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1. The Dark Energy Survey Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5000 Square Degree Footprint

Author

O’Donnell, JH, Wilkinson, RD, Diehl, HT, Aros-Bunster, C, Bechtol, K, Birrer, S, Buckley-Geer, EJ, Carnero Rosell, A, Carrasco Kind, M, Da Costa, LN, Gonzalez Lozano, SJ, Gruendl, RA, Hilton, M, Lin, H, Lindgren, KA, Martin, J, Pieres, A, Rykoff, ES, Sevilla-Noarbe, I, Sheldon, E, Sifón, C, Tucker, DL, Yanny, B, Abbott, TMC, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Bertin, E, Brooks, D, Burke, DL, Carretero, J, Costanzi, M, De Vicente, J, Desai, S, Dietrich, JP, Eckert, K, Everett, S, Ferrero, I, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gschwend, J, Gill, MSS, Gutierrez, G, Hinton, Hollowood, DL, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Nord, B, Ogando, RLC, Paz-Chinchón, F, Pereira, MES, Plazas Malagón, AA, Rodriguez-Monroy, M, Romer, AK, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Smith, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, To, C, Varga, TN, O’Donnell, JH [0000-0003-4083-1530], Wilkinson, RD [0000-0002-3908-7313], Diehl, HT [0000-0002-8357-7467], Aros-Bunster, C [0000-0002-9441-3193], Birrer, S [0000-0003-3195-5507], Buckley-Geer, EJ [0000-0002-3304-0733], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], da Costa, LN [0000-0002-7731-277X], Gonzalez Lozano, SJ [0000-0001-7282-3864], Gruendl, RA [0000-0002-4588-6517], Hilton, M [0000-0002-8490-8117], Lin, H [0000-0002-7825-3206], Lindgren, KA [0000-0002-8414-7776], Pieres, A [0000-0001-9186-6042], Rykoff, ES [0000-0001-9376-3135], Sevilla-Noarbe, I [0000-0002-1831-1953], Sheldon, E [0000-0001-9194-0441], Sifón, C [0000-0002-8149-1352], Tucker, DL [0000-0001-7211-5729], Yanny, B [0000-0002-9541-2678], Abbott, TMC [0000-0003-1587-3931], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bertin, E [0000-0002-3602-3664], Brooks, D [0000-0002-8458-5047], Burke, DL [0000-0003-1866-1950], Carretero, J [0000-0002-3130-0204], Costanzi, M [0000-0001-8158-1449], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Eckert, K [0000-0002-1407-4700], Ferrero, I [0000-0002-1295-1132], Flaugher, B [0000-0002-2367-5049], Fosalba, P [0000-0002-1510-5214], Frieman, J [0000-0003-4079-3263], 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], Gschwend, J [0000-0003-3023-8362], Gill, MSS [0000-0003-2524-5154], 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], Jeltema, T [0000-0001-6089-0365], Kuehn, K [0000-0003-0120-0808], Lahav, O [0000-0002-1134-9035], Lima, M [0000-0002-4719-3781], Maia, MAG [0000-0001-9856-9307], 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], Nord, B [0000-0001-6706-8972], Ogando, RLC [0000-0003-2120-1154], Paz-Chinchón, F [0000-0003-1339-2683], Plazas Malagón, AA [0000-0002-2598-0514], Rodriguez-Monroy, M [0000-0001-6163-1058], Romer, AK [0000-0002-9328-879X], Roodman, A [0000-0001-5326-3486], Sanchez, E [0000-0002-9646-8198], Schubnell, M [0000-0001-9504-2059], Smith, M [0000-0002-3321-1432], Suchyta, E [0000-0002-7047-9358], Swanson, MEC [0000-0002-1488-8552], Tarle, G [0000-0003-1704-0781], Thomas, D [0000-0002-6325-5671], To, C [0000-0001-7836-2261], Apollo - University of Cambridge Repository, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, European Research Council, UAM. Departamento de Física Teórica, University of California at Santa Cruz, University of Sussex, Fermi National Accelerator Laboratory, Pontificia Universidad Católica de Valparaíso, University of Wisconsin-Madison, Stanford University, 382 Via Pueblo Mall, University of Chicago, Laboratório Interinstitucional de E-Astronomia - LIneA, Observatório Nacional, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Westville Campus, Brookhaven National Laboratory, Half Hollow Hills High School East, SLAC National Accelerator Laboratory, Medioambientales y Tecnológicas (CIEMAT), NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique de Paris, University College London, The Barcelona Institute of Science and Technology, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, IIT Hyderabad, Ludwig-Maximilians-Universität, University of Pennsylvania, Santa Cruz Institute for Particle Physics, University of Oslo, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE-CSIC), Universidad Autonoma de Madrid, University of Michigan, University of Queensland, The Ohio State University, Center for Astrophysics|Harvard and Smithsonian, Macquarie University, Lowell Observatory, Universidade de São Paulo (USP), Texas AandM University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, Universität Hamburg, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Giessenbachstrasse, Ludwig-Maximilians Universität München, A O'Donnell, J. H., Wilkinson, R. D., Diehl, H. T., Aros-Bunster, C., Bechtol, K., Birrer, S., Buckley-Geer, E. J., Carnero Rosell, A., Carrasco Kind, M., da Costa, L. N., Gonzalez Lozano, S. J., Gruendl, R. A., Hilton, M., Lin, H., Lindgren, K. A., Martin, J., Pieres, A., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Sifón, C., Tucker, D. L., Yanny, B., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., De Vicente, J., Desai, S., Dietrich, J. P., Eckert, K., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gill, M. S. S., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Nord, B., Ogando, R. L. C., Paz- Chinchón, F., Pereira, M. E. S., Plazas Malagón, A. A., Rodriguez- Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Varga, T. N.

Subjects
Física, Astronomy and Astrophysics, GALÁXIAS, 5109 Space Sciences, Galaxies, High-redshift galaxie, Lens, Space and Planetary Science, Strong gravitational lensing, High-redshift galaxies, 51 Physical Sciences, Quasars, Eye Disease and Disorders of Vision
Abstract

DES Collaboration: O’Donnell et al., We report the combined results of eight searches for strong gravitational lens systems in the full 5000 square degrees of Dark Energy Survey (DES) observations. The observations accumulated by the end of the third observing season fully covered the DES footprint in five filters (grizY), with an i-band limiting magnitude (at 10σ) of 23.44. In four searches, a list of potential candidates was identified using a color and magnitude selection from the object catalogs created from the first three observing seasons. Three other searches were conducted at the locations of previously identified galaxy clusters. Cutout images of potential candidates were then visually scanned using an object viewer. An additional set of candidates came from a data-quality check of a subset of the color–coadd tiles created from the full DES six-season data set. A short list of the most promising strong-lens candidates was then numerically ranked according to whether or not we judged them to be bona fide strong gravitational lens systems. These searches discovered a diverse set of 247 strong-lens candidate systems, of which 81 are identified for the first time. We provide the coordinates, magnitudes, and photometric properties of the lens and source objects, and an estimate of the Einstein radius for 81 new systems and 166 previously reported systems. This catalog will be of use for selecting interesting systems for detailed follow up, studies of galaxy cluster and group mass profiles, as well as a training/validation set for automated strong-lens searches., 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 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

2. 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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3. Finding quadruply imaged quasars with machine learning. I. Methods

Author

Akhazhanov, A., More, A., Amini, A., Hazlett, C., Treu, T., Birrer, S., Shajib, A., Liao, K., Lemon, C., Agnello, A., Nord, B., Aguena, Michel, Allam, Sahar, Andrade-Oliveira, Felipe, Annis, J., Brooks, D., Buckley-Geer, E., Burke, David L., Carnero Rosell, Aurelio, Carrasco Kind, Matias, Carretero, J., Choi, A., Conselice, Christopher J., Costanzi, M., da Costa, L. N., Pereira, M.E.S., De Vicente, J., Desai, S., Dietrich, J.P., Doel, P., Everett, S., Ferrero, Ismael, Finley, D.A., Flaugher, Brenna, Frieman, Josh, García-Bellido, Juan, Gerdes, David W., Gruen, D., Gruendl, Robert A., Gschwend, J., Gutierrez, G., Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klaus, James, D.J., Kim, A.G., Kuehn, K., Kuropatkin, Nikolay, Lahav, Ofer, Lima, M., Lin, H., Maia, Marcio A. G., March, M., Menanteau, Felipe, Miquel, R., Morgan, R., Palmese, Antonella, Paz-Chinchón, Francisco, Pieres, A., Plazas Malagón, Andrés A., Sanchez, E., Scarpine, Vic, Serrano, S., Sevilla-Noarbe, Ignacio, Smith, M., Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Tarlé, Gregory, To, C., Varga, Tamas Norbert, Weller, Jochen, A Akhazhanov, A., More, A., Amini, A., Hazlett, C., Treu, T., Birrer, S., Shajib, A., Liao, K., Lemon, C., Agnello, A., Nord, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Choi, A., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Finley, D. A., 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., James, D. J., Kim, A. G., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., Weller, J., UAM. Departamento de Física Teórica, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, Science and Technology Facilities Council (UK), and Ministerio de Economía y Competitividad (España)

Subjects
methods: statistical, model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Survey [astronomical data bases], candidates, Física, gravitational lensing: strong, FOS: Physical sciences, ESTATÍSTICA, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Strong [gravitational lensing], Astronomical Data Bases: Catalogs, Space and Planetary Science, astronomical data bases: surveys, strong gravitational lenses, Statistical [methods], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DES Collaboration: et al., Strongly lensed quadruply imaged quasars (quads) are extraordinary objects. They are very rare in the sky and yet they provide unique information about a wide range of topics, including the expansion history and the composition of the Universe, the distribution of stars and dark matter in galaxies, the host galaxies of quasars, and the stellar initial mass function. Finding them in astronomical images is a classic ‘needle in a haystack’ problem, as they are outnumbered by other (contaminant) sources by many orders of magnitude. To solve this problem, we develop state-of-the-art deep learning methods and train them on realistic simulated quads based on real images of galaxies taken from the Dark Energy Survey, with realistic source and deflector models, including the chromatic effects of microlensing. The performance of the best methods on a mixture of simulated and real objects is excellent, yielding area under the receiver operating curve in the range of 0.86–0.89. Recall is close to 100 per cent down to total magnitude i ∼ 21 indicating high completeness, while precision declines from 85 per cent to 70 per cent in the range i ∼ 17–21. The methods are extremely fast: training on 2 million samples takes 20 h on a GPU machine, and 108 multiband cut-outs can be evaluated per GPU-hour. The speed and performance of the method pave the way to apply it to large samples of astronomical sources, bypassing the need for photometric pre-selection that is likely to be a major cause of incompleteness in current samples of known quads., TT acknowledges support from the National Science Foundation through grant NSF-AST-1906976, from NASA through grants HST-GO-15320and HST-GO-15652, and from the Packard Foundation through a Packard Research Fellowship. 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 numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2021
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4. DeepZipper: A Novel Deep Learning Architecture for Lensed Supernovae Identification

