso Giannantonio, Samuel Hinton, V. Scarpine, Peter Doel, Chun-Hao To, David J. James, G. Gutierrez, Jennifer L. Marshall, E. J. Sanchez, M Gatti, J. DeRose, Ramon Miquel, Josh Frieman, Pablo Fosalba, Joe Zuntz, Maria E. S. Pereira, S. Lee, E. Suchyta, August E. Evrard, Enrique Gaztanaga, Erin Sheldon, Daniel Thomas, H. T. Diehl, Ofer Lahav, Y. Omori, M. Costanzi, A. Carnero Rosell, R. Cawthon, Robert Morgan, Ashley J. Ross, I. Ferrero, P. Vielzeuf, Michael Schubnell, Tim Eifler, Chihway Chang, Niall MacCrann, S. Desai, E. M. Huff, C. Davis, Michel Aguena, D. L. Burke, J. Gschwend, Gary Bernstein, S. Allam, Robert A. Gruendl, S. Samuroff, Ami Choi, Ben Hoyle, Antonella Palmese, M. A. G. Maia, I. Sevilla-Noarbe, N. Kuropatkin, T. N. Varga, L. N. da Costa, J. Prat, M. E. C. Swanson, Alexandra Amon, Felipe Menanteau, K. Honscheid, Michael Troxel, Marcos Lima, S. Everett, Kyler Kuehn, M. Smith, D. L. Hollowood, S. Serrano, Daniel Gruen, D. W. Gerdes, Christopher J. Conselice, Markus Rau, F. Paz-Chinchón, Lee, S., Troxel, M. A., Choi, A., Elvin-Poole, J., Hirata, C., Honscheid, K., Huff, E. M., Maccrann, N., Ross, A. J., Eifler, T. F., Chang, C., Miquel, R., Omori, Y., Prat, J., Bernstein, G. M., Davis, C., Derose, J., Gatti, M., Rau, M. M., Samuroff, S., Sanchez, C., Vielzeuf, P., Zuntz, J., Aguena, M., Allam, S., Amon, A., Andrade-Oliveira, F., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Castander, F. J., Cawthon, R., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., de Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Hoyle, B., Huterer, D., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A. A. P., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Duke University, Ohio State University, California Institute of Technology, University of Cambridge, University of Arizona, University of Chicago, Institució Catalana de Recerca i Estudis Avançats, Barcelona Institute of Science and Technology, Stanford University, University of Pennsylvania, 501 Campbell Hall, Santa Cruz Institute for Particle Physics, Carnegie Mellon University, University of Edinburgh, Universidade de São Paulo (USP), Laboratório Interinstitucional de e-Astronomia - LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Institut d’Astrophysique de Paris, University College London, SLAC National Accelerator Laboratory, Instituto de Astrofisica de Canarias, Dpto. Astrofisica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Institut d’Estudis Espacials de Catalunya (IEEC), CSIC), University of Wisconsin-Madison, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), IIT Hyderabad, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Geneva, University of Queensland, Max Planck Institute for Extraterrestrial Physics, Harvard & Smithsonian, Macquarie University, Lowell Observatory, Texas A&M University, Peyton Hall, Brookhaven National Laboratory, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Ludwig-Maximilians Universität München, 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, UAM. Departamento de Física Teórica, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Simons Foundation, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, European Space Agency, and European Research Council
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cross-correlation, Gravitational lensing, Large-scale structure of universe, Física, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, Large-scale structure of the Universe, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES collaboration: et al., The DMASS sample is a photometric sample from the DES Year 1 data set designed to replicate the properties of the CMASS sample from BOSS, in support of a joint analysis of DES and BOSS beyond the small overlapping area. In this paper, we present the measurement of galaxy–galaxy lensing using the DMASS sample as gravitational lenses in the DES Y1 imaging data. We test a number of potential systematics that can bias the galaxy–galaxy lensing signal, including those from shear estimation, photometric redshifts, and observing conditions. After careful systematic tests, we obtain a highly significant detection of the galaxy–galaxy lensing signal, with total S/N = 25.7. With the measured signal, we assess the feasibility of using DMASS as gravitational lenses equivalent to CMASS, by estimating the galaxy-matter cross-correlation coefficient rcc. By jointly fitting the galaxy–galaxy lensing measurement with the galaxy clustering measurement from CMASS, we obtain rcc=1.09+0.12−0.11 for the scale cut of 4h−1Mpc and rcc=1.06+0.13−0.12 for 12h−1Mpc in fixed cosmology. By adding the angular galaxy clustering of DMASS, we obtain rcc = 1.06 ± 0.10 for the scale cut of 4h−1Mpc and rcc = 1.03 ± 0.11 for 12h−1Mpc⁠. The resulting values of rcc indicate that the lensing signal of DMASS is statistically consistent with the one that would have been measured if CMASS had populated the DES region within the given statistical uncertainty. The measurement of galaxy–galaxy lensing presented in this paper will serve as part of the data vector for the forthcoming cosmology analysis in preparation., AC acknowledges support from NASA grant 15-WFIRST15-0008. During the preparation of this paper, C.H. was supported by the Simons Foundation, NASA, and the U.S. Department of Energy. 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. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This work used resources at the Owens Cluster at the Ohio Supercomputer Center (OSC 1987) and the Duke Compute Cluster (DCC) at Duke University.
Published: 2022

12. Multi-wavelength Optical and NIR Variability Analysis of the Blazar PKS 0027-426

Author: E Guise, S F Hönig, T Almeyda, K Horne, M Kishimoto, M Aguena, S Allam, F Andrade-Oliveira, J Asorey, M Banerji, E Bertin, B Boulderstone, D Brooks, D L Burke, A Carnero Rosell, D Carollo, M Carrasco Kind, J Carretero, M Costanzi, L N da Costa, T M Davis, J De Vicente, P Doel, S Everett, I Ferrero, B Flaugher, J Frieman, P Gandhi, M Goad, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D J James, M A C Johnson, K Kuehn, G F Lewis, C Lidman, M Lima, M A G Maia, U Malik, F Menanteau, R Miquel, R Morgan, R L C Ogando, A Palmese, F Paz-Chinchón, M E S Pereira, A Pieres, A A Plazas Malagón, E Sanchez, V Scarpine, S Serrano, I Sevilla-Noarbe, N Seymour, M Smith, M Soares-Santos, E Suchyta, M E C Swanson, G Tarle, C To, B E Tucker, Univ Southampton, South Carolina State Univ, Univ St Andrews, Kyoto Sangyo Univ, Lab Interinst E Astron LIneA, Fermilab Natl Accelerator Lab, Universidade Estadual Paulista (UNESP), Ctr Invest Energet Medioambientales & Tecnol CIEM, Univ Cambridge, Inst Astrophys Paris, Sorbonne Univ, UCL, Stanford Univ, SLAC Natl Accelerator Lab, Inst Astrofis Canarias, Univ La Laguna, Astrophys Observ Turin, Natl Ctr Supercomp Applicat, Univ Illinois, Barcelona Inst Sci & Technol, Univ Trieste, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Observ Nacl, Univ Queensland, Santa Cruz Inst Particle Phys, Univ Oslo, Univ Chicago, Univ Leicester, Ludwig Maximilians Univ Munchen, Ohio State Univ, Ctr Astrophys Harvard & Smithsonian, DLR Inst Data Sci, Max Planck Inst Radioastron, Macquarie Univ, Lowell Observ, Univ Sydney, Australian Natl Univ, Universidade de São Paulo (USP), Inst Catalana Recerca & Estudis Avancats, Univ Wisconsin, Univ Michigan, Princeton Univ, Inst Estudis Espacials Catalunya IEEC, CSIC, Curtin Univ, Oak Ridge Natl Lab, Inst Catalan Recerca & Estudis Avancats, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Guise, E, Hönig, S F, Almeyda, T, Horne, K, Kishimoto, M, Aguena, M, Allam, S, Andrade-Oliveira, F, Asorey, J, Banerji, M, Bertin, E, Boulderstone, B, Brooks, D, Burke, D L, Rosell, A Carnero, Carollo, D, Kind, M Carrasco, Carretero, J, Costanzi, M, da Costa, L N, Davis, T M, De Vicente, J, Doel, P, Everett, S, Ferrero, I, Flaugher, B, Frieman, J, Gandhi, P, Goad, M, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hinton, S R, Hollowood, D L, Honscheid, K, James, D J, Johnson, M A C, Kuehn, K, Lewis, G F, Lidman, C, Lima, M, Maia, M A G, Malik, U, Menanteau, F, Miquel, R, Morgan, R, Ogando, R L C, Palmese, A, Paz-Chinchón, F, Pereira, M E S, Pieres, A, Malagón, A A Plaza, Sanchez, E, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Seymour, N, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, To, C, and Tucker, B E
Subjects: quasars individual PKS 0027-426, Astrophysics::High Energy Astrophysical Phenomena, galaxies active, jets [galaxies], FOS: Physical sciences, galaxies jets, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Astrophysic, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Astrophysics of Galaxie, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena, QC, Astrophysics::Galaxy Astrophysics, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies, 010308 nuclear & particles physics, galaxies jet, Astronomy and Astrophysics, DAS, Astrophysics - Astrophysics of Galaxies, individual: PKS 0027-426 [quasars], QC Physics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present multi-wavelength spectral and temporal variability analysis of PKS 0027-426 using optical griz observations from DES (Dark Energy Survey) between 2013-2018 and VOILETTE (VEILS Optical Light curves of Extragalactic TransienT Events) between 2018-2019 and near infrared (NIR) JKs observations from VEILS (VISTAExtragalactic Infrared Legacy Survey) between 2017-2019. Multiple methods of cross-correlation of each combination of light curve provides measurements of possible lags between optical-optical, optical-NIR, and NIR-NIR emission, for each observation season and for the entire observational period. Inter-band time lag measurements consistently suggest either simultaneous emission or delays between emission regions on timescales smaller than the cadences of observations. The colour-magnitude relation between each combination of filters was also studied to determine the spectral behaviour of PKS 0027-426. Our results demonstrate complex colour behaviour that changes between bluer when brighter (BWB), stable when brighter (SWB) and redder when brighter (RWB) trends over different timescales and using different combinations of optical filters. Additional analysis of the optical spectra is performed to provide further understanding of this complex spectral behaviour., Accepted for publication in MNRAS. 33 pages, 28 figures, 11 tables
Published: 2021

13. The PAU survey: estimating galaxy photometry with deep learning

Author: J. Carretero, Ramon Miquel, Martin Eriksen, F. J. Castander, E. J. Sanchez, Ricard Casas, Enrique Gaztanaga, I. Sevilla-Noarbe, S. Serrano, Hendrik Hildebrandt, C. Padilla, P. Tallada-Crespí, Enrique Fernández, Laura Cabayol, Juan Garcia-Bellido, J. De Vicente, Adam Amara, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Durham University, Netherlands Organization for Scientific Research, German Research Foundation, and University College London
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, FOS: Physical sciences, Techniques: image processing, Probability density function, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), Background noise, Observatory, 0103 physical sciences, image processing [Techniques], Astrophysics::Solar and Stellar Astrophysics, observations [Cosmology], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, photometry [Galaxies], photometric [Techniques], Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxies: photometry, Galaxy, Redshift, Space and Planetary Science, Outlier, Techniques: photometric, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: With the dramatic rise in high-quality galaxy data expected from Euclid and Vera C. Rubin Observatory, there will be increasing demand for fast high-precision methods for measuring galaxy fluxes. These will be essential for inferring the redshifts of the galaxies. In this paper, we introduce LUMOS, a deep learning method to measure photometry from galaxy images. LUMOS builds on BKGNET, an algorithm to predict the background and its associated error, and predicts the background-subtracted flux probability density function. We have developed LUMOS for data from the Physics of the Accelerating Universe Survey (PAUS), an imaging survey using a 40 narrow-band filter camera (PAUCam). PAUCam images are affected by scattered light, displaying a background noise pattern that can be predicted and corrected for. On average, LUMOS increases the SNR of the observations by a factor of 2 compared to an aperture photometry algorithm. It also incorporates other advantages like robustness towards distorting artefacts, e.g. cosmic rays or scattered light, the ability of deblending and less sensitivity to uncertainties in the galaxy profile parameters used to infer the photometry. Indeed, the number of flagged photometry outlier observations is reduced from 10 to 2 per cent, comparing to aperture photometry. Furthermore, with LUMOS photometry, the photo-z scatter is reduced by ≈10 per cent with the Deepz machine-learning photo-z code and the photo-z outlier rate by 20 per cent. The photo-z improvement is lower than expected from the SNR increment, however, currently the photometric calibration and outliers in the photometry seem to be its limiting factor., The PAU Survey is partially supported by MINECO under grants CSD2007-00060, AYA2015-71825, ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509, PID2019-111317GB-C31 and Juan de la Cierva fellowship and LACEGAL and EWC Marie Sklodowska-Curie grant No 734374 and no.776247 with ERDF funds from the EU Horizon 2020 Programme, some of which include ERDF funds from the European Union. IEEC and IFAE are partially funded by the CERCA and Beatriu de Pinos program of the Generalitat de Catalunya. Funding for PAUS has also been provided by Durham University (via the ERC StG DEGAS-259586), ETH Zurich, Leiden University (via ERC StG ADULT-279396 and Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512), Bochum University (via a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1) as well as an ERC Consolidator Grant (No. 770935)), University College London, Portsmouth support through the Royal Society Wolfson fellowship and from the European Union’s Horizon 2020 research and innovation programme under the grant agreement No 776247 EWC.
Published: 2021

14. Assessing tension metrics with dark energy survey and Planck data

Author: Martin Crocce, Antonella Palmese, G. Tarle, I. Ferrero, Matt J. Jarvis, Samuel Hinton, J. Myles, David J. James, G. Gutierrez, Tim Eifler, M. A. G. Maia, M. Rodriguez-Monroy, A. Roodman, Tommaso Giannantonio, R. P. Rollins, Pablo Fosalba, D. L. Burke, J. De Vicente, J. DeRose, E. Suchyta, M Gatti, Josh Frieman, Elisabeth Krause, M. Costanzi, M. E. C. Swanson, W. G. Hartley, Joseph J. Mohr, Ben Hoyle, August E. Evrard, Juan Garcia-Bellido, Daniel Thomas, S. Samuroff, Jack Elvin-Poole, Enrique Gaztanaga, I. Harrison, M. March, Markus Rau, S. Pandey, J. Muir, S. Allam, Robert A. Gruendl, Peter Melchior, Ofer Lahav, A. A. Plazas Malagón, J. Carretero, Tamara M. Davis, E. Bertin, Michael Schubnell, B. Flaugher, V. Scarpine, Maria E. S. Pereira, Felipe Menanteau, E. M. Huff, P. Lemos, Michel Aguena, M. Carrasco Kind, W. C. Wester, Michael Troxel, A. Choi, Robert Morgan, Youngsoo Park, J. Gschwend, K. Honscheid, Gary Bernstein, I. Sevilla-Noarbe, R. L. C. Ogando, R. Cawthon, M. Soares-Santos, Ramon Miquel, A. Carnero Rosell, Christopher J. Conselice, D. L. Hollowood, N. Weaverdyck, Peter Doel, Marco Raveri, K. D. Eckert, T. N. Varga, H. T. Diehl, David Bacon, Niall MacCrann, S. Serrano, Paul Martini, A. Campos, Agnès Ferté, David J. Brooks, J. Prat, S. Everett, Marcos Lima, M. Smith, Daniel Gruen, Jennifer L. Marshall, Dragan Huterer, D. W. Gerdes, J. Annis, Joe Zuntz, F. Paz-Chinchón, Andrew R. Liddle, Jochen Weller, F. J. Castander, C. Doux, Chun-Hao To, E. J. Sanchez, Jonathan Blazek, L. F. Secco, Scott Dodelson, Santiago Avila, Chihway Chang, S. Desai, UAM. Departamento de Física Teórica, Lemos, P., Raveri, M., Campos, A., Park, Y., Chang, C., Weaverdyck, N., Huterer, D., Liddle, A. R., Blazek, J., Cawthon, R., Choi, A., Derose, J., Dodelson, S., Doux, C., Gatti, M., Gruen, D., Harrison, I., Krause, E., Lahav, O., Maccrann, N., Muir, J., Prat, J., Rau, M. M., Rollins, R. P., Samuroff, S., Zuntz, J., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Crocce, M., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., James, D. J., Jarvis, M., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Pandey, S., Paz-Chinchón, F., Plazas Malagón, A. A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Varga, T. N., Weller, J., Wester, W., Des, Collaboration, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Fermilab, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Statistical [Methods], Physics beyond the Standard Model, Cosmic microwave background, FOS: Physical sciences, Lambda-CDM model, robustness, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology: Observations, Observations [Cosmology], Cosmological parameters, Cosmology: observations, Methods: statistical, Methods: Statistical, Bayes' theorem, symbols.namesake, statistical, cosmological parameters, cosmology: observations [methods], 0103 physical sciences, ST/T000473/1, Statistical physics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Planck, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, STFC, Physics, inference, cosmological constant, 010308 nuclear & particles physics, Tension (physics), methods: statistical, cosmological parameters, cosmology: observations, Estimator, RCUK, Física, Astronomy and Astrophysics, ST/R000476/1, universe, Astronomía, Space and Planetary Science, symbols, Dark energy, Cosmological Parameters, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Lemos, P. et al., Quantifying tensions – inconsistencies amongst measurements of cosmological parameters by different experiments – has emerged as a crucial part of modern cosmological data analysis. Statistically significant tensions between two experiments or cosmological probes may indicate new physics extending beyond the standard cosmological model and need to be promptly identified. We apply several tension estimators proposed in the literature to the dark energy survey (DES) large-scale structure measurement and Planck cosmic microwave background data. We first evaluate the responsiveness of these metrics to an input tension artificially introduced between the two, using synthetic DES data. We then apply the metrics to the comparison of Planck and actual DES Year 1 data. We find that the parameter differences, Eigentension, and Suspiciousness metrics all yield similar results on both simulated and real data, while the Bayes ratio is inconsistent with the rest due to its dependence on the prior volume. Using these metrics, we calculate the tension between DES Year 1 3 × 2pt and Planck, finding the surveys to be in ∼2.3σ tension under the ΔCDM paradigm. This suite of metrics provides a toolset for robustly testing tensions in the DES Year 3 data and beyond., 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 Ministerio de Ciencia e Innovación (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 Centres de Recerca de Catalunya (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) 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

15. Producing a BOSS CMASS sample with DES imaging

Author: A. A. Plazas, David J. James, Pablo Fosalba, Devon L. Hollowood, E. Bertin, Antonella Palmese, C. Davis, S. Serrano, A. Carnero Rosell, G. Gutierrez, V. Scarpine, J. Gschwend, Shantanu Desai, Mathew Smith, Kyler Kuehn, J. Annis, Daniel Thomas, David Brooks, M. E. C. Swanson, R. L. C. Ogando, Jochen Weller, Juan Garcia-Bellido, Tesla E. Jeltema, Christopher M. Hirata, Jennifer L. Marshall, Marcelle Soares-Santos, Ashley J. Ross, Jack Elvin-Poole, Felipe Menanteau, Peter Melchior, M. Carrasco Kind, Gregory Tarle, Michael Schubnell, Paul Martini, Michael Troxel, Marcos Lima, M. A. G. Maia, A. Choi, E. J. Sanchez, I. Sevilla-Noarbe, K. Honscheid, E. M. Huff, R. Cawthon, Niall MacCrann, Santiago Avila, L. N. da Costa, J. Carretero, Daniel Gruen, Joe Zuntz, J. De Vicente, E. Suchyta, D. W. Gerdes, B. Flaugher, Enrique Gaztanaga, Ramon Miquel, Robert A. Gruendl, Christopher J. Miller, Tim Eifler, Flavia Sobreira, Seungwon Lee, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Photometric [Techniques], Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Max planck institute, techniques: photometric, 0103 physical sciences, media_common.cataloged_instance, European union, Astronomy observatory, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, European research, RCUK, Astronomy and Astrophysics, galaxies: general, methods: data analysis, Data analysis [Methods], Space and Planetary Science, General [Galaxies], Fundamental physics, astro-ph.CO, Christian ministry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], National laboratory, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a sample of galaxies with the Dark Energy Survey (DES) photometry that replicates the properties of the BOSS CMASS sample. The CMASS galaxy sample has been well characterized by the Sloan Digital Sky Survey (SDSS) collaboration and was used to obtain the most powerful redshift-space galaxy clustering measurements to date. A joint analysis of redshift-space distortions (such as those probed by CMASS from SDSS) and a galaxy-galaxy lensing measurement for an equivalent sample from DES can provide powerful cosmological constraints. Unfortunately, the DES and SDSS-BOSS footprints have only minimal overlap, primarily on the celestial equator near the SDSS Stripe 82 region. Using this overlap, we build a robust Bayesian model to select CMASS-like galaxies in the remainder of the DES footprint. The newly defined DES-CMASS (DMASS) sample consists of 117,293 effective galaxies covering $1,244 {\rm deg}^2$. Through various validation tests, we show that the DMASS sample selected by this model matches well with the BOSS CMASS sample, specifically in the South Galactic cap (SGC) region that includes Stripe 82. Combining measurements of the angular correlation function and the clustering-z distribution of DMASS, we constrain the difference in mean galaxy bias and mean redshift between the BOSS CMASS and DMASS samples to be $\Delta b = 0.010^{+0.045}_{-0.052}$ and $\Delta z = \left( 3.46^{+5.48}_{-5.55} \right) \times 10^{-3}$ for the SGC portion of CMASS, and $\Delta b = 0.044^{+0.044}_{-0.043} $ and $\Delta z= ( 3.51^{+4.93}_{-5.91}) \times 10^{-3}$ for the full CMASS sample. These values indicate that the mean bias of galaxies and mean redshift in the DMASS sample is consistent with both CMASS samples within $1\sigma$., Comment: 22 pages, 17 figures
Published: 2019

16. First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant

Author: F. J. Castander, Geraint F. Lewis, W. G. Hartley, Alex Drlica-Wagner, T. M. C. Abbott, C. B. D'Andrea, Tesla E. Jeltema, Dragan Huterer, E. J. Sanchez, D. A. Finley, M. Carrasco Kind, Tenglin Li, Santiago Avila, Carlos E. Cunha, Robert C. Nichol, N. E. Sommer, Vinu Vikram, J. Carretero, Santiago González-Gaitán, R. H. Schindler, K. Bechtol, Tamara M. Davis, E. Swann, D. L. Burke, A. Carnero Rosell, Samuel Hinton, Ben Hoyle, J. Annis, Edward Macaulay, David Brooks, M. E. C. Swanson, Peter Nugent, Martin Crocce, G. Gutierrez, Daniel Thomas, Mark Sullivan, Joshua A. Frieman, P. Wiseman, E. Suchyta, August E. Evrard, Antonella Palmese, Ryan J. Foley, N. Kuropatkin, Daniel Scolnic, A. G. Kim, V. Scarpine, S. Allam, Robert A. Gruendl, E. Kasai, R. C. Thomas, M. A. G. Maia, Mathew Smith, C. Lidman, Peter de Nully Brown, Alistair R. Walker, Lluís Galbany, D. Brout, Jacobo Asorey, S. Serrano, Marcelle Soares-Santos, Jennifer L. Marshall, Enrique Gaztanaga, L. N. da Costa, Rob Sharp, M. Sako, Brad E. Tucker, J. Calcino, David J. James, Daniela Carollo, Bruce A. Bassett, D. L. Hollowood, Anais Möller, A. A. Plazas, Pablo Fosalba, Bonnie Zhang, Richard Kessler, Bhuvnesh Jain, J. De Vicente, K. Honscheid, S. A. Uddin, Karl Glazebrook, Marcos Lima, Flavia Sobreira, M. S. Schubnell, Ofer Lahav, I. Sevilla-Noarbe, J. Lasker, Juan Garcia-Bellido, A. Roodman, Juan Estrada, B. Flaugher, H. T. Diehl, C. Davis, Kyler Kuehn, Daniel Gruen, David Bacon, Alexei V. Filippenko, J. Gschwend, Gregory Tarle, P. Martini, Tim Eifler, Elisabeth Krause, Ramon Miquel, P. Doel, Thomas E. Collett, Huan Lin, J. K. Hoormann, A. K. Romer, and Yen-Chen Pan
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cepheid variable, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, STFC, media_common, Physics, 010308 nuclear & particles physics, Cosmic distance ladder, RCUK, SATÉLITES ARTIFICIAIS, Astronomy and Astrophysics, Universe, Redshift, Space and Planetary Science, astro-ph.CO, Dark energy, symbols, ST/N000668/1, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract: We present an improved measurement of the Hubble constant (H_0) using the 'inverse distance ladder' method, which adds the information from 207 Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) at redshift 0.018 < z < 0.85 to existing distance measurements of 122 low redshift (z < 0.07) SNe Ia (Low-z) and measurements of Baryon Acoustic Oscillations (BAOs). Whereas traditional measurements of H_0 with SNe Ia use a distance ladder of parallax and Cepheid variable stars, the inverse distance ladder relies on absolute distance measurements from the BAOs to calibrate the intrinsic magnitude of the SNe Ia. We find H_0 = 67.8 +/- 1.3 km s-1 Mpc-1 (statistical and systematic uncertainties, 68% confidence). Our measurement makes minimal assumptions about the underlying cosmological model, and our analysis was blinded to reduce confirmation bias. We examine possible systematic uncertainties and all are below the statistical uncertainties. Our H_0 value is consistent with estimates derived from the Cosmic Microwave Background assuming a LCDM universe (Planck Collaboration et al. 2018)., 15 pages, 5 figures, updated to match accepted version
Published: 2019

