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108 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. Characterizing the intracluster light over the redshift range 0.2 < z < 0.8 in the DES-ACT overlap

Author: Golden-Marx, Jesse B., Zhang, Y., Ogando, R. L. C., Allam, S., Tucker, D. L., Miller, C. J., Hilton, M., Mutlu-Pakdil, B., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Bellido, J. García, Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Marshall, J. L., Melchior, P., Mena-Fernández, J., Miquel, R., Mohr, J. J., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Sifón, C., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vincenzi, M., Weaverdyck, N., Yanny, B., and Collaboration, DES
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We characterise the properties and evolution of Bright Central Galaxies (BCGs) and the surrounding intracluster light (ICL) in galaxy clusters identified in overlapping regions of the Dark Energy Survey and Atacama Cosmology Telescope Survey (DES-ACT), covering the redshift range $0.20$14.4. We also measure the stellar mass - halo mass (SMHM) relation for the BCG+ICL system and find that the slope, $\beta$, which characterises the dependence of $M_{\rm 200m,SZ}$ on the BCG+ICL stellar mass, increases with radius. The outskirts are more strongly correlated with the halo than the core, which supports that the BCG+ICL system follows a two-phase growth, where recent growth ($z, Comment: 19 pages, 12 Figures, 3 Tables. Submitted to MNRAS on 9/7/2022 -- Metadata typo corrected
Published: 2023

3. The DES view of the Eridanus supervoid and the CMB cold spot

Author: Kovács, A, Jeffrey, N, Gatti, M, Chang, C, Whiteway, L, Hamaus, N, Lahav, O, Pollina, G, Bacon, D, Kacprzak, T, Mawdsley, B, Nadathur, S, Zeurcher, D, García-Bellido, J, Alarcon, A, Amon, A, Bechtol, K, Bernstein, G M, Campos, A, Rosell, A Carnero, Kind, M Carrasco, Cawthon, R, Chen, R, Choi, A, Cordero, J, Davis, C, Derose, J, Doux, C, Drlica-Wagner, A, Eckert, K, Elsner, F, Elvin-Poole, J, Everett, S, Ferté, A, Giannini, G, Gruen, D, Gruendl, R A, Harrison, I, Hartley, W G, Herner, K, Huff, E M, Huterer, D, Kuropatkin, N, Jarvis, M, Leget, P F, Maccrann, N, Mccullough, J, Muir, J, Myles, J, Navarro-Alsina, A, Pandey, S, Prat, J, Raveri, M, Rollins, R P, Ross, A J, Rykoff, E S, Sánchez, C, Secco, L F, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Troxel, M A, Tutusaus, I, Varga, T N, Yanny, B, Yin, B, Zhang, Y, Zuntz, J, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, D, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, Davis, T, Deundefined, Vicente, J, Desai, S, Diehl, H T, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, Gaztañaga, E, Gerdes, D, Giannantonio, T, Gschwend, J, Gutierrez, G, Hinton, S, Hollowood, D L, Honscheid, K, James, D, Kuehn, K, Lima, M, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Ogando, R, Paz-Chinchon, F, Pieres, A, Plazas, A A, Monroy, M Rodriguez, Romer, K, Roodman, A, Sanchez, E, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, C-H, To, Weller, J, UAM. Departamento de Física Teórica, Instituto de Astrofísica de Canarias (IAC), Tenerife, Univer Sité de Paris, University College London, The Barcelona Institute of Science and Technology, University of Pennsylvania, University of Chicago, Univer Sity of Chica Go, Ludwig-Maximilians Univer- Sität München, University of Portsmouth, ETH Zurich, Universidad Autonoma de Madrid, Argonne National Laboratory, Stanford University, University of Wisconsin- Madison, Carnegie Mellon University, Laboratório Interinstitucional de E-Astronomia - LIneA, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, The Ohio State Univer- Sity, University of Manchester, University of California, Santa Cruz Institute for Particle Physics, Fermi National Accelerator Laboratory, The Ohio State University, California Institute of Technology, SLAC National Accelerator Laboratory, University of Oxford, University of Gene Va, University of Michigan, University of Cambridge, Perimeter Institute for Theoretical Physics, Univer Sidade Estadual de Campinas, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, Institut D'Estudis Espacials de Catalunya (IEEC), CSIC), Max Planck Institute for Extraterrestrial Physics, University of Edinb Urgh, Universidade de São Paulo (USP), Universidade Estadual Paulista (UNESP), Institut D'Astrophysique de Paris, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, IIT Hyderabad, University of Oslo, Univer Sity of Cambridge, Harvard and Smithsonian, Lowell Observatory, Macquarie University, Texas A&M Univer Sity, Princeton University, Institució Catalana de Recerca i Estudis Avan C Ats, Univer Sity of Sussex, University of Southampton, Oak Ridge National Labo- Ratory, Kovács, A, Jeffrey, N, Gatti, M, Chang, C, Whiteway, L, Hamaus, N, Lahav, O, Pollina, G, Bacon, D, Kacprzak, T, Mawdsley, B, Nadathur, S, Zeurcher, D, García-Bellido, J, Alarcon, A, Amon, A, Bechtol, K, Bernstein, G M, Campos, A, Rosell, A Carnero, Kind, M Carrasco, Cawthon, R, Chen, R, Choi, A, Cordero, J, Davis, C, Derose, J, Doux, C, Drlica-Wagner, A, Eckert, K, Elsner, F, Elvin-Poole, J, Everett, S, Ferté, A, Giannini, G, Gruen, D, Gruendl, R A, Harrison, I, Hartley, W G, Herner, K, Huff, E M, Huterer, D, Kuropatkin, N, Jarvis, M, Leget, P F, Maccrann, N, Mccullough, J, Muir, J, Myles, J, Navarro-Alsina, A, Pandey, S, Prat, J, Raveri, M, Rollins, R P, Ross, A J, Rykoff, E S, Sánchez, C, Secco, L F, Sevilla-Noarbe, I, Sheldon, E, Shin, T, Troxel, M A, Tutusaus, I, Varga, T N, Yanny, B, Yin, B, Zhang, Y, Zuntz, J, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, D, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, Davis, T, De&nbsp, Vicente, J, Desai, S, Diehl, H T, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, Gaztañaga, E, Gerdes, D, Giannantonio, T, Gschwend, J, Gutierrez, G, Hinton, S, Hollowood, D L, Honscheid, K, James, D, Kuehn, K, Lima, M, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Ogando, R, Paz-Chinchon, F, Pieres, A, Plazas, A A, Monroy, M Rodriguez, Romer, K, Roodman, A, Sanchez, E, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, C-H, To, Weller, J, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), European Research Council, National Science Foundation (US), European Commission, and Agenzia Spaziale Italiana
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic Background Radiation, FOS: Physical sciences, Física, Astronomy and Astrophysics, cosmic background radiation, Surveys, gravitational lensing: weak, surveys, Space and Planetary Science, Weak [Gravitational Lensing], survey, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A. Kovács et al., The Cold Spot is a puzzling large-scale feature in the Cosmic Microwave Background temperature maps and its origin has been subject to active debate. As an important foreground structure at low redshift, the Eridanus supervoid was recently detected, but it was subsequently determined that, assuming the standard ΛCDM model, only about 10–20 per cent of the observed temperature depression can be accounted for via its Integrated Sachs–Wolfe imprint. However, R ≳ 100 h−1Mpc supervoids elsewhere in the sky have shown ISW imprints AISW ≈ 5.2 ± 1.6 times stronger than expected from ΛCDM (AISW = 1), which warrants further inspection. Using the Year-3 redMaGiC catalogue of luminous red galaxies from the Dark Energy Survey, here we confirm the detection of the Eridanus supervoid as a significant underdensity in the Cold Spot’s direction at z < 0.2. We also show, with S/N ≳ 5 significance, that the Eridanus supervoid appears as the most prominent large-scale underdensity in the dark matter mass maps that we reconstructed from DES Year-3 gravitational lensing data. While we report no significant anomalies, an interesting aspect is that the amplitude of the lensing signal from the Eridanus supervoid at the Cold Spot centre is about 30 per cent lower than expected from similar peaks found in N-body simulations based on the standard ΛCDM model with parameters Ωm = 0.279 and σ8 = 0.82. Overall, our results confirm the causal relation between these individually rare structures in the cosmic web and in the CMB, motivating more detailed future surveys in the Cold Spot region., AK has been supported by a Juan de la Cierva Incorporación fellowship with project number IJC2018-037730-I, and funding for this project was also available in part through SEV-2015-0548 and AYA2017-89891-P. 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 DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2021

