Author: "Marshall, J L" / Topic: astrophysics::cosmology and extragalactic astrophysics - Searchworks@Jio Institute Digital Library Search Results

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115 results on '"Marshall, J L"'

1. Constraining the baryonic feedback with cosmic shear using the DES Year-3 small-scale measurements

Author: Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, Chen, A., Aricò, G., Huterer, D., Angulo, R. E., Weaverdyck, N., Friedrich, O., Secco, L. F., Hernández-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Brandao-Souza, A., Bridle, S. L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M. E. S., Davis, C., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferté, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Hoffmann, K., Huang, H., Huff, E. M., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Nuclear Theory, High Energy Physics::Phenomenology, cosmology observations, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics Cosmology and Nongalactic Astrophysics, Space and Planetary Science, gravitational lensing weak, large-scale structure of Universe, cosmology observation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package \texttt{Baccoemu} to accelerate the evaluation of the baryonic nonlinear matter power spectrum. We design our analysis pipeline to focus on the constraints of the baryonic suppression effects, utilizing the implication given by a principal component analysis on the Fisher forecasts. Our constraint on the baryonic effects can then be used to better model and ameliorate the effects of baryons in producing cosmological constraints from the next generation large-scale structure surveys. We detect the baryonic suppression on the cosmic shear measurements with a $\sim 2 \sigma$ significance. The characteristic halo mass for which half of the gas is ejected by baryonic feedback is constrained to be $M_c > 10^{13.2} h^{-1} M_{\odot}$ (95\% C.L.). The best-fit baryonic suppression is $\sim 5\%$ at $k=1.0 {\rm Mpc}\ h^{-1}$ and $\sim 15\%$ at $k=5.0 {\rm Mpc} \ h^{-1}$. Our findings are robust with respect to the assumptions about the cosmological parameters, specifics of the baryonic model, and intrinsic alignments., Comment: 20 pages, 10 figures. DES Collaboration, Year-3 analysis
Published: 2022

2. The Dark Energy Survey supernova program: cosmological biases from supernova photometric classification

Author: Vincenzi, M., Sullivan, M., Möller, A., Armstrong, P., Bassett, B. A., Brout, D., Carollo, D., Carr, A., Davis, T. M., Frohmaier, C., Galbany, L., Glazebrook, K., Graur, O., Kelsey, L., Kessler, R., Kovacs, E., Lewis, G. F., Lidman, C., Malik, U., Nichol, R. C., Popovic, B., Sako, M., Scolnic, D., Smith, M., Taylor, G., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Annis, J., Asorey, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., Des, Collaboration, Vincenzi, M., Sullivan, M., Möller, A., Armstrong, P., Bassett, B. A., Brout, D., Carollo, D., Carr, A., Davis, T. M., Frohmaier, C., Galbany, L., Glazebrook, K., Graur, O., Kelsey, L., Kessler, R., Kovacs, E., Lewis, G. F., Lidman, C., Malik, U., Nichol, R. C., Popovic, B., Sako, M., Scolnic, D., Smith, M., Taylor, G., Tucker, B. E., Wiseman, P., Aguena, M., Allam, S., Annis, J., Asorey, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., Des, Collaboration, UAM. Departamento de Física Teórica, 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), cosmology observations, FOS: Physical sciences, Física, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Astrophysics Cosmology and Nongalactic Astrophysics, Cosmology: Observations, Supernovae: General, surveys, supernovae general, Space and Planetary Science, survey, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology observation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Artículo escrito por un elevado número de autores, solo se referencian el que aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere, This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Monthly Notices of the Royal Astronomical Society Volume 518.1 (2023): 1106-1127 is available online at: https://academic.oup.com/mnras/article-abstract/518/1/1106/6601453, Cosmological analyses of samples of photometrically identified type Ia supernovae (SNe Ia) depend on understanding the effects of ‘contamination’ from core-collapse and peculiar SN Ia events. We employ a rigorous analysis using the photometric classifier SuperNNova on state-of-the-art simulations of SN samples to determine cosmological biases due to such ‘non-Ia’ contamination in the Dark Energy Survey (DES) 5-yr SN sample. Depending on the non-Ia SN models used in the SuperNNova training and testing samples, contamination ranges from 0.8 to 3.5 per cent, with a classification efficiency of 97.7–99.5 per cent. Using the Bayesian Estimation Applied to Multiple Species (BEAMS) framework and its extension BBC (‘BEAMS with Bias Correction’), we produce a redshift-binned Hubble diagram marginalized over contamination and corrected for selection effects, and use it to constrain the dark energy equation-of-state, w. Assuming a flat universe with Gaussian ΩM prior of 0.311 ± 0.010, we show that biases on w are, This work was supported by the Science and Technology Facilities Council [grant number ST/P006760/1] through the DISCnet Cen¬tre for Doctoral Training. MS acknowledges support from EU/FP7¬ERC grant 615929, and PW acknowledges support from STFC grant ST/R000506/1. TMD acknowledges support from ARC grant FL180100168. LG acknowledges financial support from the Span¬ish Ministry of Science, Innovation and Universities (MICIU) un¬der the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. RH and MS were supported by DOE grant DE-FOA-0001781 and NASA grant NNH15ZDA001N-WFIRST. The material is based upon work sup¬ported by NASA under award number 80GSFC17M0002. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. This paper has gone through internal review by the DES collab¬oration. 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 Uni¬versity of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fun¬damental Physics and Astronomy at Texas A&M University, Finan¬ciadora 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 Forschungsgemein¬schaft 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 Cam¬bridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University Col¬lege London, the DES-Brazil Consortium, the University of Edin¬burgh, 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 Uni-versity, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the Uni¬versity of Sussex, Texas A&M University, and the OzDES Member¬ship 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 Na¬tional 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 re¬sults 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 Ciên¬cia 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. De¬partment of Energy, Office of Science, Office of High Energy Physics. This work was completed in part with resources provided by the University of Chicago’s Research Computing Center. Finally, this work was based in part on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present
Published: 2023

3. Velocity dispersions of clusters in the Dark Energy Survey Y3 redMaPPer catalogue

Author: A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, UAM. Departamento de Física Teórica, A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, Department of Energy (US), European Commission, European Research Council, Ministero dell'Istruzione, dell'Università e della Ricerca, Ministerio de Ciencia, Innovación y Universidades (España), Fundação para a Ciência e a Tecnologia (Portugal), Agencia Estatal de Investigación (España), National Science Foundation (US), Generalitat de Catalunya, and Ministerio de Economía y Competitividad (España)
Subjects: X-Rays: Galaxies: Clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Física, Astronomy and Astrophysics, galaxies: clusters: general, X-rays: galaxies: clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, clusters: general [galaxies], galaxies: clusters [X-rays], CLUSTERS, QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB, Galaxies: Clusters: General
Abstract: DES Collaboration: V. Wetzell et al., We measure the velocity dispersions of clusters of galaxies selected by the red-sequence Matched-filter Probabilistic Percolation (redMaPPer) algorithm in the first three years of data from the Dark Energy Survey (DES), allowing us to probe cluster selection and richness estimation, λ, in light of cluster dynamics. Our sample consists of 126 clusters with sufficient spectroscopy for individual velocity dispersion estimates. We examine the correlations between cluster velocity dispersion, richness, X-ray temperature, and luminosity, as well as central galaxy velocity offsets. The velocity dispersion–richness relation exhibits a bimodal distribution. The majority of clusters follow scaling relations between velocity dispersion, richness, and X-ray properties similar to those found for previous samples; however, there is a significant population of clusters with velocity dispersions that are high for their richness. These clusters account for roughly 22 per cent of the λ < 70 systems in our sample, but more than half (55 per cent) of λ < 70 clusters at z > 0.5. A couple of these systems are hot and X-ray bright as expected for massive clusters with richnesses that appear to have been underestimated, but most appear to have high velocity dispersions for their X-ray properties likely due to line-of-sight structure. These results suggest that projection effects contribute significantly to redMaPPer selection, particularly at higher redshifts and lower richnesses. The redMaPPer determined richnesses for the velocity dispersion outliers are consistent with their X-ray properties, but several are X-ray undetected and deeper data are needed to understand their nature., This work was supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Numbers DE-SC0010107 and A00-1465-001. AS is supported by the ERC-StG ‘ClustersXCosmo’ grant agreement 716762, by the FARE-MIUR grant ’ClustersXEuclid’ R165SBKTMA, and by INFN InDark Grant. PTPV was supported by Fundação para a Ciência e a Tecnologia (FCT) through research grants UIDB/04434/2020andUIDP/04434/2020. 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 University of Illinois at Urbana-Champaign - National Center for Supercomputing Applications, 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, 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. This study is 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 EU Seventh Framework Programme (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.
Published: 2022

4. Dark Energy Survey Year 3 results: Cosmology from combined galaxy clustering and lensing validation on cosmological simulations

Author: DeRose, J., Wechsler, R. H., Becker, M. R., Rykoff, E. S., Pandey, S., MacCrann, N., Amon, A., Myles, J., Krause, E., Gruen, D., Jain, B., Troxel, M. A., Prat, J., Alarcon, A., Sanchez, C., Blazek, J., Crocce, M., Giannini, G., Gatti, M., Bernstein, G. M., Zuntz, J., Dodelson, S., Fang, X., Friedrich, O., Secco, L. F., Elvin-Poole, J., Porredon, A., Everett, S., Choi, A., Harrison, I., Cordero, J., Rodriguez-Monroy, M., McCullough, J., Cawthon, R., Chen, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Gruendl, R. A., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Raveri, M., Rosenfeld, R., Ross, A. J., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Yin, B., Zhang, Y., Fosalba, P., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Castander, F. J., Chang, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Ferte, A., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., UAM. Departamento de Física Teórica, A DeRose, J., Wechsler, R. H., Becker, M. R., Rykoff, E. S., Pandey, S., Maccrann, N., Amon, A., Myles, J., Krause, E., Gruen, D., Jain, B., Troxel, M. A., Prat, J., Alarcon, A., Sánchez, C., Blazek, J., Crocce, M., Giannini, G., Gatti, M., Bernstein, G. M., Zuntz, J., Dodelson, S., Fang, X., Friedrich, O., Secco, L. F., Elvin-Poole, J., Porredon, A., Everett, S., Choi, A., Harrison, I., Cordero, J., Rodriguez-Monroy, M., Mccullough, J., Cawthon, R., Chen, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Gruendl, R. A., Hartley, W. G., Huang, H., Huff, E. M., Kuropatkin, N., Raveri, M., Rosenfeld, R., Ross, A. J., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Yin, B., Zhang, Y., Fosalba, P., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Castander, F. J., Chang, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plaza, Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Commission, European Research Council, and Generalitat de Catalunya
Subjects: data release, Gravitational Lensing, model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), sky surveys, strophysics, FOS: Physical sciences, Física, Astrophysics::Cosmology and Extragalactic Astrophysics, oscillation spectroscopic survey, calibration, des, Dark Energy, Cosmology and Nongalactic Astrophysics, strophysic, challenge, impact, astro-ph.CO, Weak, redshift distributions, sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: J. DeRose et al., We present a validation of the Dark Energy Survey Year 3 (DES Y3) 3×2-point analysis choices by testing them on Buzzard2.0, a new suite of cosmological simulations that is tailored for the testing and validation of combined galaxy clustering and weak-lensing analyses. We show that the buzzard2.0 simulations accurately reproduce many important aspects of the DES Y3 data, including photometric redshift and magnitude distributions, and the relevant set of two-point clustering and weak-lensing statistics. We then show that our model for the 3×2-point data vector is accurate enough to recover the true cosmology in simulated surveys assuming the true redshift distributions for our source and lens samples, demonstrating robustness to uncertainties in the modeling of the nonlinear matter power spectrum, nonlinear galaxy bias, and higher-order lensing corrections. Additionally, we demonstrate for the first time that our photometric redshift calibration methodology, including information from photometry, spectroscopy, clustering cross-correlations, and galaxy–galaxy lensing ratios, is accurate enough to recover the true cosmology in simulated surveys in the presence of realistic photometric redshift uncertainties., J. D. is supported by the Chamberlain fellowship at Lawrence Berkeley 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 located at Lawrence Berkeley National Laboratory, operated under Contract No. DE-AC02-05CH11231. We would like to thank Stanford University and the Stanford Research Computing Center for providing computational resources and support that contributed to these research results. 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, 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. This paper is 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. AST1138766andNo.AST-1536171.The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018094773, 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 (Grant No. FP7/2007-2013) including ERC Grants No. 240672, No.291329,andNo.306478.Weacknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia(INCT)doe-Universo(CNPqGrantNo.465376/ 2014-2). This manuscript has been authored by Fermi Research Alliance, LLC, under Contract No. DE-AC0207CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

5. The Observed Evolution of the Stellar Mass-Halo Mass Relation for Brightest Central Galaxies

Author: Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F. [UNESP], Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Costanzi, M., Crocce, M., Costa, L. N. da, Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I, Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., 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., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V, Schubnell, M., Serrano, S., Sevilla-Noarbe, I, Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Varga, T. N., DES Collaboration, Golden-Marx, JB [0000-0002-6394-045X], Zhang, Y [0000-0001-5969-4631], Ogando, RLC [0000-0003-2120-1154], Palmese, A [0000-0002-6011-0530], Abbott, TMC [0000-0003-1587-3931], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], Castander, FJ [0000-0001-7316-4573], Costanzi, M [0000-0001-8158-1449], Crocce, M [0000-0002-9745-6228], Da Costa, LN [0000-0002-7731-277X], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Diehl, HT [0000-0002-8357-7467], Drlica-Wagner, A [0000-0001-8251-933X], Evrard, AE [0000-0002-4876-956X], Ferrero, I [0000-0002-1295-1132], 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], Gruen, D [0000-0003-3270-7644], Gruendl, RA [0000-0002-4588-6517], Gschwend, J [0000-0003-3023-8362], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Jeltema, T [0000-0001-6089-0365], Kuehn, K [0000-0003-0120-0808], Kuropatkin, N [0000-0003-2511-0946], Marshall, JL [0000-0003-0710-9474], Melchior, P [0000-0002-8873-5065], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Morgan, R [0000-0002-7016-5471], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Romer, AK [0000-0002-9328-879X], Sanchez, E [0000-0002-9646-8198], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Soares-Santos, M [0000-0001-6082-8529], Tarle, G [0000-0003-1704-0781], Apollo - University of Cambridge Repository, National Science Foundation (US), Ministerio de Ciencia e Innovación (España), European Commission, UAM. Departamento de Física Teórica, A Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Castander, F. J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., 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., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares- Santos, M., Suchyta, E., Tarle, G., Varga, T. N., Shanghai Jiao Tong Univ, Univ Michigan, Fermilab Natl Accelerator Lab, Lab Interinst E Astron LIneA, Observ Nacl, Univ Chicago, NSFs Natl Opt Infrared Astron Res Lab, Universidade Estadual Paulista (UNESP), Univ Portsmouth, Inst Astrophys Paris, UPMC Univ Paris 06, UCL, Inst Astrofis Canarias, Univ La Laguna, Natl Ctr Supercomp Applicat, Univ Illinois, Inst Estudis Espacials Catalunya IEEC, CSIC, Univ Trieste, INAF Osservatorio Astron Trieste, Inst Fundamental Phys Universe, Ctr Invest Energet Medioambientales & Tecnol CIEM, IIT Hyderabad, Santa Cruz Inst Particle Phys, Univ Oslo, Univ Autonoma Madrid, Stanford Univ, SLAC Natl Accelerator Lab, Univ Geneva, Univ Queensland, Ohio State Univ, Ludwig Maximilians Univ Munchen, Ctr Astrophys Harvard & Smithsonian, Lawrence Berkeley Natl Lab, Univ Arizona, Macquarie Univ, Lowell Observ, Universidade de São Paulo (USP), Texas A&M Univ, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Barcelona Inst Sci & Technol, Max Planck Inst Extraterr Phys, Univ Wisconsin, Univ Cambridge, Univ Sussex, Univ Fed Rio Grande do Sul, Univ Southampton, and Oak Ridge Natl Lab
Subjects: Galaxy clusters, Galaxy evolution, Brightest cluster galaxies, astro-ph.GA, FOS: Physical sciences, Física, Galaxy cluster, Astronomy and Astrophysics, GALÁXIAS, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Galaxy Astrophysics
Abstract: Golden-Marx; J. B. et al. (DES Collaboration), We quantify evolution in the cluster-scale stellar mass-halo mass (SMHM) relation's parameters using 2323 clusters and brightest central galaxies (BCGs) over the redshift range 0.03 ≤ z ≤ 0.60. The precision on the inferred SMHM parameters is improved by including the magnitude gap (m gap) between the BCG and fourth-brightest cluster member (M14) as a third parameter in the SMHM relation. At fixed halo mass, accounting for m gap, through a stretch parameter, reduces the SMHM relation's intrinsic scatter. To explore this redshift range, we use clusters, BCGs, and cluster members identified using the Sloan Digital Sky Survey C4 and redMaPPer cluster catalogs and the Dark Energy Survey redMaPPer catalog. Through this joint analysis, we detect no systematic differences in BCG stellar mass, m gap, and cluster mass (inferred from richness) between the data sets. We utilize the Pareto function to quantify each parameter's evolution. We confirm prior findings of negative evolution in the SMHM relation's slope (3.5σ), and detect negative evolution in the stretch parameter (4.0σ) and positive evolution in the offset parameter (5.8σ). This observed evolution, combined with the absence of BCG growth, when stellar mass is measured within 50 kpc, suggests that this evolution results from changes in the cluster's m gap. For this to occur, late-term growth must be in the intracluster light surrounding the BCG. We also compare the observed results to IllustrisTNG 300-1 cosmological hydrodynamic simulations and find modest qualitative agreement. However, the simulations lack the evolutionary features detected in the real data., 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 Ciênciae 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: 2022