17. Weak-lensing analysis of SPT-selected galaxy clusters using Dark Energy Survey Science Verification data

Author: F. J. Castander, R. C. Smith, Donnacha Kirk, Alistair R. Walker, Michael Schubnell, Juan Garcia-Bellido, T. M. C. Abbott, Tim Schrabback, Christian L. Reichardt, E. J. Sanchez, Rafe Schindler, D. L. Burke, Robert A. Gruendl, Marcos Lima, Joe Zuntz, M. Carrasco Kind, David J. Brooks, Shantanu Desai, J. Carretero, Tesla E. Jeltema, Bradford Benson, D. Applegate, C. Stern, Sebastian Bocquet, David Rapetti, J. De Vicente, I-Non Chiu, A. Carnero Rosell, Ofer Lahav, Sarah Bridle, Flavia Sobreira, Enrique Gaztanaga, G. Gutierrez, Michael Troxel, Erin Sheldon, D. L. Hollowood, Santiago Avila, M. E. C. Swanson, Nikhel Gupta, M. A. G. Maia, J. P. Dietrich, Filipe B. Abdalla, Felipe Menanteau, Joshua A. Frieman, C. B. D'Andrea, Kyler Kuehn, Gregory Tarle, I. Sevilla-Noarbe, M. March, N. Kuropatkin, Matt J. Jarvis, Pablo Fosalba, T. Kacprzak, L. N. da Costa, E. Suchyta, August E. Evrard, Peter Melchior, R. Capasso, Joseph J. Mohr, A. Saro, Juan Estrada, B. Flaugher, Peter Doel, A. A. Plazas, H. T. Diehl, E. Bertin, C. Davis, J. Gschwend, A. K. Romer, M. Smith, Daniel Gruen, Ramon Miquel, Benjamin Saliwanchik, 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, SPT, 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 ), Stern, C., Dietrich, J. P., Bocquet, S., Applegate, D., Mohr, J. J., Bridle, S. L., Carrasco Kind, M., Gruen, D., Jarvis, M., Kacprzak, T., Saro, A., Sheldon, E., Troxel, M. A., Zuntz, J., Benson, B. A., Capasso, R., Chiu, I., Desai, S., Rapetti, D., Reichardt, C. L., Saliwanchik, Schrabback, T., Gupta, N., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., D'Andrea, C. B., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Doel, P., Estrada, J., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D., Jeltema, T., Kirk, D., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Melchior, P., Menanteau, F., Miquel, R., Plazas, A. A., Romer, A. K., Sanchez, E., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Walker, A. R., Des, Collaboration, and Spt, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Cosmology, gravitational lensing: weak, weak [gravitational lensing], 0103 physical sciences, clusters: general [galaxies], LENTES GRAVITACIONAIS, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Physics, 010308 nuclear & particles physics, GALÁXIAS, Astronomy and Astrophysics, observations [cosmology], Redshift, South Pole Telescope, True mass, galaxies: clusters: general, Space and Planetary Science, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Log-normal distribution, astro-ph.CO, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], observation [cosmology]
Abstract: We present weak lensing (WL) mass constraints for a sample of massive galaxy clusters detected by the South Pole Telescope (SPT) via the Sunyaev-Zeldovich effect (SZE). We use $griz$ imaging data obtained from the Science Verification (SV) phase of the Dark Energy Survey (DES) to fit the WL shear signal of 33 clusters in the redshift range $0.25 \le z \le 0.8$ with NFW profiles and to constrain a four-parameter SPT mass-observable relation. To account for biases in WL masses, we introduce a WL mass to true mass scaling relation described by a mean bias and an intrinsic, log-normal scatter. We allow for correlated scatter within the WL and SZE mass-observable relations and use simulations to constrain priors on nuisance parameters related to bias and scatter from WL. We constrain the normalization of the $\zeta-M_{500}$ relation, $A_\mathrm{SZ}=12.0_{-6.7}^{+2.6}$ when using a prior on the mass slope $B_\mathrm{SZ}$ from the latest SPT cluster cosmology analysis. Without this prior, we recover $A_\mathrm{SZ}=10.8_{-5.2}^{+2.3}$ and $B_\mathrm{SZ}=1.30_{-0.44}^{+0.22}$. Results in both cases imply lower cluster masses than measured in previous work with and without WL, although the uncertainties are large. The WL derived value of $B_\mathrm{SZ}$ is $\approx 20\%$ lower than the value preferred by the most recent SPT cluster cosmology analysis. The method demonstrated in this work is designed to constrain cluster masses and cosmological parameters simultaneously and will form the basis for subsequent studies that employ the full SPT cluster sample together with the DES data., Comment: Revised version in response to referee report
Published: 2019

18. Constraints on dark matter properties from observations of Milky Way satellite galaxies

Author: A. K. Romer, J. Carretero, Annika H. G. Peter, P. Doel, Antonella Palmese, M. A. G. Maia, Vera Gluscevic, Tenglin Li, Ethan O. Nadler, David J. James, A. R. Walker, Marcelle Soares-Santos, S. Desai, Gregory M. Green, Keith Bechtol, Josh Frieman, S. Everett, V. Scarpine, H. T. Diehl, Alex Drlica-Wagner, Dragan Huterer, W. C. Wester, B. Flaugher, Samuel Hinton, J. De Vicente, G. Gutierrez, S. Serrano, J. Annis, D. L. Burke, Douglas L. Tucker, Kyler Kuehn, J. Gschwend, I. Sevilla-Noarbe, Kimberly K. Boddy, M. Smith, Jennifer L. Marshall, Salcedo Romero de Ávila, N. Kuropatkin, L. N. da Costa, S. Allam, Robert A. Gruendl, S. Mau, T. M. C. Abbott, M. Costanzi, M. Carrasco Kind, Daniel Gruen, A. A. Plazas, E. J. Sanchez, M. McNanna, Michel Aguena, M. E. C. Swanson, K. Honscheid, Juan Garcia-Bellido, Andrew B. Pace, Yao-Yuan Mao, Felipe Menanteau, D. W. Gerdes, F. Paz-Chinchón, Elisabeth Krause, A. H. Riley, David J. Brooks, G. Tarle, Ramon Miquel, E. Suchyta, August E. Evrard, Risa H. Wechsler, Bhuvnesh Jain, Ofer Lahav, UAM. Departamento de Física Teórica, Nadler, E. O., Drlica-Wagner, A., Bechtol, K., Mau, S., Wechsler, R. H., Gluscevic, V., Boddy, K., Pace, A. B., T. S., Li, Mcnanna, M., Riley, A. H., García-Bellido, J., Mao, Y. -Y., Green, G., Burke, D. L., Peter, A., Jain, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Brooks, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., Huterer, D., James, D. J., 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., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Walker, A. R., Wester, W., Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), and Department of Energy (US)
Subjects: Scattering cross-section, Milky Way, Dark matter, General Physics and Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo, Particle dark matter, Dwarf Galaxies, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Thermal, Satellite galaxy, Dark Matter, Astrophysics - Cosmology and Nongalactic Astrophysic, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, Física, Astrophysics - Astrophysics of Galaxies, Galaxy, High Energy Physics - Phenomenology, Astrophysics - Cosmology and Nongalactic Astrophysics, Matter wave
Abstract: Nadler, Ethan O, et al. DES Collaboration, We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At 95% confidence, we report limits on (i) the mass of thermal relic warm DM, mWDM>6.5 keV (free-streaming length, λfs≲10h-1 kpc), (ii) the velocity-independent DM-proton scattering cross section, σ02.9×10-21 eV (de Broglie wavelength, λdB≲0.5 kpc). These constraints are complementary to other observational and laboratory constraints on DM properties., The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. 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 No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq Grant No. 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

19. Atacama Cosmology Telescope: A Catalog of >4000 Sunyaev–Zel’dovich Galaxy Clusters

Author: Eli S. Rykoff, Jo Dunkley, E. Bertin, Ofer Lahav, Nick Battaglia, M. Soares-Santos, Hironao Miyatake, Shannon M. Duff, R. D. Wilkinson, Adriaan J. Duivenvoorden, L. N. da Costa, Joel N. Ullom, Robert Morgan, D. L. Burke, Devin Crichton, Kavilan Moodley, Peter Doel, Alexandra Amon, Edward J. Wollack, N. C. Robertson, H. T. Diehl, Joseph E. Golec, Sunayana Bhargava, Samuel Hinton, Emmanuel Schaan, Enrique Gaztanaga, Megan Gralla, David N. Spergel, Johannes Hubmayr, Simon Dicker, David Bacon, S. Allam, Robert A. Gruendl, Simone Ferraro, C. Aros-Bunster, Felipe Menanteau, G. Gutierrez, Kevin M. Huffenberger, Daniel Thomas, Ramon Miquel, Michael D. Niemack, I. Ferrero, Mathew S. Madhavacheril, J. P. Dietrich, Niall MacCrann, Juan Garcia-Bellido, Tesla E. Jeltema, David J. James, Yanxi Zhang, A. K. Romer, Ben Hoyle, Hy Trac, Mark J. Devlin, Patricio A. Gallardo, J. Gschwend, A. A. Plazas, Brian J. Koopman, Rolando Dünner, Zhilei Xu, Simone Aiola, Behzad Ansarinejad, A. Choi, Jeff McMahon, Eduardo Rozo, Gary Bernstein, K. Honscheid, Michel Aguena, Tanay Bhandarkar, Dan Becker, C. Sifon, Neelima Sehgal, Bhuvnesh Jain, Laura Newburgh, Dongwon Han, F. Paz-Chinchón, J. R. Bond, Kyler Kuehn, Peter Melchior, M. Carrasco Kind, Eve M. Vavagiakis, Steve K. Choi, Suzanne T. Staggs, Paul Giles, R. L. C. Ogando, J. C. Hill, Federico Nati, M. E. C. Swanson, E. V. Denison, Kevin T. Crowley, Tony Mroczkowski, W. G. Hartley, Antonella Palmese, Martine Lokken, S. Kent, Alessandro Schillaci, Masamune Oguri, John P. Hughes, M. A. G. Maia, Maria Salatino, S. Amodeo, T. Shin, S. Adhikari, M. Hasselfield, M. Costanzi, S. I. Loubser, J. Van Lanen, B. Partridge, Sigurd Naess, Adam D. Hincks, J. A. Beall, B. Flaugher, S. M. Simon, Jason E. Austermann, S. P. Ho, John Orlowski-Scherer, M. Smith, Daniel Gruen, J. Martin, D. W. Gerdes, J. Annis, Kenda Knowles, David J. Brooks, Erminia Calabrese, Emilie R. Storer, Gene C. Hilton, Leila R. Vale, Salcedo Romero de Ávila, Phumlani Phakathi, Josh Frieman, Yen-Ting Lin, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, J. Carretero, E. Suchyta, Matt Hilton, Christopher J. Conselice, Tobias A. Marriage, Sebastian Grandis, A. Carnero Rosell, Agnès Ferté, Anton T. Jaelani, Marcos Lima, S. Everett, S. Serrano, Lyman A. Page, J. De Vicente, Atsushi J. Nishizawa, G. Tarle, UAM. Departamento de Física Teórica, Hilton, M, Sifon, C, Naess, S, Madhavacheril, M, Oguri, M, Rozo, E, Rykoff, E, Adhikari, S, Aguena, M, Aiola, S, Allam, S, Amodeo, S, Amon, A, Annis, J, Ansarinejad, B, Abbott, T, Aros-Bunster, C, Austermann, J, Avila, S, Bacon, D, Battaglia, N, Beall, J, Becker, D, Bernstein, G, Bertin, E, Bhandarkar, T, Bhargava, S, Bond, J, Brooks, D, Burke, D, Calabrese, E, Carrasco Kind, M, Carretero, J, Choi, S, Choi, A, Conselice, C, Da Costa, L, Costanzi, M, Crichton, D, Crowley, K, Dunner, R, Denison, E, Devlin, M, Dicker, S, Diehl, H, Dietrich, J, Doel, P, Duff, S, Duivenvoorden, A, Dunkley, J, Everett, S, Ferraro, S, Ferte, A, Flaugher, B, Frieman, J, Ferrero, I, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Giles, P, Golec, J, Gralla, M, Grandis, S, Gruen, D, Gerdes, D, Gruendl, R, Gschwend, J, Gutierrez, G, Han, D, Hartley, W, Hasselfield, M, Hill, J, Hilton, G, Hincks, A, Hinton, S, Ho, S, Honscheid, K, Hoyle, B, Hubmayr, J, Huffenberger, K, Hughes, J, Jaelani, A, Jain, B, James, D, Jeltema, T, Kent, S, Knowles, K, Koopman, B, Kuehn, K, Lahav, O, Lima, M, Lin, Y, Lokken, M, Loubser, S, Maccrann, N, Maia, M, Marriage, T, Martin, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Moodley, K, Morgan, R, Mroczkowski, T, Nati, F, Newburgh, L, Niemack, M, Nishizawa, A, Miyatake, H, Ogando, R, Orlowski-Scherer, J, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Phakathi, P, Plazas, A, Robertson, N, Romer, A, Carnero Rosell, A, Sanchez, E, Schaan, E, Schillaci, A, Sehgal, N, Serrano, S, Shin, T, Simon, S, Smith, M, Salatino, M, Soares-Santos, M, Spergel, D, Staggs, S, Storer, E, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Trac, H, Ullom, J, Vale, L, Van Lanen, J, Vavagiakis, E, De Vicente, J, Wilkinson, R, Wollack, E, Xu, Z, Zhan, Y, Hilton, M., Sifón, C., Naess, S., Madhavacheril, M., Oguri, M., Rozo, E., Rykoff, E., Abbott, T. M. C., Adhikari, S., Aguena, M., Aiola, S., Allam, S., Amodeo, S., Amon, A., Annis, J., Ansarinejad, B., Aros-Bunster, C., Austermann, J. E., Avila, S., Bacon, D., Battaglia, N., Beall, J. A., Becker, D. T., Bernstein, G. M., Bertin, E., Bhandarkar, T., Bhargava, S., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Carretero, J., Choi, S. K., Choi, A., Conselice, C., da Costa, L. N., Costanzi, M., Crichton, D., Crowley, K. T., Dünner, R., Denison, E. V., Devlin, M. J., Dicker, S. R., Diehl, H. T., Dietrich, J. P., Doel, P., Duff, S. M., Duivenvoorden, A. J., Dunkley, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giles, P., Golec, J. E., Gralla, M. B., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Han, D., Hartley, W. G., Hasselfield, M., Hill, J. C., Hilton, G. C., Hincks, A. D., Hinton, S. R., S-P. P., Ho, Honscheid, K., Hoyle, B., Hubmayr, J., Huffenberger, K. M., Hughes, J. P., Jaelani, A. T., Jain, B., James, D. J., Jeltema, T., Kent, S., Carrasco Kind, M., Knowles, K., Koopman, B. J., Kuehn, K., Lahav, O., Lima, M., Lin, Y-T., Lokken, M., Loubser, S. I., Maccrann, N., Maia, M. A. G., Marriage, T. A., Martin, J., Mcmahon, J., Melchior, P., Menanteau, F., Miquel, R., Miyatake, H., Moodley, K., Morgan, R., Mroczkowski, T., Nati, F., Newburgh, L. B., Niemack, M. D., Nishizawa, A. J., Ogando, R. L. C., Orlowski-Scherer, J., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Phakathi, P., Plazas, A. A., Robertson, N. C., Romer, A. K., Carnero Rosell, A., Salatino, M., Sanchez, E., Schaan, E., Schillaci, A., Sehgal, N., Serrano, S., Shin, T., Simon, S. M., Smith, M., Soares-Santos, M., Spergel, D. N., Staggs, S. T., Storer, E. R., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Trac, H., Ullom, J. N., Vale, L. R., Van Lanen, J., Vavagiakis, E. M., De Vicente, J., Wilkinson, R. D., Wollack, E. J., Xu, Z., and Zhang, Y.
Subjects: Galaxy clusters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Large-scale structure of the universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Intracluster medium, 0103 physical sciences, Cluster (physics), Sunyaev-Zeldovich Effect, 010303 astronomy & astrophysics, Cosmology, Galaxy clusters, Galaxy cluster, Astrophysics::Galaxy Astrophysics, AGLOMERADOS (GALÁXIA), Physics, 010308 nuclear & particles physics, Star formation, Física, Astronomy and Astrophysics, XMM-newton Telescope, Galaxies, Galaxy, Redshift, Space and Planetary Science, Atacama Cosmology Telescope
Abstract: Hilton, M., et al., We present a catalog of 4195 optically confirmed Sunyaev–Zel’dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M > 3.8 × 10 M, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2 4. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566 deg), the Hyper Suprime-Cam Subaru Strategic Program (469 deg), and the Kilo Degree Survey (825 deg). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr., The DES Data Management System is supported by the NSF under Grant Nos. 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 Unionʼs 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).
Published: 2021

20. Dark Energy Survey Year 3 results: Optimizing the lens sample in a combined galaxy clustering and galaxy-galaxy lensing analysis

Author: F. J. Castander, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, Sarah Bridle, Santiago Avila, Alex Drlica-Wagner, G. Tarle, Xiao Fang, Maria E. S. Pereira, A. Roodman, Tommaso Giannantonio, Samuel Hinton, Alexandra Amon, Josh Frieman, Martin Crocce, R. D. Wilkinson, G. Gutierrez, F. Paz-Chinchón, Sunayana Bhargava, V. Scarpine, Ramon Miquel, Jennifer L. Marshall, Shantanu Desai, Felipe Menanteau, N. Weaverdyck, A. Carnero Rosell, B. Flaugher, David J. Brooks, M. Carrasco Kind, M. E. C. Swanson, J. Carretero, M. Smith, Daniel Gruen, David J. James, Robert Morgan, W. G. Hartley, Pablo Fosalba, E. Gaztanaga, D. W. Gerdes, A. Choi, K. Honscheid, Juan Garcia-Bellido, E. Bertin, Elisabeth Krause, I. Ferrero, Matt J. Jarvis, Agnès Ferté, Peter Doel, D. L. Hollowood, S. Serrano, H. T. Diehl, S. Allam, Robert A. Gruendl, E. Suchyta, David Bacon, R. Cawthon, Niall MacCrann, J. Gschwend, A. Porredon, M. Costanzi, Michel Aguena, S. Pandey, I. Sevilla-Noarbe, J. De Vicente, Kyler Kuehn, N. Kuropatkin, K. D. Eckert, T. N. Varga, L. N. da Costa, M. Soares-Santos, S. Samuroff, Ben Hoyle, Antonella Palmese, M. A. G. Maia, M. Rodriguez-Monroy, Jack Elvin-Poole, A. A. Plazas, Jochen Weller, T. F. Eifler, 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), 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), DES, Porredon, A., Crocce, M., Fosalba, P., Elvin-Poole, J., Carnero Rosell, A., Cawthon, R., Eifler, T. F., Fang, X., Ferrero, I., Krause, E., Maccrann, N., Weaverdyck, N., Abbott, T. M. C., Aguena, M., Allam, S., Amon, A., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Ferte, A., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jarvis, M., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Pandey, S., Paz-Chinchon, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), Dark matter, Cosmological parameters, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, large scale structure, 01 natural sciences, 7. Clean energy, Cosmology, dark matter, Gravitational lenses, 0103 physical sciences, cosmology, Weak, Large-scale structure of the Universe, cosmological parameters, 010306 general physics, dark energy, Sky suverys, STFC, Photometric redshift, AGLOMERADOS (GALÁXIA), Physics, Gravitational Lensing, 010308 nuclear & particles physics, Equation of state (cosmology), Gravitation, Cosmology and Astrophysics, RCUK, Física, Dark enery, Dark Energy, Redshift, Galaxy, observations, 13. Climate action, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Porredon, A., et al. DES Collaboration, We investigate potential gains in cosmological constraints from the combination of galaxy clustering and galaxy-galaxy lensing by optimizing the lens galaxy sample selection using information from Dark Energy Survey (DES) Year 3 data and assuming the DES Year 1 metacalibration sample for the sources. We explore easily reproducible selections based on magnitude cuts in i-band as a function of (photometric) redshift, zphot, and benchmark the potential gains against those using the well-established redMaGiC [E. Rozo et al., Mon. Not. R. Astron. Soc. 461, 1431 (2016)MNRAA40035-871110.1093/mnras/stw1281] sample. We focus on the balance between density and photometric redshift accuracy, while marginalizing over a realistic set of cosmological and systematic parameters. Our optimal selection, the MagLim sample, satisfies i, Funding for the DES Projects was 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 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 under a cooperative agreement with the National Science Foundation. The DES data management system was supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions were partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. was partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grants No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia do e-Universo (CNPq Grant No. 465376/2014-2). This work was 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

21. Dark Energy Survey Year 3 Results: Measuring the Survey Transfer Function with Balrog

Author: S. Everett, B. Yanny, N. Kuropatkin, E. M. Huff, Y. Zhang, J. Myles, A. Masegian, J. Elvin-Poole, S. Allam, G. M. Bernstein, I. Sevilla-Noarbe, M. Splettstoesser, E. Sheldon, M. Jarvis, A. Amon, I. Harrison, A. Choi, W. G. Hartley, A. Alarcon, C. Sánchez, D. Gruen, K. Eckert, J. Prat, M. Tabbutt, V. Busti, M. R. Becker, N. MacCrann, H. T. Diehl, D. L. Tucker, E. Bertin, T. Jeltema, A. Drlica-Wagner, R. A. Gruendl, K. Bechtol, A. Carnero Rosell, T. M. C. Abbott, M. Aguena, J. Annis, D. Bacon, S. Bhargava, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, M. Costanzi, L. N. da Costa, M. E. S. Pereira, J. De Vicente, J. DeRose, S. Desai, T. F. Eifler, A. E. Evrard, I. Ferrero, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, S. Kent, E. Krause, K. Kuehn, O. Lahav, M. Lima, H. Lin, M. A. G. Maia, J. L. Marshall, P. Melchior, F. Menanteau, R. Miquel, J. J. Mohr, R. Morgan, J. Muir, R. L. C. Ogando, A. Palmese, F. Paz-Chinchón, A. A. Plazas, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, M. A. Troxel, T. N. Varga, J. Weller, R. D. Wilkinson, 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, Department of Energy (US), National Science Foundation (US), Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, Ministerio de Economía y Competitividad (España), UAM. Departamento de Física Teórica, Everett, S., Yanny, B., Kuropatkin, N., Huff, E. M., Zhang, Y., Myles, J., Masegian, A., Elvin-Poole, J., Allam, S., Bernstein, G. M., Sevilla-Noarbe, I., Splettstoesser, M., Sheldon, E., Jarvis, M., Amon, A., Harrison, I., Choi, A., Hartley, W. G., Alarcon, A., Sanchez, C., Gruen, D., Eckert, K., Prat, J., Tabbutt, M., Busti, V., Becker, M. R., Maccrann, N., Diehl, H. T., Tucker, D. L., Bertin, E., Jeltema, T., Drlica-Wagner, A., Gruendl, R. A., Bechtol, K., Rosell, A. C., Abbott, T. M. C., Aguena, M., Annis, J., Bacon, D., Bhargava, S., Brooks, D., Burke, D. L., Kind, M. C., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Derose, J., Desai, S., Eifler, T. F., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kent, S., Krause, E., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Varga, T. N., Weller, J., Wilkinson, R. D., Everett, S [0000-0002-3745-2882], Yanny, B [0000-0002-9541-2678], Kuropatkin, N [0000-0003-2511-0946], Huff, EM [0000-0002-9378-3424], Myles, J [0000-0001-6145-5859], Elvin-Poole, J [0000-0001-5148-9203], Bernstein, GM [0000-0002-8613-8259], Sevilla-Noarbe, I [0000-0002-1831-1953], Sheldon, E [0000-0001-9194-0441], Gruen, D [0000-0003-3270-7644], Eckert, K [0000-0002-1407-4700], Becker, MR [0000-0001-7774-2246], Diehl, HT [0000-0002-8357-7467], Tucker, DL [0000-0001-7211-5729], Bertin, E [0000-0002-3602-3664], Jeltema, T [0000-0001-6089-0365], Drlica-Wagner, A [0000-0001-8251-933X], Gruendl, RA [0000-0002-4588-6517], Abbott, TMC [0000-0003-1587-3931], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Carretero, J [0000-0002-3130-0204], Castander, FJ [0000-0001-7316-4573], Conselice, C [0000-0003-1949-7638], Costanzi, M [0000-0001-8158-1449], Derose, J [0000-0002-0728-0960], Fosalba, P [0000-0002-1510-5214], García-Bellido, J [0000-0002-9370-8360], Gaztanaga, E [0000-0001-9632-0815], Gerdes, DW [0000-0001-6942-2736], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Huterer, D [0000-0001-6558-0112], Kent, S [0000-0003-4207-7420], Kuehn, K [0000-0003-0120-0808], Marshall, JL [0000-0003-0710-9474], Melchior, P [0000-0002-8873-5065], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Romer, AK [0000-0002-9328-879X], Roodman, A [0000-0001-5326-3486], Serrano, S [0000-0002-0211-2861], Soares-Santos, M [0000-0001-6082-8529], Tarle, G [0000-0003-1704-0781], Weller, J [0000-0002-8282-2010], and Apollo - University of Cambridge Repository
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, Weak, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 1464, 351, 1857, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Gravitational Lensing, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Dark Energy, Space and Planetary Science, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract: DES Collaboration: Everett et al., We describe an updated calibration and diagnostic framework, Balrog, used to directly sample the selection and photometric biases of the Dark Energy Survey (DES) Year 3 (Y3) data set. We systematically inject onto the single-epoch images of a random 20% subset of the DES footprint an ensemble of nearly 30 million realistic galaxy models derived from DES Deep Field observations. These augmented images are analyzed in parallel with the original data to automatically inherit measurement systematics that are often too difficult to capture with generative models. The resulting object catalog is a Monte Carlo sampling of the DES transfer function and is used as a powerful diagnostic and calibration tool for a variety of DES Y3 science, particularly for the calibration of the photometric redshifts of distant "source" galaxies and magnification biases of nearer "lens" galaxies. The recovered Balrog injections are shown to closely match the photometric property distributions of the Y3 GOLD catalog, particularly in color, and capture the number density fluctuations from observing conditions of the real data within 1% for a typical galaxy sample. We find that Y3 colors are extremely well calibrated, typically within ∼1–8 mmag, but for a small subset of objects, we detect significant magnitude biases correlated with large overestimates of the injected object size due to proximity effects and blending. We discuss approaches to extend the current methodology to capture more aspects of the transfer function and reach full coverage of the survey footprint for future analyses., S.E. and T.J. acknowledge support from the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under award numbers DESC0010107 and A00-1465-001. Funding for the DES Projects has been provided by the US Department of Energy, the US 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 Nos. 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 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 US Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021