Author

Morgan, R, Nord, B, Bechtol, K, González, SJ, Buckley-Geer, E, Möller, A, Park, JW, Kim, AG, Birrer, S, Aguena, M, Annis, J, Bocquet, S, Brooks, D, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Cawthon, R, Da Costa, LN, Davis, TM, De Vicente, J, Doel, P, Ferrero, I, Friedel, D, Frieman, J, García-Bellido, J, Gatti, M, Gaztanaga, E, Giannini, G, Gruen, D, Gruendl, RA, Gutierrez, G, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Maia, MAG, Miquel, R, Palmese, A, Paz-Chinchón, F, Pereira, MES, Pieres, A, Plazas Malagón, AA, Reil, K, Roodman, A, Sanchez, E, Smith, M, Suchyta, E, Swanson, MEC, Tarle, G, To, C, National Science Foundation (US), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, European Research Council, Ministerio de Economía y Competitividad (España), UAM. Departamento de Física Teórica, Morgan, R [0000-0002-7016-5471], Nord, B [0000-0001-6706-8972], Bechtol, K [0000-0001-8156-0429], González, SJ [0000-0001-7282-3864], Buckley-Geer, E [0000-0002-3304-0733], Möller, A [0000-0001-8211-8608], Park, JW [0000-0002-0692-1092], Birrer, S [0000-0003-3195-5507], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bocquet, S [0000-0002-4900-805X], Brooks, D [0000-0002-8458-5047], Carnero Rosell, A [0000-0003-3044-5150], Carrasco Kind, M [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Cawthon, R [0000-0003-2965-6786], Da Costa, LN [0000-0002-7731-277X], Davis, TM [0000-0002-4213-8783], De Vicente, J [0000-0001-8318-6813], Friedel, D [0000-0002-3632-7668], Frieman, J [0000-0003-4079-3263], García-Bellido, J [0000-0002-9370-8360], Gaztanaga, E [0000-0001-9632-0815], Giannini, G [0000-0002-3730-1750], Gruen, D [0000-0003-3270-7644], Gruendl, RA [0000-0002-4588-6517], Gutierrez, G [0000-0003-0825-0517], Hollowood, DL [0000-0002-9369-4157], Honscheid, K [0000-0002-6550-2023], James, DJ [0000-0001-5160-4486], Kuehn, K [0000-0003-0120-0808], Kuropatkin, N [0000-0003-2511-0946], Maia, MAG [0000-0001-9856-9307], Miquel, R [0000-0002-6610-4836], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Plazas Malagón, AA [0000-0002-2598-0514], Roodman, A [0000-0001-5326-3486], Sanchez, E [0000-0002-9646-8198], Smith, M [0000-0002-3321-1432], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], To, C [0000-0001-7836-2261], and Apollo - University of Cambridge Repository

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Física, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies, Lens, Space and Planetary Science, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Quasars, Instrumentation and Methods for Astrophysics (astro-ph.IM), astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Morgan et al., Large-scale astronomical surveys have the potential to capture data on large numbers of strongly gravitationally lensed supernovae (LSNe). To facilitate timely analysis and spectroscopic follow-up before the supernova fades, an LSN needs to be identified soon after it begins. To quickly identify LSNe in optical survey data sets, we designed ZipperNet, a multibranch deep neural network that combines convolutional layers (traditionally used for images) with long short-term memory layers (traditionally used for time series). We tested ZipperNet on the task of classifying objects from four categories—no lens, galaxy-galaxy lens, lensed Type-Ia supernova, lensed core-collapse supernova—within high-fidelity simulations of three cosmic survey data sets: the Dark Energy Survey, Rubin Observatory's Legacy Survey of Space and Time (LSST), and a Dark Energy Spectroscopic Instrument (DESI) imaging survey. Among our results, we find that for the LSST-like data set, ZipperNet classifies LSNe with a receiver operating characteristic area under the curve of 0.97, predicts the spectroscopic type of the lensed supernovae with 79% accuracy, and demonstrates similarly high performance for LSNe 1–2 epochs after first detection. We anticipate that a model like ZipperNet, which simultaneously incorporates spatial and temporal information, can play a significant role in the rapid identification of lensed transient systems in cosmic survey experiments., R. Morgan thanks the Universities Research Association Fermilab Visiting Scholars Program for funding his work on this project. R. Morgan also 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. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 1744555. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 1744555. 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 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) e-Universe (CNPq grant 465376/2014-2).

Published
2021
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5. DeepMerge: Classifying High-redshift Merging Galaxies with Deep Neural Networks

Author

Ćiprijanović, A., Snyder, G. F., Nord, B., and Peek, J. E. G.

Subjects
FOS: Computer and information sciences, Astrophysics of Galaxies (astro-ph.GA), Computer Vision and Pattern Recognition (cs.CV), Computer Science - Computer Vision and Pattern Recognition, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We investigate and demonstrate the use of convolutional neural networks (CNNs) for the task of distinguishing between merging and non-merging galaxies in simulated images, and for the first time at high redshifts (i.e. $z=2$). We extract images of merging and non-merging galaxies from the Illustris-1 cosmological simulation and apply observational and experimental noise that mimics that from the Hubble Space Telescope; the data without noise form a "pristine" data set and that with noise form a "noisy" data set. The test set classification accuracy of the CNN is $79\%$ for pristine and $76\%$ for noisy. The CNN outperforms a Random Forest classifier, which was shown to be superior to conventional one- or two-dimensional statistical methods (Concentration, Asymmetry, the Gini, $M_{20}$ statistics etc.), which are commonly used when classifying merging galaxies. We also investigate the selection effects of the classifier with respect to merger state and star formation rate, finding no bias. Finally, we extract Grad-CAMs (Gradient-weighted Class Activation Mapping) from the results to further assess and interrogate the fidelity of the classification model., Comment: 17 pages, 8 figures, submitted to Astronomy & Computing

Published
2020
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6. Dark Energy Survey year 1 results: Constraints on extended cosmological models from galaxy clustering and weak lensing

Author

Abbott, TMC, Abdalla, FB, Avila, S, Banerji, M, Baxter, E, Bechtol, K, Becker, MR, Bertin, E, Blazek, J, Bridle, SL, Brooks, D, Brout, D, Burke, DL, Campos, A, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Cawthon, R, Chang, C, Chen, A, Crocce, M, Cunha, CE, da Costa, LN, Davis, C, De Vicente, J, DeRose, J, Desai, S, Di Valentino, E, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Eifler, TF, Elvin-Poole, J, Evrard, AE, Fernandez, E, Ferté, A, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, Hoyle, B, Huterer, D, Jain, B, Jeltema, T, Johnson, MWG, Johnson, MD, Kim, AG, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lee, S, Lemos, P, Leonard, CD, Li, TS, Liddle, AR, Lima, M, Lin, H, Maia, MAG, Marshall, JL, Martini, P, Menanteau, F, Miller, CJ, Miquel, R, Miranda, V, Mohr, JJ, Muir, J, Nichol, RC, Nord, B, Ogando, RLC, Plazas, AA, Raveri, M, Rollins, RP, Romer, AK, Roodman, A, Rosenfeld, R, Samuroff, S, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Scolnic, D, Secco, LF, Serrano, S, Sevilla-Noarbe, I, Smith, M, and Soares-Santos, M

Subjects
Quantum Physics, Particle and Plasma Physics, gr-qc, astro-ph.CO, Molecular, Nuclear, hep-ph, Atomic, Nuclear & Particles Physics, Astronomical and Space Sciences
Abstract

We present constraints on extensions of the minimal cosmological models dominated by dark matter and dark energy, ΛCDM and wCDM, by using a combined analysis of galaxy clustering and weak gravitational lensing from the first-year data of the Dark Energy Survey (DES Y1) in combination with external data. We consider four extensions of the minimal dark energy-dominated scenarios: (1) nonzero curvature ωk, (2) number of relativistic species Neff different from the standard value of 3.046, (3) time-varying equation-of-state of dark energy described by the parameters w0 and wa (alternatively quoted by the values at the pivot redshift, wp, and wa), and (4) modified gravity described by the parameters μ0 and ς0 that modify the metric potentials. We also consider external information from Planck cosmic microwave background measurements; baryon acoustic oscillation measurements from SDSS, 6dF, and BOSS; redshift-space distortion measurements from BOSS; and type Ia supernova information from the Pantheon compilation of datasets. Constraints on curvature and the number of relativistic species are dominated by the external data; when these are combined with DES Y1, we find ωk=0.0020-0.0032+0.0037 at the 68% confidence level, and the upper limit Neff3.0. For the time-varying equation-of-state, we find the pivot value (wp,wa)=(-0.91-0.23+0.19,-0.57-1.11+0.93) at pivot redshift zp=0.27 from DES alone, and (wp,wa)=(-1.01-0.04+0.04,-0.28-0.48+0.37) at zp=0.20 from DES Y1 combined with external data; in either case we find no evidence for the temporal variation of the equation of state. For modified gravity, we find the present-day value of the relevant parameters to be ς0=0.43-0.29+0.28 from DES Y1 alone, and (ς0,μ0)=(0.06-0.07+0.08,-0.11-0.46+0.42) from DES Y1 combined with external data. These modified-gravity constraints are consistent with predictions from general relativity.

Published
2019

7. First cosmology results using Type Ia supernova from the Dark Energy Survey: simulations to correct supernova distance biases

Author

Kessler, R, Brout, D, D'Andrea, CB, Davis, TM, Hinton, SR, Kim, AG, Lasker, J, Lidman, C, Macaulay, E, Moeller, A, Sako, M, Scolnic, D, Smith, M, Sullivan, M, Zhang, B, Andersen, P, Asorey, J, Avelino, A, Calcino, J, Carollo, D, Challis, P, Childress, M, Clocchiatti, A, Crawford, S, Filippenko, AV, Foley, RJ, Glazebrook, K, Hoormann, JK, Kasai, E, Kirshner, RP, Lewis, GF, Mandel, KS, March, M, Morganson, E, Muthukrishna, D, Nugent, P, Pan, Y-C, Sommer, NE, Swann, E, Thomas, RC, Tucker, BE, Uddin, SA, Abbott, TMC, Allam, S, Annis, J, Avila, S, Banerji, M, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Kind, M Carrasco, Carretero, J, Castander, FJ, Crocce, M, da Costa, LN, Davis, C, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Johnson, MWG, Johnson, MD, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Marshall, JL, Martini, P, Menanteau, F, Miller, CJ, Miquel, R, Nord, B, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Sobreira, F, Suchyta, E, Tarle, G, Thomas, D, Walker, AR, Zhang, Y, Collaboration, DES, Mandel, Kaisey [0000-0001-9846-4417], Banerji, Manda [0000-0002-0639-5141], and Apollo - University of Cambridge Repository

Subjects
(cosmology:) dark energy, supernovae, Astrophysics::Cosmology and Extragalactic Astrophysics, techniques, cosmology
Abstract

We describe catalog-level simulations of Type Ia supernova (SN~Ia) light curves in the Dark Energy Survey Supernova Program (DES-SN), and in low-redshift samples from the Center for Astrophysics (CfA) and the Carnegie Supernova Project (CSP). These simulations are used to model biases from selection effects and light curve analysis, and to determine bias corrections for SN~Ia distance moduli that are used to measure cosmological parameters. To generate realistic light curves, the simulation uses a detailed SN~Ia model, incorporates information from observations (PSF, sky noise, zero point), and uses summary information (e.g., detection efficiency vs. signal to noise ratio) based on 10,000 fake SN light curves whose fluxes were overlaid on images and processed with our analysis pipelines. The quality of the simulation is illustrated by predicting distributions observed in the data. Averaging within redshift bins, we find distance modulus biases up to 0.05~mag over the redshift ranges of the low-z and DES-SN samples. For individual events, particularly those with extreme red or blue color, distance biases can reach 0.4~mag. Therefore, accurately determining bias corrections is critical for precision measurements of cosmological parameters. Files used to make these corrections are available at this https URL.