6. Dark Energy Survey Year 3 results: Cosmology from cosmic shear and robustness to modeling uncertainty

Author: Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferté, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sánchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., 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., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Des, Collaboration, 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), 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), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-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, Secco, L. F., Samuroff, S., Krause, E., Jain, B., Blazek, J., Raveri, M., Campos, A., Amon, A., Chen, A., Doux, C., Choi, A., Gruen, D., Bernstein, G. M., Chang, C., Derose, J., Myles, J., Ferte, A., Lemos, P., Huterer, D., Prat, J., Troxel, M. A., Maccrann, N., Liddle, A. R., Kacprzak, T., Fang, X., Sanchez, C., Pandey, S., Dodelson, S., Chintalapati, P., Hoffmann, K., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E. J., Bechtol, K., Becker, M. R., Brandao-Souza, A., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Cordero, J. P., Crocce, M., Davis, C., Di Valentino, E., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elidaiana, M., Elsner, F., Elvin-Poole, J., Everett, S., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Jarvis, M., Jeffrey, N., Kuropatkin, N., Leget, P. -F., Muir, J., Mccullough, J., Navarro Alsina, A., Omori, Y., Park, Y., Porredon, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E. S., Shin, T., Tutusaus, I., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Lin, H., 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-Chinchon, F., Petravick, D., Pieres, A., Plazas Malagon, A. A., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), National Science Foundation (US), European Commission, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, University of Chicago, University of Pennsylvania, Carnegie Mellon University, Northeastern University, University of Arizona, École Polytechnique Fédérale de Lausanne (EPFL), Stanford University, University of Michigan, The Ohio State University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, University of California, California Institute of Technology, University College London, Duke University, University of Cambridge, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, ETH Zürich, Northern Illinois University, University of Zürich, Argonne National Laboratory, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, University of Hawai'i, University of Wisconsin-Madison, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnológicas (CIEMAT), Instituto de Astrofísica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, University of Manchester, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Fermi National Accelerator Laboratory, Max Planck Institute für Extraterrestrial Physics, Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, Université de Genève, Université de Paris, Laboratoire de Physique de Clermont, Laboratoire de Physique Nucléaire et de Hautes Énergies, The University of Tokyo, Ohio State University, Brookhaven National Laboratory, Ludwig-Maximilians Universität München, NSF's National Optical-Infrared Astronomy Research Laboratory, University of Portsmouth, Institut d'Astrophysique de Paris, University of Sussex, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Max Planck Institute for Extraterrestrial Physics, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas A and M University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, Oak Ridge National Laboratory, 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), and UAM. Departamento de Física Teórica
Subjects: luminous red galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, Sky surveys, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Gravitational lenses, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, Weak, baryonic feedback, 010303 astronomy & astrophysics, redshift inference, intrinsic galaxy shapes, Gravitational Lensing, 010308 nuclear & particles physics, Física, COSMOLOGIA, Dark Energy, 13. Climate action, 2-point correlation-functions, photometric data set, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Secco, L.F., et al. (DES Collaboration), This work and its companion paper, Amon et al. [Phys. Rev. D 105, 023514 (2022)PRVDAQ2470-001010.1103/PhysRevD.105.023514], present cosmic shear measurements and cosmological constraints from over 100 million source galaxies in the Dark Energy Survey (DES) Year 3 data. We constrain the lensing amplitude parameter S8σ8ωm/0.3 at the 3% level in ΛCDM: S8=0.759-0.023+0.025 (68% CL). Our constraint is at the 2% level when using angular scale cuts that are optimized for the ΛCDM analysis: S8=0.772-0.017+0.018 (68% CL). With cosmic shear alone, we find no statistically significant constraint on the dark energy equation-of-state parameter at our present statistical power. We carry out our analysis blind, and compare our measurement with constraints from two other contemporary weak lensing experiments: the Kilo-Degree Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program (HSC). We additionally quantify the agreement between our data and external constraints from the Cosmic Microwave Background (CMB). Our DES Y3 result under the assumption of ΛCDM is found to be in statistical agreement with Planck 2018, although favors a lower S8 than the CMB-inferred value by 2.3σ (a p-value of 0.02). This paper explores the robustness of these cosmic shear results to modeling of intrinsic alignments, the matter power spectrum and baryonic physics. We additionally explore the statistical preference of our data for intrinsic alignment models of different complexity. The fiducial cosmic shear model is tested using synthetic data, and we report no biases greater than 0.3σ in the plane of S8×ωm caused by uncertainties in the theoretical models., 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. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-2016-0597, and No. 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 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 number CE110001020.
Published: 2022

7. Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies

Author: A Mau, S., Nadler, E. O., Wechsler, R. H., Drlica-Wagner, A., Bechtol, K., Green, G., Huterer, D., Li, T. S., Mao, Y. -Y., Martínez-Vázquez, C. E., McNanna, M., Mutlu-Pakdil, B., Pace, A. B., Peter, A., Riley, A. H., Strigari, L., Wang, M. -Y., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., Davis, T. M., Vicente, J. De, Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Maia, M. A. G., Marshall, J. L., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Paz-Chinchón, F., Pieres, A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Weller, J., DES Collaboration, Mau, S [0000-0003-3519-4004], Nadler, EO [0000-0002-1182-3825], Wechsler, RH [0000-0003-2229-011X], Drlica-Wagner, A [0000-0001-8251-933X], Bechtol, K [0000-0001-8156-0429], Green, G [0000-0001-5417-2260], Huterer, D [0000-0001-6558-0112], Li, TS [0000-0002-9110-6163], Mao, YY [0000-0002-1200-0820], Martínez-Vázquez, CE [0000-0002-9144-7726], McNanna, M [0000-0001-5435-7820], Mutlu-Pakdil, B [0000-0001-9649-4815], Pace, AB [0000-0002-6021-8760], Peter, A [0000-0002-8040-6785], Riley, AH [0000-0001-5805-5766], Strigari, L [0000-0001-5672-6079], Wang, MY [0000-0002-8226-6237], Aguena, M [0000-0001-5679-6747], Allam, S [0000-0002-7069-7857], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bertin, E [0000-0002-3602-3664], Bocquet, S [0000-0002-4900-805X], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Rosell, AC [0000-0003-3044-5150], Kind, MC [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], Crocce, M [0000-0002-9745-6228], Davis, TM [0000-0002-4213-8783], Vicente, JD [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Ferrero, I [0000-0002-1295-1132], Flaugher, B [0000-0002-2367-5049], Frieman, J [0000-0003-4079-3263], García-Bellido, J [0000-0002-9370-8360], Giannini, G [0000-0002-3730-1750], Gruen, D [0000-0003-3270-7644], Gruendl, RA [0000-0002-4588-6517], Gschwend, J [0000-0003-3023-8362], Gutierrez, G [0000-0003-0825-0517], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Kuehn, K [0000-0003-0120-0808], Lahav, O [0000-0002-1134-9035], Maia, MAG [0000-0001-9856-9307], Marshall, JL [0000-0003-0710-9474], Miquel, R [0000-0002-6610-4836], Morgan, R [0000-0002-7016-5471], Ogando, RLC [0000-0003-2120-1154], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Sanchez, E [0000-0002-9646-8198], Serrano, S [0000-0002-0211-2861], Sevilla-Noarbe, I [0000-0002-1831-1953], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], Tucker, DL [0000-0001-7211-5729], Weller, J [0000-0002-8282-2010], Apollo - University of Cambridge Repository, UAM. Departamento de Física Teórica, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Kavli Institute for Particle Astrophysics and Cosmology, Science and Technology Facilities Council (UK), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministerio de Economía y Competitividad (España), German Research Foundation, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, A Mau, S., Nadler, E. O., Wechsler, R. H., Drlica-Wagner, A., Bechtol, K., Green, G., Huterer, D., T. S., Li, Mao, Y. -Y., Martínez-Vázquez, C. E., Mcnanna, M., Mutlu-Pakdil, B., Pace, A. B., Peter, A., Riley, A. H., Strigari, L., Wang, M. -Y., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., Davis, T. M., Vicente, J. De, Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Maia, M. A. G., Marshall, J. L., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Paz-Chinchón, F., Pieres, A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Física, Astronomy and Astrophysics, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy abundances, High Energy Physics - Phenomenology, Halo, High Energy Physics - Phenomenology (hep-ph), Dwarf Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark matter, astro-ph.CO, Dark Matter, Milky Way dark matter halo, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Mau et al., We use a recent census of the Milky Way (MW) satellite galaxy population to constrain the lifetime of particle dark matter (DM). We consider two-body decaying dark matter (DDM) in which a heavy DM particle decays with lifetime τ comparable to the age of the universe to a lighter DM particle (with mass splitting epsilon) and to a dark radiation species. These decays impart a characteristic "kick velocity," Vkick = epsilonc, on the DM daughter particles, significantly depleting the DM content of low-mass subhalos and making them more susceptible to tidal disruption. We fit the suppression of the present-day DDM subhalo mass function (SHMF) as a function of τ and Vkick using a suite of high-resolution zoom-in simulations of MW-mass halos, and we validate this model on new DDM simulations of systems specifically chosen to resemble the MW. We implement our DDM SHMF predictions in a forward model that incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk using an empirical model for the galaxy–halo connection. By comparing to the observed MW satellite population, we conservatively exclude DDM models with τ < 18 Gyr (29 Gyr) for Vkick = 20 kms−1 (40 kms−1) at 95% confidence. These constraints are among the most stringent and robust small-scale structure limits on the DM particle lifetime and strongly disfavor DDM models that have been proposed to alleviate the Hubble and S8 tensions., 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, NSF'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 No. 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: 2022

8. Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps

Author: Gatti, M., Jain, B., Chang, C., Raveri, M., Zürcher, D., Secco, L., Whiteway, L., Jeffrey, N., Doux, C., Kacprzak, T., Bacon, D., Fosalba, P., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Campos, A., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Krause, E., Leget, P. F., Lemos, P., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro, A., Pandey, S., Prat, J., Rollins, R. P., Roodman, A., Sanchez, C., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Ferrero, I., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Rodriguez-Monroyv, M., Romer, A. K., 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., DES Collaboration, Gatti, M., Jain, B., Chang, C., Raveri, M., Zürcher, D., Secco, L., Whiteway, L., Jeffrey, N., Doux, C., Kacprzak, T., Bacon, D., Fosalba, P., Alarcon, A., Amon, A., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Campos, A., Choi, A., Davis, C., Derose, J., Dodelson, S., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Harrison, I., Huterer, D., Jarvis, M., Krause, E., Leget, P. F., Lemos, P., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro, A., Pandey, S., Prat, J., Rollins, R. P., Roodman, A., Sanchez, C., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Ferrero, I., García-Bellido, J., Gaztanaga, E., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Rodriguez-Monroyv, M., Romer, A. K., 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., Des, Collaboration, UAM. Departamento de Física Teórica, Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Agencia Estatal de Investigación (España), Generalitat de Catalunya, Ministerio de Economía y Competitividad (España), Department of Energy (US), National Aeronautics and Space Administration (US), and National Science Foundation (US)
Subjects: Gravitational Lensing, data-compression, inference, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Física, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, parameter-estimation, universe, Dark Energy, Astrophysic, cosmic shear 2-point, model predictions, galaxy, simulations, Weak, peak statistics, constraints, Cosmology and Nongalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: M. Gatti et al., We present a cosmological analysis using the second and third moments of the weak lensing mass (convergence) maps from the first three years of data (Y3) data of the Dark Energy Survey. The survey spans an effective area of 4139 square degrees and uses the images of over 100 million galaxies to reconstruct the convergence field. The second moment of the convergence as a function of smoothing scale contains information similar to standard shear 2-point statistics. The third moment, or the skewness, contains additional non-Gaussian information. The data is analyzed in the context of the ΛCDM model, varying five cosmological parameters and 19 nuisance parameters modeling astrophysical and measurement systematics. Our modeling of the observables is completely analytical, and has been tested with simulations in our previous methodology study. We obtain a 1.7% measurement of the amplitude of fluctuations parameter S8≡σ8(Ωm/0.3)0.5=0.784±0.013. The measurements are shown to be internally consistent across redshift bins, angular scales, and between second and third moments. In particular, the measured third moment is consistent with the expectation of gravitational clustering under the ΛCDM model. The addition of the third moment improves the constraints on S8 and Ωm by ∼15% and ∼25% compared to an analysis that only uses second moments. We compare our results with Planck constraints from the cosmic microwave background, finding a 2.2–2.8σ tension in the full parameter space, depending on the combination of moments considered. The third moment, independently, is in 2.8σ tension with Planck, and thus provides a cross-check on the analyses of 2-point correlations., 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 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 Ciencies 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, NSF’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 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 Grant 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. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2022

9. Dark energy survey year 3 results: High-precision measurement and modeling of galaxy-galaxy lensing

Author: Prat, J., Blazek, J., Sánchez, C., Tutusaus, I., Pandey, S., Elvin-Poole, J., Krause, E., Troxel, M. A., Secco, L. F., Amon, A., Derose, J., Zacharegkas, G., Chang, C., Jain, B., Maccrann, N., Park, Y., Sheldon, E., Giannini, G., Bocquet, S., To, C., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crocce, M., Davis, C., De Vicente, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Fang, X., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Shin, T., Troja, A., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., 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., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Plazas Malagón, A. A., Sanchez, E., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., Des, Collaboration, A Prat, J., Blazek, J., Sánchez, C., Tutusaus, I., Pandey, S., Elvin- Poole, J., Krause, E., Troxel, M. A., Secco, L. F., Amon, A., Derose, J., Zacharegkas, G., Chang, C., Jain, B., Maccrann, N., Park, Y., Sheldon, E., Giannini, G., Bocquet, S., To, C., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crocce, M., Davis, C., De Vicente, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Fang, X., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Jarvis, M., Kuropatkin, N., Leget, P. -F., Lemos, P., Liddle, A. R., Mccullough, J., Muir, J., Myles, J., Navarro- Alsina, A., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Shin, T., Troja, A., Varga, T. N., Weaverdyck, N., Wechsler, R. H., Yanny, B., Yin, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., 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., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Plazas Malagón, A. A., Sanchez, E., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., and UAM. Departamento de Física Teórica
Subjects: Gravitational Lensing, Cosmology and Nongalactic Astrophysics (astro-ph.CO), cosmological parameter constraints, FOS: Physical sciences, Física, marginalization, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics, Dark Energy, Astrophysic, Cosmology and Nongalactic Astrophysics, redshift distribution, mass, Weak, photometric data set, sdss, cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics, intrinsic alignments
Abstract: DES Collaboration: J. Prat et al., We present and characterize the galaxy-galaxy lensing signal measured using the first three years of data from the Dark Energy Survey (DES Y3) covering 4132 deg2. These galaxy-galaxy measurements are used in the DES Y3 3×2pt cosmological analysis, which combines weak lensing and galaxy clustering information. We use two lens samples: a magnitude-limited sample and the redmagic sample, which span the redshift range ∼0.2–1 with 10.7 and 2.6 M galaxies, respectively. For the source catalog, we use the metacalibration shape sample, consisting of ≃100M galaxies separated into four tomographic bins. Our galaxy-galaxy lensing estimator is the mean tangential shear, for which we obtain a total SNR of ∼148 for maglim (∼120 for redmagic), and ∼67 (∼55) after applying the scale cuts of 6Mpc/h. Thus we reach percent-level statistical precision, which requires that our modeling and systematic-error control be of comparable accuracy. The tangential shear model used in the 3×2pt cosmological analysis includes lens magnification, a five-parameter intrinsic alignment model, marginalization over a point mass to remove information from small scales and a linear galaxy bias model validated with higher-order terms. We explore the impact of these choices on the tangential shear observable and study the significance of effects not included in our model, such as reduced shear, source magnification, and source clustering. We also test the robustness of our measurements to various observational and systematics effects, such as the impact of observing conditions, lens-source clustering, random-point subtraction, scale-dependent metacalibration responses, point spread function residuals, and B modes.
Published: 2022

10. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample

Author: Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Carnero Rosell, A., Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Carrasco Kind, M., Chintalapati, P., Cordero, J., Derose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., Maccrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., 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., Petravick, D., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Des, Collaboration, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), European Commission, Generalitat de Catalunya, European Research Council, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Carnero Rosell, A., Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Carrasco Kind, M., Chintalapati, P., Cordero, J., Derose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., Maccrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., 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., Petravick, D., Pieres, A., Plazas Malagón, A. A., Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Des, Collaboration, HEP, INSPIRE, 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: luminous red galaxies, data release, pau survey, Cosmology and Nongalactic Astrophysics (astro-ph.CO), roman-space-telescope, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, oscillation spectroscopic survey, Astrophysic, Cosmology and Nongalactic Astrophysics, internal consistency, digital sky survey, redshift distributions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], photometric data set, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: A. Porredon et al., The cosmological information extracted from photometric surveys is most robust when multiple probes of the large scale structure of the Universe are used. Two of the most sensitive probes are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the way galaxies trace matter (the galaxy bias factor). The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000deg2 of the Dark Energy Survey’s first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies, especially selected to optimize such combination, and 100 million background shapes. We consider two flat cosmological models, the Standard Model with dark energy and cold dark matter (ΛCDM ) a variation with a free parameter for the dark energy equation of state (wCDM). Both models are marginalized over 25 astrophysical and systematic nuisance parameters. In ΛCDM we obtain for the matter density Ωm=0.320+0.041−0.034 and for the clustering amplitude S8≡σ8(Ωm/0.3)0.5=0.778+0.037−0.031, at 68% C.L. The latter is only 1σ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In wCDM we find Ωm=0.32+0.044−0.046, S8=0.777+0.049−0.051 and dark energy equation of state w=−1.031+0.218−0.379. We find that including smaller scales, while marginalizing over nonlinear galaxy bias, improves the constraining power in the Ωm−S8 plane by 31% and in the Ωm−w plane by 41% while yielding consistent cosmological parameters from those in the linear bias case. These results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions (3×2pt)., 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 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 Ciencies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo 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 systemis 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. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds fromthe 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, and 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. 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 nonexclusive 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. Computations were made on the supercomputer Guillimin from McGill University, managed by Calcul Quebec and Compute Canada. The operation of this supercomputer is funded by the Canada Foundation for Innovation (CFI), the ministere de l’Économie, de la science et de l’innovation du Quebec (MESI) and the Fonds de recherche du Quebec-Nature et technologies (FRQ-NT). This research is part of the Blue Waters sustained-petascale computing project, which is supported by the National Science Foundation (Grants No. OCI-0725070 and No. ACI-1238993) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. This research used resources of the Ohio Supercomputer Center (OSC) [117] and 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