22. Synthetic Galaxy Clusters and Observations Based on Dark Energy Survey Year 3 Data

Author: Matthew R. Becker, I. Ferrero, Matt J. Jarvis, Yanxi Zhang, B. Flaugher, Scott Dodelson, A. Choi, Enrique Gaztanaga, M. March, M. Carrasco Kind, K. Honscheid, Maria E. S. Pereira, S. Desai, Brian Yanny, David J. Brooks, V. Scarpine, Eli S. Rykoff, Erin Sheldon, Robert Morgan, Joe Zuntz, Antonella Palmese, Sebastian Grandis, M. A. G. Maia, J. Annis, Samuel Hinton, K. Herner, J. Carretero, Alexandra Amon, Sunayana Bhargava, G. Gutierrez, I. Harrison, I. Sevilla-Noarbe, S. Allam, Robert A. Gruendl, R. P. Rollins, E. Suchyta, A. A. Plazas, M. Soares-Santos, G. Tarle, Jochen Weller, J. Myles, N. Kuropatkin, Felipe Menanteau, Kyler Kuehn, K. D. Eckert, T. N. Varga, A. Carnero Rosell, L. N. da Costa, J. McCullough, J. De Vicente, Chun-Hao To, E. J. Sanchez, M. Costanzi, F. Paz-Chinchón, Peter Melchior, Daniel Thomas, S. Everett, M. E. C. Swanson, Stella Seitz, A. K. Romer, Tesla E. Jeltema, W. G. Hartley, S. Serrano, Ramon Miquel, J. P. Dietrich, Juan Garcia-Bellido, Michael Troxel, Michel Aguena, Eduardo Rozo, M. Smith, Daniel Gruen, H. T. Diehl, Niall MacCrann, E. Bertin, J. Gschwend, Gary Bernstein, Michael Schubnell, D. W. Gerdes, Varga, T N, Gruen, D, Seitz, S, Maccrann, N, Sheldon, E, Hartley, W G, Amon, A, Choi, A, Palmese, A, Zhang, Y, Becker, M R, Mccullough, J, Rozo, E, Rykoff, E S, To, C, Grandis, S, Bernstein, G M, Dodelson, S, Eckert, K, Everett, S, Gruendl, R A, Harrison, I, Herner, K, Rollins, R P, Sevilla-Noarbe, I, Troxel, M A, Yanny, B, Zuntz, J, Diehl, H T, Jarvis, M, Aguena, M, Allam, S, Annis, J, Bertin, E, Bhargava, S, Brooks, D, Carnero&nbsp, Rosell, A, Carrasco&nbsp, Kind, M, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, De&nbsp, Vicente, J, Desai, S, Dietrich, J P, Ferrero, I, Flaugher, B, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gschwend, J, Gutierrez, G, Hinton, S R, Honscheid, K, Jeltema, T, Kuehn, K, Kuropatkin, N, Maia, M A G, March, M, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Myles, J, Paz-Chinchón, F, Plazas, A A, Romer, A K, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, Weller, J, UAM. Departamento de Física Teórica, Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology: Observations, Observations [Cosmology], weak [gravitational lensing], 0103 physical sciences, Cluster (physics), clusters: general [galaxies], 010303 astronomy & astrophysics, Galaxy cluster, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Gravitational Lensing: Weak, Física, GALÁXIAS, Astronomy and Astrophysics, Redshift, Galaxy, Distribution function, Space and Planetary Science, gravitational lensing: weak, galaxies: clusters: general, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: Clusters: General, observation [cosmology]
Abstract: T. N. Varga et al., We develop a novel data-driven method for generating synthetic optical observations of galaxy clusters. In cluster weak lensing, the interplay between analysis choices and systematic effects related to source galaxy selection, shape measurement, and photometric redshift estimation can be best characterized in end-to-end tests going from mock observations to recovered cluster masses. To create such test scenarios, we measure and model the photometric properties of galaxy clusters and their sky environments from the Dark Energy Survey Year 3 (DES Y3) data in two bins of cluster richness λ∈[30;45) ⁠, λ∈[45;60) and three bins in cluster redshift (⁠z∈[0.3;0.35) ⁠, z∈[0.45;0.5) and z∈[0.6;0.65) ⁠. Using deep-field imaging data, we extrapolate galaxy populations beyond the limiting magnitude of DES Y3 and calculate the properties of cluster member galaxies via statistical background subtraction. We construct mock galaxy clusters as random draws from a distribution function, and render mock clusters and line-of-sight catalogues into synthetic images in the same format as actual survey observations. Synthetic galaxy clusters are generated from real observational data, and thus are independent from the assumptions inherent to cosmological simulations. The recipe can be straightforwardly modified to incorporate extra information, and correct for survey incompleteness. New realizations of synthetic clusters can be created at minimal cost, which will allow future analyses to generate the large number of images needed to characterize systematic uncertainties in cluster mass measurements., This research was supported by the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strat- egy –EXC-2094-390783311. The calculations have been in part carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP). This w ork w as supported by the Department of Energy, Laboratory Directed Research and Development program at SLAC National Accelerator Laboratory, under contract DE-AC02-76SF00515 and as part of the P anofsk y Fellowship awarded to DG. 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 Supercomput- ing 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 Te xas A&M Univ ersity, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, 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 Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana- Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Fisica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit ¨at M ¨unchen 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. The DES data management system is supported by the Na- tional Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, 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 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.
Published: 2021
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23. Cosmological Constraints from DES Y1 Cluster Abundances and SPT Multi-wavelength data

Author: E. Suchyta, F. Ruppin, Samuel Hinton, Sunayana Bhargava, M. Carrasco Kind, Felipe Menanteau, Maria E. S. Pereira, V. Scarpine, S. Samuroff, G. Gutierrez, Ramon Miquel, Enrique Gaztanaga, Jennifer L. Marshall, T. N. Varga, K. Kuehn, Elisabeth Krause, P. Fosalba, A. Choi, Josh Frieman, David J. Brooks, K. Honscheid, G. Tarle, Marcelle Soares-Santos, J. Myles, Daniel Gruen, David J. James, J. P. Dietrich, Sebastian Grandis, A. Roodman, Tommaso Giannantonio, Juan Garcia-Bellido, I. Ferrero, Daniel B. Thomas, D. W. Gerdes, Nikhel Gupta, M. E. C. Swanson, J. Annis, M. Costanzi, N. MacCrann, D. Rapetti, I. Sevilla-Noarbe, Sebastian Bocquet, A. Carnero Rosell, N. Kuropatkin, F. Paz-Chinchón, Shantanu Desai, Risa H. Wechsler, S. Everett, Antonella Palmese, E. Buckley-Geer, Agnès Ferté, L. N. da Costa, M. A. G. Maia, B. Flaugher, Joseph J. Mohr, M. N. K. Smith, Z. Zhang, A. Saro, Marcos Lima, Christian L. Reichardt, O. Lahav, A. A. Plazas, Parampreet Singh, R. L. C. Ogando, J. De Vicente, T. M. C. Abbott, Robert Morgan, Santiago Avila, D. L. Hollowood, S. Serrano, T. F. Eifler, Chun-Hao To, L. Salvati, E. J. Sanchez, H. T. Diehl, David Bacon, P. Doel, A. Amara, Douglas L. Tucker, Paul Giles, Tesla E. Jeltema, Bradford Benson, Michel Aguena, D. L. Burke, S. Allam, Robert A. Gruendl, A. A. Stark, W. G. Hartley, J. Carretero, A. K. Romer, UAM. Departamento de Física Teórica, 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), National Science Foundation (US), Costanzi, M., Saro, A., Bocquet, S., Abbott, T. M. C., Aguena, M., Allam, S., Amara, A., Annis, J., Avila, S., Bacon, D., Benson, B. A., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Choi, A., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Everett, S., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giles, P., Grandis, S., Gruen, D., Gruendl, R. A., Gupta, N., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maccrann, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Rapetti, D., Reichardt, C. L., Romer, A. K., Roodman, A., Ruppin, F., Salvati, L., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Singh, P., Smith, M., Soares-Santos, M., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Wechsler, R. H., and Zhang, Z.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), media_common.quotation_subject, Cosmological parameters, FOS: Physical sciences, Galaxy clusters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, XMM-Newton Telescope, Cosmology, 0103 physical sciences, Cluster (physics), Large-scale structure of the Universe, 010306 general physics, Weak gravitational lensing, STFC, media_common, AGLOMERADOS (GALÁXIA), Physics, 010308 nuclear & particles physics, Gravitation, Cosmology and Astrophysics, RCUK, Física, Galaxies, Cosmos, Redshift, Universe, Data set, South Pole Telescope, 13. Climate action, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Costanzi, M., et al. DES and SPT Collaborations, We perform a joint analysis of the counts of redMaPPer clusters selected from the Dark Energy Survey (DES) year 1 data and multiwavelength follow-up data collected within the 2500 deg2 South Pole Telescope (SPT) Sunyaev-Zel'dovich (SZ) survey. The SPT follow-up data, calibrating the richness-mass relation of the optically selected redMaPPer catalog, enable the cosmological exploitation of the DES cluster abundance data. To explore possible systematics related to the modeling of projection effects, we consider two calibrations of the observational scatter on richness estimates: a simple Gaussian model which account only for the background contamination (BKG), and a model which further includes contamination and incompleteness due to projection effects (PRJ). Assuming either a ΛCDM+mν or wCDM+mν cosmology, and for both scatter models, we derive cosmological constraints consistent with multiple cosmological probes of the low and high redshift Universe, and in particular with the SPT cluster abundance data. This result demonstrates that the DES Y1 and SPT cluster counts provide consistent cosmological constraints, if the same mass calibration data set is adopted. It thus supports the conclusion of the DES Y1 cluster cosmology analysis which interprets the tension observed with other cosmological probes in terms of systematics affecting the stacked weak lensing analysis of optically selected low-richness clusters. Finally, we analyze the first combined optically SZ selected cluster catalog obtained by including the SPT sample above the maximum redshift probed by the DES Y1 redMaPPer sample (z=0.65). Besides providing a mild improvement of the cosmological constraints, this data combination serves as a stricter test of our scatter models: the PRJ model, providing scaling relations consistent between the two abundance and multiwavelength follow-up data, is favored over the BKG model., 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, National Science Fundation’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 Australian (aka “Oz”) Dark Energy Survey 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 Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. 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 Grants Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 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. This paper has gone through internal review by the DES Collaboration. M. C. and A. S. are supported by the ERC-StG ’ClustersXCosmo’ Grant Agreement No. 716762. A. S. is supported by the FARE-MIUR Grant
Published: 2021

24. The mass and galaxy distribution around SZ-selected clusters

Author: Edward J. Wollack, S. Goldstein, Erin S. Sheldon, Jochen Weller, L. N. da Costa, J. Elvin-Poole, Suzanne T. Staggs, Simone Ferraro, Marco Raveri, Mark J. Devlin, J. P. Dietrich, Sahar S. Allam, T. N. Varga, David Brooks, S. Pandey, M. Lokken, Brian Yanny, Maria E. S. Pereira, A. Amsellem, J. DeRose, Maria Salatino, J. McCullough, M. E. C. Swanson, M. Costanzi, C. Doux, Chun-Hao To, Cristóbal Sifón, E. J. Sanchez, Joseph J. Mohr, I. Tutusaus, I. Sevilla-Noarbe, Gary Bernstein, B. Partridge, John P. Hughes, Carlos Solans Sanchez, G. Tarle, Scott Dodelson, Chihway Chang, V. Scarpine, Keith Bechtol, Ian Harrison, Enrique Gaztanaga, B. Flaugher, Peter Doel, Nick Battaglia, Alex Drlica-Wagner, J. Myles, David J. James, N. P. Kuropatkin, H. T. Diehl, David Bacon, Kavilan Moodley, Niall MacCrann, T. M. C. Abbott, David H. Weinberg, Kyler Kuehn, M. Gatti, J. Prat, Adriano Pieres, Samuel Hinton, Bhuvnesh Jain, K. Eckert, J. De Vicente, T. Dacunha, Marcelle Soares-Santos, E. Suchyta, E. J. Baxter, D. Gruen, A. Carnero Rosell, J. Carretero, Matt Hilton, M. Belyakov, Michael Troxel, J. C. Hill, F. Paz-Chinchón, A. Alarcon, Richard P. Rollins, Antonio Campos, Ramon Miquel, S. Desai, Federico Nati, Michael D. Niemack, Sebastian Bocquet, M. Smith, M. Aguena, A. K. Romer, Daniel Thomas, E. Buckley-Geer, L. A. Page, Emmanuel Bertin, Antonella Palmese, Andrés N. Salcedo, Jeff McMahon, Agnès Ferté, Blake D. Sherwin, M. A. G. Maia, D. W. Gerdes, Ofer Lahav, I. Ferrero, Mathew S. Madhavacheril, Robert Morgan, M. Rodriguez-Monroy, Yanxi Zhang, A. A. Plazas Malagón, Andrey V. Kravtsov, S. Everett, Marco A. P. Lima, S. Adhikari, Patricio A. Gallardo, Matthew R. Becker, Basilio X. Santiago, D. L. Burke, J. Frieman, J. R. Bond, Robert A. Gruendl, M. Carrasco Kind, F. Andrade-Oliveira, Tesla E. Jeltema, Ricardo L. C. Ogando, M. Jarvis, R. Chen, Ami Choi, Elisabeth Krause, Peter Melchior, Eli S. Rykoff, Eve M. Vavagiakis, G. Gutierrez, A. Navarro-Alsina, Santiago Serrano, B. Yin, Alexandra Amon, Felipe Menanteau, James Annis, Brian J. Koopman, L. F. Secco, W. G. Hartley, Alessandro Schillaci, Devon L. Hollowood, T. Shin, University of Pennsylvania, University of Chicago, University of Hawaii, The Ohio State University, Cornell University, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians-Universität, NSF’s National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), Laboratório Interinstitucional de e-Astronomia – LIneA, Argonne National Laboratory, Fermi National Accelerator Laboratory, Stanford University, Universidade Estadual Paulista (UNESP), University of Portsmouth, University of Wisconsin-Madison, Institut d’Astrophysique de Paris, University of Toronto, University College London, Carnegie Mellon University, Duke University, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Lawrence Berkeley National Laboratory, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, California Institute of Technology, Institut d’Estudis Espacials de Catalunya (IEEC), CSIC), University of Michigan, SLAC National Accelerator Laboratory, Denys Wilkinson Building, University of Manchester, University of Geneva, Columbia University, Flatiron Institute, Westville Campus, University of Queensland, The State University of New Jersey, Center for Astrophysics | Harvard & Smithsonian, Yale University, University of Arizona, Macquarie University, Lowell Observatory, Dunlap Institute of Astronomy & Astrophysics, University of Cambridge, Perimeter Institute for Theoretical Physics, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Milano-Bicocca, Universidade Estadual de Campinas (UNICAMP), Princeton University, Haverford College, University of Sussex, UFRGS, Brookhaven National Laboratory, Pontificia Universidad Católica de Valparaíso, University of Southampton, Oak Ridge National Laboratory, NASA/Goddard Space Flight Center, Shin, T, Jain, B, Adhikari, S, Baxter, E, Chang, C, Pandey, S, Salcedo, A, Weinberg, D, Amsellem, A, Battaglia, N, Belyakov, M, Dacunha, T, Goldstein, S, Kravtsov, A, Varga, T, Abbott, T, Aguena, M, Alarcon, A, Allam, S, Amon, A, Andrade-Oliveira, F, Annis, J, Bacon, D, Bechtol, K, Becker, M, Bernstein, G, Bertin, E, Bocquet, S, Bond, J, Brooks, D, Buckley-Geer, E, Burke, D, Campos, A, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chen, R, Choi, A, Costanzi, M, da Costa, L, Derose, J, Desai, S, de Vicente, J, Devlin, M, Diehl, H, Dietrich, J, Dodelson, S, Doel, P, Doux, C, Drlica-Wagner, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferraro, S, Ferrero, I, Ferte, A, Flaugher, B, Frieman, J, Gallardo, P, Gatti, M, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Harrison, I, Hartley, W, Hill, J, Hilton, M, Hinton, S, Hollowood, D, Hughes, J, James, D, Jarvis, M, Jeltema, T, Koopman, B, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Lokken, M, Maccrann, N, Madhavacheril, M, Maia, M, Mccullough, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Myles, J, Nati, F, Navarro-Alsina, A, Niemack, M, Ogando, R, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Pereira, M, Pieres, A, Plazas Malagon, A, Prat, J, Raveri, M, Rodriguez-Monroy, M, Rollins, R, Romer, A, Rykoff, E, Salatino, M, Sanchez, C, Sanchez, E, Santiago, B, Scarpine, V, Schillaci, A, Secco, L, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Sherwin, B, Sifon, C, Smith, M, Soares-Santos, M, Staggs, S, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Troxel, M, Tutusaus, I, Vavagiakis, E, Weller, J, Wollack, E, Yanny, B, Yin, B, Zhang, Y, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Univ Penn, Univ Chicago, Univ Hawaii, Ohio State Univ, Cornell Univ, Max Planck Inst Extraterr Phys, Ludwig Maximilians Univ Munchen, NSFs Natl Opt Infrared Astron Res Lab, Lab Interinst E Astron LIneA, Argonne Natl Lab, Fermilab Natl Accelerator Lab, Stanford Univ, Univ Portsmouth, Univ Wisconsin, Inst Astrophys Paris, Sorbonne Univ, Univ Toronto, UCL, Carnegie Mellon Univ, Duke Univ, Inst Astrofis Canarias, Univ La Laguna, Natl Ctr Supercomp Applicat, Univ Illinois, Barcelona Inst Sci & Technol, Lawrence Berkeley Natl Lab, Univ Trieste, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Observ Nacl, Ctr Invest Energet Medioambientales & Tecnol CIEM, Santa Cruz Inst Particle Phys, Univ Oslo, CALTECH, Inst Estudis Espacials Catalunya IEEC, CSIC, Univ Michigan, SLAC Natl Accelerator Lab, Univ Oxford, Univ Manchester, Univ Geneva, Columbia Univ, Flatiron Inst, Univ KwaZulu Natal, Univ Queensland, Rutgers State Univ, Ctr Astrophys Harvard & Smithsonian, Yale Univ, Univ Arizona, Macquarie Univ, Lowell Observ, Dunlap Inst Astron & Astrophys, Univ Cambridge, Perimeter Inst Theoret Phys, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Univ Milano Bicocca, Haverford Coll, Univ Sussex, Univ Fed Rio Grande do Sul, Brookhaven Natl Lab, Pontificia Univ Catolica Valparaiso, Univ Southampton, Oak Ridge Natl Lab, NASA, Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., Derose, J., Desai, S., de Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferte, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., Maccrann, N., Madhavacheril, M. S., Maia, M. A. G., Mccullough, J., Mcmahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchon, F., Pereira, M. E. S., Pieres, A., Plazas Malagon, A. A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sanchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifon, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., and Zhang, Y.
Subjects: Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], Cosmology: observation, Cosmology, Galaxies clusters general, observations [Cosmology], Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Cosmology observation, Physics, Cosmology: observations, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Cosmology observations, Galaxies evolution, Galaxy, Redshift, Galaxies: clusters: general, Space and Planetary Science, Atacama Cosmology Telescope, Dark energy, Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Shin, T., et al., We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev–Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 data set. With signal-to-noise ratio of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2–20 h Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: (1) The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. (2) The full mass profile is also consistent with the simulations. (3) The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift, and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology, and astrophysics are discussed., 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 Ciência e Tecnologia (INCT) do e-Universo (CNPq grant no. 465376/2014-2).
Published: 2021

25. A Deeper Look at DES Dwarf Galaxy Candidates: Grus I and Indus II

Author: Denija Crnojevic, J. Gschwend, R. D. Wilkinson, Shantanu Desai, E. Suchyta, F. Paz-Chinchón, J. Carretero, Michael Schubnell, A. A. Plazas, Joshua D. Simon, M. Smith, A. R. Walker, K. Honscheid, Peter Doel, C. E. Martínez-Vázquez, Louis E. Strigari, S. A. Cantu, H. T. Diehl, J. De Vicente, Juan Garcia-Bellido, S. Allam, Robert A. Gruendl, Josh Frieman, David James, Felipe Menanteau, Jennifer L. Marshall, M. Costanzi, Gregory Tarle, Adam Amara, M. E. C. Swanson, M. A. G. Maia, Marcelle Soares-Santos, Michel Aguena, Santiago Serrano, I. Sevilla-Noarbe, Tim Eifler, A. Carnero Rosell, Ramon Miquel, V. Scarpine, Antonella Palmese, Alex Drlica-Wagner, Basilio X. Santiago, K. M. Stringer, Samuel Hinton, L. N. da Costa, G. Gutierrez, S. Everett, D. Gruen, D. L. Hollowood, Enrique Gaztanaga, Andrew B. Pace, M. Carrasco Kind, D. H. Brooks, E. J. Sanchez, Santiago Avila, Kyler Kuehn, Keith Bechtol, Cantu, Sarah A., Pace, Andrew B., Marshall, Jennifer, Strigari, Louis E., Crnojevic, Denija, Simon, Joshua D., Drlica-Wagner, A., Bechtol, K., Martínez-Vázquez, Clara E., Santiago, B., Amara, A., Stringer, K. M., Diehl, H. T., Aguena, M., Allam, S., Avila, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Eifler, T. F., Everett, S., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Maia, M. A. G., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Walker, A. R., Wilkinson, R. D., and Des, Collaboration
Subjects: Stellar population, Galaxy propertie, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy properties, Bayesian statistics, 01 natural sciences, Photometry (optics), Photometry, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Dwarf galaxies, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, 010308 nuclear & particles physics, Grus (geology), Astronomy data analysi, Astronomy and Astrophysics, Horizontal branch, Astronomy data analysis, 416, 1858, 1234, 615, 1900, Astrophysics - Astrophysics of Galaxies, Bayesian statistic, Stars, Dwarf galaxie, Space and Planetary Science, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), Magnitude (astronomy), Astrophysics::Earth and Planetary Astrophysics
Abstract: We present deep $g$- and $r$-band Magellan/Megacam photometry of two dwarf galaxy candidates discovered in the Dark Energy Survey (DES), Grus I and Indus II (DES J2038-4609). For the case of Grus I, we resolved the main sequence turn-off (MSTO) and $\sim 2$ mags below it. The MSTO can be seen at $g_0\sim 24$ with a photometric uncertainty of $0.03$ mag. We show Grus I to be consistent with an old, metal-poor ($\sim 13.3$ Gyr, [Fe/H]$\sim-1.9$) dwarf galaxy. We derive updated distance and structural parameters for Grus I using this deep, uniform, wide-field data set. We find an azimuthally averaged half-light radius more than two times larger ($\sim 151^{+21}_{-31}$ pc; $\sim 4.^{\prime} 16^{+0.54}_{-0.74}$) and an absolute $V$-band magnitude $\sim-4.1$ that is $\sim 1$ magnitude brighter than previous studies. We obtain updated distance, ellipticity, and centroid parameters which are in agreement with other studies within uncertainties. Although our photometry of Indus II is $\sim 2-3$ magnitudes deeper than the DES Y1 Public release, we find no coherent stellar population at its reported location. The original detection was located in an incomplete region of sky in the DES Y2Q1 data set and was flagged due to potential blue horizontal branch member stars. The best fit isochrone parameters are physically inconsistent with both dwarf galaxies and globular clusters. We conclude that Indus II is likely a false-positive, flagged due to a chance alignment of stars along the line of sight., 16 pages, 8 figures; submitted to ApJ
Published: 2021

26. Galaxy morphological classification catalogue of the Dark Energy Survey Year 3 data with convolutional neural networks