Published
2019

8. First cosmology results using Type Ia supernova from the Dark Energy Survey: Simulations to correct supernova distance biases

Author

Kessler, R, Brout, D, D’Andrea, CB, Davis, TM, Hinton, SR, Kim, AG, Lasker, J, Lidman, C, Macaulay, E, Möller, A, Sako, M, Scolnic, D, Smith, M, Sullivan, M, Zhang, B, Andersen, P, Asorey, J, Avelino, A, Calcino, J, Carollo, D, Challis, P, Childress, M, Clocchiatti, A, Crawford, S, Filippenko, AV, Foley, RJ, Glazebrook, K, Hoormann, JK, Kasai, E, Kirshner, RP, Lewis, GF, Mandel, KS, March, M, Morganson, E, Muthukrishna, D, Nugent, P, Pan, Y-C, Sommer, NE, Swann, E, Thomas, RC, Tucker, BE, Uddin, SA, Abbott, TMC, Allam, S, Annis, J, Avila, S, Banerji, M, Bechtol, K, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Crocce, M, da Costa, LN, Davis, C, De Vicente, J, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Johnson, MWG, Johnson, MD, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Marshall, JL, Martini, P, Menanteau, F, Miller, CJ, Miquel, R, Nord, B, Plazas, AA, Roodman, A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, and Soares-Santos, M

Subjects
Affordable and Clean Energy, ) dark energy [(cosmology], supernovae, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, techniques, cosmology, Astronomical and Space Sciences, astro-ph.IM
Abstract

We describe catalogue-level simulations of Type Ia supernova (SN Ia) light curves in the Dark Energy Survey Supernova Program (DES-SN) and in low-redshift samples from the Center for Astrophysics (CfA) and the Carnegie Supernova Project (CSP). These simulations are used to model biases from selection effects and light-curve analysis and to determine bias corrections for SN Ia distance moduli that are used to measure cosmological parameters. To generate realistic light curves, the simulation uses a detailed SN Ia model, incorporates information from observations (point spread function, sky noise, zero-point), and uses summary information (e.g. detection efficiency versus signal-to-noise ratio) based on 10 000 fake SN light curves whose fluxes were overlaid on images and processed with our analysis pipelines. The quality of the simulation is illustrated by predicting distributions observed in the data. Averaging within redshift bins, we find distance modulus biases up to 0.05 mag over the redshift ranges of the low-z and DES-SN samples. For individual events, particularly those with extreme red or blue colour, distance biases can reach 0.4 mag. Therefore, accurately determining bias corrections is critical for precision measurements of cosmological parameters. Files used to make these corrections are available at https://des.ncsa.illinois.edu/releases/sn.

Published
2019

9. Response to NITRD, NCO, NSF Request for Information on 'Update to the 2016 National Artificial Intelligence Research and Development Strategic Plan'

Author

Amundson, J., Annis, J., Avestruz, C., Bowring, D., Caldeira, J., Cerati, G., Chang, C., Dodelson, S., Elvira, D., Farahi, A., Genser, K., Gray, L., Gutsche, O., Harris, P., Kinney, J., Kowalkowski, J. B., Kutschke, R., Mrenna, S., Nord, B., Para, A., Pedro, K., Perdue, G. N., Scheinker, A., Spentzouris, P., John, J. St., Tran, N., Trivedi, S., Trouille, L., Wu, W. L. K., and Bom, C. R.

Subjects
FOS: Computer and information sciences, Physics - Physics and Society, Artificial Intelligence (cs.AI), Computer Science - Artificial Intelligence, FOS: Physical sciences, Physics and Society (physics.soc-ph), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We present a response to the 2018 Request for Information (RFI) from the NITRD, NCO, NSF regarding the "Update to the 2016 National Artificial Intelligence Research and Development Strategic Plan." Through this document, we provide a response to the question of whether and how the National Artificial Intelligence Research and Development Strategic Plan (NAIRDSP) should be updated from the perspective of Fermilab, America's premier national laboratory for High Energy Physics (HEP). We believe the NAIRDSP should be extended in light of the rapid pace of development and innovation in the field of Artificial Intelligence (AI) since 2016, and present our recommendations below. AI has profoundly impacted many areas of human life, promising to dramatically reshape society --- e.g., economy, education, science --- in the coming years. We are still early in this process. It is critical to invest now in this technology to ensure it is safe and deployed ethically. Science and society both have a strong need for accuracy, efficiency, transparency, and accountability in algorithms, making investments in scientific AI particularly valuable. Thus far the US has been a leader in AI technologies, and we believe as a national Laboratory it is crucial to help maintain and extend this leadership. Moreover, investments in AI will be important for maintaining US leadership in the physical sciences.

Published
2019
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10. Petabytes to Science

Author

Bauer, Amanda E., Bellm, Eric C., Bolton, Adam S., Chaudhuri, Surajit, Connolly, A. J., Cruz, Kelle L., Desai, Vandana, Drlica-Wagner, Alex, Economou, Frossie, Gaffney, Niall, Kavelaars, J., Kinney, J., Li, Ting S., Lundgren, B., Margutti, R., Narayan, G., Nord, B., Norman, Dara J., O'Mullane, W., Padhi, S., Peek, J. E. G., Schafer, C., Schwamb, Megan E., Smith, Arfon M., Tollerud, Erik J., Weijmans, Anne-Marie, and Szalay, Alexander S.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

A Kavli foundation sponsored workshop on the theme \emph{Petabytes to Science} was held 12$^{th}$ to 14$^{th}$ of February 2019 in Las Vegas. The aim of the this workshop was to discuss important trends and technologies which may support astronomy. We also tackled how to better shape the workforce for the new trends and how we should approach education and public outreach. This document was coauthored during the workshop and edited in the weeks after. It comprises the discussions and highlights many recommendations which came out of the workshop. We shall distill parts of this document and formulate potential white papers for the decadal survey., Comment: 70 pages 2 figures - this contains a few fixes

Published
2019
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11. 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

12. Dark Energy Survey Year 1 results: cross-correlation redshifts – methods and systematics characterization

Author

Gatti, M, Vielzeuf, P, Davis, C, Cawthon, R, Rau, MM, DeRose, J, De Vicente, J, Alarcon, A, Rozo, E, Gaztanaga, E, Hoyle, B, Miquel, R, Bernstein, GM, Bonnett, C, Rosell, AC, Castander, FJ, Chang, C, da Costa, LN, Gruen, D, Gschwend, J, Hartley, WG, Lin, H, MacCrann, N, Maia, MAG, Ogando, RLC, Roodman, A, Sevilla-Noarbe, I, Troxel, MA, Wechsler, RH, Asorey, J, Davis, TM, Glazebrook, K, Hinton, SR, Lewis, G, Lidman, C, Macaulay, E, Möller, A, O'Neill, CR, Sommer, NE, Uddin, SA, Yuan, F, Zhang, B, Abbott, TMC, Allam, S, Annis, J, Bechtol, K, Brooks, D, Burke, DL, Carollo, D, Kind, MC, Carretero, J, Cunha, CE, D'Andrea, CB, DePoy, DL, Desai, S, Eifler, TF, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gerdes, DW, Goldstein, DA, Gruendl, RA, Gutierrez, G, Honscheid, K, Hoormann, JK, Jain, B, James, DJ, Jarvis, M, Jeltema, T, Johnson, MWG, Johnson, MD, Krause, E, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Li, TS, Lima, M, Marshall, JL, Melchior, P, Menanteau, F, Nichol, RC, Nord, B, Plazas, AA, Reil, K, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schubnell, M, Sheldon, E, Smith, M, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, and Thomas, D

Subjects
Affordable and Clean Energy, astro-ph.CO, distances and redshifts [galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Astrophysics::Galaxy Astrophysics, observations [cosmology], Astronomical and Space Sciences
Abstract

We use numerical simulations to characterize the performance of a clustering-based method to calibrate photometric redshift biases. In particular, we cross-correlate the weak lensing source galaxies from the Dark Energy Survey Year 1 sample with redMaGiC galaxies (luminous red galaxies with secure photometric redshifts) to estimate the redshift distribution of the former sample. The recovered redshift distributions are used to calibrate the photometric redshift bias of standard photo-z methods applied to the same source galaxy sample.We apply the method to two photo-z codes run in our simulated data: Bayesian Photometric Redshift and Directional Neighbourhood Fitting. We characterize the systematic uncertainties of our calibration procedure, and find that these systematic uncertainties dominate our error budget. The dominant systematics are due to our assumption of unevolving bias and clustering across each redshift bin, and to differences between the shapes of the redshift distributions derived by clustering versus photo-zs. The systematic uncertainty in the mean redshift bias of the source galaxy sample is Δz ≲ 0.02, though the precise value depends on the redshift bin under consideration. We discuss possible ways to mitigate the impact of our dominant systematics in future analyses.