11. Dark Energy Survey Year 3 Results: Cosmology from Cosmic Shear and Robustness to Data Calibration

Author: Amon, A., Gruen, D., Troxel, M. A., MacCrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., DeRose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferté, A., Raveri, M., Lemos, P., Campos, A., Prat, J., Sánchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Rosell, A. Carnero, Kind, M. Carrasco, Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P. -F., Liddle, A. R., McCullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kron, R., Kuehn, K., Lahav, O., Lima, M., Lin, H., 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., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Weller, J., 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), Agencia Estatal de Investigación (España), European Commission, European Research Council, Generalitat de Catalunya, Department of Energy (US), National Science Foundation (US), National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Amon, A., Gruen, D., Troxel, M. A., Maccrann, N., Dodelson, S., Choi, A., Doux, C., Secco, L. F., Samuroff, S., Krause, E., Cordero, J., Myles, J., Derose, J., Wechsler, R. H., Gatti, M., Navarro-Alsina, A., Bernstein, G. M., Jain, B., Blazek, J., Alarcon, A., Ferte, A., Lemos, P., Raveri, M., Campos, A., Prat, J., Sanchez, C., Jarvis, M., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bridle, S. L., Camacho, H., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Crocce, M., Davis, C., Diehl, H. T., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Friedrich, O., Gaztanaga, E., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huang, H., Huff, E. M., Huterer, D., Kuropatkin, N., Leget, P., Liddle, A. R., Mccullough, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Refregier, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kron, R., Kuehn, K., Lahav, O., Lima, M., Lin, H., 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-Chinchon, F., Petravick, D., Pieres, A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Tarle, G., Thomas, D., To, C., Weller, J., Stanford University, 382 Via Pueblo Mall, SLAC National Accelerator Laboratory, Duke University, University of Cambridge, Carnegie Mellon University, The Ohio State University, University of Pennsylvania, University of Chicago, University of Arizona, University of Manchester, Lawrence Berkeley National Laboratory, Universidade Estadual de Campinas (UNICAMP), Laboratório Interinstitucional de E-Astronomia, Observatoire de Sauverny, Argonne National Laboratory, California Institute of Technology, University College London, University of Sussex, University of Michigan, Universidade Estadual Paulista (UNESP), University of Wisconsin-Madison, Instituto de Astrofisica de Canarias, Universidad de la Laguna, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Fermi National Accelerator Laboratory, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Santa Cruz Institute for Particle Physics, The Barcelona Institute of Science and Technology, Denys Wilkinson Building, University of Geneva, University of Edinburgh, Universidade de Lisboa, Perimeter Institute for Theoretical Physics, The University of Tokyo, ETH Zurich, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, University of Portsmouth, Institut d'Astrophysique de Paris, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics|Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Harvard University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Southampton, and UAM. Departamento de Física Teórica
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), microwave background anisotropies, systematic-errors, FOS: Physical sciences, parameter constraints, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, large-scale structure, Astrophysic, weak-lensing surveys, Cosmology and Nongalactic Astrophysics, 0103 physical sciences, internal consistency, Weak, redshift distributions, 010303 astronomy & astrophysics, Gravitational Lensing, 010308 nuclear & particles physics, Física, Dark Energy, intrinsic correlation, matter power spectrum, 2-point correlation-functions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: A. Amon et al., This work, together with its companion paper, Secco, Samuroff et al. [Phys. Rev. D 105, 023515 (2022)], present the Dark Energy Survey Year 3 cosmic-shear measurements and cosmological constraints based on an analysis of over 100 million source galaxies. With the data spanning 4143 deg2 on the sky, divided into four redshift bins, we produce a measurement with a signal-to-noise of 40. We conduct a blind analysis in the context of the Lambda-Cold Dark Matter (ΛCDM) model and find a 3% constraint of the clustering amplitude, S8≡σ8(Ωm/0.3)0.5=0.759+0.025−0.023. A ΛCDM-Optimized analysis, which safely includes smaller scale information, yields a 2% precision measurement of S8=0.772+0.018−0.017 that is consistent with the fiducial case. The two low-redshift measurements are statistically consistent with the Planck Cosmic Microwave Background result, however, both recovered S8 values are lower than the high-redshift prediction by 2.3σ and 2.1σ (p-values of 0.02 and 0.05), respectively. The measurements are shown to be internally consistent across redshift bins, angular scales and correlation functions. The analysis is demonstrated to be robust to calibration systematics, with the S8 posterior consistent when varying the choice of redshift calibration sample, the modeling of redshift uncertainty and methodology. Similarly, we find that the corrections included to account for the blending of galaxies shifts our best-fit S8 by 0.5σ without incurring a substantial increase in uncertainty. We examine the limiting factors for the precision of the cosmological constraints and find observational systematics to be subdominant to the modeling of astrophysics. Specifically, we identify the uncertainties in modeling baryonic effects and intrinsic alignments as the limiting systematics., This research manuscript made use of Astropy [204,205], GetDist [206], ChainConsumer10 [207] and Matplotlib [208], and has been prepared using NASA’s Astrophysics Data System Bibliographic Services. 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 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 Ciencies 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 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 Grant 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, and Office of High Energy Physics.
Published: 2021

12. Dark Energy Survey Year 3 Results: Constraints on cosmological parameters and galaxy bias models from galaxy clustering and galaxy-galaxy lensing using the redMaGiC sample

Author: Pandey, S., Krause, E., DeRose, J., MacCrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., 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., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., 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), DES, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Australian Research Council, European Commission, European Research Council, Pandey, S., Krause, E., Derose, J., Maccrann, N., Jain, B., Crocce, M., Blazek, J., Choi, A., Huang, H., To, C., Fang, X., Elvin-Poole, J., Prat, J., Porredon, A., Secco, L. F., Rodriguez-Monroy, M., Weaverdyck, N., Park, Y., Raveri, M., Rozo, E., Rykoff, E. S., Bernstein, G. M., Sánchez, C., Jarvis, M., Troxel, M. A., Zacharegkas, G., Chang, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Chintalapati, P., Davis, C., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Everett, S., Farahi, A., Ferté, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Huff, E. M., Huterer, D., Kovacs, A., Leget, P. F., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Rollins, R. P., Roodman, A., Rosenfeld, R., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., 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., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Weller, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysic, combination, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, Astrophysics of Galaxies, FOS: Physical sciences, marginalization, Astrophysics, Cosmology and Nongalactic Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics - Astrophysics of Galaxies, efficient, Astrophysic, scale dependence, Astrophysics of Galaxies (astro-ph.GA), halo-mass, evolution, impact, redshift distributions, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: S. Pandey et al., We constrain cosmological parameters and galaxy-bias parameters using the combination of galaxy clustering and galaxy-galaxy lensing measurements from the Dark Energy Survey (DES) year-3 data. We describe our modeling framework and choice of scales analyzed, validating their robustness to theoretical uncertainties in small-scale clustering by analyzing simulated data. Using a linear galaxy-bias model and redMaGiC galaxy sample, we obtain 10% constraints on the matter density of the Universe. We also implement a nonlinear galaxy-bias model to probe smaller scales that includes parametrization based on hybrid perturbation theory and find that it leads to a 17% gain in cosmological constraining power. We perform robustness tests of our methodology pipeline and demonstrate stability of the constraints to changes in the theory model. Using the redMaGiC galaxy sample as foreground lens galaxies and adopting the best-fitting cosmological parameters from DES year-1 data, we find the galaxy clustering and galaxy-galaxy lensing measurements to exhibit significant signals akin to decorrelation between galaxies and mass on large scales, which is not expected in any current models. This likely systematic measurement error biases our constraints on galaxy bias and the S8 parameter. We find that a scale-, redshift- and sky-area-independent phenomenological decorrelation parameter can effectively capture this inconsistency between the galaxy clustering and galaxy-galaxy lensing. We trace the source of this correlation to a color-dependent photometric issue and minimize its impact on our result by changing the selection criteria of redMaGiC galaxies. Using this new sample, our constraints on the S8 parameter are consistent with previous studies and we find a small shift in the Ωm constraints compared to the fiducial redMaGiC sample. We infer the constraints on the mean host-halo mass of the redMaGiC galaxies in this new sample from the large-scale bias constraints, finding the galaxies occupy halos of mass approximately 1.6×1013M⊙/h., E. K. is supported by the Department of Energy Grant No. DE-SC0020247 and the David and Lucile Packard Foundation. S. P. and B.J. are supported in part by the U.S. Department of Energy Grant No. DE-SC0007901 and NASA ATP Grant No. NNH17ZDA001N. 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 OhioStateUniversity, theMitchell 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 Energ´eticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität MünchenandtheassociatedExcellenceCluster 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 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. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-20160597, and No. MDM-2015-0509, some of which include ERDFfundsfromtheEuropean 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,andNo.306478.Weacknowledgesupportfrom 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 ofScience,OfficeofHighEnergyPhysics.
Published: 2021

13. Dwarf AGNs from Optical Variability for the Origins of Seeds (DAVOS): Insights from the Dark Energy Survey Deep Fields

Author: Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., Collaboration, DES, Burke, Colin J., Liu, Xin, Shen, Yue, Phadke, Kedar A., Yang, Qian, Hartley, Will G., Harrison, Ian, Palmese, Antonella, Guo, Hengxiao, Zhang, Kaiwen, Kron, Richard, Turner, David J., Giles, Paul A., Lidman, Christopher, Chen, Yu-Ching, Gruendl, Robert A., Choi, Ami, Amon, Alexandra, Sheldon, Erin, Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Reil, K., Romer, A. K., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wilkinson, R. D., and Des, Collaboration
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies active, galaxies dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, black hole physic, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We present a sample of 706, $z < 1.5$ active galactic nuclei (AGNs) selected from optical photometric variability in three of the Dark Energy Survey (DES) deep fields (E2, C3, and X3) over an area of 4.64 deg$^2$. We construct light curves using difference imaging aperture photometry for resolved sources and non-difference imaging PSF photometry for unresolved sources, respectively, and characterize the variability significance. Our DES light curves have a mean cadence of 7 days, a 6 year baseline, and a single-epoch imaging depth of up to $g \sim 24.5$. Using spectral energy distribution (SED) fitting, we find 26 out of total 706 variable galaxies are consistent with dwarf galaxies with a reliable stellar mass estimate ($M_{\ast}, 21 pages, 22 figures incl. 3 appendices; accepted for publication in MNRAS
Published: 2021
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14. Dark Energy Survey Year 3 Results: Exploiting small-scale information with lensing shear ratios

Author: Sánchez, C., Prat, J., Zacharegkas, G., Pandey, S., Baxter, E., Bernstein, G. M., Blazek, J., Cawthon, R., Chang, C., Krause, E., Lemos, P., Park, Y., Raveri, M., Sanchez, J., Troxel, M. A., Amon, A., Fang, X., Friedrich, O., Gruen, D., Porredon, A., Secco, L. F., Samuroff, S., Alarcon, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Chen, R., Choi, A., Crocce, M., Davis, C., De Vicente, J., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Ferté, A., Fosalba, P., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jarvis, M., Jain, B., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., 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), DES, National Science Foundation (US), Department of Energy (US), Ministerio de Economía y Competitividad (España), European Research Council, Generalitat de Catalunya, European Commission, A Sánchez, C., Prat, J., Zacharegkas, G., Pandey, S., Baxter, E., Bernstein, G. M., Blazek, J., Cawthon, R., Chang, C., Krause, E., Lemos, P., Park, Y., Raveri, M., Sanchez, J., Troxel, M. A., Amon, A., Fang, X., Friedrich, O., Gruen, D., Porredon, A., Secco, L. F., Samuroff, S., Alarcon, A., Alves, O., Andrade-Oliveira, F., Bechtol, K., Becker, M. R., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Chen, R., Choi, A., Crocce, M., Davis, C., De Vicente, J., Derose, J., Di Valentino, E., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Ferté, A., Fosalba, P., Gatti, M., Giannini, G., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jarvis, M., Jain, B., Kuropatkin, N., Leget, P. -F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Rollins, R. P., Roodman, A., Rosenfeld, R., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Tutusaus, I., Varga, T. N., Wechsler, R. H., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley- Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and UAM. Departamento de Física Teórica
Subjects: Gravitational Lensing, mice, Cosmology and Nongalactic Astrophysics (astro-ph.CO), challenge lightcone simulation, halo, Física, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, calibration, Astrophysics, Dark Energy, Astrophysic, Cosmology and Nongalactic Astrophysics, statistics, galaxies, luminosity, Weak, baryonic feedback, constraints, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], intrinsic alignments, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: C. Sánchez et al., Using the first three years of data from the Dark Energy Survey (DES), we use ratios of small-scale galaxy-galaxy lensing measurements around the same lens sample to constrain source redshift uncertainties, intrinsic alignments and other systematics or nuisance parameters of our model. Instead of using a simple geometric approach for the ratios as has been done in the past, we use the full modeling of the galaxy-galaxy lensing measurements, including the corresponding integration over the power spectrum and the contributions from intrinsic alignments and lens magnification. We perform extensive testing of the small-scale shear-ratio (SR) modeling by studying the impact of different effects such as the inclusion of baryonic physics, nonlinear biasing, halo occupation distribution descriptions and lens magnification, among others, and using realistic N-body simulations of the DES data. We validate the robustness of our constraints in the data by using two independent lens samples with different galaxy properties, and by deriving constraints using the corresponding large-scale ratios for which the modeling is simpler. The results applied to the DES Y3 data demonstrate how the ratios provide significant improvements in constraining power for several nuisance parameters in our model, especially on source redshift calibration and intrinsic alignments. For source redshifts, SR improves the constraints from the prior by up to 38% in some redshift bins. Such improvements, and especially the constraints it provides on intrinsic alignments, translate to tighter cosmological constraints when shear ratios are combined with cosmic shear and other 2pt functions. In particular, for the DES Y3 data, SR improves S8 constraints from cosmic shear by up to 31%, and for the full combination of probes (3×2pt) by up to 10%. The shear ratios presented in this work are used as an additional likelihood for cosmic shear, 2×2pt and the full 3×2pt in the fiducial DES Y3 cosmological analysis., C. S. is supported by Grant No. AST-1615555 from the U.S. National Science Foundation, and Grant No. DESC0007901 from the U.S. Department of Energy (DOE). J. P. is supported by DOE Grant No. DE-SC0021429. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at UrbanaChampaign, 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 Ci`encies de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State UniverFIG. 16. Correlation matrix for the lensing ratios, on the left panel using the REDMAGIC lens sample and on the right panel using the MAGLIM sample. sity, 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 Grants No. AST1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV2012-0234, No. SEV-2016-0597, and No. MDM-20150509, 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 Grants Agreement No. 240672, No. 291329, and No. 306478.
Published: 2021
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15. Dark Energy Survey Year 3 Results: Galaxy clustering and systematics treatment for lens galaxy samples

Author: Rodriguez-Monroy M., Weaverdyck N., Elvin-Poole J., Crocce M., Carnero Rosell A., Andrade-Oliveira F., Avila S., Bechtol K., Bernstein G. M., Blazek J., Camacho H., Cawthon R., De Vicente J., Derose J., Dodelson S., Everett S., Fang X., Ferrero I., Ferte A., Friedrich O., Gaztanaga E., Giannini G., Gruendl R. A., Hartley W. G., Herner K., Huff E. M., Jarvis M., Krause E., MacCrann N., Mena-Fernandez J., Muir J., Pandey S., Park Y., Porredon A., Prat J., Rosenfeld R., Ross A. J., Rozo E., Rykoff E. S., Sanchez E., Sanchez Cid D., Sevilla-Noarbe I., Tabbutt M., To C., Wagoner E. L., Wechsler R. H., Aguena M., Allam S., Amon A., Annis J., Bacon D., Baxter E., Bertin E., Bhargava S., Brooks D., Burke D. L., Carrasco Kind M., Carretero J., Castander F. J., Choi A., Conselice C., Costanzi M., Da Costa L. N., Pereira M. E. S., Desai S., Diehl H. T., Flaugher B., Fosalba P., Frieman J., Garcia-Bellido J., Giannantonio T., Gruen D., Gschwend J., Gutierrez G., Hinton S. R., Hollowood D. L., Honscheid K., Huterer D., Jain B., James D. J., Kuehn K., Kuropatkin N., Lima M., Maia M. A. G., March M., Marshall J. L., Melchior P., Menanteau F., Miller C. J., Miquel R., Mohr J. J., Morgan R., Palmese A., Paz-Chinchon F., Pieres A., Plazas Malagon A. A., Roodman A., Scarpine V., Serrano S., Smith M., Soares-Santos M., Suchyta E., Tarle G., Thomas D., Varga T. N., UAM. Departamento de Física Teórica, National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Research Council, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Educación y Ciencia (España), National Aeronautics and Space Administration (US), Generalitat de Catalunya, Medioambientales y Tecnologicas (CIEMAT), University of Michigan, The Ohio State University, Institut d'Estudis Espacials de Catalunya (IEEC), S/n, Instituto de Astrofisica de Canarias, Laboratorio Interinstitucional de E-Astronomia-LIneA, Dpto. Astrofísica, Universidade Estadual Paulista (UNESP), Universidad Autonoma de Madrid, University of WisconsinMadison, University of Pennsylvania, Northeastern University, Observatoire de Sauverny, Lawrence Berkeley National Laboratory, Carnegie Mellon University, Santa Cruz Institute for Particle Physics, University of Arizona, University of Oslo, California Institute of Technology, University of Cambridge, The Barcelona Institute of Science and Technology, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, University of Geneva, Fermi National Accelerator Laboratory, Stanford University, The University of Tokyo, University of Chicago, Slac National Accelerator Laboratory, 382 Via Pueblo Mall, University of Portsmouth, University of Hawai'i, Institut d'Astrophysique de Paris, University of Sussex, University College London, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatorio Nacional, Iit Hyderabad, University of Queensland, Center for Astrophysics | Harvard &smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas A &m University, Peyton Hall, Institucio Catalana de Recerca i Estudis Avancats, Ludwig-Maximilians-Universitat, Max Planck Institute for Extraterrestrial Physics, University of Southampton, Oak Ridge National Laboratory, Ludwig-Maximilians Universitat Munchen, 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, Rodriguez-Monroy, M., Weaverdyck, N., Elvin-Poole, J., Crocce, M., Carnero Rosell, A., Andrade-Oliveira, F., Avila, S., Bechtol, K., Bernstein, G. M., Blazek, J., Camacho, H., Cawthon, R., De Vicente, J., Derose, J., Dodelson, S., Everett, S., Fang, X., Ferrero, I., Ferte, A., Friedrich, O., Gaztanaga, E., Giannini, G., Gruendl, R. A., Hartley, W. G., Herner, K., Huff, E. M., Jarvis, M., Krause, E., Maccrann, N., Mena-Fernandez, J., Muir, J., Pandey, S., Park, Y., Porredon, A., Prat, J., Rosenfeld, R., Ross, A. J., Rozo, E., Rykoff, E. S., Sanchez, E., Sanchez Cid, D., Sevilla-Noarbe, I., Tabbutt, M., To, C., Wagoner, E. L., Wechsler, R. H., Aguena, M., Allam, S., Amon, A., Annis, J., Bacon, D., Baxter, E., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Giannantonio, T., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Jain, B., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morgan, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A. A., Roodman, A., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., and Varga, T. N.
Subjects: Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, observation [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, power spectrum, 01 natural sciences, Observations [Cosmology], Cosmological parameters, Cosmology: observations, Dark energy, Large-scale structure of the Universe, mitigation, 0103 physical sciences, emission, scale structure catalogs, cosmological parameters, dark energy, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, redshift, uncertainties, Dark Energy, Space and Planetary Science, cosmology: observations, Cosmological Parameters, large-scale structure of the universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], constraints, Large-Scale Structure of the Universe, cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: M. Rodríguez-Monroy, N. Weaverdyck, J. Elvin-Poole et al., In this work, we present the galaxy clustering measurements of the two DES lens galaxy samples: a magnitude-limited sample optimized for the measurement of cosmological parameters, MAGLIM, and a sample of luminous red galaxies selected with the REDMAGIC algorithm. MAGLIM/REDMAGIC sample contains over 10 million/2.5 million galaxies and is divided into six/five photometric redshift bins spanning the range z ∈ [0.20, 1.05]/z ∈ [0.15, 0.90]. Both samples cover 4143 deg2 over which we perform our analysis blind, measuring the angular correlation function with an S/N ∼ 63 for both samples. In a companion paper, these measurements of galaxy clustering are combined with the correlation functions of cosmic shear and galaxy–galaxy lensing of each sample to place cosmological constraints with a 3 × 2pt analysis. We conduct a thorough study of the mitigation of systematic effects caused by the spatially varying survey properties and we correct the measurements to remove artificial clustering signals. We employ several decontamination methods with different configurations to ensure the robustness of our corrections and to determine the systematic uncertainty that needs to be considered for the final cosmology analyses. We validate our fiducial methodology using lognormal mocks, showing that our decontamination procedure induces biases no greater than 0.5σ in the (Ωm, b) plane, where b is the galaxy bias., Funding for the Dark Energy Survey 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. This paper is 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 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.
Published: 2021
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16. Validation of selection function, sample contamination and mass calibration in galaxy cluster samples