Author: G. Tarle, M. Carrasco Kind, F. Andrade-Oliveira, Kyler Kuehn, D. L. Burke, Josh Frieman, I. Sevilla-Noarbe, M. Soares-Santos, H. T. Diehl, N. Kuropatkin, Ting-Yun Cheng, Daniel Thomas, Alfonso Aragón-Salamanca, A. Choi, S. Allam, Robert A. Gruendl, S. Everett, Alex Drlica-Wagner, K. D. Eckert, L. N. da Costa, K. Honscheid, J. Carretero, F. Paz-Chinchón, E. J. Sanchez, David J. Brooks, Samuel Hinton, Juan Garcia-Bellido, Maria E. S. Pereira, David J. James, D. L. Hollowood, Asa F. L. Bluck, S. Serrano, Pablo Fosalba, G. Gutierrez, M. Smith, J. Annis, A. A. Plazas Malagón, M. A. G. Maia, A. Roodman, Tommaso Giannantonio, Adriano Pieres, Daniel Gruen, M. E. C. Swanson, C To, V. Scarpine, Elisabeth Krause, E. Suchyta, August E. Evrard, D. W. Gerdes, Michel Aguena, Felipe Menanteau, I. Ferrero, M. Costanzi, Ramon Miquel, J. De Vicente, J. Gschwend, Christopher J. Conselice, M. March, Ofer Lahav, Robert Morgan, National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Australian Research Council, Durham University, University Park, University of Manchester, Universidade de São Paulo (USP), Laboratório Interinstitucional de e-Astronomia – LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), University of Cambridge, University College London, Stanford University, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, University of Illinois at Urbana–Champaign, Barcelona Institute of Science and Technology, Ohio State University, University of Trieste, INAF – Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), University of Chicago, University of Pennsylvania, Santa Cruz Institute for Particle Physics, University of Oslo, Institut d’Estudis Espacials de Catalunya (IEEC), CSIC), Universidad Autonoma de Madrid, University of Queensland, Harvard & Smithsonian, University of Arizona, Macquarie University, Lowell Observatory, Institució Catalana de Recerca i Estudis Avançats, University of Wisconsin–Madison, Peyton Hall, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Cheng, Ting-Yun, Conselice, Christopher J., Aragón-Salamanca, Alfonso, Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bluck, A. F. L., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Choi, A., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Everett, S., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and To, C.
Subjects: structure [Galaxies], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Disc galaxy, 01 natural sciences, Convolutional neural network, Methods: observational, Methods: data analysis, Galaxies: structure, 0103 physical sciences, observational [Methods], 10. No inequality, data analysis [Methods], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, methods: observational, methods: data analysis, catalogues, galaxies: structure, Astrophysics - Astrophysics of Galaxies, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Catalogues, Galaxy, Redshift, Data set, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), data analysi [methods], Magnitude (astronomy), Dark energy, catalogue, Galaxy morphological classification
Abstract: Cheng, Ting-Yun, et al., We present in this paper one of the largest galaxy morphological classification catalogues to date, including over 20 million galaxies, using the Dark Energy Survey (DES) Year 3 data based on convolutional neural networks (CNNs). Monochromatic i-band DES images with linear, logarithmic, and gradient scales, matched with debiased visual classifications from the Galaxy Zoo 1 (GZ1) catalogue, are used to train our CNN models. With a training set including bright galaxies (16 ≤ i < 18) at low redshift (z < 0.25), we furthermore investigate the limit of the accuracy of our predictions applied to galaxies at fainter magnitude and at higher redshifts. Our final catalogue covers magnitudes 16 ≤ i < 21, and redshifts z < 1.0, and provides predicted probabilities to two galaxy types – ellipticals and spirals (disc galaxies). Our CNN classifications reveal an accuracy of over 99 per cent for bright galaxies when comparing with the GZ1 classifications (i < 18). For fainter galaxies, the visual classification carried out by three of the co-authors shows that the CNN classifier correctly categorizes discy galaxies with rounder and blurred features, which humans often incorrectly visually classify as ellipticals. As a part of the validation, we carry out one of the largest examinations of non-parametric methods, including ∼100 ,000 galaxies with the same coverage of magnitude and redshift as the training set from our catalogue. We find that the Gini coefficient is the best single parameter discriminator between ellipticals and spirals for this data set., 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 MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, 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 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2021

27. A machine learning approach to galaxy properties: Joint redshift-stellar mass probability distributions with Random Forest

Author: A. A. Plazas, L. N. Da Costa, W. G. Hartley, Maria E. S. Pereira, Brian Yanny, Marcos Lima, Alex Drlica-Wagner, J. Carretero, Antonella Palmese, E. M. Huff, Juan Garcia-Bellido, Ramon Miquel, M. A. G. Maia, Michel Aguena, V. Scarpine, A. Choi, Martin Crocce, F. J. Castander, G. Tarle, R. D. Wilkinson, Ian Harrison, S. Mucesh, K. Honscheid, Sunayana Bhargava, A. Alarcon, J. De Vicente, David J. James, Huan Lin, Pablo Fosalba, M. Carrasco Kind, Chun-Hao To, Alexandra Amon, E. J. Sanchez, F. Paz-Chinchón, Keith Bechtol, E. Suchyta, August E. Evrard, M. Costanzi, M. Smith, Felipe Menanteau, Josh Frieman, D. L. Hollowood, S. Allam, Robert A. Gruendl, S. Serrano, Ofer Lahav, Daniel Gruen, Samuel Hinton, Peter Melchior, Christopher J. Conselice, Erin Sheldon, B. Flaugher, E. Bertin, G. Gutierrez, David J. Brooks, S. Desai, Enrique Gaztanaga, Robert Morgan, J. Gschwend, S. Everett, D. W. Gerdes, Gary Bernstein, I. Ferrero, H. T. Diehl, David Bacon, I. Sevilla-Noarbe, N. Kuropatkin, K. D. Eckert, T. N. Varga, Asa F. L. Bluck, Kyler Kuehn, Michael Schubnell, Daniel Thomas, L. Whiteway, A. Carnero Rosell, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), 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, Mucesh, S., Hartley, W. G., Palmese, A., Lahav, O., Whiteway, L., Amon, A., Bechtol, K., Bernstein, G. M., Carnero Rosell, A., Carrasco Kind, M., Choi, A., Eckert, K., Everett, S., Gruen, D., Gruendl, R. A., Harrison, I., Huff, E. M., Kuropatkin, N., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Drlica-Wagner, A., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lima, M., Lin, H., Maia, M. A. G., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., and Wilkinson, R. D.
Subjects: FOS: Computer and information sciences, Computer Science - Machine Learning, statistical [Methods], software: data analysis, computer.software_genre, 01 natural sciences, data analysi [software], Copula (probability theory), Machine Learning (cs.LG), Astrophysics - Cosmology and Nongalactic Astrophysic, data analysis [Methods], 010303 astronomy & astrophysics, Physics, fundamental parameter [galaxies], galaxies: fundamental parameters, Random forest, Software: public realese, fundamental parameters [Galaxies], Probability distribution, galaxies: evolution, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, public realese [Software], Cosmology and Nongalactic Astrophysics (astro-ph.CO), methods: data analysis, methods: statistical, software: public release, Astrophysics - Astrophysics of Galaxies, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Machine learning, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Galaxy formation and evolution, [INFO]Computer Science [cs], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Probability integral transform, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, business.industry, Univariate, Astronomy and Astrophysics, evolution [Galaxies], public release [software], Redshift, Galaxy, Space and Planetary Science, data analysis [Software], Astrophysics of Galaxies (astro-ph.GA), data analysi [methods], Artificial intelligence, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, computer
Abstract: We demonstrate that highly accurate joint redshift-stellar mass probability distribution functions (PDFs) can be obtained using the Random Forest (RF) machine learning (ML) algorithm, even with few photometric bands available. As an example, we use the Dark Energy Survey (DES), combined with the COSMOS2015 catalogue for redshifts and stellar masses. We build two ML models: one containing deep photometry in the $griz$ bands, and the second reflecting the photometric scatter present in the main DES survey, with carefully constructed representative training data in each case. We validate our joint PDFs for $10,699$ test galaxies by utilizing the copula probability integral transform and the Kendall distribution function, and their univariate counterparts to validate the marginals. Benchmarked against a basic set-up of the template-fitting code BAGPIPES, our ML-based method outperforms template fitting on all of our predefined performance metrics. In addition to accuracy, the RF is extremely fast, able to compute joint PDFs for a million galaxies in just under $6$ min with consumer computer hardware. Such speed enables PDFs to be derived in real time within analysis codes, solving potential storage issues. As part of this work we have developed GALPRO, a highly intuitive and efficient Python package to rapidly generate multivariate PDFs on-the-fly. GALPRO is documented and available for researchers to use in their cosmology and galaxy evolution studies., Comment: 18 pages, 8 figures, Accepted by MNRAS
Published: 2021

28. Dark energy survey year 1 results: The lensing imprint of cosmic voids on the cosmic microwave background

Author: Marcos Lima, David J. Brooks, Ofer Lahav, D. L. Hollowood, S. Serrano, J. De Vicente, Dragan Huterer, J. Carretero, Seshadri Nadathur, A. A. Plazas, Peter Melchior, Felipe Menanteau, J. Annis, Daniel Thomas, Joe Zuntz, L. Whiteway, J. Gschwend, M. Costanzi, M. March, P. Vielzeuf, Eric J. Baxter, M. Smith, Josh Frieman, E. Suchyta, Jennifer L. Marshall, Carlos Solans Sanchez, A. Carnero Rosell, Tim Eifler, Daniel Gruen, Nico Hamaus, G. Tarle, A. Kovács, B. Flaugher, S. Everett, D. W. Gerdes, K. Honscheid, W. G. Hartley, Santiago Avila, Antonella Palmese, Ramon Miquel, F. Paz-Chinchón, M. A. G. Maia, Jochen Weller, Juan Garcia-Bellido, V. Scarpine, U. Demirbozan, Peter Doel, T. M. C. Abbott, H. T. Diehl, E. J. Sanchez, G. Gutierrez, David J. James, Pablo Fosalba, G. Pollina, Shantanu Desai, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, Enrique Gaztanaga, R. Cawthon, M. Carrasco Kind, Kyler Kuehn, D. L. Burke, S. Allam, Robert A. Gruendl, Ministerio de Ciencia e Innovación (España), European Commission, UAM. Departamento de Física Teórica, Vielzeuf, P, Kovács, A, Demirbozan, U, Fosalba, P, Baxter, E, Hamaus, N, Huterer, D, Miquel, R, Nadathur, S, Pollina, G, Sánchez, C, Whiteway, L, Abbott, T M C, Allam, S, Annis, J, Avila, S, Brooks, D, Burke, D L, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Cawthon, R, Costanzi, M, da Costa, L N, De Vicente, J, Desai, S, Diehl, H T, Doel, P, Eifler, T F, Everett, S, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hartley, W G, Hollowood, D L, Honscheid, K, James, D J, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M A G, March, M, Marshall, J L, Melchior, P, Menanteau, F, Palmese, A, Paz-Chinchón, F, Plazas, A A, Sanchez, E, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Suchyta, E, Tarle, G, Thomas, D, Weller, J, and Zuntz, J
Subjects: Void (astronomy), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, symbols.namesake, TRACER, 0103 physical sciences, LENTES GRAVITACIONAIS, Planck, 010303 astronomy & astrophysics, STFC, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Física, RCUK, Astronomy and Astrophysics, Galaxy, 13. Climate action, Space and Planetary Science, Dark energy, symbols, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Cosmic voids gravitationally lens the cosmic microwave background (CMB) radiation, resulting in a distinct imprint on degree scales. We use the simulated CMB lensing convergence map from the Marenostrum Institut de Ciencias de l’Espai (MICE) N-body simulation to calibrate our detection strategy for a given void definition and galaxy tracer density. We then identify cosmic voids in Dark Energy Survey (DES) Year 1 data and stack the Planck 2015 lensing convergence map on their locations, probing the consistency of simulated and observed void lensing signals. When fixing the shape of the stacked convergence profile to that calibrated from simulations, we find imprints at the 3σ significance level for various analysis choices. The best measurement strategies based on the MICE calibration process yield S/N ≈ 4 for DES Y1, and the best-fitting amplitude recovered from the data is consistent with expectations from MICE (A ≈ 1). Given these results as well as the agreement between them and N-body simulations, we conclude that the previously reported excess integrated Sachs–Wolfe (ISW) signal associated with cosmic voids in DES Y1 has no counterpart in the Planck CMB lensing map., This work has made use of CosmoHub (see Carretero et al. 2017). CosmoHub has been developed by the Port d’Informacio Cient ´ ´ıfica (PIC), maintained through a collaboration of the Institut de F´ısica d’Altes Energies (IFAE) and the Centro de Investigaciones Energeticas, Medioambientales y Tecnol ´ ogicas (CIEMAT), and was ´ partially funded by the ‘Plan Estatal de Investigacion Cient ´ ´ıfica y Tecnica y de Innovaci ´ on’ program of the Spanish government. ´ Funding for the DES Projects has been provided by the US Department of Energy, the US 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, Fundac¸ao Carlos Chagas Filho de Amparo ˜ a Pesquisa do ` Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient´ıfico e Tecnologico and the Minist ´ erio da Ci ´ encia, Tecnologia ˆ e Inovac¸ao, the Deutsche Forschungsgemeinschaft, and the Collab- ˜ orating 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 Energeticas, Medioambien- ´ tales y Tecnologicas-Madrid, the University of Chicago, Univer- ´ sity College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) ¨ Zurich, Fermi National Accelerator Laboratory, the University of ¨ Illinois at Urbana-Champaign, the Institut de Ciencies de l’Espai ` (IEEC/CSIC), the Institut de F´ısica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat¨ Munchen and the associated Excellence Cluster Universe, the Uni- ¨ versity 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. This paper is 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 Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, 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, 306478, and 615929. We acknowledge support from the Brazilian Instituto Nacional de Cienciae Tecnologia ˆ (INCT) e-Universe (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. PV acknowledges the support from the grant MIUR PRIN 2015 ‘Cosmology and Fundamental Physics: illuminating the Dark Universe with Euclid’. AK has been supported by a Juan de la Cierva fellowship from MINECO with project number IJC2018-037730-I. Funding for this project was also available in part through SEV-2015-0548 and AYA2017-89891-P. This project has also received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 754558.
Published: 2021

29. Probing gravity with the DES-CMASS sample and BOSS spectroscopy

Author: Carlos Solans Sanchez, Alexandra Amon, Jack Elvin-Poole, Felipe Menanteau, Michael Schubnell, Dragan Huterer, S. Lee, Antonella Palmese, S. Everett, David J. Brooks, M. A. G. Maia, V. Scarpine, Daniel Thomas, Joseph J. Mohr, Erin Sheldon, Adriano Pieres, M. March, David J. James, M. Costanzi, F. Paz-Chinchón, Josh Frieman, Samuel Hinton, Vivian Miranda, Pablo Fosalba, J. DeRose, E. Suchyta, G. Gutierrez, M. Smith, Jennifer L. Marshall, August E. Evrard, Ashley J. Ross, Daniel Gruen, G. Tarle, E. M. Huff, P. Lemos, K. Honscheid, Ami Choi, Ben Hoyle, Ramon Miquel, Michel Aguena, J. Muir, D. W. Gerdes, J. De Vicente, I. Sevilla-Noarbe, Enrique Gaztanaga, L. F. Secco, N. Weaverdyck, A. Chen, Christopher J. Conselice, Maria E. S. Pereira, S. Samuroff, W. G. Hartley, J. Carretero, Marco Raveri, Hui Kong, J. P. Dietrich, Juan Garcia-Bellido, R. Cawthon, Christopher M. Hirata, I. Ferrero, N. Kuropatkin, P. Vielzeuf, Tim Eifler, C. D. Leonard, M. Carrasco Kind, F. Andrade-Oliveira, D. L. Burke, A. A. Plazas Malagón, T. N. Varga, Adam Amara, S. Allam, Robert A. Gruendl, M Gatti, L. N. da Costa, Ofer Lahav, Robert Morgan, M. E. C. Swanson, J. Prat, Marcos Lima, D. L. Hollowood, S. Serrano, A. Campos, C. Davis, J. Gschwend, A. Roodman, Tommaso Giannantonio, Gary Bernstein, Peter Doel, A. Carnero Rosell, H. T. Diehl, Kyler Kuehn, Niall MacCrann, Agnès Ferté, E. Bertin, Joe Zuntz, Markus Rau, Jonathan Blazek, Sarah Bridle, Scott Dodelson, S. Desai, Michael Troxel, Jochen Weller, F. J. Castander, Chun-Hao To, E. J. Sanchez, 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, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Generalitat de Catalunya, European Commission, Alfred P. Sloan Foundation, Ministerio de Economía y Competitividad (España), Lee, S, Huff, E M, Choi, A, Elvin-Poole, J, Hirata, C, Honscheid, K, Maccrann, N, Ross, A J, Troxel, M A, Eifler, T F, Kong, H, Ferté, A, Blazek, J, Huterer, D, Amara, A, Campos, A, Chen, A, Dodelson, S, Lemos, P, Leonard, C D, Miranda, V, Muir, J, Raveri, M, Secco, L F, Weaverdyck, N, Zuntz, J, Bridle, S L, Davis, C, Derose, J, Gatti, M, Prat, J, Rau, M M, Samuroff, S, Sánchez, C, Vielzeuf, P, Aguena, M, Allam, S, Amon, A, Andrade-Oliveira, F, Bernstein, G M, Bertin, E, Brooks, D, Burke, D L, Rosell, A Carnero, Carrasco&nbsp, Kind, M, Carretero, J, Castander, F J, Cawthon, R, Conselice, C, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, De&nbsp, Vicente, J, Desai, S, Diehl, H T, Dietrich, J P, Doel, P, Everett, S, Evrard, A E, Ferrero, I, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Giannantonio, T, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hartley, W G, Hinton, S R, Hollowood, D L, Hoyle, B, James, D J, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M A G, March, M, Marshall, J L, Menanteau, F, Miquel, R, Mohr, J J, Morgan, R, Palmese, A, Paz-Chinchón, F, Pieres, A, Malagón, A A Plaza, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Smith, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, To, C, Varga, T N, and Weller, J
Subjects: gravitation: model, Astrophysics, baryon: oscillation: acoustic, 01 natural sciences, DESI, large scales, cosmological model: parameter space, general relativity, LENTES GRAVITACIONAIS, cluster, dark energy, 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, cosmological parameters, gravitational lensing, large-scale structure of the Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, symbols, cfhtlens, cosmological parameter, satellite: Planck, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, tomography, efficient, symbols.namesake, redshift-space distortions, statistical analysis, gravitation: lens, 0103 physical sciences, overlap, structure, Planck, dark energy survey, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysics, cross-correlation, redshift, Redshift, Galaxy, testing gravity, Baryon, Boss, Space and Planetary Science, Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology
Abstract: DES Collaboration: et al., The DES-CMASS sample (DMASS) is designed to optimally combine the weak lensing measurements from the Dark Energy Survey (DES) and redshift-space distortions (RSD) probed by the CMASS galaxy sample from the Baryonic Oscillation Spectroscopic Survey. In this paper, we demonstrate the feasibility of adopting DMASS as the equivalent of CMASS for a joint analysis of DES and BOSS in the framework of modified gravity. We utilize the angular clustering of the DMASS galaxies, cosmic shear of the DES METACALIBRATION sources, and cross-correlation of the two as data vectors. By jointly fitting the combination of the data with the RSD measurements from the CMASS sample and Planck data, we obtain the constraints on modified gravity parameters μ0=−0.37+0.47−0.45 and Σ0=0.078+0.078−0.082⁠. Our constraints of modified gravity with DMASS are tighter than those with the DES Year 1 REDMAGIC sample with the same external data sets by 29 per cent for μ0 and 21 per cent for Σ0, and comparable to the published results of the DES Year 1 modified gravity analysis despite this work using fewer external data sets. This improvement is mainly because the galaxy bias parameter is shared and more tightly constrained by both CMASS and DMASS, effectively breaking the degeneracy between the galaxy bias and other cosmological parameters. Such an approach to optimally combine photometric and spectroscopic surveys using a photometric sample equivalent to a spectroscopic sample can be applied to combining future surveys having a limited overlap such as DESI and LSST., AC acknowledges support from NASA grant no. 15-WFIRST15-0008. During the preparation of this paper, C.H. was supported by the Simons Foundation, NASA, and the U.S. Department of Energy. 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 Ciência e Tecnologia (INCT) do e-Universo (CNPq grant no. 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. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science.
Published: 2021
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30. The WaZP galaxy cluster sample of the dark energy survey year 1

Author: G. Tarle, David J. Brooks, Antonella Palmese, David J. James, Josh Frieman, M. A. G. Maia, Pablo Fosalba, F. Paz-Chinchón, Michael Schubnell, M. Smith, Agnès Ferté, Samuel Hinton, Christophe Benoist, E. Suchyta, Basilio X. Santiago, August E. Evrard, G. Gutierrez, I. Ferrero, Sunayana Bhargava, J. Carretero, R. D. Wilkinson, B. Flaugher, H. Sampaio-Santos, Peter Melchior, Santiago Avila, K. Honscheid, R. L. C. Ogando, J. De Vicente, S. Everett, M. Carrasco Kind, S. Desai, Ramon Miquel, I. Sevilla-Noarbe, Juan Garcia-Bellido, Ofer Lahav, M. Soares-Santos, N. Kuropatkin, L. N. da Costa, Robert Morgan, A. Carnero Rosell, M. Costanzi, Marcos Lima, D. L. Hollowood, S. Serrano, Chun-Hao To, E. J. Sanchez, Douglas L. Tucker, Kyler Kuehn, Paul Giles, E. Bertin, J. Gschwend, Peter Doel, H. T. Diehl, David Bacon, S. Allam, Robert A. Gruendl, Tesla E. Jeltema, A. A. Plazas, Michel Aguena, A. K. Romer, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-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, Aguena, M., Benoist, C., da Costa, L. N., Ogando, R. L., Gschwend, J., Sampaio dos Santos, H., Lima, M., Maia, M. A., Allam, S., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Giles, P., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D. L., Honscheid, K., James, D., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Melchior, P., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchon, F., Plazas Malagón, A., Romer, K., Sanchez, E., Santiago, B., Schubnell, M., Serrano, S., Sevilla, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Tucker, D., Wilkinson, R., National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, and Instituto Nacional de Ciência e Tecnologia (Brasil)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Lambda, 01 natural sciences, surveys, 0103 physical sciences, distances and redshifts [Galaxies], Cluster (physics), clusters: general [galaxies], survey, distances and redshift [galaxies], data analysis [Methods], 010303 astronomy & astrophysics, Galaxy cluster, Photometric redshift, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, methods: data analysis, Galaxy, Redshift, South Pole Telescope, Space and Planetary Science, galaxies: clusters: general, data analysi [methods], Cluster sampling, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aguena, M., et al., We present a new (2+1)D galaxy cluster finder based on photometric redshifts called Wavelet Z Photometric (WaZP) applied to DES first year (Y1A1) data. The results are compared to clusters detected by the South Pole Telescope (SPT) survey and the redMaPPer cluster finder, the latter based on the same photometric data. WaZP searches for clusters in wavelet-based density maps of galaxies selected in photometric redshift space without any assumption on the cluster galaxy populations. The comparison to other cluster samples was performed with a matching algorithm based on angular proximity and redshift difference of the clusters. It led to the development of a new approach to match two optical cluster samples, following an iterative approach to minimize incorrect associations. The WaZP cluster finder applied to DES Y1A1 galaxy survey (1511.13 deg2 up to mi = 23 mag) led to the detection of 60 547 galaxy clusters with redshifts 0.05 < z < 0.9 and richness Ngals ≥ 5. Considering the overlapping regions and redshift ranges between the DES Y1A1 and SPT cluster surveys, all sz based SPT clusters are recovered by the WaZP sample. The comparison between WaZP and redMaPPer cluster samples showed an excellent overall agreement for clusters with richness Ngals (λ for redMaPPer) greater than 25 (20), with 95 per cent recovery on both directions. Based on the cluster cross-match, we explore the relative fragmentation of the two cluster samples and investigate the possible signatures of unmatched clusters., 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 Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2021