4. The Dark Energy Survey Six-Year Calibration Star Catalog

Author: Rykoff, E. S., Tucker, D. L., Burke, D. L., Allam, S. S., Bechtol, K., Bernstein, G. M., Brout, D., Gruendl, R. A., Lasker, J., Smith, J. A., Wester, W. C., Yanny, B., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Carretero, J., Castander, F. J., Choi, A., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Giannini, G., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Lahav, O., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Myles, J., Nord, B. D., Ogando, R. L. C., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodgríguez-Monroy, M., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., and Wiseman, P.
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: This Technical Note presents a catalog of calibrated reference stars that was generated by the Forward Calibration Method (FGCM) pipeline (arXiv:1706.01542) as part of the FGCM photometric calibration of the full Dark Energy Survey (DES) 6-Year data set (Y6). This catalog provides DES grizY magnitudes for 17 million stars with i-band magnitudes mostly in the range 16 < i < 21 spread over the full DES footprint covering 5000 square degrees over the Southern Galactic Cap at galactic latitudes b < -20 degrees (plus a few outlying fields disconnected from the main survey footprint). These stars are calibrated to a uniformity of better than 1.8 milli-mag (0.18%) RMS over the survey area. The absolute calibration of the catalog is computed with reference to the STISNIC.007 spectrum of the Hubble Space Telescope CalSpec standard star C26202; including systematic errors, the absolute flux system is known at the approximately 1% level. As such, these stars provide a useful reference catalog for calibrating grizY-band or grizY-like band photometry in the Southern Hemisphere, particularly for observations within the DES footprint., 21 pages, 15 figures, Fermilab Technical Note. Official Data Access Site: https://des.ncsa.illinois.edu/releases/other ; Temporary Data Access Site: https://data.darkenergysurvey.org/public_calib/DES_6yr_CalibStarCat/index.html
Published: 2023
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5. Cosmological constraints from the tomography of DES-Y3 galaxies with CMB lensing from ACT DR4

Author: Marques, G. A., Madhavacheril, M. S., Darwish, O., Shaikh, S., Aguena, M., Alves, O., Avila, S., Bacon, D., Baxter, E. J., Bechtol, K., Becker, M. R., Bertin, E., Blazek, J., Bond, J. Richard, Brooks, D., Cai, H., Calabrese, E., Rosell, A. Carnero, Carretero, M. Carrasco Kind J., Cawthon, R., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Doux, C., Drlica-Wagner, A., Dunkley, J., Elvin-Poole, J., Everett, S., Ferraro, Simone, Ferrero, I., Flaugher, B., Fosalba, P., García-Bellido, J., Gatti, M., Giannini, G., Gluscevic, V., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hill, J. Colin, Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Jeffrey, N., Kim, J., Kuehn, K., Lahav, O., Lemos, P., Lima, M., Huffenberger, K. M., MacCrann, N., Marshall, J. L., Mena-Fernández, J., Miquel, R., Mohr, J. J., Moodley, K., Muir, J., Naess, S., Nati, F., Page, L. A., Palmese, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Qu, F. J., Raveri, M., Ross, A. J., Rykoff, E. S., Farren, G. S., Samuroff, S., Sanchez, E., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Spergel, D. N., Staggs, S. T., Suchyta, E., Tarle, G., To, C., Van Engelen, A., Weaverdyck, N., Weller, J., Wenzl, L., Wiseman, P., Wollack, E. J., and Yanny, B.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present a measurement of the cross-correlation between the MagLim galaxies selected from the Dark Energy Survey (DES) first three years of observations (Y3) and cosmic microwave background (CMB) lensing from the Atacama Cosmology Telescope (ACT) Data Release 4 (DR4), reconstructed over $\sim 436$ sq.deg. of the sky. Our galaxy sample, which covers $\sim 4143$ sq.deg., is divided into six redshift bins spanning the redshift range of $0.20, Comment: 42 pages, 17 figures
Published: 2023
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6. Ultracool dwarfs candidates based on six years of the Dark Energy Survey data

Author: Ponte, M. dal, Santiago, B., Rosell, A. Carnero, De Paris, L., Pace, A. B., Bechtol, K., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., Desai, S., De Vicente, J., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Malagón, A. A. Plazas, Pieres, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Weaverdyck, N.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present a sample of 19,583 ultracool dwarf candidates brighter than z $\leq 23$ selected from the Dark Energy Survey DR2 coadd data matched to VHS DR6, VIKING DR5 and AllWISE covering $\sim$ 4,800 $deg^2$. The ultracool candidates were first pre-selected based on their (i-z), (z-Y), and (Y-J) colours. They were further classified using a method that compares their optical, near-infrared and mid-infrared colours against templates of M, L and T dwarfs. 14,099 objects are presented as new L and T candidates and the remaining objects are from the literature, including 5,342 candidates from our previous work. Using this new and deeper sample of ultracool dwarf candidates we also present: 20 new candidate members to nearby young moving groups (YMG) and associations, variable candidate sources and four new wide binary systems composed of two ultracool dwarfs. Finally, we also show the spectra of twelve new ultracool dwarfs discovered by our group and presented here for the first time. These spectroscopically confirmed objects are a sanity check of our selection of ultracool dwarfs and photometric classification method., Comment: 18 pages, 10 figures, 7 tables. Accepted for publication in MNRAS
Published: 2023
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7. Synchronous rotation in the (136199) Eris-Dysnomia system

Author: Bernstein, G. M., Holler, B. J., Navarro-Escamilla, R., Bernardinelli, P. H., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carretero, J., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Drlica-Wagner, A., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gutierrez, G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Miquel, R., Ogando, R. L. C., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Reil, K., Sanchez, E., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., and Wiseman, P.
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: We combine photometry of Eris from a 6-month campaign on the Palomar 60-inch telescope in 2015, a 1-month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013--2018 to determine a light curve of definitive period $15.771\pm 0.008$~days (1-$\sigma$ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3\%. This is consistent at part-per-thousand precision with the $P=15.78590\pm0.00005$~day period of Dysnomia's orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szakats et al (2022) with independent data. Photometry from Gaia is consistent with the same light curve. We detect a slope of $0.05\pm0.01$~mag per degree of Eris' brightness with respect to illumination phase, intermediate between Pluto's and Charon's values. Variations of $0.3$~mag are detected in Dysnomia's brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris., Comment: Submitted to Planetary Science Journal
Published: 2023
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8. 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