Author: Grandis, S., Klein, M., Mohr, J. J., Bocquet, S., Paulus, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Benson, B. A., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Capasso, R., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sheldon, E., Smith, M., Stark, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., 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, Grandis, S., Klein, M., Mohr, J. J., Bocquet, S., Paulus, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Benson, B. A., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Capasso, R., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Serrano, S., Sheldon, E., Smith, M., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R., National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, and European Research Council
Subjects: Software_OPERATINGSYSTEMS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), ComputingMethodologies_SIMULATIONANDMODELING, Calibration (statistics), statistical [methods], RAIOS X, FOS: Physical sciences, Sample (statistics), Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, methods: statistical, galaxies: clusters: general, large-scale structure of Universe, X-rays: galaxies: clusters, Astrophysics - Cosmology and Nongalactic Astrophysics, Hardware_INTEGRATEDCIRCUITS, clusters: general [galaxies], Limit (mathematics), Statistical physics, 010303 astronomy & astrophysics, Selection (genetic algorithm), Galaxy cluster, STFC, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Astronomy and Astrophysics, Function (mathematics), ComputerSystemsOrganization_PROCESSORARCHITECTURES, galaxies: cluster [X-rays], South Pole Telescope, Space and Planetary Science, Outlier, galaxies: clusters [X-rays], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: DES Collaboration: et al., We construct and validate the selection function of the MARD-Y3 galaxy cluster sample. This sample was selected through optical follow-up of the 2nd ROSAT faint source catalogue with Dark Energy Survey year 3 data. The selection function is modelled by combining an empirically constructed X-ray selection function with an incompleteness model for the optical follow-up. We validate the joint selection function by testing the consistency of the constraints on the X-ray flux–mass and richness–mass scaling relation parameters derived from different sources of mass information: (1) cross-calibration using South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) clusters, (2) calibration using number counts in X-ray, in optical and in both X-ray and optical while marginalizing over cosmological parameters, and (3) other published analyses. We find that the constraints on the scaling relation from the number counts and SPT-SZ cross-calibration agree, indicating that our modelling of the selection function is adequate. Furthermore, we apply a largely cosmology independent method to validate selection functions via the computation of the probability of finding each cluster in the SPT-SZ sample in the MARD-Y3 sample and vice versa. This test reveals no clear evidence for MARD-Y3 contamination, SPT-SZ incompleteness or outlier fraction. Finally, we discuss the prospects of the techniques presented here to limit systematic selection effects in future cluster cosmological studies., 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 Programme (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 465376/2014-2).
Published: 2020

17. Noise from undetected sources in Dark Energy Survey images

Author: Eckert, K., Bernstein, G. M., Amara, A., Amon, A., Choi, A., Everett, S., Gruen, D., Gruendl, R. A., Huff, E. M., Kuropatkin, N., Roodman, A., Sheldon, E., Yanny, B., Zhang, Y., Abbott, T. M. C., Aguena, M., Avila, S., Bechtol, K., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Eifler, T. F., Evrard, A. E., Flaugher, B., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kron, R., Kuehn, K., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinch��n, 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., Thomas, D., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Zuntz, J., Collaboration, the 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, Eckert, K., Bernstein, G. M., Amara, A., Amon, A., Choi, A., Everett, S., Gruen, D., Gruendl, R. A., Huff, E. M., Kuropatkin, N., Roodman, A., Sheldon, E., Yanny, B., Zhang, Y., Abbott, T. M. C., Aguena, M., Avila, S., Bechtol, K., Brooks, D., 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., Dietrich, J. P., Eifler, T. F., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kron, R., Kuehn, K., Maia, M. A. G., 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., 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., Wester, W., Wilkinson, R. D., Zuntz, J., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Diffuse radiation, weak, techniques: image processing, diffuse radiation [gravitational lensing], media_common.quotation_subject, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Poisson distribution, 7. Clean energy, 01 natural sciences, symbols.namesake, weak [gravitational lensing], 0103 physical sciences, Image noise, gravitational lensing: weak, techniques: image processing, diffuse radiation, education, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Weak gravitational lensing, STFC, media_common, Physics, education.field_of_study, image processing [techniques], 010308 nuclear & particles physics, Gravitational lensing: Weak, Shot noise, RCUK, Astronomy and Astrophysics, Techniques: Image processing, Galaxy, diffuse radiation, 13. Climate action, Space and Planetary Science, Sky, symbols, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract: For ground-based optical imaging with current CCD technology, the Poisson fluctuations in source and sky background photon arrivals dominate the noise budget and are readily estimated. Another component of noise, however, is the signal from the undetected population of stars and galaxies. Using injection of artifical galaxies into images, we demonstrate that the measured variance of galaxy moments (used for weak gravitational lensing measurements) in Dark Energy Survey (DES) images is significantly in excess of the Poisson predictions, by up to 30 per cent, and that the background sky levels are overestimated by current software. By cross-correlating distinct images of 'empty' sky regions, we establish that there is a significant image noise contribution from undetected static sources (US), which, on average, are mildly resolved at DES resolution. Treating these US as a stationary noise source, we compute a correction to the moment covariance matrix expected from Poisson noise. The corrected covariance matrix matches the moment variances measured on the injected DES images to within 5 per cent. Thus, we have an empirical method to statistically account for US in weak lensing measurements, rather than requiring extremely deep sky simulations. We also find that local sky determinations can remove most of the bias in flux measurements, at a small penalty in additional, but quantifiable, noise., KDE and GMB acknowledge support from NASA through a Research Support Agreement with grant 12-EUCLID11-0004, and grants AST-1615555 from the US National Science Foundation, and DE-SC0007901 from the US Department of Energy. Funding for the DES Projects has been provided by the US 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 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).
Published: 2020

18. Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis

Author: Ferrero, I., Crocce, M., Tutusaus, I., Porredon, A., Blot, L., Fosalba, P., Rosell, A. Carnero, Avila, S., Izard, A., Elvin-Poole, J., Chan, K. C., Camacho, H., Rosenfeld, R., Sanchez, E., Tallada-Crespí, P., Carretero, J., Sevilla-Noarbe, I., Gaztanaga, E., Andrade-Oliveira, F., De Vicente, J., Mena-Fernández, J., Ross, A. J., Cid, D. Sanchez, Ferté, A., Brandao-Souza, A., Fang, X., Krause, E., Gomes, D., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Kind, M. Carrasco, Castander, F. J., Cawthon, R., Choi, A., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Percival, W. J., Malagón, A. A. Plazas, Rodriguez-Monroy, M., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Ferrero, I., Crocce, M., Tutusaus, I., Porredon, A., Blot, L., Fosalba, P., Carnero Rosell, A., Avila, S., Izard, A., Elvin-Poole, J., Chan, K. C., Camacho, H., Rosenfeld, R., Sanchez, E., Tallada-Crespi, P., Carretero, J., Sevilla-Noarbe, I., Gaztanaga, E., Andrade-Oliveira, F., De Vicente, J., Mena-Fernandez, J., Ross, A. J., Sanchez Cid, D., Ferte, A., Brandao-Souza, A., Fang, X., Krause, E., Gomes, D., Aguena, M., Allam, S., Annis, J., Bertin, E., Brooks, D., Carrasco Kind, M., Castander, F. J., Cawthon, R., Choi, A., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Flaugher, B., 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., Hoyle, B., Huterer, D., James, D. J., Kuehn, K., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Percival, W. J., Plazas Malagon, A. A., Rodriguez-Monroy, M., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), The Ohio State University, Max-Planck-Institut für Astrophysik, Instituto de Astrofisica de Canarias, Laboratório Interinstitucional de e-Astronomia - LIneA, Dpto. Astrofísica, Universidad Autonoma de Madrid, University of Portsmouth, Sun Yat-sen University, Universidade Estadual Paulista (UNESP), ICTP South American Institute for Fundamental Research, Medioambientales y Tecnológicas (CIEMAT), Port d'Informació Científica (PIC), The Barcelona Institute of Science and Technology, California Institute of Technology, Universidade Estadual de Campinas (UNICAMP), University of Arizona, Universidade de São Paulo (USP), Rua General José Cristino, Fermi National Accelerator Laboratory, Institut d'Astrophysique de Paris, University College London, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, 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, University of Chicago, Santa Cruz Institute for Particle Physics, Stanford University, SLAC National Accelerator Laboratory, University of Queensland, Ludwig-Maximilians-Universität, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, University of Waterloo, Perimeter Institute for Theoretical Physics, Princeton University, University of Southampton, Oak Ridge National Laboratory, Giessenbachstrasse, and Ludwig-Maximilians Universität München
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Halo occupation distribution, Galaxies: distances and redshifts, Observational cosmology, distances and redshifts [Galaxies], halo [Galaxy], Catalogs, Galaxy: halo, Methods: numerical, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, numerical [Methods], Computer Science::Information Retrieval, distances and redshift [Galaxies], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Redshift survey, Redshift, Galaxy, Space and Planetary Science, Dark energy, Catalog, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Ferrero, I., et al. (DES Collaboration), The calibration and validation of scientific analysis in simulations is a fundamental tool to ensure unbiased and robust results in observational cosmology. In particular, mock galaxy catalogs are a crucial resource to achieve these goals in the measurement of baryon acoustic oscillation (BAO) in the clustering of galaxies. Here we present a set of 1952 galaxy mock catalogs designed to mimic the Dark Energy Survey Year 3 BAO sample over its full photometric redshift range 0:6 < zphoto < 1:1. The mocks are based upon 488 ICE-COLA fast N-body simulations of full-sky light cones and were created by populating halos with galaxies, using a hybrid halo occupation distribution halo abundance matching model. This model has ten free parameters, which were determined, for the first time, using an automatic likelihood minimization procedure.We also introduced a novel technique to assign photometric redshift for simulated galaxies, following a two-dimensional probability distribution with VIMOS Public Extragalactic Redshift Survey data. The calibration was designed to match the observed abundance of galaxies as a function of photometric redshift, the distribution of photometric redshift errors, and the clustering amplitude on scales smaller than those used for BAO measurements. An exhaustive analysis was done to ensure that the mocks reproduce the input properties. Finally, mocks were tested by comparing the angular correlation function w(θ), angular power spectrum ζp(rΓ) and projected clustering p(r?) to theoretical predictions and data. The impact of volume replication in the estimate of the covariance is also investigated. The success in accurately reproducing the photometric redshift uncertainties and the galaxy clustering as a function of redshift render this mock creation pipeline as a benchmark for future analyses of photometric galaxy surveys.
Published: 2021

19. DES Y3 results: Blending shear and redshift biases in image simulations

Author: 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., S��nchez, 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., Crocce, M., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Ferrero, I., Fert��, A., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-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-Chinch��n, 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., 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::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: As the statistical power of galaxy weak lensing reaches percent 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, $n_{\gamma}(z)$, 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 dataset. We describe the multi-band, 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 $-2\%$. By generating simulations with input shear signals that vary with redshift, we calibrate biases in our estimation of the effective redshfit 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., Comment: Submitted to MNRAS. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release. Version accepted by mnras
Published: 2021

20. Cross-correlation of DES Y3 lensing and ACT/${\it Planck}$ thermal Sunyaev Zel'dovich Effect I: Measurements, systematics tests, and feedback model constraints

Author: Gatti, M., Pandey, S., Baxter, E., Hill, J. C., Moser, E., Raveri, M., Fang, X., DeRose, J., Giannini, G., Doux, C., Huang, H., Battaglia, N., Alarcon, A., Amon, A., Becker, M., Campos, A., Chang, C., Chen, R., Choi, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Harrison, I., Maccrann, N., Mccullough, J., Myles, J., Alsina, A. Navarro, Prat, J., Rollins, R. P., Sanchez, C., Shin, T., Troxel, M., Tutusaus, I., Yin, B., Abbott, T., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bernstein, G., Bertin, E., Bolliet, B., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cawthon, R., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. da Silva, DeVicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Dunkley, J., Evrard, A. E., Ferraro, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcıa-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Herner, K., Hincks, A. D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, J. P., Huterer, D., Jain, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lokken, M., Madhavacheril, M. S., Maia, M. A. G., Marshall, J. L., Mcmahon, J. J., Melchior, P., Moodley, K., Mohr, J. J., Morgan, R., Nati, F., Niemack, M. D., Page, L., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Schaan, E., Secco, L. F., Serrano, S., Sheldon, E., Sherwin, B. D., Sifon, C., Smith, M., Soares-Santos, M., Spergel, D., Suchyta, E., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., Wollack, E. J., and Xu, Z.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a tomographic measurement of the cross-correlation between thermal Sunyaev-Zeldovich (tSZ) maps from ${\it Planck}$ and the Atacama Cosmology Telescope (ACT) and weak galaxy lensing shears measured during the first three years of observations of the Dark Energy Survey (DES Y3). This correlation is sensitive to the thermal energy in baryons over a wide redshift range, and is therefore a powerful probe of astrophysical feedback. We detect the correlation at a statistical significance of $21\sigma$, the highest significance to date. We examine the tSZ maps for potential contaminants, including cosmic infrared background (CIB) and radio sources, finding that CIB has a substantial impact on our measurements and must be taken into account in our analysis. We use the cross-correlation measurements to test different feedback models. In particular, we model the tSZ using several different pressure profile models calibrated against hydrodynamical simulations. Our analysis marginalises over redshift uncertainties, shear calibration biases, and intrinsic alignment effects. We also marginalise over $\Omega_{\rm m}$ and $\sigma_8$ using ${\it Planck}$ or DES priors. We find that the data prefers the model with a low amplitude of the pressure profile at small scales, compatible with a scenario with strong AGN feedback and ejection of gas from the inner part of the halos. When using a more flexible model for the shear profile, constraints are weaker, and the data cannot discriminate between different baryonic prescriptions., Comment: submitted to PRD
Published: 2021
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21. First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary-Black-hole Merger GW170814