31. Dark Energy Survey Year 3 results: Curved-sky weak lensing mass map reconstruction

Author: Sunayana Bhargava, Jennifer L. Marshall, David J. Brooks, Carlos Solans Sanchez, G. Tarle, Samuel Hinton, G. Gutierrez, Alexandra Amon, Peter Doel, Ami Choi, Ben Hoyle, Marco Raveri, B. Flaugher, F. Andrade-Oliveira, Jochen Weller, R. P. Rollins, H. T. Diehl, D. L. Burke, Felipe Menanteau, Alex Drlica-Wagner, J. DeRose, F. J. Castander, David Bacon, E. Suchyta, Dragan Huterer, Christopher J. Conselice, Brian Yanny, Jack Elvin-Poole, U. Demirbozan, Maria E. S. Pereira, Niall MacCrann, Keith Bechtol, Erin Sheldon, Martin Crocce, V. Scarpine, T. M. C. Abbott, Peter Melchior, D. L. Hollowood, S. Serrano, Agnès Ferté, J. De Vicente, J. Cordero, P. F. Leget, A. Campos, Eli S. Rykoff, C. Doux, Chun-Hao To, E. J. Sanchez, K. Herner, F. Paz-Chinchón, J. Carretero, Antonella Palmese, Marcos Lima, J. Myles, I. Harrison, G. Pollina, A. Roodman, David J. James, Tommaso Giannantonio, D. Zeurcher, M. A. G. Maia, M. Rodriguez-Monroy, Joe Zuntz, A. Alarcon, B. Yin, S. Allam, Robert A. Gruendl, A. Kovács, Matthew R. Becker, Pablo Fosalba, B. Mawdsley, Ashley J. Ross, S. Pandey, J. Muir, Joseph J. Mohr, Michael Troxel, I. Ferrero, Matt J. Jarvis, A. Carnero Rosell, J. McCullough, P. Vielzeuf, Yanxi Zhang, Seshadri Nadathur, M. Carrasco Kind, M. March, S. Everett, M. Smith, M. Costanzi, Jean-Luc Starck, Daniel Gruen, I. Tutusaus, Francois Lanusse, Chihway Chang, Daniel Thomas, J. Prat, L. Whiteway, F. Elsner, S. Desai, I. Sevilla-Noarbe, M. Soares-Santos, G. Giannini, W. G. Hartley, D. W. Gerdes, R. Cawthon, N. Kuropatkin, Ramon Miquel, K. D. Eckert, T. N. Varga, L. N. da Costa, J. P. Dietrich, Juan Garcia-Bellido, E. Bertin, E. M. Huff, R. Chen, Michel Aguena, Enrique Gaztanaga, R. L. C. Ogando, Bhuvnesh Jain, M Gatti, Ofer Lahav, Niall Jeffrey, Robert Morgan, L. F. Secco, Nico Hamaus, A. A. Plazas, A. Navarro-Alsina, T. Shin, T. Kacprzak, C. Davis, J. Gschwend, Gary Bernstein, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), University of Portsmouth, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-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, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Jeffrey, N., Gatti, M., Chang, C., Whiteway, L., Demirbozan, U., Kovacs, A., Pollina, G., Bacon, D., Hamaus, N., Kacprzak, T., Lahav, O., Lanusse, F., Mawdsley, B., Nadathur, S., Starck, J. L., Vielzeuf, P., Zeurcher, D., Alarcon, A., Amon, A., Bechtol, K., Bernstein, G. M., Campos, A., Rosell, A. C., Kind, M. C., Cawthon, R., Chen, R., Choi, A., Cordero, J., Davis, C., Derose, J., Doux, C., Drlica-Wagner, A., Eckert, K., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Kuropatkin, N., Jarvis, M., Leget, P. F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Pandey, S., Prat, J., Raveri, M., Rollins, R. P., Ross, A. J., Rykoff, E. S., Sanchez, C., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., 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., Becker, M. R., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Crocce, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Hoyle, B., Jain, B., James, D. J., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Weller, J., Université de Paris, University College London, Barcelona Institute of Science and Technology, University of Pennsylvania, University of Chicago, Calle Viá Láctea, Universidad de La Laguna (ULL), Ludwig-Maximilians Universität München, ETH Zurich, Argonne National Laboratory, Stanford University, University of Wisconsin-Madison, CarnegieMellon University, Instituto de Astrofisica de Canarias, Laboratorio Interinstitucional de e-Astronomia-LIneA, Dpto. Astrofisica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, Ohio State University, University of Manchester, University of California,Berkeley, Santa Cruz Institute for Particle Physics, Fermi National Accelerator Laboratory, California Institute of Technology, SLAC National Accelerator Laboratory, Denys Wilkinson Building, University of Geneva, University of Michigan, University of Cambridge, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnologicas (CIEMAT), Brookhaven National Laboratory, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Max Planck Institute for Extraterrestrial Physics, University of Edinburgh, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de Saõ Paul, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique deParis, Institut d'Astrophysique de Paris, University of Sussex, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universitat, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics | Harvard and Smithsonian, Texas A and M University, Princeton University, Institucio Catalana de Recerca i Estudis Avancats, University of Southampton, Oak Ridge National Laboratory, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Gravitational lensing: weak, 0103 physical sciences, Prior probability, Maximum a posteriori estimation, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, Methods: statistical, media_common, Physics, ST/M001334/1, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Celestial sphere, gravitational lensing: Weak, large-scale structure of Universe, methods: Statistical, ST/R000476/1, Galaxy, Space and Planetary Science, Sky, astro-ph.CO, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Jeffrey, N., et al. DES Collaboration, We present reconstructed convergence maps, mass maps, from the Dark Energy Survey (DES) third year (Y3) weak gravitational lensing data set. The mass maps are weighted projections of the density field (primarily dark matter) in the foreground of the observed galaxies. We use four reconstruction methods, each is a maximum a posteriori estimate with a different model for the prior probability of the map: Kaiser–Squires, null B-mode prior, Gaussian prior, and a sparsity prior. All methods are implemented on the celestial sphere to accommodate the large sky coverage of the DES Y3 data. We compare the methods using realistic ΛCDM simulations with mock data that are closely matched to the DES Y3 data. We quantify the performance of the methods at the map level and then apply the reconstruction methods to the DES Y3 data, performing tests for systematic error effects. The maps are compared with optical foreground cosmic-web structures and are used to evaluate the lensing signal from cosmic-void profiles. The recovered dark matter map covers the largest sky fraction of any galaxy weak lensing map to date., 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 Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper 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. NJ has been supported by funding from l’Ecole Normale Supérieure, Paris. OL and NJ acknowledge support from a European Research Council Advanced Grant TESTDE (FP7/291329) and STFC Consolidated Grants ST/M001334/1 and ST/R000476/1. AK has been supported by a Juan de la Cierva fellowship from MINECO with project number IJC2018-037730-I, and funding for this project was also available in part through SEV-2015-0548 and AYA2017-89891-P. Cosmic voids computational work has been performed on the UK SCIAMA High Performance Computing cluster supported by the ICG, SEPNet, and the University of Portsmouth.
Published: 2021

32. Pushing automated morphological classifications to their limits with the Dark Energy Survey

Author: Mariangela Bernardi, E. Suchyta, J. Carretero, M. Carrasco Kind, Christopher J. Conselice, A. G. Kim, A. Carnero Rosell, Felipe Menanteau, Marc Huertas-Company, E. Bertin, W. G. Hartley, I. Ferrero, Matt J. Jarvis, David J. Brooks, Jesús Vega-Ferrero, Samuel Hinton, Josh Frieman, J. Gschwend, M. E. C. Swanson, M. Smith, G. Gutierrez, D. L. Hollowood, Pablo Fosalba, R. L. C. Ogando, S. Serrano, Santiago Avila, Daniel Gruen, Ramon Miquel, H. Domínguez Sánchez, V. Scarpine, A. Choi, I. Sevilla-Noarbe, K. Honscheid, N. Kuropatkin, T. N. Varga, S. Desai, David Bacon, L. N. da Costa, S. Allam, Marcos Lima, G. Tarle, Michael Schubnell, Robert A. Gruendl, Ben Hoyle, Maria E. S. Pereira, Chun-Hao To, E. J. Sanchez, Antonella Palmese, B. Margalef, M. A. G. Maia, Michel Aguena, Robert Morgan, F. Tarsitano, F. Paz-Chinchón, A. K. Romer, J. De Vicente, A. A. Plazas, Douglas L. Tucker, Kyler Kuehn, M. Costanzi, R. D. Wilkinson, Juan Garcia-Bellido, J. Annis, 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), Vega-Ferrero, J., Domínguez Sánchez, H., Bernardi, M., Huertas-Company, M., Morgan, R., Margalef, B., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Choi, A., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Jarvis, M., Kim, A. G., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Tarsitano, F., To, C., Tucker, D. L., Varga, T. N., Wilkinson, R. D., Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), 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 des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), structure [Galaxies], FOS: Physical sciences, Classification scheme, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Convolutional neural network, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, observational [Methods], 010303 astronomy & astrophysics, Lenticular galaxy, catalogues, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, business.industry, Deep learning, Astronomy and Astrophysics, Pattern recognition, Catalogues, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, galaxies: structure, Artificial intelligence, methods: observational, Astrophysics - Cosmology and Nongalactic Astrophysics, catalogue, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data release
Abstract: Vega-Ferrero, J., et al., We present morphological classifications of ∼27 million galaxies from the Dark Energy Survey (DES) Data Release 1 (DR1) using a supervised deep learning algorithm. The classification scheme separates: (a) early-type galaxies (ETGs) from late-type galaxies (LTGs); and (b) face-on galaxies from edge-on. Our convolutional neural networks (CNNs) are trained on a small subset of DES objects with previously known classifications. These typically have mr ≲ 17.7 mag; we model fainter objects to mr < 21.5 mag by simulating what the brighter objects with well-determined classifications would look like if they were at higher redshifts. The CNNs reach 97 per cent accuracy to mr < 21.5 on their training sets, suggesting that they are able to recover features more accurately than the human eye. We then used the trained CNNs to classify the vast majority of the other DES images. The final catalogue comprises five independent CNN predictions for each classification scheme, helping to determine if the CNN predictions are robust or not. We obtain secure classifications for ∼87 per cent and 73 per cent of the catalogue for the ETG versus LTG and edge-on versus face-on models, respectively. Combining the two classifications (a) and (b) helps to increase the purity of the ETG sample and to identify edge-on lenticular galaxies (as ETGs with high ellipticity). Where a comparison is possible, our classifications correlate very well with Sérsic index (n), ellipticity (ϵ), and spectral type, even for the fainter galaxies. This is the largest multiband catalogue of automated galaxy morphologies to date., 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 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.
Published: 2021

33. Lensing Without Borders. I. A Blind Comparison of the Amplitude of Galaxy-Galaxy Lensing Between Independent Imaging Surveys

Author: A Leauthaud, A Amon, S Singh, D Gruen, J U Lange, S Huang, N C Robertson, T N Varga, Y Luo, C Heymans, H Hildebrandt, C Blake, M Aguena, S Allam, F Andrade-Oliveira, J Annis, E Bertin, S Bhargava, J Blazek, S L Bridle, D Brooks, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, R Cawthon, A Choi, M Costanzi, L N da Costa, M E S Pereira, C Davis, J De Vicente, J DeRose, H T Diehl, J P Dietrich, P Doel, K Eckert, S Everett, A E Evrard, I Ferrero, B Flaugher, P Fosalba, J García-Bellido, M Gatti, E Gaztanaga, R A Gruendl, J Gschwend, W G Hartley, D L Hollowood, K Honscheid, B Jain, D J James, M Jarvis, B Joachimi, A Kannawadi, A G Kim, E Krause, K Kuehn, K Kuijken, N Kuropatkin, M Lima, N MacCrann, M A G Maia, M Makler, M March, J L Marshall, P Melchior, F Menanteau, R Miquel, H Miyatake, J J Mohr, B Moraes, S More, M Surhud, R Morgan, J Myles, R L C Ogando, A Palmese, F Paz-Chinchón, A A Plazas Malagón, J Prat, M M Rau, J Rhodes, M Rodriguez-Monroy, A Roodman, A J Ross, S Samuroff, C Sánchez, E Sanchez, V Scarpine, D J Schlegel, M Schubnell, S Serrano, I Sevilla-Noarbe, C Sifón, M Smith, J S Speagle, E Suchyta, G Tarle, D Thomas, J Tinker, C To, M A Troxel, L Van Waerbeke, P Vielzeuf, A H Wright, Santa Cruz, Stanford University, Carnegie Mellon University, Berkeley, Ludwig-Maximilians Universität München, Princeton University, University of Cambridge, Max Planck Institute for Extraterrestrial Physics, Royal Observatory, German Centre for Cosmolo gical Lensing, Swinburne University of Technology, Laboratoire d'Annecy De Physique Des Particules (LAPP), Laboratório Interinstitucional de e-Astronomia LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, CNRS, Northeastern University, Observatoire de Sauverny, University of Manchester, University College London, SLAC National Accelerator Laboratory, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, The Barcelona Institute of Science and Technology, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), University of Wisconsin Madison, The Ohio State University, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, Univer sität Hamburg, Medioambientales y Tecnológicas (CIEMAT), Lawrence Berkeley National Laboratory, Santa Cruz Institute for Particle Physics, Ludwig-Maximilians-Universität, University of Pennsylvania, University of Michigan, University of Oslo, Universidad Autonoma de Madrid, University of Geneva, ASTRAVEO LLC, University of Arizona, Macquarie University, Lowell Observatory, Leiden University, Universidade de São Paulo (USP), ECyT UNSAM, Centro Brasileiro de Pesquisas Físicas, Texas A&M University, Institució Catalana de Recerca i Estudis Avancats, Nagoya University, University of Tokyo, Universidade Federal do Rio de Janeiro (UFRJ), The Inter-University Centre for Astronomy and Astrophysics, University of Chicago, University of British Columbia, California Institute of Technology, Pontificia Universidad Católica de Valparaíso, University of Southampton, University of Toronto, Oak Ridge National Laboratory, University of Portsmouth, New York University, Duke University, Leauthaud, A, Amon, A, Singh, S, Gruen, D, Lange, J U, Huang, S, Robertson, N C, Varga, T N, Luo, Y, Heymans, C, Hildebrandt, H, Blake, C, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Bhargava, S, Blazek, J, Bridle, S L, Brooks, D, Burke, D L, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, F J, Cawthon, R, Choi, A, Costanzi, M, da Costa, L N, Pereira, M E S, Davis, C, De Vicente, J, Derose, J, Diehl, H T, Dietrich, J P, Doel, P, Eckert, K, Everett, S, Evrard, A E, Ferrero, I, Flaugher, B, Fosalba, P, García-Bellido, J, Gatti, M, Gaztanaga, E, Gruendl, R A, Gschwend, J, Hartley, W G, Hollowood, D L, Honscheid, K, Jain, B, James, D J, Jarvis, M, Joachimi, B, Kannawadi, A, Kim, A G, Krause, E, Kuehn, K, Kuijken, K, Kuropatkin, N, Lima, M, Maccrann, N, Maia, M A G, Makler, M, March, M, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Miyatake, H, Mohr, J J, Moraes, B, More, S, Surhud, M, Morgan, R, Myles, J, Ogando, R L C, Palmese, A, Paz-Chinchón, F, Malagón, A A Plaza, Prat, J, Rau, M M, Rhodes, J, Rodriguez-Monroy, M, Roodman, A, Ross, A J, Samuroff, S, Sánchez, C, Sanchez, E, Scarpine, V, Schlegel, D J, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Sifón, C, Smith, M, Speagle, J S, Suchyta, E, Tarle, G, Thomas, D, Tinker, J, To, C, Troxel, M A, Van Waerbeke, L, Vielzeuf, P, Wright, A H, UAM. Departamento de Física Teórica, National Science Foundation (US), Department of Energy (US), European Commission, European Research Council, Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and DES
Subjects: photometric redshifts, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational lensing, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, bonn deep survey, 1st data, redshift distributions, shear calibration, Astrophysics::Galaxy Astrophysics, Observations, data release, Física, Astronomy and Astrophysics, observations [cosmology], Cosmology, Space and Planetary Science, cosmology: observations, cosmological constraints, cross-correlations, digital sky survey, iii. application, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmology and Nongalactic Astrophysics, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A. Leauthaud et al., Lensing without borders is a cross-survey collaboration created to assess the consistency of galaxy–galaxy lensing signals (ΔΣ) across different data sets and to carry out end-to-end tests of systematic errors. We perform a blind comparison of the amplitude of ΔΣ using lens samples from BOSS and six independent lensing surveys. We find good agreement between empirically estimated and reported systematic errors which agree to better than 2.3σ in four lens bins and three radial ranges. For lenses with zL > 0.43 and considering statistical errors, we detect a 3–4σ correlation between lensing amplitude and survey depth. This correlation could arise from the increasing impact at higher redshift of unrecognized galaxy blends on shear calibration and imperfections in photometric redshift calibration. At zL > 0.54, amplitudes may additionally correlate with foreground stellar density. The amplitude of these trends is within survey-defined systematic error budgets that are designed to include known shear and redshift calibration uncertainty. Using a fully empirical and conservative method, we do not find evidence for large unknown systematics. Systematic errors greater than 15 per cent (25 per cent) ruled out in three lens bins at 68 per cent (95 per cent) confidence at z < 0.54. Differences with respect to predictions based on clustering are observed to be at the 20–30 per cent level. Our results therefore suggest that lensing systematics alone are unlikely to fully explain the ‘lensing is low’ effect at z < 0.54. This analysis demonstrates the power of cross-survey comparisons and provides a promising path for identifying and reducing systematics in future lensing analyses., We acknowledge use of the lux supercomputer at UC Santa Cruz, funded by NSF MRI grant AST 1828315. This material is based on work supported by the U.D Department of Energy, Office of Science, Office of High Energy Physics under Award Number DE-SC0019301. AL acknowledges support from the David and Lucille Packard foundation, and from the Alfred.P Sloan foundation. CH acknowledges support from the European Research Council under grant number 647112, and support from the Max Planck Society and the Alexander von Humboldt Foundation in the framework of the Max Planck-Humboldt Research Award endowed by the Federal Ministry of Education and Research. KK acknowledges support from the Royal Society and Imperial College. HH is supported by a Heisenberg grant of the Deutsche Forschungsgemeinschaft (Hi 1495/5-1), as well as an ERC Consolidator Grant (no. 770935). AHW is supported by an European Research Council Consolidator Grant (no. 770935). 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 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) 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. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organisation (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from the Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science, and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org This paper is based [in part] on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center (ADC) at NAOJ. Data analysis was in part carried out with the cooperation of Center for Computational Astrophysics (CfCA), NAOJ. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, 177.A-3018, and 179.A-2004, and on data products produced by the KiDS consortium. The KiDS production team acknowledges support from: Deutsche Forschungsgemeinschaft, ERC, NOVA, and NWO-M grants; Target; the University of Padova, and the University Federico II (Naples). This work was supported by the Department of Energy, Laboratory Directed Research and Development program at SLAC National Accelerator Laboratory, under contract DE-AC02-76SF00515 and as a part of the Panofsky Fellowship awarded to DG. MM is partially funded by FAPERJ, CNPq, and CONICET. BM acknowledges support from the Brazilian funding agency FAPERJ.
Published: 2021
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34. The STRong lensing Insights into the Dark Energy Survey (STRIDES) 2017/2018 follow-up campaign: discovery of 10 lensed quasars and 10 quasar pairs

Author: A. A. Plazas, C. Lemon, Antonella Palmese, M. Smith, M. A. G. Maia, G C-F Chen, J. Carretero, Anowar J. Shajib, Marcos Lima, Adriano Agnello, Frederic Courbin, Ramon Miquel, Shantanu Desai, D. L. Burke, G. Gutierrez, G. Tarle, Daniel Gruen, M. March, Ofer Lahav, Paul L. Schechter, Tim Eifler, Enrique Gaztanaga, Thomas E. Collett, A. Carnero Rosell, M. Costanzi, Yordanka Apostolovski, Kyler Kuehn, Juan Garcia-Bellido, Richard G. McMahon, Christopher D. Fassnacht, S. Allam, Robert A. Gruendl, Elisabeth Krause, David J. Brooks, A. Melo, Simon Birrer, Motta, David J. James, D. W. Gerdes, Matthew W. Auger, Michael Schubnell, Tommaso Treu, Josh Frieman, Cristian E. Rusu, Felipe Menanteau, M. Carrasco Kind, A. Roodman, B. Flaugher, J. Annis, Alistair R. Walker, Marcelle Soares-Santos, Timo Anguita, E. Suchyta, S. Serrano, K. Honscheid, N. Kuropatkin, F. Paz-Chinchón, Santiago Avila, Jennifer L. Marshall, L. N. da Costa, A. G. Kim, J. De Vicente, Huan Lin, E. Buckley-Geer, T. M. C. Abbott, E. Bertin, E. J. Sanchez, J. Gschwend, Lemon, C., Auger, M. W., Mcmahon, R., Anguita, T., Apostolovski, Y., Chen, G. C. -F., Fassnacht, C. D., Melo, A. D., Motta, V., Shajib, A., Treu, T., Agnello, A., Buckley-Geer, E., Schechter, P. L., Birrer, S., Collett, T., Courbin, F., Rusu, C. E., Abbott, T. M. C., Allam, S., Annis, J., Avila, S., 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., Eifler, T. F., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kim, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., 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, McMahon, Richard [0000-0001-8447-8869], and Apollo - University of Cambridge Repository
Subjects: candidates, observational [methods], time-delay, Astrophysics, 01 natural sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, sky, Physics, Faint Object Spectrograph, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational lensing: strong, gravitational lenses, strong [gravitational lensing], Astrophysics::Earth and Planetary Astrophysics, methods: observational, sextractor, Astronomical and Space Sciences, astro-ph.GA, FOS: Physical sciences, selection, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Photometry (optics), quasars: general, Gravitational Lenses, 0103 physical sciences, Quasars, Spectrograph, STFC, Astrophysics::Galaxy Astrophysics, general [quasars], 010308 nuclear & particles physics, variability, Near-infrared spectroscopy, RCUK, Astronomy and Astrophysics, Quasar, Galaxies, Light curve, redshift, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), gaia, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmograil
Abstract: We report the results of the STRong lensing Insights from the Dark Energy Survey (STRIDES) follow-up campaign of the late 2017/early 2018 season. We obtained spectra of 65 lensed quasar candidates either with EFOSC2 on the NTT or ESI on Keck, which confirm 10 new gravitationally lensed quasars and 10 quasar pairs with similar spectra, but which do not show a lensing galaxy in DES images. Eight lensed quasars are doubly imaged with source redshifts between 0.99 and 2.90, one is triply imaged by a group (DESJ0345-2545, $z=1.68$), and one is quadruply imaged (quad: DESJ0053-2012, $z=3.8$). Singular isothermal ellipsoid models for the doubles, based on high-resolution imaging from SAMI on SOAR or NIRC2 on Keck, give total magnifications between 3.2 and 5.6, and Einstein radii between 0.49 and 1.97 arcseconds. After spectroscopic follow-up, we extract multi-epoch $grizY$ photometry of confirmed lensed quasars and contaminant quasar+star pairs from the first 4 years of DES data using parametric multi-band modelling, and compare variability in each system's components. By measuring the reduced ${\chi}^2$ associated with fitting all epochs to the same magnitude, we find a simple cut on the less variable component that retains all confirmed lensed quasars, while removing 94 per cent of contaminant systems with stellar components. Based on our spectroscopic follow-up, this variability information can improve selection of lensed quasars and quasar pairs from 34-45 per cent to 51-70 per cent, with the majority of remaining contaminants being compact star-forming galaxies. Using mock lensed quasar lightcurves we demonstrate that selection based only on variability will over-represent the quad fraction by 10 per cent over a complete DES magnitude-limited sample (excluding microlensing differences), explained by the magnification bias and hence lower luminosity (more variable) sources in quads., Comment: 22 pages, 16 figures, submitted to MNRAS
Published: 2020

35. Blinding multiprobe cosmological experiments

Author: Michael Troxel, Matt J. Jarvis, Kyler Kuehn, I. Sevilla-Noarbe, Tim Eifler, Josh Frieman, N. Kuropatkin, G. Tarle, Jochen Weller, Shantanu Desai, J. Gschwend, Alistair R. Walker, Gary Bernstein, W. G. Hartley, L. N. da Costa, M. Smith, Ramon Miquel, W. C. Wester, Peter Melchior, Daniel Gruen, E. J. Sanchez, Michael Schubnell, David J. James, A. A. Plazas, Felipe Menanteau, Elisabeth Krause, Pablo Fosalba, R. Cawthon, Antonella Palmese, Keith Bechtol, E. Bertin, D. L. Burke, J. Carretero, Santiago Avila, Daniel Thomas, D. W. Gerdes, E. Buckley-Geer, F. Elsner, Peter Doel, S. Allam, Robert A. Gruendl, V. Scarpine, Joe Zuntz, F. Paz-Chinchón, M. Carrasco Kind, A. Carnero Rosell, A. K. Romer, M. Costanzi, J. Muir, R. L. C. Ogando, Dragan Huterer, J. P. Dietrich, Juan Garcia-Bellido, J. Annis, David J. Brooks, Jennifer L. Marshall, Ofer Lahav, E. Suchyta, J. De Vicente, A. Roodman, M. March, D. L. Hollowood, S. Serrano, S. Everett, 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, Muir, J., Bernstein, G. M., Huterer, D., Elsner, F., Krause, E., Roodman, A., Allam, S., Annis, J., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hollowood, D. L., James, D. J., Jarvis, M., Kuehn, K., Kuropatkin, N., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Troxel, M. A., Walker, A. R., Weller, J., Wester, W., Zuntz, J., and Des, Collaboration
Subjects: Accuracy and precision, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Blinding, statistical [methods], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, methods: numerical, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Cluster analysis, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Weak gravitational lensing, Physics, methods: statistical, 010308 nuclear & particles physics, Estimation theory, Astronomy and Astrophysics, numerical [methods], methods: data analysis, Galaxy, Space and Planetary Science, cosmology: observations, data analysi [methods], Dark energy, astro-ph.CO, large-scale structure of Universe, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology], astro-ph.IM
Abstract: The goal of blinding is to hide an experiment's critical results -- here the inferred cosmological parameters -- until all decisions affecting its analysis have been finalised. This is especially important in the current era of precision cosmology, when the results of any new experiment are closely scrutinised for consistency or tension with previous results. In analyses that combine multiple observational probes, like the combination of galaxy clustering and weak lensing in the Dark Energy Survey (DES), it is challenging to blind the results while retaining the ability to check for (in)consistency between different parts of the data. We propose a simple new blinding transformation that works by modifying the summary statistics that are input to parameter estimation, such as two-point correlation functions. The transformation shifts the measured statistics to new values that are consistent with (blindly) shifted cosmological parameters, while preserving internal (in)consistency. We apply the blinding transformation to simulated data for the projected DES Year 3 galaxy clustering and weak lensing analysis, demonstrating that practical blinding is achieved without significant perturbation of internal-consistency checks, as measured here by degradation of the $\chi^2$ between data and best-fitting model. Our blinding method conserves $\chi^2$ more precisely as experiments evolve to higher precision., Comment: 18 pages, 13 figures, data available upon request. Updated to match published version
Published: 2020