Published
2018

13. COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses 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, CD, Frieman, J, Lin, H, Marshall, PJ, Suyu, SH, Treu, T, Anguita, T, Motta, V, Meylan, G, Paic, E, Tewes, M, Agnello, A, Chao, DCY, Chijani, M, Gilman, D, Rojas, K, Williams, P, Hempel, A, Kim, S, Lachaume, R, Rabus, M, Abbott, TMC, Allam, S, Annis, J, Banerji, M, Bechtol, K, Benoit-Lévy, A, Brooks, D, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, D'Andrea, CB, Da Costa, LN, Davis, C, Depoy, DL, Desai, S, Flaugher, B, Fosalba, P, García-Bellido, J, Gaztanaga, E, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Marshall, JL, McMahon, RG, Menanteau, F, Miquel, R, Nord, B, Plazas, AA, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sobreira, F, Suchyta, E, Banerji, Manda [0000-0002-0639-5141], McMahon, Richard [0000-0001-8447-8869], and Apollo - University of Cambridge Repository

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, gravitational lensing: strong, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmological parameters, methods: data analysis, Astrophysics::Galaxy Astrophysics
Abstract

© ESO, 2018. We present time-delay measurements for the new quadruple imaged quasar DES J04085354, the first quadruple 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 2.2 m telescope at La Silla observatory and deep exposures reaching a signal-to-noise ratio of about 1000 per quasar image. This data qualityallows us to catch small photometric variations (a few mmag rms) of the quasar, acting on temporal scales much shorter than microlensing, and hence making the time delay measurement very robust against microlensing. In only seven months we very accurately measured one of the time delays in DES J04085354: - "t(AB) = 112.1 ± 2.1 days (1.8%) using only the MPIA 2.2 m data. In combination with data taken with the 1.2 m Euler Swiss telescope, we also measured two delays involving the D component of the system - "t(AD) = ± 12.8 days (8.2%) and - "t(BD) = 42.4 ± 17.6 days (41%), where all the error bars include systematics. Turning these time delays into cosmological constraints will require deep Hubble Space Telescope (HST) imaging or ground-based adaptive optics (AO), and information on the velocity field of the lensing galaxy.

Published
2018
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14. A measurement of CMB cluster lensing with SPT and DES year 1 data

Author

Baxter, EJ, Raghunathan, S, Crawford, TM, Fosalba, P, Hou, Z, Holder, GP, Omori, Y, Patil, S, Rozo, E, Abbott, TMC, Annis, J, Aylor, K, Benoit-Lévy, A, Benson, BA, Bertin, E, Bleem, L, Buckley-Geer, E, Burke, DL, Carlstrom, J, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Chang, CL, Cho, H-M, Crites, AT, Crocce, M, Cunha, CE, da Costa, LN, D'Andrea, CB, Davis, C, de Haan, T, Desai, S, Dietrich, JP, Dobbs, MA, Dodelson, S, Doel, P, Drlica-Wagner, A, Estrada, J, Everett, WB, Neto, A Fausti, Flaugher, B, Frieman, J, García-Bellido, J, George, EM, Gaztanaga, E, Giannantonio, T, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Halverson, NW, Harrington, NL, Hartley, WG, Holzapfel, WL, Honscheid, K, Hrubes, JD, Jain, B, James, DJ, Jarvis, M, Jeltema, T, Knox, L, Krause, E, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lahav, O, Lee, AT, Leitch, EM, Li, TS, Lima, M, Luong-Van, D, Manzotti, A, March, M, Marrone, DP, Marshall, JL, Martini, P, McMahon, JJ, Melchior, P, Menanteau, F, Meyer, SS, Miller, CJ, Miquel, R, Mocanu, LM, Mohr, JJ, Natoli, T, Nord, B, Ogando, RLC, Padin, S, Plazas, AA, Pryke, C, Rapetti, D, Reichardt, CL, Romer, AK, Roodman, A, Ruhl, JE, Rykoff, E, Sako, M, Sanchez, E, Sayre, JT, and Scarpine, V

Subjects
weak [gravitational lensing], Astrophysics::Instrumentation and Methods for Astrophysics, astro-ph.CO, clusters: general [galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, Astronomy & Astrophysics, Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences
Abstract

Clusters of galaxies gravitationally lens the cosmic microwave background (CMB) radiation, resulting in a distinct imprint in the CMB on arcminute scales. Measurement of this effect offers a promising way to constrain the masses of galaxy clusters, particularly those at high redshift. We use CMB maps from the South Pole Telescope Sunyaev-Zel'dovich (SZ) survey to measure the CMB lensing signal around galaxy clusters identified in optical imaging from first year observations of the Dark Energy Survey. The cluster catalogue used in this analysis contains 3697 members with mean redshift of z = 0.45. We detect lensing of the CMB by the galaxy clusters at 8.1s significance. Using the measured lensing signal, we constrain the amplitude of the relation between cluster mass and optical richness to roughly 17 per cent precision, finding good agreement with recent constraints obtained with galaxy lensing. The error budget is dominated by statistical noise but includes significant contributions from systematic biases due to the thermal SZ effect and cluster miscentring.

Published
2018

15. 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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16. New Science, New Media: An Assessment of the Online Education and Public Outreach Initiatives of The Dark Energy Survey

Author

Wolf, R. C., Romer, A. K., Nord, B., Avila, S., Bechtol, K., Biron, L., Cawthon, R., Chang, C., Das, R., Ferte, A., Gill, M. S. S., Gupta, R. R., Hamilton, S., Hislop, J. M., Jennings, E., Krawiec, C., Kremin, A., Li, T. S., Lingard, T., Moller, A., Muir, J., Nagasawa, D. Q., Ogando, R. L. C., Plazas, A. A., Sevilla-Noarbe, I., Suchyta, E., Zhang, Y., and Zuntz, J.

Subjects
Physics Education (physics.ed-ph), Physics - Physics Education, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

As large-scale international collaborations become the standard for astronomy research, a wealth of opportunities have emerged to create innovative education and public outreach (EPO) programming. In the past two decades, large collaborations have focused EPO strategies around published data products. Newer collaborations have begun to explore other avenues of public engagement before and after data are made available. We present a case study of the online EPO program of The Dark Energy Survey, currently one of the largest international astronomy collaborations actively taking data. DES EPO is unique at this scale in astronomy, as far as we are aware, as it evolved organically from scientists' passion for EPO and is entirely organized and implemented by the volunteer efforts of collaboration scientists. We summarize the strategy and implementation of eight EPO initiatives. For content distributed via social media, we present reach and user statistics over the 2016 calendar year. DES EPO online products reached ~2,500 users per post, and 94% of these users indicate a predisposition to science-related interests. We find no obvious correlation between post type and post reach, with the most popular posts featuring the intersections of science and art and/or popular culture. We conclude that one key issue of the online DES EPO program was designing material which would inspire new interest in science. The greatest difficulty of the online DES EPO program was sustaining scientist participation and collaboration support; the most successful programs are those which capitalized on the hobbies of participating scientists. We present statistics and recommendations, along with observations from individual experience, as a potentially instructive resource for scientists or EPO professionals interested in organizing EPO programs and partnerships for large science collaborations or organizations., Comment: 50 pages, 3 appendices, 15 total figures

Published
2018
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17. OzDES multifibre spectroscopy for the Dark Energy Survey: 3-yr results and first data release

Author

Childress, MJ, Lidman, C, Davis, TM, Tucker, BE, Asorey, J, Yuan, F, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Banerji, M, Benoit-Lévy, A, Bernard, SR, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carollo, D, Carrasco Kind, M, Carretero, J, Castander, FJ, Cunha, CE, da Costa, LN, D'Andrea, CB, Doel, P, Eifler, TF, Evrard, AE, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, García-Bellido, J, Glazebrook, K, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gupta, RR, Gutierrez, G, Hinton, SR, Hoormann, JK, James, DJ, Kessler, R, Kim, AG, King, AL, Kovacs, E, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lagattuta, DJ, Lewis, GF, Li, TS, Lima, M, Lin, H, Macaulay, E, Maia, MAG, Marriner, J, March, M, Marshall, JL, Martini, P, McMahon, RG, Menanteau, F, Miquel, R, Moller, A, Morganson, E, Mould, J, Mudd, D, Muthukrishna, D, Nichol, RC, Nord, B, Ogando, RLC, Ostrovski, F, Parkinson, D, Plazas, AA, Reed, SL, Reil, K, Romer, AK, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Scolnic, D, Sevilla-Noarbe, I, Seymour, N, Sharp, R, Smith, M, Soares-Santos, M, Sobreira, F, Sommer, NE, Spinka, H, Suchyta, E, Sullivan, M, Swanson, MEC, Tarle, G, Uddin, SA, Walker, AR, and Wester, W

Subjects
astro-ph.GA, astro-ph.CO, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, dark energy, general [supernovae], Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences
Abstract

We present results for the first three years of OzDES, a six year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multiyear baseline and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17 000 objects, including the redshifts of 2566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise ratio (S/N), magnitude and exposure time, finding that our redshift success rate increases significantly at a S/N of 2-3 per 1-Å bin. We also find that the change in S/N with exposure time closely matches the Poisson limit for stacked exposures as long as 10 h. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as (i.e. the 4-m Multi-Object Spectroscopic Telescope, the Subaru Prime Focus Spectrograph and the Maunakea Spectroscopic Explorer). This work marks the first OzDES data release, comprising 14 693 redshifts. OzDES is on target to obtain over 30 000 redshifts over the 6-yr duration of the survey, including a yield of approximately 5700 supernova host-galaxy redshifts.

Published
2017

18. Eight new luminous z = 6 quasars discovered via SED model fitting of VISTA, WISE and Dark Energy Survey Year 1 observations

Author

Reed, SL, McMahon, RG, Martini, P, Banerji, M, Auger, M, Hewett, PC, Koposov, SE, Gibbons, SLJ, Gonzalez-Solares, E, Ostrovski, F, Tie, SS, Abdalla, FB, Allam, S, Benoit-Levy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Da Costa, LN, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Evrard, AE, Finley, DA, Flaugher, B, Frieman, J, Fosalba, P, García-Bellido, J, Gaztanaga, E, Goldstein, DA, Gruen, D, Gruendl, RA, Gutierrez, G, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Melchior, P, Miller, CJ, Miquel, R, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Tucker, DL, Walker, AR, Wester, W, McMahon, Richard [0000-0001-8447-8869], Hewett, Paul [0000-0002-6528-1937], Koposov, Sergey [0000-0003-2644-135X], and Apollo - University of Cambridge Repository

Subjects
galaxies: high redshift, reionization, first stars, galaxies: active, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, galaxies: formation, quasars individual: VDES J0224-4711, Astrophysics::Cosmology and Extragalactic Astrophysics, dark ages, 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-{\alpha} 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 $\chi^{2}$-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.