Author: Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D. E, Lin, H, Pereira, M. E. S, Garcia, A, Herner, K, Kessler, R, Peiris, V, H, Sako, M, Allam, S, Brout, D, Carnero Rosell, A, Chen, H. Y, Conselice, C, Derose, J, Devicente, J, Diehl, H. T, Gill, M. S. S, Gschwend, J, Sevilla-Noarbe, I and Tucker, D. L., Wechsler, R, Berger, E, Cowperthwaite, P. S, Metzger, B. D, Williams, P. K. G, Abbott, T. M. C, Abdalla, F. B, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D. L, Kind, Carrasco and Carretero, M., J, Castander, F. J, Crocce, M, Cunha, C. E, D'Andrea, C. B, da Costa, L. N, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, T. F, Evrard, A. E, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, D. W, Gruen, D, Gruendl, R. A, Gutierrez, G, Hollowood, D. L, Hoyle, B, James, D. J, Jeltema, T, Kuehn, K, Kuropatkin, N, T. S, Li, Lima, M, Maia, M. A. G, Marshall, J. L, Menanteau, F, Miquel, R, Neilsen, E, Ogando, R. L. C, Plazas, A. A, Romer, A. K, Roodman, A, Sanchez, E, Scarpine, V and Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, R. C, Sobreira, F, Suchyta, E, Swanson, M. E. C, Tarle, G, Thomas, R. C, Walker, A. R, Wester, W, Zuntz, J, Abbott, B. P, Abbott, R, Abbott, T. D, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R. X, Adya, V. B, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O. D, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M. A, Altin, P. A, Amato, A, Ananyeva, A, Anderson, S. B, Anderson, W. G, Angelova, S, Appert, S, Arai, K, Araya, M. C, Areeda, J. S, Arene, M, Ascenzi, S, Ashton, G, Aston, S. M, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V and Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M. K. M, Bae, S, Baker, P. T, Baldaccini, F, Ballardin, G, Ballmer, S. W, Banagiri, S, Barayoga, J. C, Barclay, S. E, Barish, B. C, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I and Bassiri, Basti, A, Bawaj, M, Bayley, J. C, Bazzan, M, Becsy, B, Bejger, M, Bell, A. S, Beniwal, D, Bergmann, G, Bernuzzi, S, Bero, J. J, Berry, C. P. L, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I. A, Bilgili, S. A, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Blackburn, J. K, Blair, C. D, Blair, D. G, Blair, R. M, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B. A, Booth, C. D, Bork, R, Boschi, V and Bose, Bossie, K, Bossilkov, V and Bosveld, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P. R, Bramley, A, Branchesi, M, Brau, J. E, Briant, T, Briggs, J. H, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A. F, Brown, D. D, Brunett, S, Buikema, A, Bulik, T, Bulten, H. J, Buonanno, A, Buskulic, D, Buy, C, Byer, R. L, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, Calderon and Callister, J., T. A., Calloni, E, Camp, J. B, Campbell, W. A, Cannon, K. C, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M. F, Carullo, G, Diaz, Casanueva and Casentini, J., C, Caudill, S, Cavaglia, M, Cavalieri, R, Cella, G, Cerda-Duran, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S. J, Chan, M, Chao, S, Charlton, P, Chase, E. A, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chatziioannou, K, Cheeseboro, B. D, Chen, X, Chen, Y, Cheng, H-P and Cheong, C. K., Chia, H. Y, Chincarini, A, Chiummo, A, Cho, G, Cho, H. S, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K. W, Chung, S, Ciani, G, Ciobanu, A. A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J. A, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Colgan, R, Colleoni, M, Collette, C. G, Collins, C, Cominsky, L. R, Constancio Jr, M, Conti, L, Cooper, S. 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L, Doravari, S, Dorrington, I and Downes, T. P., Drago, M, Driggers, J. C, Du, Z, Dupej, P, Dwyer, S. E, Easter, P. J, Edo, T. B, Edwards, M. C, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S. S, Eisenmann, M, Eisenstein, R. A, Estelles, H, Estevez, D, Etienne, Z. B, Etzel, T, Evans, M, Evans, T. M, Fafone, V and Fair, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W. M, Fauchon-Jones, E. J, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M. M, Feng, F, Fernandez-Galiana, A, Ferrante, I and Ferreira, E. C., Ferreira, T. A, Ferrini, F, Fidecaro, F, Fiori, I and Fiorucci, Fisher, R. P, Fishner, J. M, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Fournier, J-D and Font, J. A., Forsyth, P. W. F, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V. V, Fulda, P, Fyffe, M, Gabbard, H. A, Gadre, B. U, Gaebel, S. M, Gair, J. R, Gammaitoni, L, Ganija, M. R, Gaonkar, S. 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A, Khursheed, M, Kijbunchoo, N, Kim, Chunglee and Kim, J. C., Kim, K, Y-M and Kim, W, Kim, W. S, Kimball, C, King, E. J, King, P. J, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J. S, Kleybolte, L, Klika, J. H, Klimenko, S, Knowles, T. D, Koch, P, Koehlenbeck, S. M, Koekoek, G, Koley, S, Kondrashov, V and Kontos, Koper, N, Korobko, M, Korth, W. Z, Kowalska, I and Kozak, D. B., Kringel, V and Krishnendu, Krolak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B. D, Lai, K. H, Lam, T. L, Landry, M, Lane, B. B, Lang, R. N, Lange, J, Lantz, B, Lanza, R. K, Lasky, P. D, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y. K, Lee, C. H, Lee, H. K, Lee, H. M, Lee, H. W, Lee, J, Lee, K, Lehmann, J, Lenon, A, Letendre, N, Levin, Y, Li, J, K. J. L, Li, T. G. F, Li, Li, X, Lin, F, Linde, F, Linker, S. D, Littenberg, T. B, Liu, J, Liu, X, R. K. L, Lo, Lockerbie, N. A, London, L. 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(UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire Kastler Brossel (LKB [Collège de France]), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Collège de France (CdF)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon, ESPCI ParisTech, DES, LIGO Scientific, Virgo, Van Swinderen Institute for Particle Physics and G, Soares-Santos, M, Palmese, A, Hartley, W, Annis, J, Garcia-Bellido, J, Lahav, O, Doctor, Z, Fishbach, M, Holz, D, Lin, H, Pereira, M, Garcia, A, Herner, K, Kessler, R, Peiris, H, Sako, M, Allam, S, Brout, D, Rosell, A, Chen, H, Conselice, C, Derose, J, Devicente, J, Diehl, H, Gill, M, Gschwend, J, Sevilla-Noarbe, I, Tucker, D, Wechsler, R, Berger, E, Cowperthwaite, P, Metzger, B, Williams, P, Abbott, T, Abdalla, F, Avila, S, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, D, Kind, M, Carretero, J, Castander, F, Crocce, M, Cunha, C, D’Andrea, C, Costa, L, Davis, C, Desai, S, Doel, P, Drlica-Wagner, A, Eifler, T, Evrard, A, Flaugher, B, Fosalba, P, Frieman, J, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Hollowood, D, Hoyle, B, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Li, T, Lima, M, Maia, M, Marshall, J, Menanteau, F, Miquel, R, Neilsen, E, Ogando, R, Plazas, A, Romer, A, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Smith, M, Smith, R, Sobreira, F, Suchyta, E, Swanson, M, Tarle, G, Thomas, R, Walker, A, Wester, W, Zuntz, J, Abbott, B, Abbott, R, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R, Adya, V, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M, Altin, P, Amato, A, Ananyeva, A, Anderson, S, Anderson, W, Angelova, S, Appert, S, Arai, K, Araya, M, Areeda, J, Arène, M, Ascenzi, S, Ashton, G, Aston, S, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M, Bae, S, Baker, P, Baldaccini, F, Ballardin, G, Ballmer, S, Banagiri, S, Barayoga, J, Barclay, S, Barish, B, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Bazzan, M, Bécsy, B, Bejger, M, Bell, A, Beniwal, D, Bergmann, G, Bernuzzi, S, Bero, J, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, I, Bilgili, S, Billingsley, G, Birch, J, Birney, R, Birnholtz, O, Biscans, S, Biscoveanu, S, Bisht, A, Bitossi, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bloemen, S, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Booth, C, Bork, R, Boschi, V, Bose, S, Bossie, K, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branchesi, M, Brau, J, Briant, T, Briggs, J, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brown, D, Brunett, S, Buikema, A, Bulik, T, Bulten, H, Buonanno, A, Buskulic, D, Buy, C, Byer, R, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callister, T, Calloni, E, Camp, J, Campbell, W, Cannon, K, Cao, H, Cao, J, Capocasa, E, Carbognani, F, Caride, S, Carney, M, Carullo, G, Diaz, J, Casentini, C, Caudill, S, Cavaglià, M, Cavalieri, R, Cella, G, Cerdá-Durán, P, Cerretani, G, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S, Chan, M, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Chatziioannou, K, Cheeseboro, B, Chen, X, Chen, Y, Cheng, H, Cheong, C, Chia, H, Chincarini, A, Chiummo, A, Cho, G, Cho, H, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K, Chung, S, Ciani, G, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J, Clearwater, P, Cleva, F, Cocchieri, C, Coccia, E, Cohadon, P, Colgan, R, Colleoni, M, Collette, C, Collins, C, Cominsky, L, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrión, I, Corley, K, Cornish, N, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Couvares, P, Covas, P, Cowan, E, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Cripe, J, Croquette, M, Crowder, S, Cullen, T, Cumming, A, Cunningham, L, Cuoco, E, Canton, T, Dálya, G, Danilishin, S, D’Antonio, S, Danzmann, K, Dasgupta, A, Datrier, L, Dattilo, V, Dave, I, Davis, D, Daw, E, Debra, D, Deenadayalan, M, Degallaix, J, Laurentis, M, Deléglise, S, Pozzo, W, Demarchi, L, Demos, N, Dent, T, Pietri, R, Derby, J, Rosa, R, Rossi, C, Desalvo, R, Varona, O, Dhurandhar, S, Díaz, M, Dietrich, T, Fiore, L, Giovanni, M, Girolamo, T, Lieto, A, Ding, B, Pace, S, Palma, I, Renzo, F, Dmitriev, A, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Downes, T, Drago, M, Driggers, J, Du, Z, Dupej, P, Dwyer, S, Easter, P, Edo, T, Edwards, M, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M, Feng, F, Fernandez-Galiana, A, Ferrante, I, Ferreira, E, Ferreira, T, Ferrini, F, Fidecaro, F, Fiori, I, Fiorucci, D, Fisher, R, Fishner, J, Fitz-Axen, M, Flaminio, R, Fletcher, M, Flynn, E, Fong, H, Font, J, Forsyth, P, Fournier, J, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Gammaitoni, L, Ganija, M, Gaonkar, S, García-Quirós, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V, Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Germain, V, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giaime, J, Giardina, K, Giazotto, A, Gill, K, Giordano, G, Glover, L, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, González, G, Castro, J, Gopakumar, A, Gorodetsky, M, Gossan, S, Gosselin, M, Gouaty, R, Grado, A, Graef, C, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, E, Groot, P, Grote, H, Grunewald, S, Guidi, G, Gulati, H, Guo, Y, Gupta, A, Gupta, M, Gustafson, E, Gustafson, R, Haegel, L, Halim, O, Hall, B, Hall, E, Hamilton, E, Hammond, G, Haney, M, Hanke, M, Hanks, J, Hanna, C, Hannuksela, O, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Haster, C, Haughian, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heitmann, H, Hemming, G, Hendry, M, Heng, I, Hennig, J, Heptonstall, A, Vivanco, F, Heurs, M, Hild, S, Hinderer, T, Hoak, D, Hochheim, S, Hofman, D, Holgado, A, Holland, N, Holt, K, Hopkins, P, Horst, C, Hough, J, Howell, E, Hoy, C, Hreibi, A, Huerta, E, Hughey, B, Hulko, M, Husa, S, Huttner, S, Huynh-Dinh, T, Idzkowski, B, Iess, A, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, H, Isac, J, Isi, M, Iyer, B, Izumi, K, Jacqmin, T, Jadhav, S, Jani, K, Janthalur, N, Jaranowski, P, Jenkins, A, Jiang, J, Johnson, D, Jones, A, Jones, D, Jones, R, Jonker, R, Ju, L, Junker, J, Kalaghatgi, C, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, J, Kapadia, S, Karki, S, Karvinen, K, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kéfélian, F, Keitel, D, Kennedy, R, Key, J, Khalili, F, Khan, H, Khan, I, Khan, S, Khan, Z, Khazanov, E, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, King, E, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klika, J, Klimenko, S, Knowles, T, Koch, P, Koehlenbeck, S, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, W, Kowalska, I, Kozak, D, Kringel, V, Krishnendu, N, Królak, A, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kumar, S, Kuo, L, Kutynia, A, Kwang, S, Lackey, B, Lai, K, Lam, T, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, Lanza, R, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, C, Lee, H, Lee, J, Lee, K, Lehmann, J, Lenon, A, Letendre, N, Levin, Y, Li, J, Li, K, Li, X, Lin, F, Linde, F, Linker, S, Littenberg, T, Liu, J, Liu, X, Lo, R, Lockerbie, N, London, L, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Lower, M, Lück, H, Lumaca, D, Lundgren, A, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D, Macquet, A, Hernandez, I, Magaña-Sandoval, F, Zertuche, L, Magee, R, Majorana, E, Maksimovic, I, Malik, A, Man, N, Mandic, V, Mangano, V, Mansell, G, Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Márka, S, Márka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martynov, D, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Matone, L, Mavalvala, N, Mazumder, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mccormick, S, Mcculler, L, Mcguire, S, Mciver, J, Mcmanus, D, Mcrae, T, Mcwilliams, S, Meacher, D, Meadors, G, Mehmet, M, Mehta, A, Meidam, J, Melatos, A, Mendell, G, Mercer, R, Mereni, L, Merilh, E, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Metzdorff, R, Meyers, P, Miao, H, Michel, C, Middleton, H, Mikhailov, E, Milano, L, Miller, A, Millhouse, M, Mills, J, Milovich-Goff, M, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Mo, G, Moffa, D, Mogushi, K, Mohapatra, S, Montani, M, Moore, C, 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K, Piccinni, O, Pichot, M, Piergiovanni, F, Pillant, G, Pinard, L, Pirello, M, Pitkin, M, Poggiani, R, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Prajapati, A, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Privitera, S, Prodi, G, Prokhorov, L, Puncken, O, Punturo, M, Puppo, P, Pürrer, M, Qi, H, Quetschke, V, Quinonez, P, Quintero, E, Quitzow-James, R, Radkins, H, Radulescu, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D, Ren, W, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riles, K, Rizzo, M, Robertson, N, Robie, R, Rocchi, A, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, R, Romel, C, Romie, J, Rose, K, Rosińska, D, Rosofsky, S, Ross, M, Rowan, S, Rüdiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, L, 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Summerscales, T, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Swinkels, B, Szczepańczyk, M, Tacca, M, Tait, S, Talbot, C, Talukder, D, Tanner, D, Tápai, M, Taracchini, A, Tasson, J, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forné, A, Torrie, C, Töyrä, D, Travasso, F, Traylor, G, Tringali, M, Trovato, A, Trozzo, L, Trudeau, R, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, J, Broeck, C, Vander-Hyde, D, van Heijningen, J, van der Schaaf, L, van Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasúth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Viceré, A, Viets, A, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, 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Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), ITA, USA, GBR, FRA, DEU, ESP, RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, Soares-Santos, M., Palmese, A., Hartley, W., Annis, J., Garcia-Bellido, J., Lahav, O., Doctor, Z., Fishbach, M., Holz, D. E., Lin, H., Pereira, M. E. S., Garcia, A., Herner, K., Kessler, R., Peiris, H. V., Sako, M., Allam, S., Brout, D., Rosell, A. Carnero, Chen, H. Y., Conselice, C., Derose, J., Devicente, J., Diehl, H. T., Gill, M. S. S., Gschwend, J., Sevilla-Noarbe, I., Tucker, D. L., Wechsler, R., Berger, E., Cowperthwaite, P. S., Metzger, B. D., Williams, P. K. G., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D’Andrea, C. B., Costa, L. N. da, Davis, C., Desai, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Romer, A. 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De, Desalvo, R., Varona, O. de, Dhurandhar, S., Díaz, M. C., Dietrich, T., Fiore, L. Di, Giovanni, M. Di, Di Girolamo, T., Lieto, A. Di, Ding, B., Pace, S. Di, Palma, I. Di, Renzo, F. Di, Dmitriev, A., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. 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S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O’Brien, B. D., O’Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O’Reilly, B., Ormiston, R. G., Ortega, L. F., O’Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, K., Rosińska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Santiago, K. A., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Shao, L., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shyamsundar, S., Siellez, K., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tápai, M., Taracchini, A., Tasson, J. D., Taylor, R., Thies, F., Thomas, M., Thomas, P., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Tringali, M. C., Trovato, A., Trozzo, L., Trudeau, R., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., Broeck, C. Van Den, Vander-Hyde, D. C., van Heijningen, J. V., van der Schaaf, L., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Viceré, A., Viets, A. D., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Weßels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Yvert, M., Zadrożny, A. K., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A., Zucker, M. E., Zweizig, J., Centre National de la Recherche Scientifique (CNRS)-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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution))
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, cosmic background radiation, 01 natural sciences, black hole, LIGO, dark energy, 010303 astronomy & astrophysics, gravitational wave, QC, Photometric redshift, QB, Physics, Settore FIS/01, Hubble constant, CATALOG, observations [cosmology], gravitational waves, Physical Sciences, symbols, astro-ph.CO, STELLAR MASS, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, AST-1138766, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, gravitational radiation: direct detection, electromagnetic field: production, symbols.namesake, SDG 17 - Partnerships for the Goals, Binary black hole, statistical analysis, surveys, 0103 physical sciences, supernova, AST-1536171, Luminosity distance, STFC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, ONDAS GRAVITACIONAIS, Science & Technology, catalogs, cosmology: observations, gravitational radiation, RCUK, Astronomy and Astrophysics, redshift, Galaxy, Redshift, gravitational radiation detector, VIRGO, Physics and Astronomy, black hole: binary, RESOLUTION, Space and Planetary Science, gravitational radiation: emission, Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract: We present a multi-messenger measurement of the Hubble constant H_0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the LIGO/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black-hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black-hole merger. Our analysis results in $H_0 = 75.2^{+39.5}_{-32.4}~{\rm km~s^{-1}~Mpc^{-1}}$, which is consistent with both SN Ia and CMB measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20,140] ${\rm km~s^{-1}~Mpc^{-1}}$, and it depends on the assumed prior range. If we take a broader prior of [10,220] ${\rm km~s^{-1}~Mpc^{-1}}$, we find $H_0 = 78^{+ 96}_{-24}~{\rm km~s^{-1}~Mpc^{-1}}$ ($57\%$ of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on $H_0$., Comment: 18 pages, 2 Figures, submitted to ApJL
Published: 2019

22. Milky Way Satellite Census. III. Constraints on Dark Matter Properties from Observations of Milky Way Satellite Galaxies

Author: Nadler, E. O., Drlica-Wagner, A., Bechtol, K., Mau, S., Wechsler, R. H., Gluscevic, V., Boddy, K., Pace, A. B., Li, T. S., McNanna, M., Riley, A. H., Garc��a-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., Kind, M. Carrasco, 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-Chinch��n, 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., and Wester, W.
Subjects: High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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, $m_{\rm WDM} > 6.5\ \mathrm{keV}$ (free-streaming length, $\lambda_{\rm{fs}} \lesssim 10\,h^{-1}\ \mathrm{kpc}$), (ii) the velocity-independent DM-proton scattering cross section, $\sigma_{0} < 8.8\times 10^{-29}\ \mathrm{cm}^{2}$ for a $100\ \mathrm{MeV}$ DM particle mass (DM-proton coupling, $c_p \lesssim (0.3\ \mathrm{GeV})^{-2}$), and (iii) the mass of fuzzy DM, $m_{\phi}> 2.9 \times 10^{-21}\ \mathrm{eV}$ (de Broglie wavelength, $\lambda_{\rm{dB}} \lesssim 0.5\ \mathrm{kpc}$). These constraints are complementary to other observational and laboratory constraints on DM properties., Comment: 15 pages, 5 figures, 2 tables. Updated to published version
Published: 2020

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

Author: 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chiu, L, Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., Garcia-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-Chinchon, 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: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843 MHz radio active galactic nuclei (AGNs) population in galaxy clusters from two large catalogues created using the Dark Energy Survey (DES): similar to 11 800 optically selected RM-Y3 and similar to 1000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGNs are highly concentrated around cluster centres to z similar to 1. We measure the halo occupation number for cluster radio AGNs above a threshold luminosity, finding that the number of radio AGNs per cluster increases with cluster halo mass as N proportional to M-1(.2 +/- 0.1) (N proportional to M-0.(68 +/- 0.34)) 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 colours 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 AGNs luminosity function (LF). The LF exhibits a redshift trend of the form (1 + z)(gamma) in density and luminosity, respectively, of gamma(D) = 3.0 +/- 0.4 and gamma(P) = 0.21 +/- 0.15 in the RM-Y3 sample, and gamma(D) = 2.6 +/- 0.7 and gamma(P) = 0.31 +/- 0.15 in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGNs, 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 (
Published: 2020

24. A chemo-dynamical link between the Gj��ll stream and NGC 3201

Author: Hansen, T. T., Riley, A. H., Strigari, L. E., Marshall, J. L., Ferguson, P. S., Zepeda, J., and Sneden, C.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Recent analysis of the second data release of Gaia has revealed a number of new stellar streams surrounding the Milky Way. It has been suggested that one of these streams, Gj��ll, is associated with the globular cluster NGC 3201, but thus far the association has only been based on kinematics of the stream stars. In this work we identify five likely stream members in the Gaia data that are bright enough for high-resolution spectroscopic follow-up with the Harlan J. Smith telescope at McDonald Observatory. One star is ruled out as a member based on its radial velocity. Abundance analysis of the remaining four kinematic members reveals a good chemical match to NGC 3201 for two of the stars, driven by their similar Al and $��$-element abundances. Of the remaining two, one shows no chemical similarity to NGC 3201 and is likely an unassociated Milky Way halo field star, while the other exhibits a similar Al abundance but has somewhat lower $��$-element abundances. The chemical tagging of stars in the Gj��ll stream to NGC 3201 confirms this association and provides direct proof of the hierarchical formation of the Milky Way., 12 pages, 10 Tables and 4 Figures, Accepted for publication in ApJ
Published: 2020
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25. $��_{\star}$ Masses: Weak Lensing Calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using Stellar Masses

Author: Pereira, M. E. S., Palmese, A., Varga, T. N., McClintock, T., Soares-Santos, M., Burgad, J., Annis, J., Farahi, A., Lin, H., Choi, A., DeRose, J., Esteves, J., Gatti, M., Gruen, D., Hartley, W. G., Hoyle, B., Jeltema, T., MacCrann, N., Roodman, A., S��nchez, C., Shin, T., von der Linden, A., Zuntz, J., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Estrada, J., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinch��n, 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., Wechsler, R. H., Weller, J., and Zhang, Y.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the weak lensing mass calibration of the stellar mass based $��_{\star}$ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time we are able to perform a calibration of $��_{\star}$ at high redshifts, $z>0.33$. In a blinded analysis, we use $\sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 \leqslant z, 20 pages, 10 figures, submitted to MNRAS
Published: 2020
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26. The Host Galaxies of Rapidly Evolving Transients in the Dark Energy Survey