9. 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

10. 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

11. 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

12. 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

13. C/2014 UN 271 (Bernardinelli-Bernstein): The Nearly Spherical Cow of Comets

Author: Bernardinelli, Pedro H., Bernstein, Gary M., Montet, Benjamin T., Weryk, Robert, Wainscoat, Richard, Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Kind, M. Carrasco, Carretero, J., Cawthon, R., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Paz-Chinch��n, F., Pieres, A., Malag��n, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Varga, T. N., Walker, A. R., Zhang, Y., Bernardinelli, Pedro H. [0000-0003-0743-9422], Bernstein, Gary M. [0000-0002-8613-8259], Montet, Benjamin T. [0000-0001-7516-8308], Weryk, Robert [0000-0002-0439-9341], Wainscoat, Richard [0000-0002-1341-0952], Aguena, M. [0000-0001-5679-6747], Annis, J. [0000-0002-0609-3987], Bertin, E. [0000-0002-3602-3664], Brooks, D. [0000-0002-8458-5047], Carretero, J. [0000-0002-3130-0204], Cawthon, R. [0000-0003-2965-6786], Conselice, C. [0000-0003-1949-7638], Costanzi, M. [0000-0001-8158-1449], Diehl, H. T. [0000-0002-8357-7467], García-Bellido, J. [0000-0002-9370-8360], Gaztanaga, E. [0000-0001-9632-0815], Gerdes, D. W. [0000-0001-6942-2736], Gruendl, R. A. [0000-0002-4588-6517], Gschwend, J. [0000-0003-3023-8362], Hinton, S. R. [0000-0003-2071-9349], Hollowood, D. L. [0000-0002-9369-4157], Kuehn, K. [0000-0003-0120-0808], Marshall, J. L. [0000-0003-0710-9474], 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], Roodman, A. [0000-0001-5326-3486], Sevilla-Noarbe, I. [0000-0002-1831-1953], Swanson, M. E. C. [0000-0002-1488-8552], Tarle, G. [0000-0003-1704-0781], To, C. [0000-0001-7836-2261], and Apollo - University of Cambridge Repository
Abstract: Comet C/2014 UN271 (Bernardinelli-Bernstein), incoming from the Oort cloud, is remarkable in having the brightest (and presumably largest) nucleus of any well-measured comet and having been discovered at the heliocentric distance r h �� 29 au, farther than any Oort cloud comet. In this work, we describe the discovery process and observations and the properties that can be inferred from images recorded until the first reports of activity in 2021 June. The orbit has i = 95��, with a perihelion of 10.97 au to be reached in 2031 and a previous aphelion at 40,400 �� 260 au. Backward integration of the orbit under a standard Galactic tidal model and known stellar encounters suggests a perihelion of q �� 18 au on its previous perihelion passage 3.5 Myr ago; hence, the current data could be the first ever obtained of a comet that has not been inside Uranus��s orbit in 4 Gyr. The photometric data show an unresolved nucleus with absolute magnitude H r = 8.0, colors that are typical of comet nuclei or Damocloids, and no secular trend as it traversed the range 34��23 au. For the r-band geometric albedo p r , this implies a diameter of 150(pr/0.04)��0.5 km. There is strong evidence of brightness fluctuations at the ��0.2 mag level, but no rotation period can be discerned. A coma, nominally consistent with a ��stationary�� 1/�� surface brightness distribution, grew in scattering cross section at an exponential rate from A f �� 1 to ��150 m as the comet approached from 28 to 20 au. The activity rate is consistent with a very simple model of sublimation of a surface species in radiative equilibrium with the Sun. The inferred enthalpy of sublimation matches those of CO2 and NH3. More volatile species, such as N2, CH4, and CO, must be far less abundant on the sublimating surfaces.
Published: 2021

14. The DECam Local Volume Exploration Survey Data Release 2

Author: Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Allam, S., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., de Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., T. S., Li, Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., Mcnanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Nilo Castellon, J. L., Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Plazas Malagón, A. A., Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., J. F., Wu, Yanny, B., Zaborowski, E., Zenteno, A., Delve, Collaboration, Des, Collaboration, Astro Data Lab, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, and Fundação de Amparo à Pesquisa do Estado de São Paulo
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astronomy and Astrophysics, Surveys, Astrophysics - Astrophysics of Galaxies, Catalogs, Local Group, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Catalog, Survey, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Full list of authors: Drlica-Wagner, A.; Ferguson, P. S.; Adamow, M.; Aguena, M.; Allam, S.; Andrade-Oliveira, F.; Bacon, D.; Bechtol, K.; Bell, E. F.; Bertin, E.; Bilaji, P.; Bocquet, S.; Bom, C. R.; Brooks, D.; Burke, D. L.; Carballo-Bello, J. A.; Carlin, J. L.; Carnero Rosell, A.; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cerny, W.; Chang, C.; Choi, Y.; Conselice, C.; Costanzi, M.; Crnojevic, D.; da Costa, L. N.; De Vicente, J.; Desai, S.; Esteves, J.; Everett, S.; Ferrero, I; Fitzpatrick, M.; Flaugher, B.; Friedel, D.; Frieman, J.; Garcia-Bellido, J.; Gatti, M.; Gaztanaga, E.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Hartley, W. G.; Hernandez-Lang, D.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Hughes, A. K.; Jacques, A.; James, D. J.; Johnson, M. D.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lidman, C.; Lin, H.; March, M.; Marshall, J. L.; Martinez-Delgado, D.; Martinez-Vazquez, C. E.; Massana, P.; Mau, S.; McNanna, M.; Melchior, P.; Menanteau, F.; Miller, A. E.; Miquel, R.; Mohr, J. J.; Morgan, R.; Mutlu-Pakdil, B.; Munoz, R. R.; Neilsen, E. H.; Nidever, D. L.; Nikutta, R.; Nilo Castellon, J. L.; Noel, N. E. D.; Ogando, R. L. C.; Olsen, K. A. G.; Pace, A. B.; Palmese, A.; Paz-Chinchon, F.; Pereira, M. E. S.; Pieres, A.; Malagon, A. A. Plazas; Prat, J.; Riley, A. H.; Rodriguez-Monroy, M.; Romer, A. K.; Roodman, A.; Sako, M.; Sakowska, J. D.; Sanchez, E.; Sanchez, F. J.; Sand, D. J.; Santana-Silva, L.; Santiago, B.; Schubnell, M.; Serrano, S.; Sevilla-Noarbe, I; Simon, J. D.; Smith, M.; Soares-Santos, M.; Stringfellow, G. S.; Suchyta, E.; Suson, D. J.; Tan, C. Y.; Tarle, G.; Tavangar, K.; Thomas, D.; To, C.; Tollerud, E. J.; Troxel, M. A.; Tucker, D. L.; Varga, T. N.; Vivas, A. K.; Walker, A. R.; Weller, J.; Wilkinson, R. D.; Wu, J. F.; Yanny, B.; Zaborowski, E.; Zenteno, A.; DELVE Collaboration; DES Collaboration; Astro Data Lab.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We present the second public data release (DR2) from the DECam Local Volume Exploration survey (DELVE). DELVE DR2 combines new DECam observations with archival DECam data from the Dark Energy Survey, the DECam Legacy Survey, and other DECam community programs. DELVE DR2 consists of ∼160,000 exposures that cover >21,000 deg2 of the high-Galactic-latitude (∣b∣ > 10°) sky in four broadband optical/near-infrared filters (g, r, i, z). DELVE DR2 provides point-source and automatic aperture photometry for ∼2.5 billion astronomical sources with a median 5σ point-source depth of g = 24.3, r = 23.9, i = 23.5, and z = 22.8 mag. A region of ∼17,000 deg2 has been imaged in all four filters, providing four-band photometric measurements for ∼618 million astronomical sources. DELVE DR2 covers more than 4 times the area of the previous DELVE data release and contains roughly 5 times as many astronomical objects. DELVE DR2 is publicly available via the NOIRLab Astro Data Lab science platform. © 2022. The Author(s). Published by the American Astronomical Society., The DELVE project is partially supported by Fermilab LDRD project L2019-011, the NASA Fermi Guest Investigator Program Cycle 9 grant 91201, and the National Science Foundation (NSF) under grant AST-2108168. This work is supported by the Fermilab Visiting Scholars Award Program from the Universities Research Association. A.B.P. acknowledges support from NSF grant AST-1813881. J.L.C. acknowledges support from NSF grant AST-1816196. J.D.S. acknowledges support from NSF grant AST-1714873. S.R.M. acknowledges support from NSF grant AST-1909497. D.J.S. acknowledges support from NSF grants AST-1821967 and AST-1813708. D.C. acknowledges support from NSF grant AST-1814208. B.M.P. acknowledges support from the NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2001663. S.M. acknowledges support from the NSF Graduate Research Fellowship under grant DGE-1656518. D.M.D. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the "Centre of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). C.P.M.B. and M.R.L.C. acknowledge support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement no. 682115). L.S.S. acknowledges the financial support from FAPESP through the grant #2020/03301-5. J.A.C.B. acknowledges support from ANID FONDECYT Regular 1220083. 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 á 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. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
Published: 2022