Published
2017

19. 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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20. 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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21. 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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22. Redshift distributions of galaxies in the Dark Energy Survey Science Verification shear catalogue and implications for weak lensing

Author

Bonnett, C, Troxel, MA, Hartley, W, Amara, A, Leistedt, B, Becker, MR, Bernstein, GM, Bridle, SL, Bruderer, C, Busha, MT, Kind, M Carrasco, Childress, MJ, Castander, FJ, Chang, C, Crocce, M, Davis, TM, Eifler, TF, Frieman, J, Gangkofner, C, Gaztanaga, E, Glazebrook, K, Gruen, D, Kacprzak, T, King, A, Kwan, J, Lahav, O, Lewis, G, Lidman, C, Lin, H, MacCrann, N, Miquel, R, O’Neill, CR, Palmese, A, Peiris, HV, Refregier, A, Rozo, E, Rykoff, ES, Sadeh, I, Sánchez, C, Sheldon, E, Uddin, S, Wechsler, RH, Zuntz, J, Abbott, T, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Bauer, AH, Benoit-Lévy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Rosell, A Carnero, Carretero, J, Cunha, CE, D’Andrea, CB, da Costa, LN, DePoy, DL, Desai, S, Diehl, HT, Dietrich, JP, Doel, P, Neto, A Fausti, Fernandez, E, Flaugher, B, Fosalba, P, Gerdes, DW, Gruendl, RA, Honscheid, K, Jain, B, James, DJ, Jarvis, M, Kim, AG, Kuehn, K, Kuropatkin, N, Li, TS, Lima, M, Maia, MAG, March, M, Marshall, JL, Martini, P, Melchior, P, Miller, CJ, Neilsen, E, Nichol, RC, Nord, B, Ogando, R, Plazas, AA, Reil, K, Romer, AK, Roodman, A, Sako, M, Sanchez, E, Santiago, B, Smith, RC, Soares-Santos, M, and Sobreira, F

Subjects
Quantum Physics, Particle and Plasma Physics, Affordable and Clean Energy, Astrophysics::Instrumentation and Methods for Astrophysics, astro-ph.CO, Molecular, Nuclear, Astrophysics::Cosmology and Extragalactic Astrophysics, Atomic, Nuclear & Particles Physics, Astronomical and Space Sciences, Astrophysics::Galaxy Astrophysics
Abstract

We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model- or machine learning-based photometric redshift methods - annz2, bpz calibrated against BCC-Ufig simulations, skynet, and tpz - are analyzed. For training, calibration, and testing of these methods, we construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evaluated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-z's. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72±0.01 over the range 0.3

Published
2016

23. The Dark Energy Survey: more than dark energy – an overview

Author

Abbott, T, Abdalla, FB, Aleksić, J, Allam, S, Amara, A, Bacon, D, Balbinot, E, Banerji, M, Bechtol, K, Benoit-Lévy, A, Bernstein, GM, Bertin, E, Blazek, J, Bonnett, C, Bridle, S, Brooks, D, Brunner, RJ, Buckley-Geer, E, Burke, DL, Caminha, GB, Capozzi, D, Carlsen, J, Carnero-Rosell, A, Carollo, M, Carrasco-Kind, M, Carretero, J, Castander, FJ, Clerkin, L, Collett, T, Conselice, C, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Davis, TM, Desai, S, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Estrada, J, Etherington, J, Evrard, AE, Fabbri, J, Finley, DA, Flaugher, B, Foley, RJ, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Giannantonio, T, Goldstein, DA, Gruen, D, Gruendl, RA, Guarnieri, P, Gutierrez, G, Hartley, W, Honscheid, K, Jain, B, James, DJ, Jeltema, T, Jouvel, S, Kessler, R, King, A, Kirk, D, Kron, R, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Lin, H, Maia, MAG, Makler, M, Manera, M, Maraston, C, Marshall, JL, Martini, P, McMahon, RG, Melchior, P, Merson, A, Miller, CJ, Miquel, R, Mohr, JJ, Morice-Atkinson, X, Naidoo, K, Neilsen, E, Nichol, RC, Nord, B, Ogando, R, Ostrovski, F, Palmese, A, Papadopoulos, A, Peiris, HV, Peoples, J, Percival, WJ, and Plazas, AA

Subjects
surveys, general [quasars], astro-ph.GA, minor planets, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, general [supernovae], Astrophysics::Galaxy Astrophysics, general [Galaxy], Astronomical and Space Sciences, general [asteroids], general [galaxies]
Abstract

This overview paper describes the legacy prospect and discovery potential of the Dark Energy Survey (DES) beyond cosmological studies, illustrating it with examples from the DES early data. DES is using a wide-field camera (DECam) on the 4 m Blanco Telescope in Chile to image 5000 sq deg of the sky in five filters (grizY). By its completion, the survey is expected to have generated a catalogue of 300 million galaxies with photometric redshifts and 100 million stars. In addition, a time-domain survey search over 27 sq deg is expected to yield a sample of thousands of Type Ia supernovae and other transients. The main goals of DES are to characterize dark energy and dark matter, and to test alternative models of gravity; these goals will be pursued by studying large-scale structure, cluster counts, weak gravitational lensing and Type Ia supernovae. However, DES also provides a rich data set which allows us to study many other aspects of astrophysics. In this paper, we focus on additional science with DES, emphasizing areas where the survey makes a difference with respect to other current surveys. The paper illustrates, using early data (from 'Science Verification', and from the first, second and third seasons of observations), what DES can tell us about the Solar system, the Milky Way, galaxy evolution, quasars and other topics. In addition, we show that if the cosmological model is assumed to be Λ+cold dark matter, then important astrophysics can be deduced from the primary DES probes. Highlights from DES early data include the discovery of 34 trans-Neptunian objects, 17 dwarf satellites of the Milky Way, one published z > 6 quasar (and more confirmed) and two published superluminous supernovae (and more confirmed).

Published
2016

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

Author

Abbott, T, Abdalla, FB, Allam, S, Amara, A, Annis, J, Armstrong, R, Bacon, D, Banerji, M, Bauer, AH, Baxter, E, Becker, MR, Benoit-Lévy, A, Bernstein, RA, Bernstein, GM, Bertin, E, Blazek, J, Bonnett, C, Bridle, SL, Brooks, D, Bruderer, C, Buckley-Geer, E, Burke, DL, Busha, MT, Capozzi, D, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Castander, FJ, Chang, C, Clampitt, J, Crocce, M, Cunha, CE, D’Andrea, CB, da Costa, LN, Das, R, DePoy, DL, Desai, S, Diehl, HT, Dietrich, JP, Dodelson, S, Doel, P, Drlica-Wagner, A, Efstathiou, G, Eifler, TF, Erickson, B, Estrada, J, Evrard, AE, Neto, A Fausti, Fernandez, E, Finley, DA, Flaugher, B, Fosalba, P, Friedrich, O, Frieman, J, Gangkofner, C, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, Hartley, W, Hirsch, M, Honscheid, K, Huff, EM, Jain, B, James, DJ, Jarvis, M, Kacprzak, T, Kent, S, Kirk, D, Krause, E, Kravtsov, A, Kuehn, K, Kuropatkin, N, Kwan, J, Lahav, O, Leistedt, B, Li, TS, Lima, M, Lin, H, MacCrann, N, March, M, Marshall, JL, Martini, P, McMahon, RG, Melchior, P, Miller, CJ, Miquel, R, Mohr, JJ, Neilsen, E, Nichol, RC, Nicola, A, Nord, B, Ogando, R, Palmese, A, Peiris, HV, Plazas, AA, Refregier, A, and Roe, N

Subjects
Quantum Physics, Particle and Plasma Physics, astro-ph.CO, Molecular, Nuclear, Astrophysics::Cosmology and Extragalactic Astrophysics, Atomic, Nuclear & Particles Physics, Astronomical and Space Sciences
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 w.

Published
2016

25. 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

26. A DARK ENERGY CAMERA SEARCH FOR AN OPTICAL COUNTERPART TO THE FIRST ADVANCED LIGO GRAVITATIONAL WAVE EVENT GW150914

Author

Soares-Santos, M, Kessler, R, Berger, E, Annis, J, Brout, D, Buckley-Geer, E, Chen, H, Cowperthwaite, PS, Diehl, HT, Doctor, Z, Drlica-Wagner, A, Farr, B, Finley, DA, Flaugher, B, Foley, RJ, Frieman, J, Gruendl, RA, Herner, K, Holz, D, Lin, H, Marriner, J, Neilsen, E, Rest, A, Sako, M, Scolnic, D, Sobreira, F, Walker, AR, Wester, W, Yanny, B, Abbott, TMC, Abdalla, FB, Allam, S, Armstrong, R, Banerji, M, Benoit-Lévy, A, Bernstein, RA, Bertin, E, Brown, DA, Burke, DL, Capozzi, D, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Cenko, SB, Chornock, R, Crocce, M, D'Andrea, CB, Da Costa, LN, Desai, S, Dietrich, JP, Drout, MR, Eifler, TF, Estrada, J, Evrard, AE, Fairhurst, S, Fernandez, E, Fischer, J, Fong, W, Fosalba, P, Fox, DB, Fryer, CL, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gutierrez, G, Honscheid, K, James, DJ, Karliner, I, Kasen, D, Kent, S, Kuropatkin, N, Kuehn, K, Lahav, O, Li, TS, Lima, M, Maia, MAG, Margutti, R, Martini, P, Matheson, T, McMahon, RG, Metzger, BD, Miller, CJ, Miquel, R, Mohr, JJ, Nichol, RC, Nord, B, Ogando, R, Peoples, J, Plazas, AA, Quataert, E, Romer, AK, Roodman, A, Rykoff, ES, Sanchez, E, Scarpine, V, Schindler, R, and Schubnell, M

Subjects
neutron [stars], close [binaries], gravitational waves, surveys, astro-ph.CO, Astronomy & Astrophysics, catalogs, Astronomical and Space Sciences, astro-ph.IM
Abstract

We report the results of a deep search for an optical counterpart to the gravitational wave (GW) event GW150914, the first trigger from the Advanced LIGO GW detectors. We used the Dark Energy Camera (DECam) to image a 102 deg2 area, corresponding to 38% of the initial trigger high-probability sky region and to 11% of the revised high-probability region. We observed in the i and z bands at 4-5, 7, and 24 days after the trigger. The median 5σ point-source limiting magnitudes of our search images are i = 22.5 and z = 21.8 mag. We processed the images through a difference-imaging pipeline using templates from pre-existing Dark Energy Survey data and publicly available DECam data. Due to missing template observations and other losses, our effective search area subtends 40 deg2, corresponding to a 12% total probability in the initial map and 3% in the final map. In this area, we search for objects that decline significantly between days 4-5 and day 7, and are undetectable by day 24, finding none to typical magnitude limits of i = 21.5, 21.1, 20.1 for object colors (i - z) = 1, 0, -1, respectively. Our search demonstrates the feasibility of a dedicated search program with DECam and bodes well for future research in this emerging field.