36. Observation and confirmation of nine strong-lensing systems in Dark Energy Survey Year 1 data

Author: M. Smith, Daniel Gruen, V. Scarpine, A. K. Romer, Felipe Menanteau, M. E. C. Swanson, Eli S. Rykoff, E. Suchyta, Enrique Gaztanaga, August E. Evrard, J. Carretero, Marco A. P. Lima, Juan Garcia-Bellido, Brian Nord, Michael Schubnell, Adriano Agnello, C. Davis, Keith Bechtol, Flavia Sobreira, Santiago Avila, M. Carrasco Kind, A. Carnero Rosell, I. Sevilla-Noarbe, Carlos E. Cunha, Yanxi Zhang, Douglas L. Tucker, Kyler Kuehn, Tim Eifler, G. Gutierrez, G. Tarle, A. A. Plazas, N. Kuropatkin, Enrique Fernández, L. N. da Costa, Huan Lin, Josh Frieman, M. March, K. Honscheid, David J. James, David J. Brooks, R. H. Schindler, Pablo Fosalba, T. M. C. Abbott, D. L. Burke, Ofer Lahav, Peter Doel, E. J. Sanchez, S. Allam, Robert A. Gruendl, Marcelle Soares-Santos, H. T. Diehl, J. Annis, D. L. Hollowood, J. De Vicente, W. G. Hartley, Jennifer L. Marshall, Daniel Thomas, E. Buckley-Geer, Adam Amara, Ramon Miquel, Thomas E. Collett, A. Roodman, B. Flaugher, Ben Hoyle, M. A. G. Maia, Peter Melchior, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, 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 de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), and German Research Foundation
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, Gravitational lensing: strong, DES [surveys], astro-ph.GA, Library science, Techniques: spectroscopic, FOS: Physical sciences, clusters [gravitational lensing], Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, survey [gravitational lensing], Galaxies: individual, 0103 physical sciences, media_common.cataloged_instance, Astrophysics::Solar and Stellar Astrophysics, European union, general [gravitational lenses], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, STFC, media_common, Physics, 010308 nuclear & particles physics, business.industry, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, gravitational lensing individual, Alliance, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), strong [gravitational lensing], Fundamental physics, astro-ph.CO, Christian ministry, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract: We describe the observation and confirmation of nine new strong gravitational lenses discovered in Year 1 data from the Dark Energy Survey (DES). We created candidate lists based on (i) galaxy group and cluster samples, and (ii) photometrically selected galaxy samples. We selected 46 candidates through visual inspection and then used the Gemini Multi-Object Spectrograph (GMOS) at the Gemini South telescope to acquire a spectroscopic follow-up of 21 of these candidates. Through an analysis of these spectroscopic follow-up data, we confirmed nine new lensing systems and rejected two candidates, and the analysis was inconclusive on 10 candidates. For each of the confirmed systems, our report measured spectroscopic properties, estimated source image-lens separations, and estimated enclosed masses as well. The sources that we targeted have an i-band surface brightness range of i ∼ 22-24 mag arcsec and a spectroscopic redshift range of z ∼ 0.8−2.6. The lens galaxies have a photometric redshift range of z ∼ 0.3−0.7. The lensing systems range in source image-lens separation from 2 to 9 arcsec and in enclosed mass from 10 to 10 M, 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, Fundac¸ão 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 e Tecnologia, the Deutsche Forschungsge-meinschaft, and the Collaborating Institutions in the DES. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. 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

37. Monte Carlo control loops for cosmic shear cosmology with DES Year 1 data

Author: L. F. Secco, G. Tarle, Sarah Bridle, Santiago Avila, David J. Brooks, M. A. G. Maia, S. Desai, M. Carrasco Kind, David J. James, Claudio Bruderer, G. Gutierrez, M. E. C. Swanson, Raphael Sgier, Jörg Herbel, Robert A. Gruendl, Matt J. Jarvis, W. G. Hartley, Vinu Vikram, E. Suchyta, Ben Hoyle, Juan Garcia-Bellido, J. Carretero, Adam Amara, V. Scarpine, E. Buckley-Geer, Alexandre Refregier, Peter Doel, M. Smith, Daniel Gruen, H. T. Diehl, I. Sevilla-Noarbe, L. N. da Costa, E. Bertin, Ramon Miquel, Joe Zuntz, A. A. Plazas, J. Gschwend, Marcos Lima, T. Kacprzak, Enrique Gaztanaga, Jochen Weller, J. De Vicente, E. J. Sanchez, F. Paz-Chinchón, D. L. Hollowood, S. Serrano, Andrina Nicola, Felipe Menanteau, Alex Drlica-Wagner, J. Annis, F. Tarsitano, Peter Melchior, Jennifer L. Marshall, A. Carnero Rosell, K. Honscheid, UAM. Departamento de Física Teórica, National Science Foundation (US), Science and Technology Facilities Council (UK), Department of Energy (US), German Research Foundation, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, 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: Point spread function, Software_OPERATINGSYSTEMS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ComputingMethodologies_SIMULATIONANDMODELING, Monte Carlo method, FOS: Physical sciences, Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Cosmology, Parameter Contraints, cosmic rays, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, Experiments in gravity, Weak, 010306 general physics, Weak gravitational lensing, STFC, Gravitational Lensing, Physics, COSMIC cancer database, Code, 010308 nuclear & particles physics, Power Spectra, Física, Spectral density, RCUK, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Galaxies, Dark Energy, Accurate Halo-Model, Redshift, Computational physics, Vlt Deep Survey, 13. Climate action, Dark energy, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: et al., Weak lensing by large-scale structure is a powerful probe of cosmology and of the dark universe. This cosmic shear technique relies on the accurate measurement of the shapes and redshifts of background galaxies and requires precise control of systematic errors. Monte Carlo control loops (MCCL) is a forward modeling method designed to tackle this problem. It relies on the ultra fast image generator (UFig) to produce simulated images tuned to match the target data statistically, followed by calibrations and tolerance loops. We present the first end-to-end application of this method, on the Dark Energy Survey (DES) Year 1 wide field imaging data. We simultaneously measure the shear power spectrum Cℓ and the redshift distribution n(z) of the background galaxy sample. The method includes maps of the systematic sources, point spread function (PSF), an approximate Bayesian computation (ABC) inference of the simulation model parameters, a shear calibration scheme, and a fast method to estimate the covariance matrix. We find a close statistical agreement between the simulations and the DES Y1 data using an array of diagnostics. In a nontomographic setting, we derive a set of Cℓ and n(z) curves that encode the cosmic shear measurement, as well as the systematic uncertainty. Following a blinding scheme, we measure the combination of Ωm, σ8, and intrinsic alignment amplitude AIA, defined as S8DIA=σ8(Ωm/0.3)0.5DIA, where DIA=1−0.11(AIA−1). We find S8DIA=0.895+0.054−0.039, where systematics are at the level of roughly 60% of the statistical errors. We discuss these results in the context of earlier cosmic shear analyses of the DES Y1 data. Our findings indicate that this method and its fast runtime offer good prospects for cosmic shear measurements with future wide-field surveys., 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 a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio 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 Energeticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DESBrazil 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 Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the LudwigMaximilians 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 Inter-American 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 Grants No, AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-66861, No. FPA2015-68048, No. SEV-2016-0588, No. SEV2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. 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 No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant No. 465376/2014-2).
Published: 2020

38. Detection of Cross-Correlation between Gravitational Lensing and γ Rays

Author: Michael Troxel, Shin'ichiro Ando, Matt J. Jarvis, E. Bertin, Tesla E. Jeltema, Yanxi Zhang, I. Sevilla-Noarbe, Tim Eifler, A. Choi, N. Kuropatkin, K. Honscheid, F. J. Castander, Shantanu Desai, Nicolao Fornengo, Simone Ammazzalorso, M. Gatti, L. N. da Costa, M. A. G. Maia, Marcelle Soares-Santos, Enrique Gaztanaga, Ramon Miquel, Stefano Camera, Peter Melchior, Y. Omori, M. Smith, S. Samuroff, E. J. Sanchez, Carlos Solans Sanchez, Marco Regis, G. Gutierrez, Steve Kent, A. A. Plazas, Felipe Menanteau, Pablo Fosalba, Erin Sheldon, Antonella Palmese, D. H. Brooks, Keith Bechtol, D. L. Burke, M. E. C. Swanson, Tenglin Li, J. Carretero, Sarah Bridle, B. Flaugher, Gregory Tarle, Santiago Avila, Eli S. Rykoff, Daniel Thomas, D. W. Gerdes, Peter Doel, Robert A. Gruendl, V. Scarpine, H. T. Diehl, Joe Zuntz, Niall MacCrann, M. Carrasco Kind, A. Carnero Rosell, A. K. Romer, M. Costanzi, Vinu Vikram, Santiago Serrano, R. L. C. Ogando, J. P. Dietrich, Juan Garcia-Bellido, David Goldstein, J. Annis, Jennifer L. Marshall, Ofer Lahav, E. Suchyta, David James, J. De Vicente, Flavia Sobreira, Marcos Lima, A. Roodman, Tommaso Giannantonio, D. Gruen, D. L. Hollowood, S. Everett, 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, GRAPPA (ITFA, IoP, FNWI), Ammazzalorso, S., Gruen, D., Regis, M., Camera, S., Ando, S., Fornengo, N., Bechtol, K., Bridle, S. L., Choi, A., Eifler, T. F., Gatti, M., Maccrann, N., Omori, Y., Samuroff, S., Sheldon, E., Troxel, M. A., Zuntz, J., Carrasco Kind, M., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Everett, S., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kent, S., Kuropatkin, N., Lahav, O., T. S., Li, Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, C., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vikram, V., Zhang, Y., Ministerio de Economía y Competitividad (España), European Commission, European Research Council, and UAM. Departamento de Física Teórica
Subjects: Small Scale Effects, Software_OPERATINGSYSTEMS, Gamma-Ray Energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ComputingMethodologies_SIMULATIONANDMODELING, Astrophysical Sources, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, General Physics and Astronomy, FOS: Physical sciences, Data_CODINGANDINFORMATIONTHEORY, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitation and Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 01 natural sciences, Gamma Ray Sources, law.invention, Gravitation, Telescope, law, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, Astrophysics - Cosmology and Nongalactic Astrophysic, Large Area Telescopes, 010306 general physics, Blazar, Cross Correlations, STFC, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, astro-ph.HE, Gravitational Lensing, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.CO, RCUK, Física, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Gravitational lens, Dark energy, Weak Gravitational Lensing, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract: DES Collaboration: et al., In recent years, many γ-ray sources have been identified, yet the unresolved component hosts valuable information on the faintest emission. In order to extract it, a cross-correlation with gravitational tracers of matter in the Universe has been shown to be a promising tool. We report here the first identification of a cross-correlation signal between γ rays and the distribution of mass in the Universe probed by weak gravitational lensing. We use data from the Dark Energy Survey Y1 weak lensing data and the Fermi Large Area Telescope 9-yr γ-ray data, obtaining a signal-to-noise ratio of 5.3. The signal is mostly localized at small angular scales and high γ-ray energies, with a hint of correlation at extended separation. Blazar emission is likely the origin of the small-scale effect. We investigate implications of the large-scale component in terms of astrophysical sources and particle dark matter emission., The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-66861, No. FPA2015-68048, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. 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 Grants No. 240672, No. 291329, and No. 306478.
Published: 2020

39. Perturbation theory for modeling galaxy bias: Validation with simulations of the Dark Energy Survey

Author: Ramon Miquel, Elisabeth Krause, Martin Crocce, I. Ferrero, A. Roodman, M. E. C. Swanson, J. DeRose, E. Suchyta, D. L. Burke, S. Serrano, Niall MacCrann, J. Annis, Jochen Weller, Felipe Menanteau, Bhuvnesh Jain, Xiao Fang, M. Costanzi, A. Carnero Rosell, Jack Elvin-Poole, G. Tarle, Jennifer L. Marshall, S. Allam, Robert A. Gruendl, Josh Frieman, M. Carrasco Kind, K. Honscheid, Juan Garcia-Bellido, Michael Schubnell, F. Paz-Chinchón, S. Pandey, Oliver Friedrich, J. Gschwend, A. A. Plazas, J. Carretero, M. Smith, Antonella Palmese, Michel Aguena, Daniel Gruen, Gary Bernstein, M. A. G. Maia, Pablo Fosalba, V. Scarpine, S. Everett, David J. Brooks, E. J. Sanchez, Shantanu Desai, Jonathan Blazek, G. Gutierrez, Santiago Avila, J. De Vicente, I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, Kyler Kuehn, L. N. da Costa, Pandey, S., Krause, E., Jain, B., Maccrann, N., Blazek, J., Crocce, M., Derose, J., Fang, X., Ferrero, I., Friedrich, O., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Elvin-Poole, J., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, growth, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, estimators, 01 natural sciences, Measure (mathematics), evolution, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, Statistical physics, Perturbation theory, 010306 general physics, Astrophysics::Galaxy Astrophysics, Physics, survey cosmological implications, 010308 nuclear & particles physics, Matter power spectrum, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, halo occupation distribution, Galaxy, Nonlinear system, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Configuration space, constraints
Abstract: We describe perturbation theory (PT) models of galaxy bias for applications to photometric galaxy surveys. We model the galaxy-galaxy and galaxy-matter correlation functions in configuration space and validate against measurements from mock catalogs designed for the Dark Energy Survey (DES). We find that an effective PT model with five galaxy bias parameters provides a good description of the 3D correlation functions above scales of 4 Mpc/$h$ and $z < 1$. Our tests show that at the projected precision of the DES-Year 3 analysis, two of the non-linear bias parameters can be fixed to their co-evolution values, and a third (the $k^2$ term for higher derivative bias) set to zero. The agreement is typically at the 2 percent level over scales of interest, which is the statistical uncertainty of our simulation measurements. To achieve this level of agreement, our {\it fiducial} model requires using the full non-linear matter power spectrum (rather than the 1-loop PT one). We also measure the relationship between the non-linear and linear bias parameters and compare them to their expected co-evolution values. We use these tests to motivate the galaxy bias model and scale cuts for the cosmological analysis of the Dark Energy Survey; our conclusions are generally applicable to all photometric surveys., 19 pages, 14 figures, 1 table
Published: 2020

40. Euclid preparation

Author: Stein Vidar Hagfors Haugan, S. Paltani, S. de la Torre, W. A. Holmes, Javier Graciá-Carpio, Ghassem Gozaliasl, Remi A. Cabanac, S. Niemi, Ibrahim Almosallam, S. Galeotta, X. Dupac, Natalia Auricchio, Lauro Moscardini, Carlo Giocoli, Giuseppe Longo, Valeria Pettorino, Carmelita Carbone, E. Zucca, Luigi Guzzo, C. Bodendorf, Enzo Branchini, A. Secroun, N. Martinet, H. Degaudenzi, M. Kilbinger, F. Raison, M. Kuemmel, Roberto P. Saglia, Stefano Cavuoti, Audrey Galametz, B. Gillis, Fabio Finelli, N. Mauri, Massimo Meneghetti, S. Kermiche, M. H. Fabricius, Ismael Tereno, D. Stern, Frank Grupp, P. B. Lilje, Pablo Fosalba, V. Scottez, Andy Taylor, A. Cappi, W. G. Hartley, Giulio Fabbian, E. Keihänen, V. Capobianco, C. C. Kirkpatrick, L. Patrizii, Martin Kunz, Doug Potter, Andrea Tramacere, P. Tallada Crespí, M. Poncet, A. Alvarez-Ayllon, Sandrine Pires, Andrea Biviano, S. Serrano, C. Colodro-Conde, Chiara Sirignano, Joshua S. Speagle, K. Markovic, Yu Wang, Marco Castellano, Andrea Zacchei, Gianluca Castignani, G. Congedo, Emiliano Merlin, G. Desprez, G. Zamorani, F. Sureau, Sebastiano Ligori, Domenico Sapone, I. Lloro, A. Renzi, S. Bardelli, O. Ilbert, Stefano Andreon, A. Da Silva, M. Tenti, Michele Moresco, V. Amaro, Davide Maino, R. Saha, Felix Hormuth, A. Ealet, P. W. Hatfield, Ole Marggraf, G. Polenta, A. Balaguera-Antolinez, S. Farrens, M. Frailis, Carlo Baccigalupi, R. Benton Metcalf, Simona Mei, Sotiria Fotopoulou, Andrew Humphrey, Mark Brodwin, Federico Marulli, M. Fumana, E. Medinaceli, Rafael Toledo-Moreo, Ralf Bender, Pedro G. Ferreira, Emanuel Rossetti, Jarle Brinchmann, G. Meylan, Hannu Kurki-Suonio, C. Padilla, Leonardo Corcione, M. Hailey, Jason Rhodes, Jean-Gabriel Cuby, N. Welikala, L. Conversi, J. De Vicente-Albendea, Thomas D. Kitching, Peter Schneider, Andrea Cimatti, Luca Valenziano, Hélène M. Courtois, Matt J. Jarvis, D. Tavagnacco, Julien Zoubian, T. Vassallo, N. Fourmanoit, S. Pilo, Joseph J. Mohr, Enrico Bozzo, F. Dubath, F. J. Castander, D. Bonino, Marian Douspis, Carlo Burigana, L. Stanco, Elisabetta Maiorano, E. Munari, C. S. Carvalho, G. Sirri, L. Whittaker, Stefano Camera, Matteo Viel, L. Popa, R. Cledassou, Matteo Maturi, Ricard Casas, Fabio Pasian, Jussi-Pekka Väliviita, Jean Coupon, Marco Baldi, F. Torradeflot, Y. Copin, Massimo Brescia, D. Di Ferdinando, C. A. J. Duncan, Mara Salvato, C. J. Conselice, B. Garilli, Clotilde Laigle, B. Kubik, S. Maurogordato, Richard Massey, Knud Jahnke, M. M. Rau, Giuseppe Riccio, S. Casas, R. Kohley, Lucia Pozzetti, W. Gillard, J. Carretero, E. Franceschi, Swiss National Science Foundation, German Research Foundation, Agenzia Nazionale di Valutazione del Sistema Universitario e della Ricerca, European Commission, Academy of Finland, Agenzia Spaziale Italiana, Belgian Science Policy Office, Canadian Euclid Consortium, Centre National D'Etudes Spatiales (France), German Centre for Air and Space Travel, Danish Space Research Institute, Fundação para a Ciência e a Tecnologia (Portugal), Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), Netherlands Research School for Astronomy, Norwegian Space Agency, Romanian Space Agency, State Secretariat for Education, Research and Innovation (Switzerland), UK Space Agency, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etudes et Recherche en Mathématiques Appliquées (LERMA), Ecole Mohammadia d'Ingénieurs (EMI), EUCLID Collaboration, Department of Physics, Helsinki Institute of Physics, ITA, USA, GBR, FRA, DEU, ESP, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Desprez, G., Paltani, S., Coupon, J., Almosallam, I., Alvarez-Ayllon, A., Amaro, V., Brescia, M., Brodwin, M., Cavuoti, S., De Vicente-Albendea, J., Fotopoulou, S., Hatfield, P. W., Hartley, W. G., Ilbert, O., Jarvis, M. J., Longo, G., Rau, M. M., Saha, R., Speagle, J. S., Tramacere, A., Castellano, M., Dubath, F., Galametz, A., Kuemmel, M., Laigle, C., Merlin, E., Mohr, J. J., Pilo, S., Salvato, M., Andreon, S., Auricchio, N., Baccigalupi, C., Balaguera-Antolinez, A., Baldi, M., Bardelli, S., Bender, R., Biviano, A., Bodendorf, C., Bonino, D., Bozzo, E., Branchini, E., Brinchmann, J., Burigana, C., Cabanac, R., Camera, S., Capobianco, V., Cappi, A., Carbone, C., Carretero, J., Carvalho, C. S., Casas, R., Casas, S., Castander, F. J., Castignani, G., Cimatti, A., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Courtois, H. M., Cuby, J. -G., Da Silva, A., De La Torre, S., Degaudenzi, H., DI Ferdinando, D., Douspis, M., Duncan, C. A. J., Dupac, X., Ealet, A., Fabbian, G., Fabricius, M., Farrens, S., Ferreira, P. G., Finelli, F., Fosalba, P., Fourmanoit, N., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gozaliasl, G., Gracia-Carpio, J., Grupp, F., Guzzo, L., Hailey, M., Haugan, S. V. H., Holmes, W., Hormuth, F., Humphrey, A., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kitching, T. D., Kohley, R., Kubik, B., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maino, D., Maiorano, E., Marggraf, O., Markovic, K., Martinet, N., Marulli, F., Massey, R., Maturi, M., Mauri, N., Maurogordato, S., Medinaceli, E., Mei, S., Meneghetti, M., Benton Metcalf, R., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S., Padilla, C., Pasian, F., Patrizii, L., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Potter, D., Pozzetti, L., Raison, F., Renzi, A., Rhodes, J., Riccio, G., Rossetti, E., Saglia, R., Sapone, D., Schneider, P., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Stern, D., Sureau, F., Tallada Crespi, P., Tavagnacco, D., Taylor, A. N., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valenziano, L., Valiviita, J., Vassallo, T., Viel, M., Wang, Y., Welikala, N., Whittaker, L., Zacchei, A., Zamorani, G., Zoubian, J., Zucca, E., Desprez G., Paltani S., Coupon J., Almosallam I., Alvarez-Ayllon A., Amaro V., Brescia M., Brodwin M., Cavuoti S., De Vicente-Albendea J., Fotopoulou S., Hatfield P.W., Hartley W.G., Ilbert O., Jarvis M.J., Longo G., Rau M.M., Saha R., Speagle J.S., Tramacere A., Castellano M., Dubath F., Galametz A., Kuemmel M., Laigle C., Merlin E., Mohr J.J., Pilo S., Salvato M., Andreon S., Auricchio N., Baccigalupi C., Balaguera-Antolinez A., Baldi M., Bardelli S., Bender R., Biviano A., Bodendorf C., Bonino D., Bozzo E., Branchini E., Brinchmann J., Burigana C., Cabanac R., Camera S., Capobianco V., Cappi A., Carbone C., Carretero J., Carvalho C.S., Casas R., Casas S., Castander F.J., Castignani G., Cimatti A., Cledassou R., Colodro-Conde C., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Courtois H.M., Cuby J.-G., Da Silva A., De La Torre S., Degaudenzi H., DI Ferdinando D., Douspis M., Duncan C.A.J., Dupac X., Ealet A., Fabbian G., Fabricius M., Farrens S., Ferreira P.G., Finelli F., Fosalba P., Fourmanoit N., Frailis M., Franceschi E., Fumana M., Galeotta S., Garilli B., Gillard W., Gillis B., Giocoli C., Gozaliasl G., Gracia-Carpio J., Grupp F., Guzzo L., Hailey M., Haugan S.V.H., Holmes W., Hormuth F., Humphrey A., Jahnke K., Keihanen E., Kermiche S., Kilbinger M., Kirkpatrick C.C., Kitching T.D., Kohley R., Kubik B., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maino D., Maiorano E., Marggraf O., Markovic K., Martinet N., Marulli F., Massey R., Maturi M., Mauri N., Maurogordato S., Medinaceli E., Mei S., Meneghetti M., Benton Metcalf R., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S., Padilla C., Pasian F., Patrizii L., Pettorino V., Pires S., Polenta G., Poncet M., Popa L., Potter D., Pozzetti L., Raison F., Renzi A., Rhodes J., Riccio G., Rossetti E., Saglia R., Sapone D., Schneider P., Scottez V., Secroun A., Serrano S., Sirignano C., Sirri G., Stanco L., Stern D., Sureau F., Tallada Crespi P., Tavagnacco D., Taylor A.N., Tenti M., Tereno I., Toledo-Moreo R., Torradeflot F., Valenziano L., Valiviita J., Vassallo T., Viel M., Wang Y., Welikala N., Whittaker L., Zacchei A., Zamorani G., Zoubian J., and Zucca E.
Subjects: PREDICTION, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics, Surveys, 01 natural sciences, TELESCOPE ADVANCED CAMERA, Cosmology, galaxies, Galaxies: distances and redshift, PROBABILITY DENSITY-ESTIMATION, Survey, 010303 astronomy & astrophysics, Photometric redshift, COSMOS, Physics, Ground truth, distances and redshift [Galaxies], distances and redshifts -surveys -techniques, Outlier, astro-ph.CO, Probability distribution, Catalog, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Algorithm, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, miscellaneous [Techniques], Catalogs, Galaxies: distances and redshifts, Techniques: miscellaneous, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometry (optics), Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, distances and redshifts [Galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, 115 Astronomy, Space science, Catalogues, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, EVOLUTION, miscellaneous -catalogs, MACHINE, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), EMISSION
Abstract: Forthcoming large photometric surveys for cosmology require precise and accurate photometric redshift (photo-z) measurements for the success of their main science objectives. However, to date, no method has been able to produce photo-zs at the required accuracy using only the broad-band photometry that those surveys will provide. An assessment of the strengths and weaknesses of current methods is a crucial step in the eventual development of an approach to meet this challenge. We report on the performance of 13 photometric redshift code single value redshift estimates and redshift probability distributions (PDZs) on a common set of data, focusing particularly on the 0.2pdbl-pdbl2.6 redshift range that the Euclid mission will probe. We designed a challenge using emulated Euclid data drawn from three photometric surveys of the COSMOS field. The data was divided into two samples: one calibration sample for which photometry and redshifts were provided to the participants; and the validation sample, containing only the photometry to ensure a blinded test of the methods. Participants were invited to provide a redshift single value estimate and a PDZ for each source in the validation sample, along with a rejection flag that indicates the sources they consider unfit for use in cosmological analyses. The performance of each method was assessed through a set of informative metrics, using cross-matched spectroscopic and highly-accurate photometric redshifts as the ground truth. We show that the rejection criteria set by participants are efficient in removing strong outliers, that is to say sources for which the photo-z deviates by more than 0.15(1pdbl+pdblz) from the spectroscopic-redshift (spec-z). We also show that, while all methods are able to provide reliable single value estimates, several machine-learning methods do not manage to produce useful PDZs. We find that no machine-learning method provides good results in the regions of galaxy color-space that are sparsely populated by spectroscopic-redshifts, for example zpdbl> pdbl1. However they generally perform better than template-fitting methods at low redshift (zpdbl< pdbl0.7), indicating that template-fitting methods do not use all of the information contained in the photometry. We introduce metrics that quantify both photo-z precision and completeness of the samples (post-rejection), since both contribute to the final figure of merit of the science goals of the survey (e.g., cosmic shear from Euclid). Template-fitting methods provide the best results in these metrics, but we show that a combination of template-fitting results and machine-learning results with rejection criteria can outperform any individual method. On this basis, we argue that further work in identifying how to best select between machine-learning and template-fitting approaches for each individual galaxy should be pursued as a priority., GD and AG acknowledge the support from the Sinergia program of the Swiss National Science Foundation. Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2–1. MB acknowledges the financial contribution from the agreement ASI/INAF 2018-23-HH.0, Euclid ESA mission – Phase D and the INAF PRIN-SKA 2017 program 1.05.01.88.04. SC acknowledges the financial contribution from FFABR 2017. The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the Centre National d’Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Romanian Space Agency, the State Secretariat for Education, Research and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid website (http://www.euclid-ec.org).
Published: 2020