15. OzDES Reverberation Mapping Program: H$β$ lags from the 6-year survey

Author: Malik, Umang, Sharp, Rob, Penton, A., Yu, Z., Martini, P., Lidman, C., Tucker, B. E., Davis, T. M., Lewis, G. F., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Asorey, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Carretero, 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., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Taylor, G., Tucker, D. L., Weaverdyck, N., and Wilkinson, R. D.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: Reverberation mapping measurements have been used to constrain the relationship between the size of the broad-line region and luminosity of active galactic nuclei (AGN). This $R-L$ relation is used to estimate single-epoch virial black hole masses, and has been proposed for use to standardise AGN to determine cosmological distances. We present reverberation measurements made with H$β$ from the six-year Australian Dark Energy Survey (OzDES) Reverberation Mapping Program. We successfully recover reverberation lags for eight AGN at $0.12, Published in MNRAS
Published: 2022
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16. Dark Energy Survey Year 3 Results: Constraints on extensions to $Λ$CDM with weak lensing and galaxy clustering

Author: DES Collaboration, Abbott, T. M. C., Aguena, M., Alarcon, A., Alves, O., Amon, A., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Birrer, S., Blazek, J., Bocquet, S., Brandao-Souza, A., Bridle, S. L., Brooks, D., Burke, D. L., Camacho, H., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, C., Davis, T. M., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Farahi, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Friedrich, O., Frieman, J., García-Bellido, J., Gatti, M., Giani, L., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamaus, N., Harrison, I., Hartley, W. G., Herner, K., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huang, H., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Leget, P. -F., Lemos, P., Leonard, C. D., Liddle, A. R., Lima, M., Lin, H., MacCrann, N., Marshall, J. L., McCullough, J., Mena-Fernández, J., Menanteau, F., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R. C., Ogando, R. L. C., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paterno, M., Paz-Chinchón, F., Percival, W. J., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scarpine, V., Scolnic, D., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M. A., Tutusaus, I., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Yin, B., Zhang, Y., and Zuntz, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences
Abstract: We constrain extensions to the $Λ$CDM model using measurements from the Dark Energy Survey's first three years of observations and external data. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data and blind analyses of real data to validate the robustness of our results. In many cases, constraining power is limited by the absence of nonlinear predictions that are reliable at our required precision. The models are: dark energy with a time-dependent equation of state, non-zero spatial curvature, sterile neutrinos, modifications of gravitational physics, and a binned $σ_8(z)$ model which serves as a probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find $(w_{\rm p}, w_a)= (-0.99^{+0.28}_{-0.17},-0.9\pm 1.2)$ at 68% confidence with $z_{\rm p}=0.24$ from the DES measurements alone, and $(w_{\rm p}, w_a)= (-1.03^{+0.04}_{-0.03},-0.4^{+0.4}_{-0.3})$ with $z_{\rm p}=0.21$ for the combination of all data considered. Curvature constraints of $Ω_k=0.0009\pm 0.0017$ and effective relativistic species $N_{\rm eff}=3.10^{+0.15}_{-0.16}$ are dominated by external data. For massive sterile neutrinos, we improve the upper bound on the mass $m_{\rm eff}$ by a factor of three compared to previous analyses, giving 95% limits of $(ΔN_{\rm eff},m_{\rm eff})\leq (0.28, 0.20\, {\rm eV})$. We also constrain changes to the lensing and Poisson equations controlled by functions $Σ(k,z) = Σ_0 Ω_Λ(z)/Ω_{Λ,0}$ and $μ(k,z)=μ_0 Ω_Λ(z)/Ω_{Λ,0}$ respectively to $Σ_0=0.6^{+0.4}_{-0.5}$ from DES alone and $(Σ_0,μ_0)=(0.04\pm 0.05,0.08^{+0.21}_{-0.19})$ for the combination of all data. Overall, we find no significant evidence for physics beyond $Λ$CDM., Updated to match published version. 46 pages, 25 figures, data available at https://dev.des.ncsa.illinois.edu/releases/y3a2/Y3key-extensions
Published: 2022
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17. Identification of Galaxy-Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning

Author: Zaborowski, E., Drlica-Wagner, A., Ashmead, F., Wu, J. F., Morgan, R., Bom, C. R., Shajib, A. J., Birrer, S., Cerny, W., Buckley-Geer, L., Mutlu-Pakdil, B., Ferguson, P. S., Glazebrook, K., Lozano, S. J. Gonzalez, Gordon, Y., Martinez, M., Manwadkar, V., O'Donnell, J., Poh, J., Riley, A., Sakowska, J. D., Santana-Silva, L., Santiago, B. X., Sluse, D., Tan, C. Y., Tollerud, E. J., Verma, A., Carballo-Bello, J. A., Choi, Y., James, D. J., Kuropatkin, N., Martínez-Vázquez, C. E., Nidever, D. L., Castellon, J. L. Nilo, Noël, N. E. D., Olsen, K. A. G., Pace, A. B., Mau, S., Yanny, B., Zenteno, A., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Conselice, C. J., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Lin, H., Marshall, J. L., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., To, C., and Weaverdyck, N.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: We perform a search for galaxy-galaxy strong lens systems using a convolutional neural network (CNN) applied to imaging data from the first public data release of the DECam Local Volume Exploration Survey (DELVE), which contains $\sim 520$ million astronomical sources covering $\sim 4,000$ $\mathrm{deg}^2$ of the southern sky to a $5σ$ point-source depth of $g=24.3$, $r=23.9$, $i=23.3$, and $z=22.8$ mag. Following the methodology of similar searches using DECam data, we apply color and magnitude cuts to select a catalog of $\sim 11$ million extended astronomical sources. After scoring with our CNN, the highest scoring 50,000 images were visually inspected and assigned a score on a scale from 0 (definitely not a lens) to 3 (very probable lens). We present a list of 617 strong lens candidates, 599 of which are previously unreported. We categorize our candidates using their human-assigned scores, resulting in 60 Grade A candidates, 160 Grade B candidates, and 397 Grade C candidates. We additionally highlight 8 potential quadruply lensed quasars from this sample. Due to the location of our search footprint in the northern Galactic cap ($b > 10$ deg) and southern celestial hemisphere (${\rm Dec.}, 27 pages; added machine-readable table
Published: 2022
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18. 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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19. 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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20. 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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21. 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