Published
2016

27. A DARK ENERGY CAMERA SEARCH for MISSING SUPERGIANTS in the LMC after the ADVANCED LIGO GRAVITATIONAL-WAVE EVENT GW150914

Author

Annis, J, Soares-Santos, M, Berger, E, Brout, D, Chen, H, Chornock, R, Cowperthwaite, PS, Diehl, HT, Doctor, Z, Drlica-Wagner, A, Drout, MR, Farr, B, Finley, DA, Flaugher, B, Foley, RJ, Frieman, J, Gruendl, RA, Herner, K, Holz, D, Kessler, R, Lin, H, Marriner, J, Neilsen, E, Rest, A, Sako, M, Smith, M, Smith, N, Sobreira, F, Walker, AR, Yanny, B, Abbott, TMC, Abdalla, FB, Allam, S, Benoit-Levy, A, Bernstein, RA, Bertin, E, Buckley-Geer, E, Burke, DL, Capozzi, D, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Castander, FJ, Cenko, SB, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Desai, S, Dietrich, JP, Eifler, TF, Evrard, AE, Fernandez, E, Fischer, J, Fong, W, Fosalba, P, Fox, DB, Fryer, CL, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gutierrez, G, Honscheid, K, James, DJ, Karliner, I, Kasen, D, Kent, S, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Maia, MAG, Martini, P, Metzger, BD, Miller, CJ, Miquel, R, Mohr, JJ, Nichol, RC, Nord, B, Ogando, R, Peoples, J, Petravic, D, Plazas, AA, Quataert, E, Romer, AK, Roodman, A, Rykoff, ES, Sanchez, E, Santiago, B, Scarpine, V, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Sheldon, E, Smith, RC, Stebbins, A, and Swanson, MEC

Subjects
astro-ph.HE, gravitational waves, Astrophysics::High Energy Astrophysical Phenomena, Magellanic Clouds, astro-ph.CO, Astrophysics::Solar and Stellar Astrophysics, individual [galaxies], supergiants, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, general [supernovae], Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences
Abstract

The collapse of a stellar core is expected to produce gravitational waves (GWs), neutrinos, and in most cases a luminous supernova. Sometimes, however, the optical event could be significantly less luminous than a supernova and a direct collapse to a black hole, where the star just disappears, is possible. The GW event GW150914 was detected by the LIGO Virgo Collaboration via a burst analysis that gave localization contours enclosing the Large Magellanic Cloud (LMC). Shortly thereafter, we used DECam to observe 102 deg2 of the localization area, including 38 deg2 on the LMC for a missing supergiant search. We construct a complete catalog of LMC luminous red supergiants, the best candidates to undergo invisible core collapse, and collected catalogs of other candidates: less luminous red supergiants, yellow supergiants, blue supergiants, luminous blue variable stars, and Wolf-Rayet stars. Of the objects in the imaging region, all are recovered in the images. The timescale for stellar disappearance is set by the free-fall time, which is a function of the stellar radius. Our observations at 4 and 13 days after the event result in a search sensitive to objects of up to about 200 solar radii. We conclude that it is unlikely that GW150914 was caused by the core collapse of a relatively compact supergiant in the LMC, consistent with the LIGO Collaboration analyses of the gravitational waveform as best interpreted as a high mass binary black hole merger. We discuss how to generalize this search for future very nearby core-collapse candidates.

Published
2016

28. 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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29. 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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30. SPOKES: an End-to-End Simulation Facility for Spectroscopic Cosmological Surveys

Author

Nord, B., Amara, A., Refregier, A., Gamper, La., Gamper, Lu., Hambrecht, B., Chang, C., Forero-Romero, J. E., Serrano, S., Cunha, C., Coles, O., Nicola, A., Busha, M., Bauer, A., Saunders, W., Jouvel, S., Kirk, D., and Wechsler, R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The nature of dark matter, dark energy and large-scale gravity pose some of the most pressing questions in cosmology today. These fundamental questions require highly precise measurements, and a number of wide-field spectroscopic survey instruments are being designed to meet this requirement. A key component in these experiments is the development of a simulation tool to forecast science performance, define requirement flow-downs, optimize implementation, demonstrate feasibility, and prepare for exploitation. We present SPOKES (SPectrOscopic KEn Simulation), an end-to-end simulation facility for spectroscopic cosmological surveys designed to address this challenge. SPOKES is based on an integrated infrastructure, modular function organization, coherent data handling and fast data access. These key features allow reproducibility of pipeline runs, enable ease of use and provide flexibility to update functions within the pipeline. The cyclic nature of the pipeline offers the possibility to make the science output an efficient measure for design optimization and feasibility testing. We present the architecture, first science, and computational performance results of the simulation pipeline. The framework is general, but for the benchmark tests, we use the Dark Energy Spectrometer (DESpec), one of the early concepts for the upcoming project, the Dark Energy Spectroscopic Instrument (DESI). We discuss how the SPOKES framework enables a rigorous process to optimize and exploit spectroscopic survey experiments in order to derive high-precision cosmological measurements optimally., Comment: 24 pages, 8 figures, 2 tables

Published
2016
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31. ERRATUM: 'AUTOMATED TRANSIENT IDENTIFICATION IN THE DARK ENERGY SURVEY' (2015, AJ, 150, 82)

Author

Goldstein, DA, D’Andrea, CB, Fischer, JA, Foley, RJ, Gupta, RR, Kessler, R, Kim, AG, Nichol, RC, Nugent, PE, Papadopoulos, A, Sako, M, Smith, M, Sullivan, M, Thomas, RC, Wester, W, Wolf, RC, Abdalla, FB, Banerji, M, Benoit-Lévy, A, Bertin, E, Brooks, D, Rosell, A Carnero, Castander, FJ, da Costa, LN, Covarrubias, R, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Neto, A Fausti, Finley, DA, Flaugher, B, Fosalba, P, Frieman, J, Gerdes, D, Gruen, D, Gruendl, RA, James, D, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Maia, MAG, Makler, M, March, M, Marshall, JL, Martini, P, Merritt, KW, Miquel, R, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, and Walker, AR

Subjects
Astronomy & Astrophysics, Astronomical and Space Sciences
Published
2015

32. AUTOMATED TRANSIENT IDENTIFICATION IN THE DARK ENERGY SURVEY (vol 150, 82, 2015)

Author

Goldstein, DA, D'Andrea, CB, Fischer, JA, Foley, RJ, Gupta, RR, Kessler, R, Kim, AG, Nichol, RC, Nugent, PE, Papadopoulos, A, Sako, M, Smith, M, Sullivan, M, Thomas, RC, Wester, W, Wolf, RC, Abdalla, FB, Banerji, M, Benoit-Levy, A, Bertin, E, Brooks, D, Carnero Rosell, A, Castander, FJ, da Costa, LN, Covarrubias, R, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Fausti Neto, A, Finley, DA, Flaugher, B, Fosalba, P, Frieman, J, Gerdes, D, Gruen, D, Gruendl, RA, James, D, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Maia, MAG, Makler, M, March, M, Marshall, JL, Martini, P, Merritt, KW, Miquel, R, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Roodman, A, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, and Walker, AR

Subjects
Astronomy & Astrophysics, Astronomical and Space Sciences
Published
2015

33. DES J0454-4448: Discovery of the First Luminous z > 6 Quasar from the Dark Energy Survey

Author

Reed, S. L., McMahon, R. G., Banerji, M., Becker, G. D., Gonzalez-Solares, E., Martini, P., Ostrovski, F., Rauch, M., Abbott, T., Abdalla, F. B., Allam, S., Benoit-Levy, A., Bertin, E., Buckley-Geer, E., Burke, D., Rosell, A. Carnero, da Costa, L. N., ��Andrea, C., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Cunha, C. E, Estrada, J., Evrard, A. E., Neto, A. Fausti, Finley, D. A., Fosalba, P., Frieman, J., Gruen, D., Honscheid, K., James, D., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Makler, M., Marshall, J., Merritt, K., Miquel, R., Mohr, J., Nord, B., Ogando, R., Plazas, A., Romer, K., Roodman, A., Rykoff, E., Sako, M., Sanchez, E., Santiago, B., Schubnell, M., Sevilla, I., Smith, C., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D., Walker, A., and Wechsler, R. H.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract

We present the first results of a survey for high redshift, z $\ge$ 6, quasars using izY multi-colour photometric observations from the Dark Energy Survey (DES). Here we report the discovery and spectroscopic confirmation of the $\rm z_{AB}, Y_{AB}$ = 20.2, 20.2 (M$_{1450}$ = $-$26.5) quasar DES J0454$-$4448 with an emission line redshift of z = 6.10$\pm$0.03 and a HI near zone size of 4.6 $\pm$ 1.7 Mpc.The quasar was selected as an i-band drop out with i$-$z = 2.46 and z$_{AB} < 21.5$ from an area of $\rm \sim$300 deg$^2$. It is the brightest of our 43 candidates and was identified for follow-up spectroscopically solely based on the DES i$-$z and z$-$Y colours. The quasar is detected by WISE and has $W1_{AB} = 19.68$. The discovery of one spectroscopically confirmed quasar with 5.7 $$ 50-100 new quasars with z $>$ 6 including 3-10 with z $>$ 7 dramatically increasing the numbers of quasars currently known that are suitable for detailed studies including determination of the neutral HI fraction of the intergalactic medium (IGM) during the epoch of Hydrogen reionization., 9 pages, 13 figures, this is a pre-copyedited, author-produced version of an article accepted for publication in MNRAS following peer review

Published
2015
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34. SUPPLEMENT: 'lOCALIZATION and BROADBAND FOLLOW-UP of the GRAVITATIONAL-WAVE TRANSIENT GW150914' (2016, ApJL, 826, L13)