Author: Wiseman, P., Pursiainen, M., Childress, M., Swann, E., Smith, M., Galbany, L., Lidman, C., Davis, T. M., Gutiérrez, C. P., Möller, A., Thomas, B. P., Frohmaier, C., Foley, R. J., Hinton, S. R., Kelsey, L., Kessler, R., Lewis, G. F., Sako, M., Scolnic, D., Sullivan, M., Vincenzi, M., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sommer, N. E., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, B. E., Tucker, D. L., Varga, T. N., Walker, A. R., Wiseman, P, Pursiainen, M, Childress, M, Swann, E, Smith, M, Galbany, L, Lidman, C, M Davis, T, P Gutiérrez, C, Möller, A, P Thomas, B, Frohmaier, C, J Foley, R, R Hinton, S, Kelsey, L, Kessler, R, F Lewis, G, Sako, M, Scolnic, D, Sullivan, M, Vincenzi, M, T M, C Abbott, Aguena, M, Allam, S, Annis, J, Bertin, E, Bhargava, S, Brooks, D, L Burke, D, A Carnero Rosell, Carollo, D, M Carrasco Kind, Carretero, J, Costanzi, M, N da Costa, L, T Diehl, H, Doel, P, Everett, S, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Glazebrook, K, Gruen, D, A Gruendl, R, Gschwend, J, Gutierrez, G, L Hollowood, D, Honscheid, K, J James, D, Kuehn, K, Kuropatkin, N, Lima, M, M A, G Maia, L Marshall, J, Martini, P, Menanteau, F, Miquel, R, Palmese, A, Paz-Chinchón, F, A Plazas, A, K Romer, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, E Sommer, N, Suchyta, E, M E, C Swanson, Tarle, G, E Tucker, B, L Tucker, D, N Varga, T, and R Walker, A
Subjects: abundances – galaxies: photometry – galaxies: star formation – transients: supernovae [galaxies], endocrine system, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), galaxies: abundances – galaxies: photometry – galaxies: star formation – transients: supernovae, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: Rapidly evolving transients (RETs), also termed fast blue optical transients (FBOTs), are a distinct class of astrophysical event. They are characterised by lightcurves that decline much faster than common classes supernovae (SNe), span vast ranges in peak luminosity and can be seen to redshifts greater than 1. Their evolution on fast timescales has hindered high quality follow-up observations, and thus their origin and explosion/emission mechanism remains unexplained. In this paper we define the largest sample of RETs to date, comprising 106 objects from the Dark Energy Survey, and perform the most comprehensive analysis of RET host galaxies. Using deep-stacked photometry and emission-lines from OzDES spectroscopy, we derive stellar masses and star-formation rates (SFRs) for 49 host galaxies, and metallicities for 37. We find that RETs explode exclusively in star-forming galaxies and are thus likely associated with massive stars. Comparing RET hosts to samples of host galaxies of other explosive transients as well as field galaxies, we find that RETs prefer galaxies with high specific SFRs, indicating a link to young stellar populations, similar to stripped-envelope SNe. RET hosts appear to show a lack of chemical enrichment, their metallicities akin to long duration gamma-ray bursts and superluminous SN host galaxies. There are no clear relationships between properties of the host galaxies and the peak magnitudes or decline rates of the transients themselves., Comment: 16 pages, 15 figures, submitted to MNRAS
Published: 2020

27. Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 12 quadruply+ imaged quasars

Author: Shajib, A. J., Birrer, S., Treu, T., Auger, M. W., Agnello, A., Anguita, T., Buckley-Geer, E. J., Chan, J. H. H., Collett, T. E., Courbin, F., Fassnacht, C. D., Frieman, J., Kayo, I., Lemon, C., Lin, H., Marshall, P. J., McMahon, R., More, A., Morgan, N. D., Motta, V., Oguri, M., Ostrovski, F., Rusu, C. E., Schechter, P. L., Shanks, T., Suyu, S. H., Meylan, G., Abbott, T. M. C., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., Costa, L. N. da, Vicente, J. De, Desai, S., Doel, P., Flaugher, B., Fosalba, P., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., 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., Melchior, P., Menanteau, F., Miquel, R., Plazas, A. A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., and Walker, A. R.
Subjects: astro-ph.GA, RCUK, Astrophysics::Cosmology and Extragalactic Astrophysics, STFC
Abstract: Strong-gravitational lens systems with quadruply-imaged quasars (quads) are unique probes to address several fundamental problems in cosmology and astrophysics. Although they are intrinsically very rare, ongoing and planned wide-field deep-sky surveys are set to discover thousands of such systems in the next decade. It is thus paramount to devise a general framework to model strong-lens systems to cope with this large influx without being limited by expert investigator time. We propose such a general modelling framework (implemented with the publicly available software Lenstronomy) and apply it to uniformly model three band Hubble Space Telescope Wide Field Camera 3 images of 12 quads. This is the largest uniformly modelled sample of quads to date and paves the way for a variety of studies. To illustrate the scientific content of the sample, we investigate the alignment between the mass and light distribution in the deflectors. The position angles of these distributions are well-aligned, except when there is strong external shear. However, we find no correlation between the ellipticity of the light and mass distributions. We also show that the observed flux-ratios between the images depart significantly from the predictions of simple smooth models. The departures are strongest in the bluest band, consistent with microlensing being the dominant cause in addition to millilensing. Future papers will exploit this rich dataset in combination with ground based spectroscopy and time delays to determine quantities such as the Hubble constant, the free streaming length of dark matter, and the normalization of the initial stellar mass function.
Published: 2019

28. Dark Energy Survey year 1 results: Joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions

Author: Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Allam, S., Annis, J., Avila, S., Aylor, K., Banerji, M., Banik, N., Baxter, E. J., Bechtol, K., Becker, M. R., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Blazek, J., Bleem, L., Bleem, L. E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chang, C. L., Cho, H-M., Choi, A., Chown, R., Crawford, T. M., Crites, A. T., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., de Haan, T., DeRose, J., Desai, S., De Vicente, J., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Everett, W. B., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Garc��a-Bellido, J., Gatti, M., Gaztanaga, E., George, E. M., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Holder, G. P., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Kirk, D., Knox, L., Kokron, N., Krause, E., Kuehn, K., Lahav, O., Lee, A. T., Leitch, E. M., Li, T. S., Lima, M., Lin, H., Luong-Van, D., MacCrann, N., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Menanteau, F., Meyer, S. S., Miquel, R., Mocanu, L. M., Mohr, J. J., Muir, J., Natoli, T., Nicola, A., Nord, B., Omori, Y., Padin, S., Pandey, S., Plazas, A. A., Porredon, A., Prat, J., Pryke, C., Rau, M. M., Reichardt, C. L., Rollins, R. P., Romer, A. K., Roodman, A., Ross, A. J., Rozo, E., Ruhl, J. E., Rykoff, E. S., Samuroff, S., S��nchez, C., Sanchez, E., Sayre, J. T., Scarpine, V., Schaffer, K. K., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Simard, G., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vanderlinde, K., Vieira, J. D., Vielzeuf, P., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Williamson, R., Wu, W. L. K., Yanny, B., Zahn, O., Zhang, Y., Zuntz, J., 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, and SPT
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Cosmic microwave background, FOS: Physical sciences, Context (language use), Field (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Omega, Galaxy, Cosmology, South Pole Telescope, 0103 physical sciences, Dark energy, astro-ph.CO, LENTES GRAVITACIONAIS, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Weak gravitational lensing, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform a joint analysis of the auto and cross-correlations between three cosmic fields: the galaxy density field, the galaxy weak lensing shear field, and the cosmic microwave background (CMB) weak lensing convergence field. These three fields are measured using roughly 1300 sq. deg. of overlapping optical imaging data from first year observations of the Dark Energy Survey and millimeter-wave observations of the CMB from both the South Pole Telescope Sunyaev-Zel'dovich survey and Planck. We present cosmological constraints from the joint analysis of the two-point correlation functions between galaxy density and galaxy shear with CMB lensing. We test for consistency between these measurements and the DES-only two-point function measurements, finding no evidence for inconsistency in the context of flat $\Lambda$CDM cosmological models. Performing a joint analysis of five of the possible correlation functions between these fields (excluding only the CMB lensing autospectrum) yields $S_{8}\equiv \sigma_8\sqrt{\Omega_{\rm m}/0.3} = 0.782^{+0.019}_{-0.025}$ and $\Omega_{\rm m}=0.260^{+0.029}_{-0.019}$. We test for consistency between these five correlation function measurements and the Planck-only measurement of the CMB lensing autospectrum, again finding no evidence for inconsistency in the context of flat $\Lambda$CDM models. Combining constraints from all six two-point functions yields $S_{8}=0.776^{+0.014}_{-0.021}$ and $\Omega_{\rm m}= 0.271^{+0.022}_{-0.016}$. These results provide a powerful test and confirmation of the results from the first year DES joint-probes analysis., Comment: 20 pages, 7 figures
Published: 2019

29. First Cosmology Results Using Type Ia Supernovae From the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation

Author: Brout, D., Scolnic, D., Kessler, R., D'Andrea, C. B., Davis, T. M., Gupta, R. R., Hinton, S. R., Kim, A. G., Lasker, J., Lidman, C., Macaulay, E., M��ller, A., Nichol, R. C., Sako, M., Smith, M., Sullivan, M., Zhang, B., Andersen, P., Asorey, J., Avelino, A., Bassett, B. A., Brown, P., Calcino, J., Carollo, D., Challis, P., Childress, M., Clocchiatti, A., Filippenko, A. V., Foley, R. J., Galbany, L., Glazebrook, K., Hoormann, J. K., Kasai, E., Kirshner, R. P., Kuehn, K., Kuhlmann, S., Lewis, G. F., Mandel, K. S., March, M., Miranda, V., Morganson, E., Muthukrishna, D., Nugent, P., Palmese, A., Pan, Y. -C., Sharp, R., Sommer, N. E., Swann, E., Thomas, R. C., Tucker, B. E., Uddin, S. A., Wester, W., Abbott, T. M. C., Allam, S., Annis, J., Avila, S., Bechtol, K., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Estrada, J., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jarvis, M., Jeltema, T., Krause, E., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., Marriner, J., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Zhang, Y., 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, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified type Ia supernovae (SNe Ia) from the first three years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017, Comment: 30 Pages, 18 Figures, 12 Tables. Submitted to ApJ. Comments welcome
Published: 2019

30. First Cosmology Results Using Type Ia Supernovae From the Dark Energy Survey: Survey Overview and Supernova Spectroscopy

Author: D'Andrea, C. B., Smith, M., Sullivan, M., Nichol, R. C., Thomas, R. C., Kim, A. G., Möller, A., Sako, M., Castander, F. J., Filippenko, A. V., Foley, R. J., Galbany, L., González-Gaitán, S., Kasai, E., Kirshner, R. P., Lidman, C., Scolnic, D., Brout, D., Davis, T. M., Gupta, R. R., Hinton, S. R., Kessler, R., Lasker, J., Macaulay, E., Wolf, R. C., Zhang, B., Asorey, J., Avelino, A., Bassett, B. A., Calcino, J., Carollo, D., Casas, R., Challis, P., Childress, M., Clocchiatti, A., Crawford, S., Glazebrook, K., Goldstein, D. A., Graham, M. L., Hoormann, J. K., Kuehn, K., Lewis, G. F., Mandel, K. S., Morganson, E., Muthukrishna, D., Nugent, P., Pan, Y. -C., Pursiainen, M., Sharp, R., Sommer, N. E., Swann, E., Tucker, B. E., Uddin, S. A., Wiseman, P., Zheng, W., Abbott, T. M. C., Annis, J., Avila, S., Bechtol, K., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Eifler, T. F., Estrada, J., 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., Hoyle, B., James, D. J., Johnson, M. W. G., Johnson, M. D., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sobreira, F., Suchyta, E., Tarle, G., Tucker, D. L., Wester, W., 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, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present spectroscopy from the first three seasons of the Dark Energy Survey Supernova Program (DES-SN). We describe the supernova spectroscopic program in full: strategy, observations, data reduction, and classification. We have spectroscopically confirmed 307 supernovae, including 251 type Ia supernovae (SNe Ia) over a redshift range of $0.017 < z < 0.85$. We determine the effective spectroscopic selection function for our sample, and use it to investigate the redshift-dependent bias on the distance moduli of SNe Ia we have classified. We also provide a full overview of the strategy, observations, and data products of DES-SN, which has discovered 12,015 likely supernovae during these first three seasons. The data presented here are used for the first cosmology analysis by DES-SN ('DES-SN3YR'), the results of which are given in DES Collaboration (2018a)., 25 pages, 14 figures, 8 tables. Submitted to AJ
Published: 2018

31. Dark Energy Survey Year 1 Results: Methods for Cluster Cosmology and Application to the SDSS

Author: Costanzi, M., Rozo, E., Simet, M., Zhang, Y., Evrard, A. E., Mantz, A., Rykoff, E. S., Jeltema, T., Gruen, D., McClintock, S. Allen T., Romer, A. K., von der Linden, A., Farahi, A., DeRose, J., Varga, T. N., Weller, J., Giles, P., Hollowood, D. L., Bhargava, S., Bermeo-Hernandez, A., Chen, X., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., Hoyle, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Wechsler, R. H.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform the first blind analysis of cluster abundance data. Specifically, we derive cosmological constraints from the abundance and weak-lensing signal of \redmapper\ clusters of richness $\lambda\geq 20$ in the redshift range $z\in[0.1,0.3]$ as measured in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness--mass relation of the clusters. For a flat $\Lambda$CDM cosmological model with massive neutrinos, we find $S_8 \equiv \sigma_{8}(\Omega_m/0.3)^{0.5}=0.79^{+0.05}_{-0.04}$. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES) and the Kilo-Degree Survey (KiDS), and with the Cosmic Microwave Background (CMB) anisotropies as measured by \planck. We demonstrate that the cosmological posteriors are robust against variation of the richness--mass relation model and to systematics associated with the calibration of the selection function. In combination with Baryon Acoustic Oscillation (BAO) data and Big-Bang Nucleosynthesis (BBN) data, we constrain the Hubble rate to be $h=0.66\pm 0.02$, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness--mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set., Comment: 25 pages, 14 figures
Published: 2018

32. Dark Energy Survey Year 1 Results: Cross-correlation between DES Y1 galaxy weak lensing and SPT+Planck CMB weak lensing

Author: Omori, Y., Baxter, E., Chang, C., Kirk, D., Alarcon, A., Bernstein, G. M., Bleem, L. E., Cawthon, R., Choi, A., Chown, R., Crawford, T. M., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T. F., Fosalba, P., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Gruen, D., Hartley, W. G., Holder, G. P., Hoyle, B., Huterer, D., Jain, B., Jarvis, M., Krause, E., MacCrann, N., Miquel, R., Prat, J., Rau, M. M., Reichardt, C. L., Rozo, E., Samuroff, S., S��nchez, C., Secco, L. F., Sheldon, E., Simard, G., Troxel, M. A., Vielzeuf, P., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Aylor, K., Benson, B. A., Bertin, E., Bridle, S. L., Brooks, D., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Cho, H-M., Crites, A. T., Crocce, M., Cunha, C. E., da Costa, L. N., de Haan, T., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Everett, W. B., Fernandez, E., Flaugher, B., Frieman, J., Garc��a-Bellido, J., George, E. M., Gruendl, R. A., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hollowood, D. L., Honscheid, K., Holzapfel, W. L., Hou, Z., Hrubes, J. D., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Lee, A. T., Leitch, E. M., Luong-Van, D., Maia, M. A. G., Manzotti, A., Marrone, D. P., Marshall, J. L., Martini, P., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Mocanu, L. M., Mohr, J. J., Natoli, T., Ogando, R. L. C., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Rykoff, E. S., Sanchez, E., Scarpine, V., Schaffer, K. K., Schindler, R., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J. D., Vikram, V., Walker, A. R., Weller, J., Williamson, R., Wu, W. L. K., and Zahn, O.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one (Y1) data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg$^{2}$. With the combined measurements from four source galaxy redshift bins, we reject the hypothesis of no lensing with a significance of $10.8\sigma$. When employing angular scale cuts, this significance is reduced to $6.8\sigma$, which remains the highest signal-to-noise measurement of its kind to date. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial $\Lambda$CDM model, finding $A = 0.99 \pm 0.17$. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the $\Lambda$CDM model, we obtain the marginalized constraints of $\Omega_{\rm m}=0.261^{+0.070}_{-0.051}$ and $S_{8}\equiv \sigma_{8}\sqrt{\Omega_{\rm m}/0.3} = 0.660^{+0.085}_{-0.100}$. These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT and Planck data., Comment: 15 pages, 6 figures
Published: 2018

33. A Search for Optical Emission from Binary-Black-Hole Merger GW170814 with the Dark Energy Camera

Author: Doctor, Z., Kessler, R., Herner, K., Palmese, A., Soares-Santos, M., Annis, J., Brout, D., Holz, D. E., Sako, M., Rest, A., Cowperthwaite, P., Berger, E., Foley, R. J., Conselice, C. J., Gill, M. S. S., Allam, S., Balbinot, E., Butler, R. E., Chen, H. -Y., Chornock, R., Cook, E., Diehl, H. T., Farr, B., Fong, W., Frieman, J., Fryer, C., García-Bellido, J., Margutti, R., Marshall, J. L., Matheson, T., Metzger, B. D., Nicholl, M., Paz-Chinchón, F., Salim, S., Sauseda, M., Secco, L. F., Smith, R. C., Smith, N., Vivas, A. K., Tucker, D. L., Abbott, T. M. C., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., D'Andrea, C. B., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Menanteau, F., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., Wester, W., Collaboration, DES, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, and Astronomy
Subjects: coalescence, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, interferometer, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, localization, techniques: photometric, Binary black hole, star, surveys, Coincident, 0103 physical sciences, supernova, optical, LIGO, dark energy, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, ONDAS GRAVITACIONAIS, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, gravitational radiation, RCUK, imaging, Astronomy and Astrophysics, Galaxy, Supernova, VIRGO, electromagnetic, gravitational waves, black hole: binary, Space and Planetary Science, Sky, Dark energy, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], stars: black holes
Abstract: Binary black hole (BBH) mergers found by the LIGO and Virgo detectors are of immense scientific interest to the astrophysics community, but are considered unlikely to be sources of electromagnetic emission. To test whether they have rapidly fading optical counterparts, we used the Dark Energy Camera to perform an $i$-band search for the BBH merger GW170814, the first gravitational wave detected by three interferometers. The 87-deg$^2$ localization region (at 90\% confidence) centered in the Dark Energy Survey (DES) footprint enabled us to image 86\% of the probable sky area to a depth of $i\sim 23$ mag and provide the most comprehensive dataset to search for EM emission from BBH mergers. To identify candidates, we perform difference imaging with our search images and with templates from pre-existing DES images. The analysis strategy and selection requirements were designed to remove supernovae and to identify transients that decline in the first two epochs. We find two candidates, each of which is spatially coincident with a star or a high-redshift galaxy in the DES catalogs, and they are thus unlikely to be associated with GW170814. Our search finds no candidates associated with GW170814, disfavoring rapidly declining optical emission from BBH mergers brighter than $i\sim 23$ mag ($L_{\rm optical} \sim 5\times10^{41}$ erg/s) 1-2 days after coalescence. In terms of GW sky map coverage, this is the most complete search for optical counterparts to BBH mergers to date, Comment: 11 pages, 3 figures
Published: 2018
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34. Dark Energy Survey Year 1 Results: tomographic cross-correlations between DES galaxies and CMB lensing from SPT+Planck