22. Machine Learning for Searching the Dark Energy Survey for Trans-Neptunian Objects

Author: Henghes, B., Lahav, O., Gerdes, D. W., Lin, H. W., Morgan, R., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sánchez, C., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Wilkinson, R. D., DES Collaboration, UAM. Departamento de Física Teórica, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Henghes, B., Lahav, O., Gerdes, D. W., Lin, H. W., Morgan, R., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sánchez, C., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Wilkinson, R. D., and Des, Collaboration
Subjects: Random Forests, FOS: Computer and information sciences, Solar System, Computer Science - Machine Learning, 010504 meteorology & atmospheric sciences, Computer science, FOS: Physical sciences, Machine learning, computer.software_genre, 01 natural sciences, Minor Planets, Machine Learning (cs.LG), Planet, 0103 physical sciences, Minor planet, Astrophysics - Earth and Planetary Astrophysic, [INFO]Computer Science [cs], Trans-Neptunian object, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), Random Forest, Receiver operating characteristic, business.industry, Trans-Neptunian objects, Minor planets, Computational methods, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Física, Astronomy and Astrophysics, Computational method, Trans-Neptunian Objects, Random forest, Space and Planetary Science, Asteroid, Artificial intelligence, business, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], computer, Classifier (UML), Computational Methods
Abstract: In this paper we investigate how implementing machine learning could improve the efficiency of the search for Trans-Neptunian Objects (TNOs) within Dark Energy Survey (DES) data when used alongside orbit fitting. The discovery of multiple TNOs that appear to show a similarity in their orbital parameters has led to the suggestion that one or more undetected planets, an as yet undiscovered "Planet 9", may be present in the outer Solar System. DES is well placed to detect such a planet and has already been used to discover many other TNOs. Here, we perform tests on eight different supervised machine learning algorithms, using a dataset consisting of simulated TNOs buried within real DES noise data. We found that the best performing classifier was the Random Forest which, when optimised, performed well at detecting the rare objects. We achieve an area under the receiver operating characteristic (ROC) curve, (AUC) $= 0.996 \pm 0.001$. After optimizing the decision threshold of the Random Forest, we achieve a recall of 0.96 while maintaining a precision of 0.80. Finally, by using the optimized classifier to pre-select objects, we are able to run the orbit-fitting stage of our detection pipeline five times faster., Comment: Published in PASP, 16 pages, 6 figures
Published: 2020
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23. Shadows in the Dark: Low-Surface-Brightness Galaxies Discovered in the Dark Energy Survey

Author: Tanoglidis, D., Drlica-Wagner, A., Wei, K., Li, T. S., Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., DeRose, J., Conselice, C., Gagnon, L., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., Walker, A. R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), UAM. Departamento de Física Teórica, Tanoglidis, D., Drlica-Wagner, A., Wei, K., T. S., Li, Sánchez, F. J., Zhang, Y., Peter, A. H. G., Feldmeier-Krause, A., Prat, J., Casey, K., Palmese, A., Sánchez, C., Derose, J., Conselice, C., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Huterer, D., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, D. L., and Walker, A. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, Sky surveys, 01 natural sciences, Imaging data, Luminosity, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Coma Cluster, Surface brightness, Sky survey, Global Air Sampling Program, education, 010303 astronomy & astrophysics, STFC, Low surface brightness galaxie, Physics, education.field_of_study, 010308 nuclear & particles physics, Física, RCUK, Astronomy and Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Star Formation, Dark energy, Low surface brightness galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a catalog of 23,790 extended low-surface-brightness galaxies (LSBGs) identified in $\sim 5000 ��^2$ from the first three years of imaging data from the Dark Energy Survey (DES). Based on a single-component S��rsic model fit, we define extended LSBGs as galaxies with $g$-band effective radii $R_{eff}(g) > 2.5''$ and mean surface brightness $\bar��_{eff}(g) > 24.2 \,mag ��rcsec^{-2}$. We find that the distribution of LSBGs is strongly bimodal in $(g-r)$ vs.\ $(g-i$) color space. We divide our sample into red ($g-i \geq 0.60$) and blue ($g-i 1.5 \,kpc$ and central surface brighthness $��_0(g) > 24.0\, mag \,arcsec^{-2}$. The wide-area sample of LSBGs in DES can be used to test the role of environment on models of LSBG formation and evolution., 31 pages, 19 figures. Version accepted for publication in ApJS. Data products related to this work can be found in: https://des.ncsa.illinois.edu/releases/other/y3-lsbg
Published: 2020
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24. A DESGW search for the electromagnetic counterpart to the LIGO/Virgo gravitational-wave binary neutron star merger candidate S190510g