Author

Abbott, BP, Abbott, R, Abbott, TD, Abernathy, MR, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, RX, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, B, Allocca, A, Altin, PA, Anderson, SB, Anderson, WG, Arai, K, Araya, MC, Arceneaux, CC, Areeda, JS, Arnaud, N, Arun, KG, Ascenzi, S, Ashton, G, Ast, M, Aston, SM, Astone, P, Aufmuth, P, Aulbert, C, Babak, S, Bacon, P, Bader, MKM, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Barayoga, JC, Barclay, SE, Barish, BC, Barker, D, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Barthelmy, S, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Batch, JC, Baune, C, Bavigadda, V, Bazzan, M, Behnke, B, Bejger, M, Bell, AS, Bell, CJ, Berger, BK, Bergman, J, Bergmann, G, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhagwat, S, Bhandare, R, Bilenko, IA, Billingsley, G, Birch, J, Birney, R, Biscans, S, Bisht, A, Bitossi, M, Biwer, C, Bizouard, MA, Blackburn, JK, Blair, CD, Blair, DG, Blair, RM, Bloemen, S, Bock, O, Bodiya, TP, Boer, M, Bogaert, G, Bogan, C, Bohe, A, Bojtos, P, Bond, C, Bondu, F, Bonnand, R, Boom, BA, Bork, R, Boschi, V, Bose, S, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, PR, Braginsky, VB, Branchesi, M, Brau, JE, Briant, T, Brillet, A, Brinkmann, M, Brisson, V, Brockill, P, Brooks, AF, Brown, DA, Brown, DD, Brown, NM, Buchanan, CC, Buikema, A, Bulik, T, Bulten, HJ, Buonanno, A, Buskulic, D, Buy, C, Byer, RL, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, JC, Callister, T, Calloni, E, Camp, JB, Cannon, KC, Cao, J, Capano, CD, Capocasa, E, Carbognani, F, Caride, S, Diaz, JC, Casentini, C, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cepeda, CB, Baiardi, LC, Cerretani, G, Cesarini, E, Chakraborty, R, Chalermsongsak, T, Chamberlin, SJ, Chan, M, Chao, S, Charlton, P, Chassande-Mottin, E, Chen, HY, Chen, Y, Cheng, C, Chincarini, A, Chiummo, A, Cho, HS, Cho, M, Chow, JH, Christensen, N, Chu, Q, Chua, S, Chung, S, Ciani, G, Clara, F, Clark, JA, Cleva, F, Coccia, E, Cohadon, P-F, Colla, A, Collette, CG, Cominsky, L, Jr, Constancio M, Conte, A, Conti, L, Cook, D, Corbitt, TR, Cornish, N, Corsi, A, Cortese, S, Costa, CA, Coughlin, MW, Coughlin, SB, Coulon, J-P, Countryman, ST, Couvares, P, Cowan, EE, Coward, DM, Cowart, MJ, Coyne, DC, Coyne, R, Craig, K, Creighton, JDE, Cripe, J, Crowder, SG, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Danilishin, SL, D'Antonio, S, Danzmann, K, Darman, NS, Dattilo, V, Dave, I, Daveloza, HP, Davier, M, Davies, GS, Daw, EJ, Day, R, DeBra, D, Debreczeni, G, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Denker, T, Dent, T, Dereli, H, Dergachev, V, DeRosa, RT, De Rosa, R, DeSalvo, R, Dhurandhar, S, Diaz, MC, 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, KL, Doravari, S, Douglas, R, Downes, TP, Drago, M, Drever, RWP, Driggers, JC, Du, Z, Ducrot, M, Dwyer, SE, Edo, TB, Edwards, MC, Effler, A, Eggenstein, H-B, Ehrens, P, Eichholz, J, Eikenberry, SS, Engels, W, Essick, RC, Etzel, T, Evans, M, Evans, TM, Everett, R, Factourovich, M, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Fang, Q, Farinon, S, Farr, B, Farr, WM, Favata, M, Fays, M, Fehrmann, H, Fejer, MM, Ferrante, I, Ferreira, EC, Ferrini, F, Fidecaro, F, Fiori, I, Fiorucci, D, Fisher, RP, Flaminio, R, Fletcher, M, Fournier, J-D, Franco, S, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fricke, TT, Fritschel, P, Frolov, VV, Fulda, P, Fyffe, M, Gabbard, HAG, Gair, JR, Gammaitoni, L, Gaonkar, SG, 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, JA, Giardina, KD, Giazotto, A, Gill, K, Glaefke, A, Goetz, E, Goetz, R, Gondan, L, Gonzalez, G, Castro, JMG, Gopakumar, A, Gordon, NA, Gorodetsky, ML, Gossan, SE, Gosselin, M, Gouaty, R, Graef, C, Graff, PB, Granata, M, Grant, A, Gras, S, Gray, C, Greco, G, Green, AC, Groot, P, Grote, H, Grunewald, S, Guidi, GM, Guo, X, Gupta, A, Gupta, MK, Gushwa, KE, Gustafson, EK, Gustafson, R, Hacker, JJ, Hall, BR, Hall, ED, Hammond, G, Haney, M, Hanke, MM, Hanks, J, Hanna, C, Hannam, MD, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, GM, Harry, IW, Hart, MJ, Hartman, MT, Haster, C-J, Haughian, K, Heidmann, A, Heintze, MC, Heitmann, H, Hello, P, Hemming, G, Hendry, M, Heng, IS, Hennig, J, Heptonstall, AW, Heurs, M, Hild, S, Hoak, D, Hodge, KA, Hofman, D, Hollitt, SE, Holt, K, Holz, DE, Hopkins, P, Hosken, DJ, Hough, J, Houston, EA, Howell, EJ, Hu, YM, Huang, S, Huerta, EA, Huet, D, Hughey, B, Husa, S, Huttner, SH, Huynh-Dinh, T, Idrisy, A, Indik, N, Ingram, DR, Inta, R, Isa, HN, Isac, J-M, Isi, M, Islas, G, Isogai, T, Iyer, BR, Izumi, K, Jacqmin, T, Jang, H, Jani, K, Jaranowski, P, Jawahar, S, Jimenez-Forteza, F, Johnson, WW, Jones, DI, Jones, R, Jonker, RJG, Ju, L, Kalaghatgi, CV, Kalogera, V, Kandhasamy, S, Kang, G, Kanner, JB, Karki, S, Kasprzack, M, Katsavounidis, E, Katzman, W, Kaufer, S, Kaur, T, Kawabe, K, Kawazoe, F, Kefelian, F, Kehl, MS, Keitel, D, Kelley, DB, Kells, W, Kennedy, R, Key, JS, Khalaidovski, A, Khalili, FY, Khan, I, Khan, S, Khan, Z, Khazanov, EA, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, N, Kim, Y-M, King, EJ, King, PJ, Kinzel, DL, Kissel, JS, Kleybolte, L, Klimenko, S, Koehlenbeck, SM, Kokeyama, K, Koley, S, Kondrashov, V, Kontos, A, Korobko, M, Korth, WZ, Kowalska, I, Kozak, DB, Kringel, V, Krolak, A, Krueger, C, Kuehn, G, Kumar, P, Kuo, L, Kutynia, A, Lackey, BD, Landry, M, Lange, J, Lantz, B, Lasky, PD, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lebigot, EO, Lee, CH, Lee, HK, Lee, HM, Lee, K, Lenon, A, Leonardi, M, Leong, JR, Leroy, N, Letendre, N, Levin, Y, Levine, BM, Li, TGF, Libson, A, Littenberg, TB, Lockerbie, NA, Logue, J, Lombardi, AL, Lord, JE, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, JD, Lueck, H, Lundgren, P, Luo, J, Lynch, R, Ma, Y, MacDonald, T, Machenschalk, B, MacInnis, M, Macleod, DM, Magana-Sandoval, F, Magee, RM, Mageswaran, M, Majorana, E, Maksimovic, I, Malvezzi, V, Man, N, Mandel, I, Mandic, V, Mangano, V, Mansell, GL, Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markosyan, AS, Maros, E, Martelli, F, Martellini, L, Martin, IW, Martin, RM, Martynov, DV, Marx, JN, Mason, K, Masserot, A, Massinger, TJ, Masso-Reid, M, Matichard, F, Matone, L, Mavalvala, N, Mazumder, N, Mazzolo, G, McCarthy, R, McClelland, DE, McCormick, S, McGuire, SC, McIntyre, G, McIver, J, McManus, DJ, McWilliams, ST, Meacher, D, Meadors, GD, Meidam, J, Melatos, A, Mendell, G, Mendoza-Gandara, D, Mercer, RA, Merilh, E, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Meyers, PM, Mezzani, F, Miao, H, Michel, C, Middleton, H, Mikhailov, EE, Milano, L, Miller, J, Millhouse, M, Minenkov, Y, Ming, J, Mirshekari, S, Mishra, C, Mitra, S, Mitrofanov, VP, Mitselmakher, G, Mittleman, R, Moggi, A, Mohan, M, Mohapatra, SRP, Montani, M, Moore, BC, Moore, CJ, Moraru, D, Moreno, G, Morriss, SR, Mossavi, K, Mours, B, Mow-Lowry, CM, Mueller, CL, Mueller, G, Muir, AW, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Murphy, DJ, Murray, PG, Mytidis, A, Nardecchia, I, Naticchioni, L, Nayak, RK, Necula, V, Nedkova, K, Nelemans, G, Neri, M, Neunzert, A, Newton, G, Nguyen, TT, Nielsen, AB, Nissanke, S, Nitz, A, Nocera, F, Nolting, D, Normandin, MEN, Nuttall, LK, Oberling, J, Ochsner, E, O'Dell, J, Oelker, E, Ogin, GH, Oh, JJ, Oh, SH, Ohme, F, Oliver, M, Oppermann, P, Oram, RJ, O'Reilly, B, O'Shaughnessy, R, Ottaway, DJ, Ottens, RS, Overmier, H, Owen, BJ, Pai, A, Pai, SA, Palamos, JR, Palashov, O, Palliyaguru, N, Palomba, C, Pal-Singh, A, Pan, H, Pankow, C, Pannarale, F, Pant, BC, Paoletti, F, Paoli, A, Papa, MA, Paris, HR, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patricelli, B, Patrick, Z, Pearlstone, BL, 