41. Dark Energy Survey Year 3 Results: Covariance Modelling and its Impact on Parameter Estimation and Quality of Fit

Author: R. Buchs, Jochen Weller, Samuel Hinton, G. Tarle, Marco Raveri, G. Gutierrez, Ian Harrison, A. Troja, J. Prat, Alexandra Amon, Y. Omori, H. Camacho, Brian Yanny, V. Scarpine, J. McCullough, Josh Frieman, M. Smith, M. Costanzi, Bhuvnesh Jain, I. Sevilla-Noarbe, Keith Bechtol, Daniel Gruen, David J. Brooks, M. Soares-Santos, Sunayana Bhargava, Ramon Miquel, Rogerio Rosenfeld, D. L. Hollowood, S. Serrano, Felipe Menanteau, Carlos Solans Sanchez, T. N. Varga, N. Weaverdyck, L. N. da Costa, M. Gatti, Ofer Lahav, Xiao Fang, A. Campos, J. DeRose, E. Suchyta, August E. Evrard, I. Ferrero, Matt J. Jarvis, J. Myles, David J. James, D. W. Gerdes, A. Roodman, Tommaso Giannantonio, Elisabeth Krause, Pablo Fosalba, Alex Drlica-Wagner, Tim Eifler, H. T. Diehl, Robert Morgan, Javier Sanchez, Dragan Huterer, Eli S. Rykoff, Marcos Lima, J. Carretero, J. Cordero, Erin Sheldon, C. Doux, Chun-Hao To, V. Terra, E. J. Sanchez, S. Samuroff, David Bacon, F. Paz-Chinchón, Martin Crocce, O. Alves, A. Carnero Rosell, R. D. Wilkinson, Michael Troxel, L. F. Secco, S. Pandey, J. Muir, A. Choi, K. Honscheid, Jack Elvin-Poole, Kyler Kuehn, A. Alarcon, Niall MacCrann, A. A. Plazas, G. Giannini, C. Davis, S. Everett, Scott Dodelson, Santiago Avila, Chihway Chang, S. Desai, J. Gschwend, Antonella Palmese, Gary Bernstein, Maria E. S. Pereira, M. A. G. Maia, M. Rodriguez-Monroy, A. Porredon, E. Baxter, E. Bertin, W. G. Hartley, Juan Garcia-Bellido, Oliver Friedrich, M. Carrasco Kind, F. Andrade-Oliveira, Enrique Gaztanaga, R. Cawthon, Daniel Thomas, F. Elsner, J. De Vicente, Michel Aguena, D. L. Burke, Robert A. Gruendl, 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, 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), University of Cambridge, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de e-Astronomia - LIneA, University of Michigan, Fermi National Accelerator Laboratory, University of Arizona, California Institute of Technology, University of Chicago, Stanford University, University of Hawaii, Ohio State University, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, Medioambientales y Tecnológicas (CIEMAT), University of Portsmouth, University of Sussex, Princeton University, University of Southampton, Oak Ridge National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, Friedrich, O., Andrade-Oliveira, F., Camacho, H., Alves, O., Rosenfeld, R., Sanchez, J., Fang, X., Eifler, T. F., Krause, E., Chang, C., Omori, Y., Amon, A., Baxter, E., Elvin-Poole, J., Huterer, D., Porredon, A., Prat, J., Terra, V., Troja, A., Alarcon, A., Bechtol, K., Bernstein, G. M., Buchs, R., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Choi, A., Cordero, J., Crocce, M., Davis, C., Derose, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Elsner, F., Everett, S., Fosalba, P., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Jain, B., Jarvis, M., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Pandey, S., Raveri, M., Roodman, A., Rodriguez-Monroy, M., Rykoff, E. S., Samuroff, S., Sánchez, C., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Troxel, M. A., Weaverdyck, N., Yanny, B., Aguena, M., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Evrard, A. E., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Soares-Santos, M., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gaussian, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, symbols.namesake, 0103 physical sciences, Applied mathematics, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Equation of state (cosmology), Estimation theory, Covariance matrix, Astronomy and Astrophysics, Covariance, cosmology: observations, large-scale structure of Universe, observations [cosmology], Weighting, Space and Planetary Science, symbols, Dark energy, Trispectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology]
Abstract: Friedrich, O., et al. DES Collaboration, We describe and test the fiducial covariance matrix model for the combined two-point function analysis of the Dark Energy Survey Year 3 (DES-Y3) data set. Using a variety of new ansatzes for covariance modelling and testing, we validate the assumptions and approximations of this model. These include the assumption of Gaussian likelihood, the trispectrum contribution to the covariance, the impact of evaluating the model at a wrong set of parameters, the impact of masking and survey geometry, deviations from Poissonian shot noise, galaxy weighting schemes, and other sub-dominant effects. We find that our covariance model is robust and that its approximations have little impact on goodness of fit and parameter estimation. The largest impact on best-fitting figure-of-merit arises from the so-called fsky approximation for dealing with finite survey area, which on average increases the χ2 between maximum posterior model and measurement by 3.7 per cent (Δχ2 ≈ 18.9). Standard methods to go beyond this approximation fail for DES-Y3, but we derive an approximate scheme to deal with these features. For parameter estimation, our ignorance of the exact parameters at which to evaluate our covariance model causes the dominant effect. We find that it increases the scatter of maximum posterior values for Ωm and σ8 by about 3 per cent and for the dark energy equation-of-state parameter by about 5 per cent⁠., 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 MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, 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 Ciência e Tecnologia (INCT) e-Universe (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: 2020
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42. Identifying RR Lyrae Variable Stars in Six Years of the Dark Energy Survey

Author: H. T. Diehl, A. R. Walker, David Bacon, A. Roodman, M. Smith, Samuel Hinton, G. Gutierrez, Daniel Gruen, David J. James, Tenglin Li, Michael Schubnell, J. De Vicente, G. Tarle, J. Gschwend, D. L. Hollowood, Maria E. S. Pereira, S. Serrano, Michel Aguena, R. L. C. Ogando, D. W. Gerdes, Jennifer L. Marshall, A. Carnero Rosell, D. L. Burke, S. Desai, M. Costanzi, David J. Brooks, I. Ferrero, P. S. Ferguson, Yanxi Zhang, S. Allam, Robert A. Gruendl, Daniel Thomas, Eric H. Neilsen, Lucas M. Macri, Antonella Palmese, Martin Crocce, W. C. Wester, T. M. C. Abbott, R. D. Wilkinson, Alex Drlica-Wagner, C. E. Martínez-Vázquez, M. A. G. Maia, Juan Garcia-Bellido, E. Bertin, Chun-Hao To, Robert Morgan, F. Paz-Chinchón, Keith Bechtol, Felipe Menanteau, E. J. Sanchez, K. M. Stringer, E. Suchyta, Ben Hoyle, A. K. Vivas, Kyler Kuehn, Ramon Miquel, K. Honscheid, A. A. Plazas, I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, T. N. Varga, L. N. da Costa, K. Tavangar, J. Carretero, Enrique Gaztanaga, Andrew B. Pace, M. Carrasco Kind, Peter Doel, 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), DES, Stringer, K. M., Drlica-Wagner, A., Macri, L., Martínez-Vázquez, C. E., Vivas, A. K., Ferguson, P., Pace, A. B., Walker, A. R., Neilsen, E., Tavangar, K., Wester, W., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Ferrero, I., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., T. S., Li, Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., Zhang, Y., the DES Collaboration, National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), and Australian Research Council
Subjects: Proper motion, Milky Way stellar halo, 010504 meteorology & atmospheric sciences, RR Lyrae variable stars, Milky Way, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, RR Lyrae variable, 01 natural sciences, Milky Way Galaxy, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Satellite galaxy, Astrophysics::Solar and Stellar Astrophysics, Eridanus, RRab variable star, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Dwarf galaxy, Physics, RRab variable stars, the Milky Way, 1410, 1413, 1060, 1054, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics, Física, Astronomy and Astrophysics, RR Lyrae variable star, Stars, Space and Planetary Science, Globular cluster, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Stringer, K. M., et al. (DES Collaboration), We present a search for RR Lyrae stars using the full six-year data set from the Dark Energy Survey covering ∼5000 deg2 of the southern sky. Using a multistage multivariate classification and light-curve template-fitting scheme, we identify RR Lyrae candidates with a median of 35 observations per candidate. We detect 6971 RR Lyrae candidates out to ∼335 kpc, and we estimate that our sample is >70% complete at ∼150 kpc. We find excellent agreement with other wide-area RR Lyrae catalogs and RR Lyrae studies targeting the Magellanic Clouds and other Milky Way satellite galaxies. We fit the smooth stellar halo density profile using a broken-power-law model with fixed halo flattening (q = 0.7), and we find strong evidence for a break at = - R 32.1+ kpc 0 0.9 1.1 with an inner slope of = - - n 2.54+ 1 0.09 0.09 and an outer slope of = - - n 5.42+ 2 0.14 0.13. We use our catalog to perform a search for Milky Way satellite galaxies with large sizes and low luminosities. Using a set of simulated satellite galaxies, we find that our RR Lyrae-based search is more sensitive than those using resolved stellar populations in the regime of large (rh 500 pc), low-surface-brightness dwarf galaxies. A blind search for large, diffuse satellites yields three candidate substructures. The first can be confidently associated with the dwarf galaxy Eridanus II. The second has a distance and proper motion similar to the ultrafaint dwarf galaxy Tucana II but is separated by ∼5 deg. The third is close in projection to the globular cluster NGC 1851 but is ∼10 kpc more distant and appears to differ in proper motion., 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).
Published: 2020
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43. Dark Energy Survey Year 1 Results: Wide Field Mass Maps via Forward Fitting in Harmonic Space

Author: B. Flaugher, Peter Doel, Michael Troxel, Ben Hoyle, H. T. Diehl, T. M. C. Abbott, David Bacon, E. J. Sanchez, Erin Sheldon, G. Gutierrez, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, M. E. C. Swanson, Joshua A. Frieman, Peter Melchior, Douglas L. Tucker, Kyler Kuehn, K. Honscheid, Shantanu Desai, Matt J. Jarvis, J. Carretero, V. Scarpine, Jennifer L. Marshall, Sarah Bridle, Chihway Chang, G. Tarle, Stella Seitz, D. L. Hollowood, M. Smith, David J. James, Tesla E. Jeltema, Daniel Gruen, M. A. G. Maia, Alistair R. Walker, W. G. Hartley, Joe Zuntz, S. Serrano, B. Mawdsley, David J. Brooks, Pablo Fosalba, A. Roodman, Vinu Vikram, D. W. Gerdes, J. Annis, Marcos Lima, J. Gschwend, D. L. Burke, A. Carnero Rosell, E. Buckley-Geer, Robert A. Gruendl, A. A. Plazas, E. Suchyta, August E. Evrard, M. Gatti, Ramon Miquel, S. Samuroff, R. C. Smith, Niall Jeffrey, Juan Garcia-Bellido, E. Bertin, Eduardo Rozo, Flavia Sobreira, M. Carrasco Kind, Enrique Gaztanaga, J. De Vicente, 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, Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, and UAM. Departamento de Física Teórica
Subjects: ST/S000550/1, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, gravitational lensing: weak, 0103 physical sciences, Dark matter, media_common.cataloged_instance, Weak, European union, 010303 astronomy & astrophysics, License, Publication, STFC, media_common, Physics, Matter, Harmonic space, 010308 nuclear & particles physics, business.industry, Non-Gaussianity, European research, Física, RCUK, Astronomy and Astrophysics, Galaxies, Des, Wide field, Cosmology, Alliance, Space and Planetary Science, Constraints, astro-ph.CO, large-scale structure of Universe, Resolution, business, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Minkowski Functionals
Abstract: We present new wide-field weak lensing mass maps for the Year 1 Dark Energy Survey (DES) data, generated via a forward fitting approach. This method of producing maps does not impose any prior constraints on the mass distribution to be reconstructed. The technique is found to improve the map reconstruction on the edges of the field compared to the conventional Kaiser–Squires method, which applies a direct inversion on the data; our approach is in good agreement with the previous direct approach in the central regions of the footprint. The mapping technique is assessed and verified with tests on simulations; together with the Kaiser–Squires method, the technique is then applied to data from the DES Year 1 data and the differences between the two methods are compared. We also produce the first DES measurements of the convergence Minkowski functionals and compare them to those measured in simulations., 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 MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, 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 Ciencia e Tecnologia (INCT) e-Universe (CNPq grant ˆ 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. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.
Published: 2020

44. Optical follow-up of gravitational wave triggers with DECam during the first two LIGO/VIRGO observing runs

Author: R. E. Butler, D. L. Burke, F. Paz-Chinchón, Keith Bechtol, Brian Yanny, Ken Herner, William G. Hartley, M. Smith, N. P. Kuropatkin, D. W. Gerdes, Masao Sako, Eric H. Neilsen, I. Sevilla-Noarbe, G. Gutierrez, Alex Drlica-Wagner, Edo Berger, L. N. da Costa, S. Desai, H. S. Chen, Ben Farr, Marcelle Soares-Santos, James Annis, Elisabeth Krause, Huan Lin, M. Carrasco-Kind, G. Tarle, A. A. Plazas, K. Honscheid, Pablo Fosalba, Philip S. Cowperthwaite, M. A. G. Maia, Daniel E. Holz, J. Marriner, Nora Sherman, David James, Alejandro Garcia, V. Scarpine, J. De Vicente, Antonella Palmese, Douglas L. Tucker, Felipe Menanteau, Enrique Gaztanaga, Robert A. Gruendl, E. Suchyta, Tenglin Li, A. Carnero Rosell, Santiago Avila, Ramon Miquel, Peter K. G. Williams, M. Sauseda, William Wester, Kyler Kuehn, D. J. Brout, Ofer Lahav, J. Gschwend, Christopher J. Conselice, E. Buckley-Geer, Devon L. Hollowood, Juan Garcia-Bellido, E. Bertin, M. S. Schubnell, J. L. Marshall, Thomas Matheson, Peter Doel, H. T. Diehl, M. S. S. Gill, S. Everett, Daniel Scolnic, Marco A. P. Lima, Edward R. Cook, Santiago Serrano, Yanxi Zhang, Tim Eifler, Richard Kessler, Flavia Sobreira, D. A. Finley, J. Carretero, Tamara M. Davis, M. March, Sahar S. Allam, Zoheyr Doctor, N. Glaeser, Joshua A. Frieman, R. J. Foley, E. J. Sanchez, 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), DECam, National Science Foundation (US), Department of Energy (US), University of Illinois, Stanford University, New York State Office of Science, Technology and Academic Research, Lawrence Berkeley National Laboratory, University of Pennsylvania, The Ohio State University, University of Chicago, University of Michigan, Texas A&M University, University of Portsmouth, Science and Technology Facilities Council (UK), University College London, European Research Council, University of Nottingham, University of Sussex, German Research Foundation, Ministerio de Economía y Competitividad (España), Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, and Financiadora de Estudos e Projetos (Brasil)
Subjects: cosmological model, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Cosmology, Gravitational waves, General Relativity and Quantum Cosmology, star, 0103 physical sciences, supernova, black hole, optical, Software and its engineering software infrastructure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], LIGO, cosmic string, neutron star, dark energy, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation, Astronomy, imaging, Astronomy and Astrophysics, trigger, Computer Science Applications, Black hole, Neutron star, Supernova, electromagnetic, VIRGO, 13. Climate action, Space and Planetary Science, Grid computing, Dark energy, Astrophysics - Instrumentation and Methods for Astrophysics, signature
Abstract: Gravitational wave (GW) events detectable by LIGO and Virgo have several possible progenitors, including black hole mergers, neutron star mergers, black hole–neutron star mergers, supernovae, and cosmic string cusps. A subset of GW events is expected to produce electromagnetic (EM) emission that, once detected, will provide complementary information about their astrophysical context. To that end, the LIGO–Virgo Collaboration (LVC) sends GW candidate alerts to the astronomical community so that searches for their EM counterparts can be pursued. The DESGW group, consisting of members of the Dark Energy Survey (DES), the LVC, and other members of the astronomical community, uses the Dark Energy Camera (DECam) to perform a search and discovery program for optical signatures of LVC GW events. DESGW aims to use a sample of GW events as standard sirens for cosmology. Due to the short decay timescale of the expected EM counterparts and the need to quickly eliminate survey areas with no counterpart candidates, it is critical to complete the initial analysis of each night's images as quickly as possible. We discuss our search area determination, imaging pipeline, and candidate selection processes. We review results from the DESGW program during the first two LIGO–Virgo observing campaigns and introduce other science applications that our pipeline enables., Funding for the DES Projects has been provided by the DOE and NSF, MEC/MICINN/MINECO (Spain), STFC, HEFCE, NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA (Texas A&M), CNPQ, FAPERJ, FINEP, DFG and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Zürich, Fermilab, University of Illinois, ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU München and the associated Excellence Cluster Universe, University of Michigan, NOAO, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford University, 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, 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 NSF under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-88861, FPA2015-68048, and Centro de Excelencia SEV-2016-0588, SEV-2016-0597 and MDM-2015-0509. Research leading to these results has received funding from the ERC under the EU’s 7th Framework Programme including grants ERC 240672, 291329 and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) , through project number CE110001020. This research uses services or data provided by the NOAO Science Archive. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. 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. The U.S. Government retains and the publisher, by accepting the article for publication, acknowledges that the U.S. Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for U.S. Government purposes.
Published: 2020

45. The Dark Energy Survey Supernova Program: Modelling selection efficiency and observed core collapse supernova contamination

Author: M Vincenzi, M Sullivan, O Graur, D Brout, T M Davis, C Frohmaier, L Galbany, C P Gutiérrez, S R Hinton, R Hounsell, L Kelsey, R Kessler, E Kovacs, S Kuhlmann, J Lasker, C Lidman, A Möller, R C Nichol, M Sako, D Scolnic, M Smith, E Swann, P Wiseman, J Asorey, G F Lewis, R Sharp, B E Tucker, M Aguena, S Allam, S Avila, E Bertin, D Brooks, D L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, F J Castander, A Choi, M Costanzi, L N da Costa, M E S Pereira, J De Vicente, S Desai, H T Diehl, P Doel, S Everett, I Ferrero, P Fosalba, J Frieman, J García-Bellido, E Gaztanaga, D W Gerdes, D Gruen, R A Gruendl, G Gutierrez, D L Hollowood, K Honscheid, B Hoyle, D J James, K Kuehn, N Kuropatkin, M A G Maia, P Martini, F Menanteau, R Miquel, R Morgan, A Palmese, F Paz-Chinchón, A A Plazas, A K Romer, E Sanchez, V Scarpine, S Serrano, I Sevilla-Noarbe, M Soares-Santos, E Suchyta, G Tarle, D Thomas, C To, T N Varga, A R Walker, R D Wilkinson, null (DES Collaboration), Vincenzi, M., Sullivan, M., Graur, O., Brout, D., Davis, T. M., Frohmaier, C., Galbany, L., Gutiérrez, C. P., Hinton, S. R., Hounsell, R., Kelsey, L., Kessler, R., Kovacs, E., Kuhlmann, S., Lasker, J., Lidman, C., Möller, A., Nichol, R. C., Sako, M., Scolnic, D., Smith, M., Swann, E., Wiseman, P., Asorey, J., Lewis, G. F., Sharp, R., Tucker, B. E., Aguena, M., Allam, S., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Martini, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Walker, A. R., Wilkinson, R. D., Des, Collaboration, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Luminosity, surveys, supernovae: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, survey, 010306 general physics, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, Physics, RCUK, Astronomy and Astrophysics, cosmology: observations, Type II supernova, Redshift, Galaxy, observations [cosmology], ST/R000506/1, Supernova, 13. Climate action, Space and Planetary Science, ST/P006760/1, Dark energy, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The analysis of current and future cosmological surveys of Type Ia supernovae (SNe Ia) at high redshift depends on the accurate photometric classification of the SN events detected. Generating realistic simulations of photometric SN surveys constitutes an essential step for training and testing photometric classification algorithms, and for correcting biases introduced by selection effects and contamination arising from core-collapse SNe in the photometric SN Ia samples. We use published SN time-series spectrophotometric templates, rates, luminosity functions, and empirical relationships between SNe and their host galaxies to construct a framework for simulating photometric SN surveys. We present this framework in the context of the Dark Energy Survey (DES) 5-yr photometric SN sample, comparing our simulations of DES with the observed DES transient populations. We demonstrate excellent agreement in many distributions, including Hubble residuals, between our simulations and data. We estimate the core collapse fraction expected in the DES SN sample after selection requirements are applied and before photometric classification. After testing different modelling choices and astrophysical assumptions underlying our simulation, we find that the predicted contamination varies from 7.2 to 11.7 per cent, with an average of 8.8 per cent and an r.m.s. of 1.1 per cent. Our simulations are the first to reproduce the observed photometric SN and host galaxy properties in high-redshift surveys without fine-tuning the input parameters. The simulation methods presented here will be a critical component of the cosmology analysis of the DES photometric SN Ia sample: correcting for biases arising from contamination, and evaluating the associated systematic uncertainty.
Published: 2020
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46. OzDES multi-object fibre spectroscopy for the Dark Energy Survey: Results and second data release