Author: Garcia, A., Morgan, R., Herner, K., Palmese, A., Soares-Santos, M., Annis, J., Brout, D., Vivas, A. K., Drlica-Wagner, A., Santana-Silva, L., Tucker, D. L., Allam, S., Wiesner, M., García-Bellido, J., Gill, M. S. S., Sako, M., Kessler, R., Davis, T. M., Scolnic, D., Casares, J., Chen, H., Conselice, C., Cooke, J., Doctor, Z., Foley, R. J., Horvath, J., Howell, D. A., Kilpatrick, C. D., Lidman, C., E. , F. Olivares, Paz-Chinchón, F., Pineda-G. , J., Quirola-Vásquez, J., Rest, A., Sherman, N., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., 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., Everett, S., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Weller, J., Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), Higher Education Funding Council for England, University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), German Research Foundation, University of California, Argonne National Laboratory (US), University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (España), University College London, University of London, University of Edinburgh, Federal Institute of Technology Zurich, Consejo Superior de Investigaciones Científicas (España), University of Michigan, University of Pennsylvania, Stanford University, European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Garcia, A., Morgan, R., Herner, K., Palmese, A., Soares-Santos, M., Annis, J., Brout, D., Vivas, A. K., Drlica-Wagner, A., Santana-Silva, L., Tucker, D. L., Allam, S., Wiesner, M., García-Bellido, J., Gill, M. S. S., Sako, M., Kessler, R., Davis, T. M., Scolnic, D., Casares, J., Chen, H., Conselice, C., Cooke, J., Doctor, Z., Foley, R. J., Horvath, J., Howell, D. A., Kilpatrick, C. D., Lidman, C., F. Olivares, E., Paz-Chinchón, F., Pineda-G., J., Quirola-Vásquez, J., Rest, A., Sherman, N., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., 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., Everett, S., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., and Weller, J.
Subjects: neutron star: binary, Software_OPERATINGSYSTEMS, 010504 meteorology & atmospheric sciences, Binary number, Astrophysics, Kilonova, 7. Clean energy, 01 natural sciences, optical, LIGO, dark energy, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), ComputerSystemsOrganization_PROCESSORARCHITECTURES, Supernova, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, data analysis method, ComputingMethodologies_SIMULATIONANDMODELING, FOS: Physical sciences, Data_CODINGANDINFORMATIONTHEORY, Gravitational-wave astronomy, electromagnetic field: production, Gravitational wave astronomy (675), binary: coalescence, 0103 physical sciences, Binary star, supernova, Hardware_INTEGRATEDCIRCUITS, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], detector: optical, Instrumentation and Methods for Astrophysics (astro-ph.IM), STFC, 0105 earth and related environmental sciences, Gravitational wave, gravitational radiation, RCUK, Astronomy and Astrophysics, Neutron star, VIRGO, 13. Climate action, Space and Planetary Science, gravitational radiation: emission, gravitational wave astronomy, Gravitational wave astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: DES Collaboration: et al., We present the results from a search for the electromagnetic counterpart of the LIGO/Virgo event S190510g using the Dark Energy Camera (DECam). S190510g is a binary neutron star (BNS) merger candidate of moderate significance detected at a distance of 227 ± 92 Mpc and localized within an area of 31 (1166) square degrees at 50% (90%) confidence. While this event was later classified as likely nonastrophysical in nature within 30 hours of the event, our short latency search and discovery pipeline identified 11 counterpart candidates, all of which appear consistent with supernovae following offline analysis and spectroscopy by other instruments. Later reprocessing of the images enabled the recovery of six more candidates. Additionally, we implement our candidate selection procedure on simulated kilonovae and supernovae under DECam observing conditions (e.g., seeing and exposure time) with the intent of quantifying our search efficiency and making informed decisions on observing strategy for future similar events. This is the first BNS counterpart search to employ a comprehensive simulation-based efficiency study. We find that using the current follow-up strategy, there would need to be 19 events similar to S190510g for us to have a 99% chance of detecting an optical counterpart, assuming a GW170817-like kilonova. We further conclude that optimization of observing plans, which should include preference for deeper images over multiple color information, could result in up to a factor of 1.5 reduction in the total number of follow-ups needed for discovery., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, 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 InterAmerican Observatory at NSFs NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007–2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 1744555. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. R.M. thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant #1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. F.O.E. acknowledges support from the FONDECYT grant No. 1201223.
Published: 2020

25. 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

26. 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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27. OzDES Reverberation Mapping Program: The first Mg II lags from five years of monitoring

Author: Yu, Zhefu, Martini, Paul, Penton, A., Davis, T. M., Malik, U., Lidman, C., Tucker, B. E., Sharp, R., Kochanek, C. S., Peterson, B. M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Asorey, J., Bertin, E., Brooks, D., Burke, D. L., Calcino, J., Rosell, A. Carnero, Carollo, D., Kind, M. Carrasco, Costanzi, M., da Costa, L. N., Pereira, M. E. S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kim, A. G., Kron, R., Kuehn, K., Kuropatkin, N., Lewis, G. F., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Möller, A., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., and Tucker, D. L.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract: Reverberation mapping is a robust method to measure the masses of supermassive black holes (SMBHs) outside of the local Universe. Measurements of the radius -- luminosity ($R-L$) relation using the Mg II emission line are critical for determining these masses near the peak of quasar activity at $z \approx 1 - 2$, and for calibrating secondary mass estimators based on Mg II that can be applied to large samples with only single-epoch spectroscopy. We present the first nine Mg II lags from our five-year Australian Dark Energy Survey (OzDES) reverberation mapping program, which substantially improves the number and quality of Mg II lag measurements. As the Mg II feature is somewhat blended with iron emission, we model and subtract both the continuum and iron contamination from the multi-epoch spectra before analyzing the Mg II line. We also develop a new method of quantifying correlated spectroscopic calibration errors based on our numerous, contemporaneous observations of F-stars. The lag measurements for seven of our nine sources are consistent with both the H$\beta$ and Mg II $R-L$ relations reported by previous studies. Our simulations verify the lag reliability of our nine measurements, and we estimate that the median false positive rate of the lag measurements is $4\%$., Comment: 18 pages, 12 figures. MNRAS, Volume 507, Issue 3, November 2021, Pages 3771-3788
Published: 2021
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28. 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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29. $��_{\star}$ 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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30. Three new VHS-DES Quasars at 6.7 < z < 6.9 and Emission Line Properties at z > 6.5

Author: Reed, S. L., Banerji, M., Becker, G. D., Hewett, P. C., Martini, P., McMahon, R. G., Pons, E., Rauch, M., Abbott, T. M. C., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Evrard, A. E., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., and Vikram, V.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: We report the results from a search for z > 6.5 quasars using the Dark Energy Survey (DES) Year 3 dataset combined with the VISTA Hemisphere Survey (VHS) and WISE All-Sky Survey. Our photometric selection method is shown to be highly efficient in identifying clean samples of high-redshift quasars leading to spectroscopic confirmation of three new quasars - VDESJ 0244-5008 (z=6.724), VDESJ 0020-3653 (z=6.834) and VDESJ 0246-5219 (z=6.90) - which were selected as the highest priority candidates in the survey data without any need for additional follow-up observations. The new quasars span the full range in luminosity covered by other z>6.5 quasar samples (J AB = 20.2 to 21.3; M1450 = -25.6 to -26.6). We have obtained spectroscopic observations in the near infrared for VDESJ 0244-5008 and VDESJ 0020-3653 as well as our previously identified quasar, VDESJ 0224-4711 at z=6.50 from Reed et al. (2017). We use the near infrared spectra to derive virial black-hole masses from the full-width-half-maximum of the MgII line. These black-hole masses are ~ 1 - 2 x 10$^9$M$_\odot$. Combining with the bolometric luminosities of these quasars of L$_{\rm{bol}}\simeq$ 1 - 3 x 10$^{47}$implies that the Eddington ratios are high - $\simeq$0.6-1.1. We consider the C\textrm{\textsc{IV}} emission line properties of the sample and demonstrate that our high-redshift quasars do not have unusual C\textrm{\textsc{IV}} line properties when compared to carefully matched low-redshift samples. Our new DES+VHS $z>6.5$ quasars now add to the growing census of luminous, rapidly accreting supermassive black-holes seen well into the epoch of reionisation., 12 pages, 9 figures
Published: 2019
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31. 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

32. 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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33. 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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34. 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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35. 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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36. 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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37. Multi-messenger Observations of a Binary Neutron Star Merger