Author: Omori, Y., Giannantonio, T., Porredon, A., Baxter, E., Chang, C., Crocce, M., Fosalba, P., Alarcon, A., Banik, N., Blazek, J., Bleem, L. E., Bridle, S. L., Cawthon, R., Choi, A., Chown, R., Crawford, T., Dodelson, S., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Friedrich, O., Gruen, D., Holder, G. P., Huterer, D., Jain, B., Jarvis, M., Kirk, D., Kokron, N., Krause, E., MacCrann, N., Muir, J., Prat, J., Reichardt, C. L., Ross, A. J., Rozo, E., Rykoff, E. S., Sánchez, C., Secco, L. F., Simard, G., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Avila, S., Aylor, K., Benson, B. A., Bernstein, G. M., Bertin, E., Bianchini, F., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Chang, C. L., Cho, H-M., Crites, A. T., Cunha, C. E., da Costa, L. N., de Haan, T., Davis, C., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dobbs, M. A., Everett, W. B., Doel, P., Estrada, J., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., George, E. M., Gruendl, R. A., Gschwend, J., Gutierrez, G., Halverson, N. W., Harrington, N. L., Hartley, W. G., Hollowood, D. L., Holzapfel, W. L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J. D., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lee, A. T., Leitch, E. M., Lima, M., Luong-Van, D., Manzotti, A., Marrone, D. P., Marshall, J. L., McMahon, J. J., Melchior, P., Menanteau, F., Meyer, S. S., Miller, C. J., Miquel, R., Mocanu, L. M., Mohr, J. J., Natoli, T., Padin, S., Plazas, A. A., Pryke, C., Romer, A. K., Roodman, A., Ruhl, J. E., Sanchez, E., Scarpine, V., Schaffer, K. K., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A. A., Story, K. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Vanderlinde, K., Vieira, J. D., Walker, A. R., Wu, W. L. K., and Zahn, O.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We measure the cross-correlation between redMaGiC galaxies selected from the Dark Energy Survey (DES) Year-1 data and gravitational lensing of the cosmic microwave background (CMB) reconstructed from South Pole Telescope (SPT) and Planck data over 1289 sq. deg. When combining measurements across multiple galaxy redshift bins spanning the redshift range of $0.15, Comment: 17 pages, 7 figures
Published: 2018
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35. Observation and Confirmation of Six Strong Lensing Systems in The Dark Energy Survey Science Verification Data

Author: Nord, B., Buckley-Geer, E., Lin, H., Diehl, H. T., Helsby, J., Kuropatkin, N., Amara, A., Collett, T., Allam, S., Caminha, G. B., de Bom, C., Desai, S., Dúmet-Montoya, H., Pereira, M. Elidaiana da S., Finley, D. A., Flaugher, B., Furlanetto, C., Gaitsch, H., Gill, M., Merritt, K. W., More, A., Tucker, D., Saro, A., Rykoff, E. S., Rozo, E., Birrer, S., Abdalla, F. B., Agnello, A., Auger, M., Brunner, R. J., Carrasco Kind, M., Castander, F. J., Cunha, C. E., da Costa, L. N., Foley, R. J., Gerdes, D. W., Glazebrook, K., Gschwend, J., Hartley, W., Kessler, R., Lagattuta, D., Lewis, G., Maia, M. A. G., Makler, M., Menanteau, F., Niernberg, A., Scolnic, D., Vieira, J. D., Gramillano, R., Abbott, T. M. C., Banerji, M., Benoit-Lévy, A., Brooks, D., Burke, D. L., Capozzi, D., Carnero Rosell, A., Carretero, J., d'Andrea, C. B., Dietrich, J. P., Doel, P., Evrard, A. E., Frieman, J., Gaztanaga, E., Gruen, D., Honscheid, K., James, D. J., Kuehn, K., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Neilsen, E., Nichol, R. C., Ogando, R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Walker, A. R., Wester, W., Zhang, Y., Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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), Nord, B., Buckley-Geer, E., Lin, H., Diehl, H. T., Helsby, J., Kuropatkin, N., Amara, A., Collett, T., Allam, S., Caminha, G. B., De Bom, C., Desai, S., Dumet-Montoya, H., Da Pereira, M. Elidaiana S., Finley, D. A., Flaugher, B., Furlanetto, C., Gaitsch, H., Gill, M., Merritt, K. W., More, A., Tucker, D., Saro, A., Rykoff, E. S., Rozo, E., Birrer, S., Abdalla, F. B., Agnello, A., Auger, M., Brunner, R. J., Kind, M. Carrasco, Castander, F. J., Cunha, C. E., Da Costa, L. N., Foley, R. J., Gerdes, D. W., Glazebrook, K., Gschwend, J., Hartley, W., Kessler, R., Lagattuta, D., Lewis, G., Maia, M. A. G., Makler, M., Menanteau, F., Niernberg, A., Scolnic, D., Vieira, J. D., Gramillano, R., Abbott, T. M. C., Banerji, M., Benoit-Lévy, A., Brooks, D., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Carretero, J., D'Andrea, C. B., Dietrich, J. P., Doel, P., Evrard, A. E., Frieman, J., Gaztanaga, E., Gruen, D., Honscheid, K., James, D. J., Kuehn, K., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Neilsen, E., Nichol, R. C., Ogando, R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Walker, A. R., Wester, W., and Zhang, Y.
Subjects: Strong gravitational lensing, observational [methods], Astrophysics, 01 natural sciences, cosmology: observations, galaxies: clusters: general, galaxies: distances and redshifts, gravitational lensing: strong, methods: observational, techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Einstein radius, law.invention, law, clusters: general [galaxies], Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, QB, Physics, Solar mass, Astrophysics::Instrumentation and Methods for Astrophysics, observations [cosmology], strong [gravitational lensing], astro-ph.CO, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, 0103 physical sciences, distances and redshift [galaxies], Spectrograph, distances and reshifts [galaxies], Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [SDU]Sciences of the Universe [physics], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), uploaded-in-3-months-elsewhere
Abstract: We report the observation and confirmation of the first group- and cluster-scale strong gravitational lensing systems found in Dark Energy Survey (DES) data. Through visual inspection of data from the Science Verification (SV) season, we identified 53 candidate systems. We then obtained spectroscopic follow-up of 21 candidates using the Gemini Multi-Object Spectrograph (GMOS) at the Gemini South telescope and the Inamori-Magellan Areal Camera and Spectrograph (IMACS) at the Magellan/Baade telescope. With this follow-up, we confirmed six candidates as gravitational lenses: Three of the systems are newly discovered, and the remaining three were previously known. Of the 21 observed candidates, the remaining 15 were either not detected in spectroscopic observations, were observed and did not exhibit continuum emission (or spectral features), or were ruled out as lensing systems. The confirmed sample consists of one group-scale and five galaxy cluster-scale lenses. The lensed sources range in redshift z ~ 0.80-3.2, and in i-band surface brightness i_{SB} ~ 23-25 mag/sq.-arcsec. (2" aperture). For each of the six systems, we estimate the Einstein radius and the enclosed mass, which have ranges ~ 5.0 - 8.6" and ~ 7.5 x 10^{12} - 6.4 x 10^{13} solar masses, respectively., 17 pages, 7 figures, 4 tables; submitted to ApJ
Published: 2015

36. OzDES multifibre spectroscopy for the Dark Energy Survey: Three year results and first data release

Author: Childress, M. J., Lidman, C., Davis, T. M., Tucker, B. E., Asorey, J., Yuan, F., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Banerji, M., Benoit-Levy, A., Stephanie Bernard, Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Cunha, C. E., Da Costa, L. N., D Andrea, C. B., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Foley, R. J., Fosalba, P., Frieman, J., Garcia-Bellido, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hinton, S. R., Hoormann, J. K., James, D. J., Kessler, R., Kim, A. G., King, A. L., Kovacs, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lagattuta, D. J., Lewis, G. F., Li, T. S., Lima, M., Lin, H., Macaulay, E., Maia, M. A. G., Marriner, J., March, M., Marshall, J. L., Martini, P., Mcmahon, R. G., Menanteau, F., Miquel, R., Moller, A., Morganson, E., Mould, J., Mudd, D., Muthukrishna, D., Nichol, R. C., Nord, B., Ogando, R. L. C., Ostrovski, F., Parkinson, D., Plazas, A. A., Reed, S. L., Reil, K., Romer, A. K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Seymour, N., Sharp, R., Smith, M., Soares-Santos, M., Sobreira, F., Sommer, N. E., Spinka, H., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Uddin, S. A., Walker, A. R., Wester, W., and Zhang, B. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results for the first three years of OzDES, a six-year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multi-year baseline, and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17,000 objects, including the redshifts of 2,566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise, magnitude, and exposure time, finding that our redshift success rate increases significantly at a signal-to-noise of 2 to 3 per 1-Angstrom bin. We also find that the change in signal-to-noise with exposure time closely matches the Poisson limit for stacked exposures as long as 10 hours. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as the 4m Multi-Object Spectroscopic Telescope (4MOST), the Subaru Prime Focus Spectrograph (PFS), and the Maunakea Spectroscopic Explorer (MSE). This work marks the first OzDES data release, comprising 14,693 redshifts. OzDES is on target to obtain over a yield of approximately 5,700 supernova host-galaxy redshifts., Accepted for publication in MNRAS. Redshift data release is available at http://www.mso.anu.edu.au/ozdes/DR1
Published: 2017

37. Chemical Abundance Analysis of Three $��$-Poor, Metal-Poor Stars in the Ultra-Faint Dwarf Galaxy Horologium I

Author: Nagasawa, D. Q., Marshall, J. L., Simon, J. D., Hansen, T. T., Li, T. S., Bernstein, R. A., Balbinot, E., Drlica-Wagner, A., Pace, A. B., Strigari, L. E., Pellegrino, C. M., DePoy, D. L., Suntzeff, N. B., Bechtol, K., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Benoit-L��vy, A., Bertin, E., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Doel, P., Eifler, T. F., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., March, M., Miquel, R., Nord, B., Roodman, A., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., Wechsler, R. H., Wolf, R. C., and Yanny, B.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present chemical abundance measurements of three stars in the ultra-faint dwarf galaxy Horologium I, a Milky Way satellite discovered by the Dark Energy Survey. Using high resolution spectroscopic observations we measure the metallicity of the three stars as well as abundance ratios of several $��$-elements, iron-peak elements, and neutron-capture elements. The abundance pattern is relatively consistent among all three stars, which have a low average metallicity of [Fe/H] $\sim -2.6$ and are not $��$-enhanced ([$��$/Fe] $\sim 0.0$). This result is unexpected when compared to other low-metallicity stars in the Galactic halo and other ultra-faint dwarfs and hints at an entirely different mechanism for the enrichment of Hor I compared to other satellites. We discuss possible scenarios that could lead to this observed nucleosynthetic signature including extended star formation, a Population III supernova, and a possible association with the Large Magellanic Cloud.
Published: 2017
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38. Eight new luminous z > 6 quasars selected via SED model fitting of VISTA, WISE and Dark Energy Survey Year 1 Observations

Author: Reed, S. L., McMahon, R. G., Martini, P., Banerji, M., Auger, M., Hewett, P. C., Koposov, S. E., Gibbons, S. L. J., Gonzalez-Solares, E., Ostrovski, F., Tie, S. S., Abdalla, F. B., Allam, S., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., da Costa, L. N., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Evrard, A. E., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Miller, C. J., Miquel, R., Nord, B., Ogando, R., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Walker, A. R., and Wester, W.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present the discovery and spectroscopic confirmation with the ESO NTT and Gemini South telescopes of eight new 6.0 < z < 6.5 quasars with z$_{AB}$ < 21.0. These quasars were photometrically selected without any star-galaxy morphological criteria from 1533 deg$^{2}$ using SED model fitting to photometric data from the Dark Energy Survey (g, r, i, z, Y), the VISTA Hemisphere Survey (J, H, K) and the Wide-Field Infrared Survey Explorer (W1, W2). The photometric data was fitted with a grid of quasar model SEDs with redshift dependent Lyman-�� forest absorption and a range of intrinsic reddening as well as a series of low mass cool star models. Candidates were ranked using on a SED-model based $��^{2}$-statistic, which is extendable to other future imaging surveys (e.g. LSST, Euclid). Our spectral confirmation success rate is 100% without the need for follow-up photometric observations as used in other studies of this type. Combined with automatic removal of the main types of non-astrophysical contaminants the method allows large data sets to be processed without human intervention and without being over run by spurious false candidates. We also present a robust parametric redshift estimating technique that gives comparable accuracy to MgII and CO based redshift estimators. We find two z $\sim$ 6.2 quasars with HII near zone sizes < 3 proper Mpc which could indicate that these quasars may be young with ages < 10$^6$ - 10$^7$ years or lie in over dense regions of the IGM. The z = 6.5 quasar VDESJ0224-4711 has J$_{AB}$ = 19.75 is the second most luminous quasar known with z > 6.5., 19 pages, 15 figures
Published: 2017
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39. Baryon Content in a Sample of 91 Galaxy Clusters Selected by the South Pole Telescope at 0.2 < z < 1.25

Author: Chiu, I., Mohr, J. J., McDonald, M., Bocquet, S., Desai, S., Klein, M., Israel, H., Ashby, M. L. N., Stanford, A., Benson, B. A., Brodwin, M., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bayliss, M., Benoit-L��vy, A., Bertin, E., Bleem, L., Brooks, D., Buckley-Geer, E., Bulbul, E., Capasso, R., Carlstrom, J. E., Rosell, A. Carnero, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., Garc��a-Bellido, J., Garmire, G., Gaztanaga, E., Gerdes, D. W., Gonzalez, A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, N., Gutierrez, G., Hlavacek-L., J., Honscheid, K., James, D. J., Jeltema, T., Kraft, R., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Murray, S., Nord, B., Ogando, R. L. C., Plazas, A. A., Rapetti, D., Reichardt, C. L., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Sharon, K., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Stalder, B., Stern, C., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., Walker, A. R., Weller, J., and Zhang, Y.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We estimate total mass ($M_{500}$), intracluster medium (ICM) mass ($M_{\mathrm{ICM}}$) and stellar mass ($M_{\star}$) in a Sunyaev-Zel'dovich effect (SZE) selected sample of 91 galaxy clusters with masses $M_{500}\gtrsim2.5\times10^{14}M_{\odot}$ and redshift $0.2 < z < 1.25$ from the 2500 deg$^2$ South Pole Telescope SPT-SZ survey. The total masses $M_{500}$ are estimated from the SZE observable, the ICM masses $M_{\mathrm{ICM}}$ are obtained from the analysis of $Chandra$ X-ray observations, and the stellar masses $M_{\star}$ are derived by fitting spectral energy distribution templates to Dark Energy Survey (DES) $griz$ optical photometry and $WISE$ or $Spitzer$ near-infrared photometry. We study trends in the stellar mass, the ICM mass, the total baryonic mass and the cold baryonic fraction with cluster mass and redshift. We find significant departures from self-similarity in the mass scaling for all quantities, while the redshift trends are all statistically consistent with zero, indicating that the baryon content of clusters at fixed mass has changed remarkably little over the past $\approx9$ Gyr. We compare our results to the mean baryon fraction (and the stellar mass fraction) in the field, finding that these values lie above (below) those in cluster virial regions in all but the most massive clusters at low redshift. Using a simple model of the matter assembly of clusters from infalling groups with lower masses and from infalling material from the low density environment or field surrounding the parent halos, we show that the measured mass trends without strong redshift trends in the stellar mass scaling relation could be explained by a mass and redshift dependent fractional contribution from field material. Similar analyses of the ICM and baryon mass scaling relations provide evidence for the so-called "missing baryons" outside cluster virial regions., Accepted by MNRAS with further clarification and discussion of the mass calibration added
Published: 2017
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40. Joint analysis of galaxy-galaxy lensing and galaxy clustering: Methodology and forecasts for Dark Energy Survey

Author: Park, Y., Krause, E., Dodelson, S., Jain, B., Amara, A., Becker, M. R., Bridle, S. L., Clampitt, J., Crocce, M., Fosalba, P., Gaztanaga, E., Honscheid, K., Rozo, E., Sobreira, F., Sanchez, C., Wechsler, R. H., Abbott, T., Abdalla, F. B., Allam, S., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Da Costa, L. N., Depoy, D. L., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., James, D. J., Kent, S., Kuehn, K., Kuropatkin, N., Marcos Lima, Maia, M. A. G., Marshall, J. L., Melchior, P., Miller, C. J., Miquel, R., Nichol, R. C., Ogando, R., Plazas, A. A., Roe, N., Romer, A. K., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Vikram, V., Walker, A. R., Weller, J., and Zuntz, J.
Subjects: Quantum Physics, Particle and Plasma Physics, Molecular, Nuclear, Astrophysics::Cosmology and Extragalactic Astrophysics, Atomic, Nuclear & Particles Physics, Astronomical and Space Sciences, Astrophysics::Galaxy Astrophysics
Abstract: The joint analysis of galaxy-galaxy lensing and galaxy clustering is a promising method for inferring the growth function of large-scale structure. Anticipating a near future application of this analysis to Dark Energy Survey (DES) measurements of galaxy positions and shapes, we develop a practical approach to modeling the assumptions and systematic effects affecting the joint analysis of small-scale galaxy-galaxy lensing and large-scale galaxy clustering. Introducing parameters that characterize the halo occupation distribution (HOD), photometric redshift uncertainties, and shear measurement errors, we study how external priors on different subsets of these parameters affect our growth constraints. Degeneracies within the HOD model, as well as between the HOD and the growth function, are identified as the dominant source of complication, with other systematic effects being subdominant. The impact of HOD parameters and their degeneracies necessitate the detailed joint modeling of the galaxy sample that we employ. We conclude that DES data will provide powerful constraints on the evolution of structure growth in the Universe, conservatively/optimistically constraining the growth function to 7.9%/4.8% with its first-year data that cover over 1000 square degrees, and to 3.9%/2.3% with its full five-year data that will survey 5000 square degrees, including both statistical and systematic uncertainties.
Published: 2016