Author: Enrique Gaztanaga, C. Lidman, J. Carretero, Tim Eifler, B. E. Tucker, E. Swann, Tamara M. Davis, Lluís Galbany, Sara Webb, J. Gschwend, S. Allam, Robert A. Gruendl, Samuel Hinton, Eli S. Rykoff, J. K. Hoormann, Krzysztof Bolejko, W. G. Hartley, G. Gutierrez, M. E. C. Swanson, Mark Sullivan, Edward Macaulay, Anais Möller, Paul Martini, Michael Schubnell, A. Carnero Rosell, Douglas L. Tucker, Kyler Kuehn, Ryan J. Foley, R. D. Wilkinson, Peter Doel, I. Sevilla-Noarbe, Daniel Scolnic, Andrew J. King, N. Kuropatkin, N. E. Sommer, Bonnie Zhang, Felipe Menanteau, M. Pursiainen, G. Tarle, Zhefu Yu, A. Kremin, Fang Yuan, V. Scarpine, Anthony Carr, M. Carrasco Kind, Sunayana Bhargava, David Parkinson, T. N. Varga, L. N. da Costa, S. A. Uddin, A. R. Walker, Robert C. Nichol, A. Roodman, M. Childress, Daniela Carollo, M. Costanzi, K. Honscheid, Juan Garcia-Bellido, E. Bertin, D. Lagattuta, Antonella Palmese, Jennifer L. Marshall, J. De Vicente, Joshua A. Frieman, M. A. G. Maia, D. Mudd, W. C. Wester, Fiona H. Panther, U. Malik, M. March, Basilio X. Santiago, Geraint F. Lewis, Peter Melchior, Richard Scalzo, J. Annis, Rob Sharp, M. Sako, D. L. Hollowood, S. Serrano, Richard Kessler, P. Wiseman, S. Everett, David J. Brooks, Marcos Lima, E. Suchyta, A. A. Plazas, F. J. Castander, Jacobo Asorey, T. M. C. Abbott, D. J. Brout, Michel Aguena, Huan Lin, J. Calcino, David J. James, Pablo Fosalba, E. J. Sanchez, Karl Glazebrook, Ramon Miquel, F. Paz-Chinchón, M. Smith, Daniel Gruen, Tenglin Li, Santiago Avila, A. G. Kim, Lidman, C., Tucker, B. E., Davis, T. M., Uddin, S. A., Asorey, J., Bolejko, K., Brout, D., Calcino, J., Carollo, D., Carr, A., Childress, M., Hoormann, J. K., Foley, R. J., Galbany, L., Glazebrook, K., Hinton, S. R., Kessler, R., Kim, A. G., King, A., Kremin, A., Kuehn, K., Lagattuta, D., Lewis, G. F., Macaulay, E., Malik, U., March, M., Martini, P., Moller, A., Mudd, D., Nichol, R. C., Panther, F., Parkinson, D., Pursiainen, M., Sako, M., Swann, E., Scalzo, R., Scolnic, D., Sharp, R., Smith, M., Sommer, N. E., Sullivan, M., Webb, S., Wiseman, P., Yu, Z., Yuan, F., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., Da Costa, L. N., De Vicente, J., Doel, P., Eifler, T. F., Everett, S., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., T. S., Li, Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., 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., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Laboratoire de Physique de Clermont (LPC), 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), 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, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, 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 de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Australian Research Council, and 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)
Subjects: transients: supernovae, Astrophysics, dark energy [cosmology], 01 natural sciences, 7. Clean energy, law.invention, cosmology: dark energy, supermassive black hole [quasars], law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010303 astronomy & astrophysics, catalogues, Physics, quasars: supermassive black holes, Astrophysics::Instrumentation and Methods for Astrophysics, GALÁXIAS, Supernova, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, surveys, techniques: spectroscopic, catalogue, Astrophysics - Cosmology and Nongalactic Astrophysics, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, supermassive black holessurveys [Quasars], 0103 physical sciences, survey, Spectrograph, Astrophysics::Galaxy Astrophysics, STFC, 010308 nuclear & particles physics, supermassive black holes [quasars], RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Photometry (astronomy), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Quasars: supermassive black holessurveys, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], supernovae [transients]
Abstract: We present a description of the Australian Dark Energy Survey (OzDES) and summarize the results from its 6 years of operations. Using the 2dF fibre positioner and AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope, OzDES has monitored 771 active galactic nuclei, classified hundreds of supernovae, and obtained redshifts for thousands of galaxies that hosted a transient within the 10 deep fields of the Dark Energy Survey. We also present the second OzDES data release, containing the redshifts of almost 30 000 sources, some as faint as r = 24 mag, and 375 000 individual spectra. These data, in combination with the time-series photometry from the Dark Energy Survey, will be used to measure the expansion history of the Universe out to z ∼1.2 and the masses of hundreds of black holes out to z ∼4. OzDES is a template for future surveys that combine simultaneous monitoring of targets with wide-field imaging cameras and wide-field multi-object spectrographs., 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, Fi-nanciadora de Estudos e Projetos, Fundac¸ão 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 Forschungsgemein-schaft, and the Collaborating Institutions in the DES. LG was funded by the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement no. 839090. 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 MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, 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 Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). Parts of this research were supported by the Australian Research Council under grants DP160100930, FL180100168, and FT140101270.
Published: 2020

47. First cosmology results using type Ia supernovae from the Dark Energy Survey: the effect of host galaxy properties on supernova luminosity

Author: Geraint F. Lewis, C. Frohmaier, David J. Brooks, Samuel Hinton, G. Gutierrez, Sunayana Bhargava, Jennifer L. Marshall, Brad E. Tucker, Eli S. Rykoff, Michel Aguena, A. R. Walker, Josh Frieman, Mark Sullivan, B. Flaugher, Elisabeth Krause, A. Carnero Rosell, M. Pursiainen, G. Tarle, R. R. Gupta, Tim Eifler, D. L. Burke, David J. James, Lluís Galbany, M. E. C. Swanson, Michael Schubnell, Pablo Fosalba, E. Macaulay, R. C. Thomas, S. Allam, Robert A. Gruendl, M. Carrasco Kind, I. Sevilla-Noarbe, J. De Vicente, Robert C. Nichol, Ramon Miquel, E. Suchyta, C. B. D'Andrea, K. Honscheid, Karl Glazebrook, Douglas L. Tucker, Antonella Palmese, N. Kuropatkin, Kyler Kuehn, M. A. G. Maia, Marcus Lima, P. Wiseman, T. N. Varga, L. N. da Costa, Tamara M. Davis, Juan Garcia-Bellido, Daniela Carollo, Peter Melchior, Peter Nugent, Claudia P. Gutiérrez, Felipe Menanteau, Daniel Scolnic, M. Costanzi, A. Roodman, M. Vincenzi, Enrique Gaztanaga, Ryan J. Foley, V. Scarpine, S. Everett, M. Sako, D. L. Hollowood, S. Serrano, Richard Kessler, A. A. Plazas, L. Kelsey, D. J. Brout, W. G. Hartley, N. E. Sommer, A. K. Romer, Paul Martini, F. Paz-Chinchón, M. Smith, Daniel Gruen, Anais Möller, E. Bertin, Peter Doel, H. T. Diehl, Niall MacCrann, J. Gschwend, C. Lidman, E. Swann, Daniel Thomas, E. Buckley-Geer, Santiago Avila, S. Desai, T. M. C. Abbott, E. J. Sanchez, 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, Smith, M., Sullivan, M., Wiseman, P., Kessler, R., Scolnic, D., Brout, D., D'Andrea, C. B., Davis, T. M., Foley, R. J., Frohmaier, C., Galbany, L., Gupta, R. R., Gutiérrez, C. P., Hinton, S. R., Kelsey, L., Lidman, C., Macaulay, E., Möller, A., Nichol, R. C., Nugent, P., Palmese, A., Pursiainen, M., Sako, M., Swann, E., Thomas, R. C., Tucker, B. E., Vincenzi, M., Carollo, D., Lewis, G. F., Sommer, N. E., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maccrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Walker, A. R., Des, Collaboration, 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), and 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)
Subjects: transients: supernovae, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Cosmology, Luminosity, surveys, supernovae: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, survey, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Equation of state (cosmology), RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Dark energy, Astrophysics::Earth and Planetary Astrophysics, supernovae [transients], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae], observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present improved photometric measurements for the host galaxies of 206 spectroscopically confirmed type Ia supernovae discovered by the Dark Energy Survey Supernova Program (DES-SN) and used in the first DES-SN cosmological analysis. Fitting spectral energy distributions to the $griz$ photometric measurements of the DES-SN host galaxies, we derive stellar masses and star-formation rates. For the DES-SN sample, when considering a 5D ($z$, $x_1$, $c$, $\alpha$, $\beta$) bias correction, we find evidence of a Hubble residual `mass step', where SNe Ia in high mass galaxies ($>10^{10} \textrm{M}_{\odot}$) are intrinsically more luminous (after correction) than their low mass counterparts by $\gamma=0.040\pm0.019$mag. This value is larger by $0.031$mag than the value found in the first DES-SN cosmological analysis. This difference is due to a combination of updated photometric measurements and improved star formation histories and is not from host-galaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with $\gamma=0.066\pm0.020$mag. The 1D-5D $\gamma$ difference for DES-SN is $0.026\pm0.009$mag. We show that this difference is due to a strong correlation between host galaxy stellar mass and the $x_1$ component of the 5D distance-bias correction. To better understand this effect, we include an intrinsic correlation between light-curve width and stellar mass in simulated SN Ia samples. We show that a 5D fit recovers $\gamma$ with $-9$mmag bias compared to a $+2$mmag bias for a 1D fit. This difference can explain part of the discrepancy seen in the data. Improvements in modeling correlations between galaxy properties and SN is necessary to determine the implications for $\gamma$ and ensure unbiased precision estimates of the dark energy equation-of-state as we enter the era of LSST., Comment: 27 pages, 13 figures; Submitted to MNRAS
Published: 2020
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48. A joint SZ-X-ray-optical analysis of the dynamical state of 288 massive galaxy clusters

Author: Matthew B. Bayliss, Eli S. Rykoff, M. Smith, Daniel Gruen, J. Gschwend, A. Roodman, A. Carnero Rosell, D. W. Gerdes, A. Katzenberger, M. E. C. Swanson, V. Scarpine, Sunayana Bhargava, Samuel Hinton, J. Carretero, G. Gutierrez, Matthias Klein, E. Suchyta, Felipe Menanteau, V. Ojeda, August E. Evrard, C. Vergara Cervantes, Marcos Lima, D. L. Burke, Michael Schubnell, Shantanu Desai, Peter Doel, Josh Frieman, A. A. Plazas, M. Carrasco Kind, Alistair R. Walker, Kyler Kuehn, H. T. Diehl, Marcelle Soares-Santos, F. Paz-Chinchón, I. Sevilla-Noarbe, D. Hernandez-Lang, R. Capasso, S. Allam, Robert A. Gruendl, Antonella Palmese, D. L. Hollowood, David J. James, K. Honscheid, R. D. Wilkinson, S. Serrano, Tesla E. Jeltema, M. A. G. Maia, Pablo Fosalba, T. N. Varga, David J. Brooks, W. G. Hartley, L. N. da Costa, R. L. C. Ogando, C. Lidman, J. De Vicente, Michel Aguena, Daniel Thomas, E. Buckley-Geer, Joseph J. Mohr, B. Floyd, Peter Melchior, A. Saro, A. K. Romer, T. F. Eifler, F. J. Castander, V. Strazzullo, Ofer Lahav, E. J. Sanchez, Santiago Avila, Ramon Miquel, M. March, G. Tarle, Alfredo Zenteno, Juan Garcia-Bellido, B. Flaugher, E. Bertin, Mike McDonald, J. R. Gonzalez, M. Costanzi, Zenteno, A., Hernández-Lang, D., Klein, M., Vergara Cervantes, C., Hollowood, D. L., Bhargava, S., Palmese, A., Strazzullo, V., Romer, A. K., Mohr, J. J., Jeltema, T., Saro, A., Lidman, C., Gruen, D., Ojeda, V., Katzenberger, A., Aguena, M., Allam, S., Avila, S., Bayliss, M., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capasso, R., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Floyd, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gonzalez, J. R., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lima, M., Mcdonald, M., Maia, M. A. G., March, M., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wilkinson, R. D., Des, Collaboration, 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: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, galaxies: luminosity function, mass function, galaxies: clusters: general, 01 natural sciences, 0103 physical sciences, Cluster (physics), clusters: general [galaxies], Brightest cluster galaxy, education, 010303 astronomy & astrophysics, Galaxy cluster, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: luminosity function, South Pole Telescope, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), Cluster sampling, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use imaging from the first three years of the Dark Energy Survey to characterize the dynamical state of 288 galaxy clusters at $0.1 \lesssim z \lesssim 0.9$ detected in the South Pole Telescope (SPT) Sunyaev-Zeldovich (SZ) effect survey (SPT-SZ). We examine spatial offsets between the position of the brightest cluster galaxy (BCG) and the center of the gas distribution as traced by the SPT-SZ centroid and by the X-ray centroid/peak position from Chandra and XMM data. We show that the radial distribution of offsets provides no evidence that SPT SZ-selected cluster samples include a higher fraction of mergers than X-ray-selected cluster samples. We use the offsets to classify the dynamical state of the clusters, selecting the 43 most disturbed clusters, with half of those at $z \gtrsim 0.5$, a region seldom explored previously. We find that Schechter function fits to the galaxy population in disturbed clusters and relaxed clusters differ at $z>0.55$ but not at lower redshifts. Disturbed clusters at $z>0.55$ have steeper faint-end slopes and brighter characteristic magnitudes. Within the same redshift range, we find that the BCGs in relaxed clusters tend to be brighter than the BCGs in disturbed samples, while in agreement in the lower redshift bin. Possible explanations includes a higher merger rate, and a more efficient dynamical friction at high redshift. The red-sequence population is less affected by the cluster dynamical state than the general galaxy population., 21 pages, 12 Figures, 4 Tables. Accepted for publication in MNRAS
Published: 2020

49. DES16C3cje: A low-luminosity, long-lived supernova

Author: T. W. Chen, D. L. Burke, M. Della Valle, M. Pursiainen, Lluís Galbany, Mark Sullivan, Mariusz Gromadzki, A. A. Plazas, Nidia Morrell, Cristina Barbarino, Geraint F. Lewis, P. Wiseman, Juna A. Kollmeier, C. R. Angus, A. R. Walker, M. A. G. Maia, H. T. Diehl, Daniela Carollo, C. Frohmaier, Claudia P. Gutiérrez, Josh Frieman, Peter Nugent, Daniel Gruen, Ramon Miquel, P. Doel, R. D. Wilkinson, R. Kokotanekova, Kyler Kuehn, Juan Garcia-Bellido, E. Bertin, Marcos Lima, A. Pastorello, Jesper Sollerman, David J. James, Felipe Menanteau, Gregory Tarle, Pablo Fosalba, I. Sevilla-Noarbe, David Brooks, Michael Schubnell, Kate Maguire, E. Suchyta, Samuel Hinton, J. Gschwend, N. Kuropatkin, G. Gutierrez, Matt Nicholl, T. N. Varga, L. N. da Costa, D. W. Gerdes, T. F. Eifler, J. De Vicente, K. Honscheid, Michel Aguena, Ryan J. Foley, M. R. Magee, J. Carretero, Marcelle Soares-Santos, L. Martinez, Tamara M. Davis, N. E. Sommer, M. Sako, Cosimo Inserra, Mathew Smith, Anais Möller, D. L. Hollowood, M. Carrasco Kind, M. March, S. Serrano, S. Allam, A. Carnero Rosell, Robert A. Gruendl, B. E. Tucker, M. E. C. Swanson, E. Swann, F. Paz-Chinchón, Daniel Thomas, E. Buckley-Geer, Yen-Chen Pan, Erkki Kankare, Eric Morganson, Antonella Palmese, E. J. Sanchez, Santiago González-Gaitán, Morgan Fraser, Santiago Avila, S. Desai, Joseph P. Anderson, M. Costanzi, B. Flaugher, V. Scarpine, Melina C. Bersten, Ofer Lahav, Laboratoire de Physique de Clermont (LPC), 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), 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 (UCA)-Centre National de la Recherche Scientifique (CNRS), Gutierrez, C. P., Sullivan, M., Martinez, L., Bersten, M. C., Inserra, C., Smith, M., Anderson, J. P., Pan, Y. -C., Pastorello, A., Galbany, L., Nugent, P., Angus, C. R., Barbarino, C., Carollo, D., Chen, T. -W., Davis, T. M., Della Valle, M., Foley, R. J., Fraser, M., Frohmaier, C., Gonzalez-Gaitan, S., Gromadzki, M., Kankare, E., Kokotanekova, R., Kollmeier, J., Lewis, G. F., Magee, M. R., Maguire, K., Moller, A., Morrell, N., Nicholl, M., Pursiainen, M., Sollerman, J., Sommer, N. E., Swann, E., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morganson, E., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wilkinson, R., Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, 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 de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, and 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)
Subjects: Absolute magnitude, long-lived, general [Supernovae], Astrophysics, 01 natural sciences, Luminosity, High Energy Physics - Phenomenology (hep-ph), star, model: hydrodynamics, accretion, Astrophysics::Solar and Stellar Astrophysics, Red supergiant, dark energy, FALLBACK, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, PAIR-INSTABILITY, Accretion (meteorology), hep-ph, supernovae: general, supernovae: individual: (DES16C3cje), High Energy Physics - Phenomenology, Supernova, radioactivity, SUPERNOVAS, Astrophysics - High Energy Astrophysical Phenomena, Astronomical and Space Sciences, LATE TIMES, TIDAL DISRUPTION, Astrophysics::High Energy Astrophysical Phenomena, individual: [supernovae], individual: (DES16C3cje) [supernovae], brightness, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, STAR-FORMATION, Affordable and Clean Energy, bolometer, 0103 physical sciences, supernova, PHOTOMETRY, luminosity, numerical calculations, STFC, Astrophysics::Galaxy Astrophysics, LIGHT CURVES, 010308 nuclear & particles physics, velocity: expansion, RCUK, TRANSIENTS, Astronomy and Astrophysics, Light curve, Type II supernova, redshift, EVOLUTION, Redshift, Automatic Keywords, Space and Planetary Science, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], galaxy, SN 2005CS, individual (DES16C3cje) [Supernovae], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present DES16C3cje, a low-luminosity, long-lived type II supernova (SN II) at redshift 0.0618, detected by the Dark Energy Survey (DES). DES16C3cje is a unique SN. The spectra are characterized by extremely narrow photospheric lines corresponding to very low expansion velocities of . 1500 km s−1 , and the light curve shows an initial peak that fades after 50 days before slowly rebrightening over a further 100 days to reach an absolute brightness of M푟 ∼ −15.5 mag. The decline rate of the late-time light curve is then slower than that expected from the powering by radioactive decay of 56Co, but is comparable to that expected from accretion power. Comparing the bolometric light curve with hydrodynamical models, we find that DES16C3cje can be explained by either i) a low explosion energy (0.11 foe) and relatively large 56Ni production of 0.075 M from a ∼ 15 M red supergiant progenitor typical of other SNe II, or ii) a relatively compact ∼ 40 M star, explosion energy of 1 foe, and 0.08 M of 56Ni. Both scenarios require additional energy input to explain the late-time light curve, which is consistent with fallback accretion at a rate of ∼ 0.5 × 10−8 M s−1., EU/FP7-ERC grant 615929, European Union (EU) 839090, Alexander von Humboldt Foundation, Science Foundation Ireland, Polish NCN MAESTRO 2014/14/A/ST9/00121, Royal Astronomical Society Research Fellowship, European Organisation for Astronomical Research in the Southern Hemisphere, Chile 299.D-5040(A) 299.D-5040(B) 0100.D-0461(A) 194.C-0207(I), PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO program 197.D1075 199.D-0143, Programme NOAO GS-2016B-Q-9, United States Department of Energy (DOE), National Science Foundation (NSF), Spanish Government, Science & Technology Facilities Council (STFC), Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Kavli Institute of Cosmological Physics at the University of Chicago, Ohio State University, Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University, Ciencia Tecnologia e Inovacao (FINEP), Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, National Council for Scientific and Technological Development (CNPq), Ministerio da Ciencia, Tecnologia e Inovacao, German Research Foundation (DFG), Collaborating Institutions in the Dark Energy Survey, United States Department of Energy (DOE) University of Chicago, University of California at Santa Cruz, University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Zurich, University of Illinois at Urbana-Champaign, Institut de Ciencies de l'Espai (IEEC/CSIC), Institut de Fisica d'Altes Energies, Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, University of Michigan System, National Science Foundation (NSF) NSF - Directorate for Mathematical & Physical Sciences (MPS), University of Nottingham, University of Pennsylvania, University of Portsmouth, Stanford University United States Department of Energy (DOE), Stanford University, University of Sussex, Texas AM University, OzDES Membership Consortium, German Research Foundation (DFG) HA 1850/28-1, European Union (EU) PGC2018-095317-B-C21, National Science Foundation (NSF) AST-1138766 AST-1536171, MINECO AYA2015-71825 ESP2015-66861 FPA2015-68048 SEV-2016-0588 SEV2016-0597 MDM-2015-0509, ERDF funds from the European Union, CERCA program of the Generalitat de Catalunya, European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013), European Research Council (ERC) 240672 291329 306478, National Council for Scientific and Technological Development (CNPq) 465376/2014-2, National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility DE-AC02-05CH11231, United States Department of Energy (DOE) DE-AC02-07CH11359
Published: 2020

50. Dark energy survey year 1 results: Cosmological constraints from cluster abundances and weak lensing

Author: Alex Drlica-Wagner, Dragan Huterer, J. Annis, I. Sevilla-Noarbe, Daniel Scolnic, N. Kuropatkin, Tesla E. Jeltema, F. Paz-Chinchón, K. D. Eckert, T. N. Varga, Brian Nord, Adam Mantz, L. N. da Costa, M. Costanzi, M. A. G. Maia, Michel Aguena, E. Suchyta, August E. Evrard, Brian Yanny, Shantanu Desai, A. Alarcon, M. W. G. Johnson, A. K. Romer, J. Carretero, Paul Martini, V. Scarpine, I. Ferrero, Matt J. Jarvis, Tamara M. Davis, Yanxi Zhang, Tim Eifler, Arya Farahi, David James, Z. Zhang, D. W. Gerdes, Joshua A. Frieman, D. Gruen, R. Cawthon, Antonella Palmese, Pablo Fosalba, Carlos Solans Sanchez, D. H. Brooks, A. R. Walker, B. Flaugher, Risa H. Wechsler, P. Rooney, Keith Bechtol, M. Sako, C. Lidman, A. von der Linden, Erin Sheldon, D. L. Hollowood, M. E. C. Swanson, Huan Lin, Sebastian Bocquet, Julian A. Mayers, Steve Kent, J. De Vicente, Martin Crocce, R. D. Wilkinson, D. L. Burke, Daniel Thomas, E. Buckley-Geer, M. Carrasco Kind, S. Everett, Robert C. Nichol, S. Allam, Robert A. Gruendl, R. L. C. Ogando, J. P. Dietrich, Juan Garcia-Bellido, E. Bertin, Marcos Lima, Michael Troxel, Eduardo Rozo, Jack Elvin-Poole, Enrique Gaztanaga, Peter Doel, Peter Melchior, Ofer Lahav, M. Smith, H. T. Diehl, Douglas L. Tucker, Kyler Kuehn, J. Allyn Smith, Paul Giles, David Bacon, Niall MacCrann, Ami Choi, Ben Hoyle, A. Roodman, Markus Rau, Tommaso Giannantonio, J. Gschwend, Gary Bernstein, Hao-Yi Wu, Tenglin Li, Scott Dodelson, S. W. Allen, Santiago Avila, Chihway Chang, M. D. Johnson, Ramon Miquel, A. Bermeo, Elisabeth Krause, Sebastian Grandis, J. Mena-Fernández, Joe Zuntz, Jochen Weller, F. J. Castander, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, K. Honscheid, Eli S. Rykoff, Richard G. Kron, A. Carnero Rosell, Felipe Menanteau, S. Samuroff, Gregory Tarle, Santiago Serrano, J. DeRose, D. J. Brout, J. Prat, Samuel Hinton, G. Gutierrez, Xi Chen, A. A. Plazas, Sunayana Bhargava, Joseph J. Mohr, A. Saro, Jennifer L. Marshall, W. G. Hartley, M. Gatti, Juan Estrada, Michael Schubnell, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, European Research Council, 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, UAM. Departamento de Física Teórica, Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Allen, S., Annis, J., Avila, S., Bacon, D., Bechtol, K., Bermeo, A., Bernstein, G. M., Bertin, E., Bhargava, S., Bocquet, S., Brooks, D., Brout, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, X., Choi, A., Costanzi, M., Crocce, M., Da Costa, L. N., Davis, T. M., De Vicente, J., Derose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Estrada, J., Everett, S., Evrard, A. E., Farahi, A., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giles, P., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lima, M., Lin, H., Maccrann, N., Maia, M. A. G., Mantz, A., Marshall, J. L., Martini, P., Mayers, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Prat, J., Rau, M. M., Romer, A. K., Roodman, A., Rooney, P., Rozo, E., Rykoff, E. S., Sako, M., Samuroff, S., Sanchez, C., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, J. A., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tucker, D. L., Varga, T. N., Von Der Linden, A., Walker, A. R., Wechsler, R. H., Weller, J., Wilkinson, R. D., Wu, H., Yanny, B., Zhang, Y., Zhang, Z., and Zuntz, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Data_CODINGANDINFORMATIONTHEORY, 01 natural sciences, XMM-Newton Telescope, symbols.namesake, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, Planck, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Physics, 010308 nuclear & particles physics, Física, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Galaxies, Cosmos, Redshift, Galaxy, Cosmology, Dark energy, symbols, Baryon acoustic oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: et al., We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for S8=σ8(Ωm/0.3)0.5=0.65±0.04, driven by a low matter density parameter, Ωm=0.179+0.031−0.038, with σ8−Ωm posteriors in 2.4σ tension with the DES Y1 3x2pt results, and in 5.6σ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with x-ray and microwave data, as well as independent constraints on the observable-mass relation from Sunyaev-Zeldovich selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold (λ≥30) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model., The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-66861, No. FPA2015-68048, No. SEV2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. 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 No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through Project No. CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. M. C. and A. S. are supported by the ERC-StG “ClustersXCosmo” Grant agreement No. 716762. A. S. is supported by the FAREMIUR grant “ClustersXEuclid”. E. R. was supported by the DOE Grant No. DE-SC0015975, by the Sloan Foundation, Grant No. FG-2016-6443, and the Cottrell Scholar program of the Research Corporation for Science Advancement. This research used simulations that were performed resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DEAC02-05CH11231.
Published: 2020

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