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., 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., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., 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, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H.-P., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, A. K. W., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P.-F., Cohen, D., Colla, A., Collette, C. G., Cominsky, L. R., Jr., M. Constancio, Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J.-P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., Danilishin, S. L., D’Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., Laurentis, M. De, Deléglise, S., Pozzo, W. Del, Demos, N., Denker, T., Dent, T., Pietri, R. De, Dergachev, V., Rosa, R. De, DeRosa, R. T., Rossi, C. De, DeSalvo, R., Varona, O. de, Devenson, J., Dhurandhar, S., Díaz, M. C., Fiore, L. Di, Giovanni, M. Di, Girolamo, T. Di, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Renzo, F. Di, Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Álvarez, M. Dovale, Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J.-D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Griswold, B., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C.-J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J.-M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kéfélian, F., Keitel, D., Kemball, A. J., Kennedy, R., Kent, C., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y.-M., Kimbrell, S. J., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Krämer, C., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Landry, M., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Larson, S. L., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T. G. F., Linker, S. D., Littenberg, T. B., Liu, J., Lo, R. K. L., Lockerbie, N. A., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Hernandez, I. Magaña, Magaña-Sandoval, F., Zertuche, L. Magaña, Magee, R. M., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsh, P., Martelli, F., Martellini, L., 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., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McNeill, L., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R. A., 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, B. B., Miller, J., Millhouse, M., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Newport, J. M., Newton, G., Ng, K. K. Y., Nguyen, P., Nguyen, T. T., Nichols, D., Nielsen, A. B., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L. K., Oberling, J., O’Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O’Reilly, B., Ormiston, R., Ortega, L. F., O’Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Page, J., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C. J., Perreca, A., Perri, L. M., Pfeiffer, H. P., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pirello, M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Porter, E. K., Post, A., Powell, J., Prasad, J., Pratt, J. W. W., Pratten, G., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Reyes, S. D., Ricci, F., Ricker, P. M., Rieger, S., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romel, C. L., Romie, J. H., Rosińska, D., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L. M., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T. J., Shah, A. A., Shahriar, M. S., Shaner, M. B., Shao, L., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, A., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, B., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sonnenberg, J. A., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A. P., Srivastava, A. K., Staats, K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., 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, J. A., Taylor, R., Tewari, S. V., Theeg, T., Thies, F., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. 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O., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Kukec Mezek, G., Kunka, N., Kuotb Awad, A., Lago, B. L., LaHurd, D., Lang, R. G., Lauscher, M., Legumina, R., Leigui de Oliveira, M. A., Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lo Presti, D., Lopes, L., López, R., López Casado, A., Lorek, R., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A. G., Maris, I. C., Marsella, G., Martello, D., Martinez, H., Martínez Bravo, O., Masías Meza, J. J., Mathes, H. J., Mathys, S., Matthews, J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K.-D., Michal, S., Micheletti, M. I., Middendorf, L., Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Morlino, G., Müller, A. L., Müller, G., Muller, M. A., Müller, S., Mussa, R., Naranjo, I., Nguyen, P. H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pȩkala, J., Peña-Rodriguez, J., Pereira, L. A. S., Perlin, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Poh, J., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos-Pollan, R., Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., Rodrigues de Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Saleh, A., Salina, G., Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schröder, S., Schumacher, J., Sciutto, S. J., Segreto, A., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Soriano, J. F., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez-Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Šupík, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Timmermans, C., Todero Peixoto, C. J., Tomankova, L., Tomé, B., Torralba Elipe, G., Travnicek, P., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, M., Valdés Galicia, J. F., Valiño, I., Valore, L., Aar, G. van, Bodegom, P. van, van den Berg, A. M., Vliet, A. van, Varela, E., Cárdenas, B. Vargas, Vázquez, R. A., Veberič, D., Ventura, C., Vergara Quispe, I. D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiedeński, M., Wiencke, L., Wilczyński, H., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Kim, S., Schulze, S., Corral-Santana, J. M., de Gregorio-Monsalvo, I., González-López, J., Hartmann, D. H., Ishwara-Chandra, C. H., Martín, S., Mehner, A., Misra, K., Michałowski, M. J., Resmi, L., Paragi, Z., Agudo, I., An, T., Beswick, R., Casadio, C., Frey, S., Jonker, P., Kettenis, M., Marcote, B., Moldon, J., Szomoru, A., van Langevelde, H. J., Cwiek, A., Cwiok, M., Czyrkowski, H., Dabrowski, R., Kasprowicz, G., Mankiewicz, L., Nawrocki, K., Opiela, R., Piotrowski, L. W., Wrochna, G., Zaremba, M., Żarnecki, A. F., Haggard, D., Nynka, M., Ruan, J. J., Bland, P. A., Booler, T., Devillepoix, H. A. R., Gois, J. S. de, Hancock, P. J., Howie, R. M., Paxman, J., Sansom, E. K., Towner, M. C., Tonry, J., Coughlin, M., Stubbs, C. W., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R. P., Kramer, M., Kraus, A., Piro, L., González, J. Becerra, Butler, N. R., Khandrika, H. G., Kutyrev, A., Lee, W. H., Ricci, R., Ryan Jr., R. E., Sánchez-Ramírez, R., Veilleux, S., Watson, A. M., Wieringa, M. H., Burgess, J. M., Eerten, H. van, Fontes, C. J., Korobkin, O., Wollaeger, R. T., Camilo, F., Foley, A. R., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O. M., and Woudt, P. A.
Subjects: ddc
Published: 2016

38. 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

39. 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

40. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F, Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P, Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Danilishin, S. L., Antonio de Ugarte Postigo, Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., Debra, D., Debreczeni, G., Degallaix, J., Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., Derosa, R. T., Rosa, R., Desalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B, Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D, Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J, Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M, Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., K, H., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. -M, King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O Reilly, B., O Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal-Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Bakel, N., Beuzekom, M., Den Brand, J. F. J., Den Broeck, C., Vander-Hyde, D. C., Schaaf, L., Heijningen, J. V., Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. -Y, Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. -W, Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. -P, Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Ligo, For The Scientific Collaboration, the Virgo Collaboration, Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey-Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., Mcconnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Australian Square Kilometer Array Pathfinder, For The, Collaboration, Castro-Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Zhang, B. -B, Hu, Y. -D, Kubánek, P., Guziy, S., Castellón, A., García-Cerezo, A., Muñoz, V. F., Pérez Del Pulgar, C., Castillo-Carrión, S., Castro Cerón, J. M., Hudec, R., Caballero-García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Mateo Sanguino, T. J., Fernández-Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, Ch, Fan, Y., Wang, Ch, Hiriart, D., Lee, W. H., Claret, A., Sánchez-Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau-Graziati, L., Bootes, For The Collaboration, Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit-Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D Andrea, C. B., Da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. -F, Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares-Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Dark Energy Survey, For The, Gw-Em, The Dark Energy Camera Collaborations, Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Hui, C. M., Jenke, P., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., Kienlin, A., Kippen, R. M., Mcbreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. -F, Blackburn, L., Gbm, For The Fermi Collaboration, Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D Ammando, F., Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., Mcenery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Saz Parkinson, P. M., Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Lat, For The Fermi Collaboration, Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D Avanzo, P., D Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., for the GRAvitational Wave Inaf TeAm, Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L, Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Integral, For The Collaboration, Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Intermediate Palomar Transient Factory, For The, Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Interplanetary Network, For The, Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., J-Gem, For The Collaboration, Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., La Silla--Quest Survey, For The, Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., for the Liverpool Telescope Collaboration, Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Low Frequency Array, For The, Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra-Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Master, For The Collaboration, Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Maxi, For The Collaboration, Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Murchison Wide-Field Array, For The, Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., for the Pan-STARRS Collaboration, Olivares E, F., Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. -W, Valle, M. D., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Le Guillou, L., Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal-Yam, A., Pessto, For The Collaboration, Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., for the Pi of the Sky Collaboration, Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., for the SkyMapper Collaboration, Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O Brien, P., Osborne, J. P., Palmer, D., Perri, M., Racusin, J., Siegel, M., Tagliaferri, G., for the Swift Collaboration, Klotz, A., Turpin, D., Laugier, R., Tarot, For The, Zadko, National Observatory, Algerian, Pu Collaboration, C., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., Depoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Toros, For The Collaboration, Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang-Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., Mcmahon, R. G., Banerji, M., Gonzalez-Solares, E., Schulze, S., Postigo, A. U., Thoene, C. C., Cano, Z., Rosswog, S., Vista, For The Collaboration, LIGO, California Institute of Technology (CALTECH), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire des matériaux avancés (LMA), 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, Institut Lumière Matière [Villeurbanne] (ILM), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), 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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), VIRGO, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut National de 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), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)
Subjects: astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Gravitation, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], gr-qc, ST/I001123/1, gravitational radiation, RCUK, FOS: Physical sciences, electromagnetic [current], General Relativity and Quantum Cosmology (gr-qc), gravitational radiation detector, localization, General Relativity and Quantum Cosmology, electromagnetic, emission [gravitational radiation], ST/L000709/1, Computer Science::Multimedia, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], ddc:520, Astrophysics - High Energy Astrophysical Phenomena, STFC, QB
Abstract: This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492
Published: 2016
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41. 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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42. 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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43. 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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44. COSMOGRAIL XVI: Time delays for the quadruply imaged quasar DES J0408-5354 with high-cadence photometric monitoring