41. Cosmology from cosmic shear with Dark Energy Survey Science Verification data

Author: Abbott, T., Abdalla, F. B., Allam, S., Amara, A., Annis, J., Armstrong, R., Bacon, D., Banerji, M., Bauer, A. H., Baxter, E., Becker, M. R., Benoit-Lévy, A., Bernstein, R. A., Bernstein, G. M., Bertin, E., Blazek, J., Bonnett, C., Bridle, S. L., Brooks, D., Bruderer, C., Buckley-Geer, E., Burke, D. L., Busha, M. T., Capozzi, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Chang, C., Clampitt, J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., DePoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Efstathiou, G., Eifler, T. F., Erickson, B., Estrada, J., Evrard, A. E., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Gangkofner, C., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W., Hirsch, M., Honscheid, K., Huff, E. M., Jain, B., James, D. J., Jarvis, M., Kacprzak, T., Kent, S., Kirk, D., Krause, E., Kravtsov, A., Kuehn, K., Kuropatkin, N., Kwan, J., Lahav, O., Leistedt, B., Li, T. S., Lima, M., Lin, H., MacCrann, N., March, M., Marshall, J. L., Martini, P., McMahon, R. G., Melchior, P., Miller, C. J., Miquel, R., Mohr, J. J., Neilsen, E., Nichol, R. C., Nicola, A., Nord, B., Ogando, R., Palmese, A., Peiris, H. V., Plazas, A. A., Refregier, A., Roe, N., Romer, A. K., Roodman, A., Rowe, B., Rykoff, E. S., Sabiu, C., Sadeh, I., Sako, M., Samuroff, S., Sanchez, E., Sánchez, C., Seo, H., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Troxel, M. A., Vikram, V., Walker, A. R., Wechsler, R. H., Weller, J., Zhang, Y., Zuntz, J., and Dark Energy Survey Collaboration, [Unknown]
Subjects: Cosmology and Gravitation, PARAMETER CONSTRAINTS, Dark matter, Cosmic microwave background, WEAK-LENSING TOMOGRAPHY, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, GALAXY ELLIPTICITIES, 01 natural sciences, Cosmology, Physics, Particles & Fields, symbols.namesake, PRECISION COSMOLOGY, MATTER POWER SPECTRUM, LARGE-SCALE STRUCTURE, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, QB, Photometric redshift, Physics, Science & Technology, 010308 nuclear & particles physics, RCUK, Astronomy, INTRINSIC ALIGNMENTS, Redshift, Physical Sciences, astro-ph.CO, Dark energy, symbols, COVARIANCE-MATRIX, BARYON ACOUSTIC-OSCILLATIONS, HUBBLE CONSTANT
Abstract: We present the first constraints on cosmology from the Dark Energy Survey (DES), using weak lensing measurements from the preliminary Science Verification (SV) data. We use 139 square degrees of SV data, which is less than 3% of the full DES survey area. Using cosmic shear 2-point measurements over three redshift bins we find σ8(Ωm/0.3)0.5=0.81±0.06 (68% confidence), after marginalizing over 7 systematics parameters and 3 other cosmological parameters. We examine the robustness of our results to the choice of data vector and systematics assumed, and find them to be stable. About 20% of our error bar comes from marginalizing over shear and photometric redshift calibration uncertainties. The current state-of-the-art cosmic shear measurements from CFHTLenS are mildly discrepant with the cosmological constraints from Planck CMB data; our results are consistent with both data sets. Our uncertainties are ∼30% larger than those from CFHTLenS when we carry out a comparable analysis of the two data sets, which we attribute largely to the lower number density of our shear catalogue. We investigate constraints on dark energy and find that, with this small fraction of the full survey, the DES SV constraints make negligible impact on the Planck constraints. The moderate disagreement between the CFHTLenS and Planck values of σ8(Ωm/0.3)0.5 is present regardless of the value of ω.
Published: 2016

42. Galaxy bias from the DES Science Verification data:combining galaxy density maps and weak lensing maps

Author: Chang, C., Pujol, A., Gaztanaga, E., Amara, A., Refregier, A., Bacon, D., Becker, M. R., Bonnett, C., Carretero, J., Castander, F. J., Crocce, M., Fosalba, P., Giannantonio, T., Hartley, W., Jarvis, M., Kacprzak, T., Ross, A. J., Sheldon, E., Troxel, M. A., Vikram, V., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Cunha, C. E., D'Andrea, C. B., Costa, L. N. da, Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Evrard, A. E., Flaugher, B., Frieman, J., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Walker, A. R.
Subjects: Cosmology and Gravitation, astro-ph.CO, RCUK, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, STFC
Abstract: We measure the redshift evolution of galaxy bias for a magnitude-limited galaxy sample by combining the galaxy density maps and weak lensing shear maps for a ∼116 deg2 area of the Dark Energy Survey (DES) Science Verification (SV) data. This method was first developed in Amara et al. and later re-examined in a companion paper with rigorous simulation tests and analytical treatment of tomographic measurements. In this work we apply this method to the DES SV data and measure the galaxy bias for a i < 22.5 galaxy sample. We find the galaxy bias and 1σ error bars in four photometric redshift bins to be 1.12 ± 0.19 (z = 0.2–0.4), 0.97 ± 0.15 (z = 0.4–0.6), 1.38 ± 0.39 (z = 0.6–0.8), and 1.45 ± 0.56 (z = 0.8–1.0). These measurements are consistent at the 2σ level with measurements on the same data set using galaxy clustering and cross-correlation of galaxies with cosmic microwave background lensing, with most of the redshift bins consistent within the 1σ error bars. In addition, our method provides the only σ8 independent constraint among the three. We forward model the main observational effects using mock galaxy catalogues by including shape noise, photo-z errors, and masking effects. We show that our bias measurement from the data is consistent with that expected from simulations. With the forthcoming full DES data set, we expect this method to provide additional constraints on the galaxy bias measurement from more traditional methods. Furthermore, in the process of our measurement, we build up a 3D mass map that allows further exploration of the dark matter distribution and its relation to galaxy evolution.
Published: 2016

43. A Study of Quasar Selection in the Dark Energy Survey Supernova fields

Author: Tie, S. S., Martini, P., Mudd, D., Ostrovski, F., Reed, S. L., Lidman, C., Kochanek, C., Davis, T. M., Sharp, R., Uddin, S., King, A., Wester, W., Tucker, B. E., Tucker, D. L., Buckley-Geer, E., Carollo, D., Childress, M., Glazebrook, K., Hinton, S. R., Lewis, G., Macaulay, E., O Neill, C. R., Abbott, T. M. C., Filipe Abdalla, Annis, J., Benoit-L Evy, A., Bertin, E., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., Da Costa, L. N., Depoy, D. L., Desai, S., Doel, P., Eifler, T. F., Evrard, A. E., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miller, C. J., Miquel, R., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., and Des, The Collaboration
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We present a study of quasar selection using the DES supernova fields. We used a quasar catalog from an overlapping portion of the SDSS Stripe 82 region to quantify the completeness and efficiency of selection methods involving color, probabilistic modeling, variability, and combinations of color/probabilistic modeling with variability. We only considered objects that appear as point sources in the DES images. We examine color selection methods based on the WISE mid-IR W1-W2 color, a mixture of WISE and DES colors (g-i and i-W1) and a mixture of VHS and DES colors (g-i and i-K). For probabilistic quasar selection, we used XDQSOz, an algorithm that employs an empirical multi-wavelength flux model of quasars to assign quasar probabilities. Our variability selection uses the multi-band chi2-probability that sources are constant in the DES Year 1 griz-band light curves. The completeness and efficiency are calculated relative to an underlying sample of point sources that are detected in the required selection bands and pass our data quality and photometric error cuts. We conduct our analyses at two magnitude limits, i85% for both i-band magnitude limits and efficiencies of >80% to the bright limit and >60% to the faint limit; however, the giW1 and giW1+variability methods give the highest quasar surface densities. The XDQSOz method and combinations of W1W2/giW1/XDQSOz with variability are among the better selection methods when both high completeness and high efficiency are desired. We also present the OzDES Quasar Catalog of 1,263 spectroscopically-confirmed quasars taken by the OzDES survey. The catalog includes quasars with redshifts up to z~4 and brighter than i=22 mag, although the catalog is not complete up this magnitude limit., 16 pages, 12 figures, 3 tables; Submitted to ApJ. The OzDES Quasar Catalog can be downloaded at http://bit.ly/2fWsK9t . For a video summary of the paper, please see https://www.youtube.com/watch?v=JeQNdUATze0
Published: 2016
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44. Joint Analysis of Galaxy-Galaxy Lensing and Galaxy Clustering: Methodology and Forecasts for DES

Author: Park, Y., Krause, E., Dodelson, S., Jain, B., Amara, A., Becker, M. R., Bridle, S. L., Clampitt, J., Crocce, M., Fosalba, P., Gaztanaga, E., Honscheid, K., Rozo, E., Sobreira, F., Sánchez, C., Wechsler, R. H., Abbott, T., Abdalla, F. B., Allam, S., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Da Costa, L. N., Depoy, D. L., Desai, S., Jörg Dietrich, Doel, P., Eifler, T. F., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., James, D. J., Kent, S., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Miller, C. J., Miquel, R., Nichol, R. C., Ogando, R., Plazas, A. A., Roe, N., Romer, A. K., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Vikram, V., Walker, A. R., Weller, J., and Zuntz, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The joint analysis of galaxy-galaxy lensing and galaxy clustering is a promising method for inferring the growth function of large scale structure. This analysis will be carried out on data from the Dark Energy Survey (DES), with its measurements of both the distribution of galaxies and the tangential shears of background galaxies induced by these foreground lenses. We develop a practical approach to modeling the assumptions and systematic effects affecting small scale lensing, which provides halo masses, and large scale galaxy clustering. Introducing parameters that characterize the halo occupation distribution (HOD), photometric redshift uncertainties, and shear measurement errors, we study how external priors on different subsets of these parameters affect our growth constraints. Degeneracies within the HOD model, as well as between the HOD and the growth function, are identified as the dominant source of complication, with other systematic effects sub-dominant. The impact of HOD parameters and their degeneracies necessitate the detailed joint modeling of the galaxy sample that we employ. We conclude that DES data will provide powerful constraints on the evolution of structure growth in the universe, conservatively/optimistically constraining the growth function to 7.9\%/4.8\% with its first-year data that covered over 1000 square degrees, and to 3.9\%/2.3\% with its full five-year data that will survey 5000 square degrees, including both statistical and systematic uncertainties., Comment: 26 pages, 15 figures. Author list corrected
Published: 2015
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45. DECal: A Spectrophotometric Calibration System For DECam

Author: Marshall, J. L., Rheault, Jean-Philippe, DePoy, D. L., Prochaska, Travis, Allen, Richard, Behm, Tyler W., Martin, Emily C., Veal, Brannon, Villanueva, Steven, Williams, Patrick, and Wise, Jason
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: DECal is a new calibration system for the CTIO 4 m Blanco telescope. It is currently being installed as part of the Dark Energy Survey and will provide both broadband flat fields and narrowband (about 1 nm bandwidth) spectrophotometric calibration for the new Dark Energy Camera (DECam). Both of these systems share a new Lambertian flat field screen. The broadband flat field system uses LEDs to illuminate each photometric filter. The spectrophotometric calibration system consists of a monochromator-based tunable light source that is projected onto the flat field screen using a custom line-to-spot fiber bundle and an engineered diffuser. Several calibrated photodiodes positioned along the beam monitor the telescope throughput as a function of wavelength. This system will measure the wavelength-dependent instrumental response function of the total telescope+instrument system in the range 300 < lambda < 1100nm. The spectrophotometric calibration will be performed regularly (roughly once per month) to determine the spectral response of the DECam system and to monitor changes in instrumental throughput during the five year Dark Energy Survey project., 10 pages, 5 figures. To appear in conference proceedings: "Calibration and Standardization of Large Surveys and Missions in Astronomy and Astrophysics" (Fermilab, April 16-19, 2012)
Published: 2013

46. A Study of the Type Ia/IIn Supernova 2005gj from X-ray to the Infrared: Paper I

Author: Jose Prieto, Garnavich, P. M., Phillips, M. M., Depoy, D. L., Parrent, J., Pooley, D., Dwarkadas, V. V., Baron, E., Bassett, B., Becker, A., Cinabro, D., Dejongh, F., Dilday, B., Doi, M., Frieman, J. A., Hogan, C. J., Holtzman, J., Jha, S., Kessler, R., Konishi, K., Lampeitl, H., Marriner, J., Marshall, J. L., Miknaitis, G., Nichol, R. C., Riess, A. G., Richmond, M. W., Romani, R., Sako, M., Schneider, D. P., Smith, M., Takanashi, N., Tokita, K., Heyden, K., Yasuda, N., Zheng, C., Wheeler, J. C., Barentine, J., Dembicky, J., Eastman, J., Frank, S., Ketzeback, W., Mcmillan, R. J., Morrell, N., Folatelli, G., Contreras, C., Burns, C. R., Freedman, W. L., Gonzalez, S., Hamuy, M., Krzeminski, W., Madore, B. F., Murphy, D., Persson, S. E., Roth, M., and Suntzeff, N. B.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present extensive ugrizYHJK photometry and optical spectroscopy of SN 2005gj obtained by the SDSS-II and CSP Supernova Projects, which give excellent coverage during the first 150 days after the time of explosion. These data show that SN 2005gj is the second clear case, after SN 2002ic, of a thermonuclear explosion in a dense circumstellar environment. Both the presence of singly and doubly ionized iron-peak elements (FeIII and weak SII, SiII) near maximum light as well as the spectral evolution show that SN 2002ic-like events are Type Ia explosions. Independent evidence comes from the exponential decay in luminosity of SN 2005gj, pointing to an exponential density distribution of the ejecta. The interaction of the supernova ejecta with the dense circumstellar medium is stronger than in SN 2002ic: (1) the supernova lines are weaker; (2) the Balmer emission lines are more luminous; and (3) the bolometric luminosity is higher close to maximum light. The velocity evolution of the Halpha components suggest that the CSM around SN 2005gj is clumpy and it has a flatter density distribution compared with the steady wind solution, in agreement with SN 2002ic. An early X-ray observation with Chandra gives an upper-limit on the mass loss rate from the companion of < 2x10^{-4} Msun/yr., 63 pages, 16 figures, submitted to AJ
Published: 2007

47. Early Results from the KELT Transit Survey

Author: Pepper, J., Pogge, R., Depoy, D. L., Marshall, J. L., Stanek, K., Amelia Stutz, Trueblood, M., and Trueblood, P.
Subjects: Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Kilodegree Extremely Little Telescope (KELT) project is a small-aperture transit survey of bright stars. The project has completed commissioning runs searching for transits in the Hyades and Praesepe, and is well into a multi-year survey of a large portion of the Northern Hemisphere. Here we describe the setup of the telescope and discuss the early data., Comment: 6 pages, 4 figures; To appear in Proceedings of "Transiting Extrasolar Planets Workshop" MPIA Heidelberg Germany, 25th-28th September 2006. Eds: Cristina Afonso, David Weldrake & Thomas Henning
Published: 2006
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48. Survey for Transiting Extrasolar Planets in Stellar Systems (STEPSS): The Frequency of Planets in NGC 1245

Author: Burke, Christopher J., DePoy, D. L., Gaudi, B. Scott, Marshall, J. L., and Pogge, Richard W.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics
Abstract: We present first results from the Survey for Transiting Extrasolar Planets in Stellar Systems (STEPSS). Our goal is to assess the frequency of close-in extrasolar planets around main-sequence stars in several open clusters. By concentrating on main-sequence stars in clusters of known (and varied) age, metallicity, and stellar density, we will gain insight into how these various properties affect planet formation, migration, and survival. We show preliminary results from our 19 night photometric campaign of the old, solar metallicity cluster NGC 1245. Taking into account the photometric precision, observational window function, transit probability, and total number of stars monitored, we estimate that we should be able to probe planetary companion fractions of, 4 pages, 5 figures. To appear in the ASP Conference Series: Scientific Frontiers in Research on Extrasolar Planets, eds. D. Deming and S. Seager
Published: 2002

49. DES Y1 Results: Validating cosmological parameter estimation using simulated Dark Energy Surveys

Author: Maccrann, N., Derose, J., Wechsler, R. H., Blazek, J., Gaztanaga, E., Crocce, M., Rykoff, E. S., Becker, M. R., Jain, B., Krause, E., Eifler, T. F., Gruen, D., Zuntz, J., Troxel, M. A., Elvin-Poole, J., Prat, J., Wang, M., Dodelson, S., Kravtsov, A., Fosalba, P., Busha, M. T., Evrard, A. E., Huterer, D., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Cunha, C. E., D Andrea, C. B., Da Costa, L. N., Davis, C., Vicente, J., Diehl, H. T., Doel, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hollowood, D., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kirk, D., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Felipe Menanteau, Miquel, R., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., and Weller, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), bias, Large-scale structure of Universe, Cosmological parameters, FOS: Physical sciences, science verification data, Astrophysics::Cosmology and Extragalactic Astrophysics, power spectra, 01 natural sciences, Omega, large-scale structure, Cosmology, 0103 physical sciences, luminosity, Statistical physics, cosmological parameters, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, large-scale structure of universe, Physics, 010308 nuclear & particles physics, Estimation theory, RCUK, Sigma, alignments, Astronomy and Astrophysics, matter, Redshift, Galaxy, Space and Planetary Science, Dark energy, digital sky survey, galaxy, cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use mock galaxy survey simulations designed to resemble the Dark Energy Survey Year 1 (DES Y1) data to validate and inform cosmological parameter estimation. When similar analysis tools are applied to both simulations and real survey data, they provide powerful validation tests of the DES Y1 cosmological analyses presented in companion papers. We use two suites of galaxy simulations produced using different methods, which therefore provide independent tests of our cosmological parameter inference. The cosmological analysis we aim to validate is presented in DES Collaboration et al. (2017) and uses angular two-point correlation functions of galaxy number counts and weak lensing shear, as well as their cross-correlation, in multiple redshift bins. While our constraints depend on the specific set of simulated realisations available, for both suites of simulations we find that the input cosmology is consistent with the combined constraints from multiple simulated DES Y1 realizations in the $\Omega_m-\sigma_8$ plane. For one of the suites, we are able to show with high confidence that any biases in the inferred $S_8=\sigma_8(\Omega_m/0.3)^{0.5}$ and $\Omega_m$ are smaller than the DES Y1 $1-\sigma$ uncertainties. For the other suite, for which we have fewer realizations, we are unable to be this conclusive; we infer a roughly 70% probability that systematic biases in the recovered $\Omega_m$ and $S_8$ are sub-dominant to the DES Y1 uncertainty. As cosmological analyses of this kind become increasingly more precise, validation of parameter inference using survey simulations will be essential to demonstrate robustness., Comment: 22 pages, 13 figures, accepted for publication in MNRAS

50. Physical properties of star clusters in the outer LMC as observed by the Dark Energy Survey

Author: Pieres, A., Santiago, B., Balbinot, E., Luque, E., Queiroz, A. B. A., Da Costa, L. N., Maia, M. A. G., Drlica-Wagner, A., Roodman, A., Abbott, C., Allam, S., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., Desai, S., Diehl, H. T., Eifler, T. F., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Marshall, J. L., Martini, P., Miller, C. J., Miquel, R., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Douglas Tucker, and Walker, A. R.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: The Large Magellanic Cloud (LMC) harbors a rich and diverse system of star clusters, whose ages, chemical abundances, and positions provide information about the LMC history of star formation. We use Science Verification imaging data from the Dark Energy Survey to increase the census of known star clusters in the outer LMC and to derive physical parameters for a large sample of such objects using a spatially and photometrically homogeneous data set. Our sample contains 255 visually identified cluster candidates, of which 109 were not listed in any previous catalog. We quantify the crowding effect for the stellar sample produced by the DES Data Management pipeline and conclude that the stellar completeness is < 10% inside typical LMC cluster cores. We therefore develop a pipeline to sample and measure stellar magnitudes and positions around the cluster candidates using DAOPHOT. We also implement a maximum-likelihood method to fit individual density profiles and colour-magnitude diagrams. For 117 (from a total of 255) of the cluster candidates (28 uncatalogued clusters), we obtain reliable ages, metallicities, distance moduli and structural parameters, confirming their nature as physical systems. The distribution of cluster metallicities shows a radial dependence, with no clusters more metal-rich than [Fe/H] ~ -0.7 beyond 8 kpc from the LMC center. The age distribution has two peaks at ~ 1.2 Gyr and ~ 2.7 Gyr., 41 pages, 16 figures, 1 appendix

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