Author: Courbin, F., Bonvin, V., Buckley-Geer, E., Fassnacht, C. D., Frieman, J., Lin, H., Marshall, P. J., Suyu, S. H., Treu, T., Anguita, T., Motta, V., Meylan, G., Paic, E., Tewes, M., Agnello, A., Chao, D. C. -Y, Chijani, M., Gilman, D., Rojas, K., Williams, P., Hempel, A., Kim, S., Lachaume, R., Rabus, M., Abbott, T. M. C., Allam, S., Annis, J., Banerji, M., Bechtol, K., Benoit-Lévy, A., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., D Andrea, C. B., Da Costa, L. N., Davis, C., Depoy, D. L., Desai, S., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Richard McMahon, Menanteau, F., Miquel, R., Nord, B., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Tucker, D. L., Walker, A. R., and Wester, W.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies
Abstract: We present time-delay measurements for the new quadruply imaged quasar DES J0408-5354, the first quadruply imaged quasar found in the Dark Energy Survey (DES). Our result is made possible by implementing a new observational strategy using almost daily observations with the MPIA 2.2m telescope at La Silla observatory and deep exposures reaching a signal-to-noise ratio of about 1000 per quasar image. This data quality allows us to catch small photometric variations (a few mmag rms) of the quasar, acting on temporal scales much shorter than microlensing, hence making the time delay measurement very robust against microlensing. In only 7 months we measure very accurately one of the time delays in DES J0408-5354: Dt(AB) = -112.1 +- 2.1 days (1.8%) using only the MPIA 2.2m data. In combination with data taken with the 1.2m Euler Swiss telescope, we also measure two delays involving the D component of the system Dt(AD) = -155.5 +- 12.8 days (8.2%) and Dt(BD) = -42.4 +- 17.6 days (41%), where all the error bars include systematics. Turning these time delays into cosmological constraints will require deep HST imaging or ground-based Adaptive Optics (AO), and information on the velocity field of the lensing galaxy., 9 pages, 5 figures, accepted for publication in Astronomy & Astrophysics

45. Dark Energy Survey Year 3 Results: Multi-Probe Modeling Strategy and Validation

Author: Krause, E., Xiao Fang, Pandey, S., Secco, L. F., Alves, O., Huang, H., Blazek, J., Prat, J., Zuntz, J., Eifler, T. F., Maccrann, N., Derose, J., Crocce, M., Porredon, A., Jain, B., Troxel, M. A., Dodelson, S., Huterer, D., Liddle, A. R., Leonard, C. D., Amon, A., Chen, A., Elvin-Poole, J., Ferté, A., Muir, J., Park, Y., Samuroff, S., Brandao-Souza, A., Weaverdyck, N., Zacharegkas, G., Rosenfeld, R., Campos, A., Prudhvi Raj Varma Chintalapati, Choi, A., Di Valentino, E., Doux, C., Herner, K., Lemos, P., Mena-Fernández, J., Omori, Y., Paterno, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R. P., Troja, A., Tutusaus, I., Wechsler, R. H., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Baxter, E., Bechtol, K., Bernstein, G. M., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Myles, J., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., and Weller, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper details the modeling pipeline and validates the baseline analysis choices of the DES Year 3 joint analysis of galaxy clustering and weak lensing (a so-called "3$\times$2pt" analysis). These analysis choices include the specific combination of cosmological probes, priors on cosmological and systematics parameters, model parameterizations for systematic effects and related approximations, and angular scales where the model assumptions are validated. We run a large number of simulated likelihood analyses using synthetic data vectors to test the robustness of our baseline analysis. We demonstrate that the DES Year 3 modeling pipeline, including the calibrated scale cuts, is sufficiently accurate relative to the constraining power of the DES Year 3 analyses. Our systematics mitigation strategy accounts for astrophysical systematics, such as galaxy bias, intrinsic alignments, source and lens magnification, baryonic effects, and source clustering, as well as for uncertainties in modeling the matter power spectrum, reduced shear, and estimator effects. We further demonstrate excellent agreement between two independently-developed modeling pipelines, and thus rule out any residual uncertainties due to the numerical implementation., Comment: part of the DES year-3 combined 2-point function analysis; see https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release

46. 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

47. 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., Risa Wechsler, 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., Dietrich, J. P., 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., 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.

48. The redMaPPer Galaxy Cluster Catalog From DES Science Verification Data

Author: Rykoff, E. S., Rozo, E., Hollowood, D., Bermeo-Hernandez, A., Jeltema, T., Mayers, J., Romer, A. K., Rooney, P., Saro, A., Vergara Cervantes, C., Wilcox, H., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Capozzi, D., Carnero Rosell, A., Carrasco Kind, M., Castander, F. J., Childress, M., Collins, C. A., Cunha, C. E., D Andrea, C. B., Da Costa, L. N., Davis, T. M., Desai, S., Diehl, H. T., Jörg Dietrich, Doel, P., Evrard, A. E., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Hilton, M., Honscheid, K., Hoyle, B., James, D. J., Kay, S. T., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Mann, R. G., 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., Sahlén, M., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Stott, J. P., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D., Viana, P. T. P., Vikram, V., Walker, A. R., and Zhang, Y.

49. 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

50. Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey Data: Stellar Mass Growth of Bright Central Galaxies Since z~1.2

Author: Zhang, Y., Miller, C., Mckay, T., Rooney, P., August Evrard, Romer, A. K., Perfecto, R., Song, J., Desai, S., Mohr, J., Wilcox, H., Bermeo, A., Jeltema, T., Hollowood, D., Bacon, D., Capozzi, D., Collins, C., Das, R., Gerdes, D., Hennig, C., Hilton, M., Hoyle, B., Kay, S., Liddle, A., Mann, R. G., Mehrtens, N., Nichol, R. C., Papovich, C., Sahlén, M., Soares-Santos, M., Stott, J., Viana, P. T., Abbott, T., Abdalla, F. B., Banerji, M., Bauer, A. H., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Castander, F. J., Diehl, H. T., Doel, P., Cunha, C. E., Eifler, T. F., Fausti Neto, A., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Makler, M., Marshall, J. L., Martini, Paul, Miquel, R., Ogando, R., Plazas, A. A., Roodman, A., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla, I., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Tucker, D., Vikram, V., and Da Costa, L. N.

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