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, IM, Pitkin, M, Poggiani, R, Popolizio, P, Post, A, Powell, J, Prasad, J, Predoi, V, Premachandra, SS, Prestegard, T, Price, LR, Prijatelj, M, Principe, M, Privitera, S, Prodi, GA, Prokhorov, L, Puncken, O, Punturo, M, Puppo, P, Puerrer, M, Qi, H, Qin, J, Quetschke, V, Quintero, EA, Quitzow-James, R, Raab, FJ, Rabeling, DS, Radkins, H, Raffai, P, Raja, S, Rakhmanov, M, Rapagnani, P, Raymond, V, Razzano, M, Re, V, Read, J, Reed, CM, Regimbau, T, Rei, L, Reid, S, Reitze, DH, Rew, H, Reyes, SD, Ricci, F, Riles, K, Robertson, NA, Robie, R, Robinet, F, Rocchi, A, Rolland, L, Rollins, JG, Roma, VJ, Romano, R, Romanov, G, Romie, JH, Rosinska, D, Rowan, S, Ruediger, A, Ruggi, P, Ryan, K, Sachdev, S, Sadecki, T, Sadeghian, L, Salconi, L, Saleem, M, Salemi, F, Samajdar, A, Sammut, L, Sanchez, EJ, Sandberg, V, Sandeen, B, Sanders, JR, Sassolas, B, Sathyaprakash, BS, Saulson, PR, Sauter, O, Savage, RL, Sawadsky, A, Schale, P, Schilling, R, Schmidt, J, Schmidt, P, Schnabel, R, Schofield, RMS, Schoenbeck, A, Schreiber, E, Schuette, D, Schutz, BF, Scott, J, Scott, SM, Sellers, D, Sentenac, D, Sequino, V, Sergeev, A, Serna, G, Setyawati, Y, Sevigny, A, Shaddock, DA, Shah, S, Shahriar, MS, Shaltev, M, Shao, Z, Shapiro, B, Shawhan, P, Sheperd, A, Shoemaker, DH, Shoemaker, DM, Siellez, K, Siemens, X, Sigg, D, Silva, AD, Simakov, D, Singer, A, Singh, A, Singh, R, Singhal, A, Sintes, AM, Slagmolen, BJJ, Smith, JR, Smith, ND, Smith, RJE, Son, EJ, Sorazu, B, Sorrentino, F, Souradeep, T, Srivastava, AK, Staley, A, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stephens, BC, Stone, R, Strain, KA, Straniero, N, Stratta, G, Strauss, NA, Strigin, S, Sturani, R, Stuver, AL, Summerscales, TZ, Sun, L, Sutton, PJ, Swinkels, BL, SzczepaNczyk, MJ, Tacca, M, Talukder, D, Tanner, DB, Tpai, M, Tarabrin, SP, Taracchini, A, Taylor, R, Theeg, T, Thirugnanasambandam, P, Thomas, EG, Thomas, M, Thomas, P, Thorne, KA, Thorne, KS, Thrane, E, Tiwari, S, Tiwari, V, Tokmakov, KV, Tomlinson, C, Tonelli, M, Torres, CV, Torrie, CI, Tyr, D, Travasso, F, Traylor, G, Trifiro, D, Tringali, MC, Trozzo, L, Tse, M, Turconi, M, Tuyenbayev, D, Ugolini, D, Unnikrishnan, CS, Urban, AL, Usman, SA, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, JFJ, Van den Broeck, C, Vander-Hyde, DC, van der Schaaf, L, van Heijningen, JV, van Veggel, AA, Vardaro, M, Vass, S, Vasuth, M, Vaulin, R, Vecchio, A, Vedovato, G, Veitch, J, Veitch, PJ, Venkateswara, K, Verkindt, D, Vetrano, F, Vicere, A, Vinciguerra, S, Vine, DJ, Vinet, J-Y, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Voss, D, Vousden, WD, Vyatchanin, SP, Wade, AR, Wade, LE, Wade, M, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, M, Wang, X, Wang, Y, Ward, RL, Warner, J, Was, M, Weaver, B, Wei, L-W, Weinert, M, Weinstein, AJ, Weiss, R, Welborn, T, Wen, L, Wessels, P, Westphal, T, Wette, K, Whelan, JT, White, DJ, Whiting, BF, Williams, RD, Williamson, AR, Willis, JL, Willke, B, Wimmer, MH, Winkler, W, Wipf, CC, Wittel, H, Woan, G, Worden, J, Wright, JL, Wu, G, Yablon, J, Yam, W, Yamamoto, H, Yancey, CC, Yap, MJ, Yu, H, Yvert, M, Zadrozny, 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, XJ, Zucker, ME, Zuraw, SE, Zweizig, J, Allison, J, Bannister, K, Bell, ME, Chatterjee, S, Chippendale, AP, Edwards, PG, Harvey-Smith, L, Heywood, Ian, Hotan, A, Indermuehle, B, Marvil, J, McConnell, D, Murphy, T, Popping, A, Reynolds, J, Sault, RJ, Voronkov, MA, Whiting, MT, Castro-Tirado, AJ, Cunniffe, R, Jelinek, M, Tello, JC, Oates, SR, Hu, Y-D, Kubanek, P, Guziy, S, Castellon, A, Garcia-Cerezo, A, Munoz, VF, Perez del Pulgar, C, Castillo-Carrion, S, Castro Ceron, JM, Hudec, R, Caballero-Garcia, MD, Pata, P, Vitek, S, Adame, JA, Konig, S, Rendon, F, Mateo Sanguino, T de J, Fernandez-Munoz, R, Yock, PC, Rattenbury, N, Allen, WH, Querel, R, Jeong, S, Park, IH, Bai, J, Cui, Ch, Fan, Y, Wang, Ch, Hiriart, D, Lee, WH, Claret, A, Sanchez-Ramirez, R, Pandey, SB, Mediavilla, T, Sabau-Graziati, L, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Armstrong, R, Benoit-Levy, A, Berger, E, Bernstein, RA, Bertin, E, Brout, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Carretero, J, Castander, FJ, Chornock, R, Cowperthwaite, PS, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Desai, S, Diehl, HT, Dietrich, JP, Doctor, Z, Drlica-Wagner, A, Drout, MR, Eifler, TF, Estrada, J, Evrard, AE, Fernandez, E, Finley, DA, Flaugher, B, Foley, RJ, Fong, W-F, Fosalba, P, Fox, DB, Frieman, J, Fryer, CL, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gutierrez, G, Herner, K, Honscheid, K, James, DJ, Johnson, MD, Johnson, MWG, Karliner, I, Kasen, D, Kent, S, Kessler, R, Kim, AG, Kind, MC, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Lin, H, Maia, MAG, Margutti, R, Marriner, J, Martini, P, Matheson, T, Melchior, P, Metzger, BD, Miller, CJ, Miquel, R, Neilsen, E, Nichol, RC, Nord, B, Nugent, P, Ogando, R, Petravick, D, Plazas, AA, Quataert, E, Roe, N, Romer, AK, Roodman, A, Rosell, AC, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Scolnic, D, Sevilla-Noarbe, I, Sheldon, E, Smith, N, Smith, RC, Soares-Santos, M, Sobreira, F, Stebbins, A, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Thomas, RC, Tucker, DL, Vikram, V, Walker, AR, Wechsler, RH, Wester, W, Yanny, B, Zuntz, J, Connaughton, V, Burns, E, Goldstein, A, Briggs, MS, Zhang, B-B, Hui, CM, Jenke, P, Wilson-Hodge, CA, Bhat, PN, Bissaldi, E, Cleveland, W, Fitzpatrick, G, Giles, MM, Gibby, MH, Greiner, J, von Kienlin, A, Kippen, RM, McBreen, S, Mailyan, B, Meegan, CA, Paciesas, WS, Preece, RD, Roberts, O, Sparke, L, Stanbro, M, Toelge, K, Veres, P, Yu, H-F, Blackburn, L, Ackermann, M, Ajello, M, Albert, A, Anderson, B, Atwood, WB, Axelsson, M, Baldini, L, Barbiellini, G, Bastieri, D, Bellazzini, R, Blandford, RD, Bloom, ED, Bonino, R, Bottacini, E, Brandt, TJ, Bruel, P, Buson, S, Caliandro, GA, Cameron, RA, Caragiulo, M, Caraveo, PA, Cavazzuti, E, Charles, E, Chekhtman, A, Chiang, J, Chiaro, G, Ciprini, S, Cohen-Tanugi, J, Cominsky, LR, Costanza, F, Cuoco, A, D'Ammando, F, de Palma, F, Desiante, R, Digel, SW, Di Lalla, N, Di Mauro, M, Di Venere, L, Dominguez, A, Drell, PS, Dubois, R, Favuzzi, C, Ferrara, EC, 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, GA, Green, D, Grenier, IA, Grove, JE, Guiriec, S, Hadasch, D, Harding, AK, Hays, E, Hewitt, JW, Hill, AB, Horan, D, Jogler, T, Johannesson, G, Johnson, AS, Kensei, S, Kocevski, D, Kuss, M, La Mura, G, Larsson, S, Latronico, L, Li, J, Li, L, Longo, F, Loparco, F, Lovellette, MN, Lubrano, P, Magill, J, Maldera, S, Manfreda, A, Marelli, M, Mayer, M, Mazziotta, MN, McEnery, JE, Meyer, M, Michelson, PF, Mirabal, N, Mizuno, T, Moiseev, AA, Monzani, ME, Moretti, E, Morselli, A, Moskalenko, IV, Negro, M, Nuss, E, Ohsugi, T, Omodei, N, Orienti, M, Orlando, E, Ormes, JF, Paneque, D, Perkins, JS, Pesce-Rollins, M, Piron, F, Pivato, G, Porter, TA, Racusin, JL, Raino, S, Rando, R, Razzaque, S, Reimer, A, Reimer, O, Salvetti, D, Parkinson, PM Saz, Sgro, C, Simone, D, Siskind, EJ, Spada, F, Spandre, G, Spinelli, P, Suson, DJ, Tajima, H, Thayer, JB, Thompson, DJ, Tibaldo, L, Torres, DF, Troja, E, Uchiyama, Y, Venters, TM, Vianello, G, Wood, KS, Wood, M, Zhu, S, Zimmer, S, Brocato, E, Cappellaro, E, Covino, S, Grado, A, Nicastro, L, Palazzi, E, Pian, E, Amati, L, Antonelli, LA, 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, Bazzano, A, Bozzo, E, Brandt, S, Courvoisier, TJ-L, Ferrigno, C, Hanlon, L, Kuulkers, E, Laurent, P, Mereghetti, S, Roques, JP, Savchenko, V, Ubertini, P, Kasliwal, MM, Singer, LP, Cao, Y, Duggan, G, Kulkarni, SR, Bhalerao, V, Miller, AA, Barlow, T, Bellm, E, Manulis, I, Rana, J, Laher, R, Masci, F, Surace, J, Rebbapragada, U, Van Sistine, A, Sesar, B, Perley, D, Ferreti, R, Prince, T, Kendrick, R, Horesh, A, Hurley, K, Golenetskii, SV, Aptekar, RL, Frederiks, DD, Svinkin, DS, Rau, A, Zhang, X, Smith, DM, Cline, T, Krimm, H, Abe, F, Doi, M, Fujisawa, K, Kawabata, KS, Morokuma, T, Motohara, K, Tanaka, M, Ohta, K, Yanagisawa, K, Yoshida, M, Baltay, C, Rabinowitz, D, Ellman, N, Rostami, S, Bersier, DF, Bode, MF, Collins, CA, Copperwheat, CM, Darnley, MJ, Galloway, DK, Gomboc, A, Kobayashi, S, Mazzali, P, Mundell, CG, Piascik, AS, Pollacco, Don, Steele, IA, Ulaczyk, K, Broderick, JW, Fender, RP, Jonker, PG, Rowlinson, A, Stappers, BW, Wijers, RAMJ, Lipunov, V, Gorbovskoy, E, Tyurina, N, Kornilov, V, Balanutsa, P, Kuznetsov, A, Buckley, D, Rebolo, R, Serra-Ricart, 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Subjects
TELESCOPE, gravitational waves – methods: observational, Astronomy, media_common.quotation_subject, observational [methods], GW150914, ADVANCED LIGO, supplement, 01 natural sciences, localization, SEARCH, Computer Science::Multimedia, 0103 physical sciences, Broadband, EM follow-up, 010303 astronomy & astrophysics, gravitational wave, QC, media_common, QB, Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Gravitational waves, methods: observational, Space and Planetary Science, Astronomy and Astrophysic, Computational physics, GW150914, localization, EM follow-up, supplement, gravitational waves, Sky, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, DARK ENERGY, Transient (oscillation), Current (fluid), SYSTEM
Abstract

Made available in DSpace on 2018-11-26T16:56:32Z (GMT). No. of bitstreams: 0 Previous issue date: 2016-07-01 United States National Science Foundation (NSF) Science and Technology Facilities Council (STFC) of the United Kingdom Max-Planck Society State of Niedersachsen/Germany Australian Research Council Netherlands Organisation for Scientific Research EGO consortium Council of Scientific and Industrial Research of India Department of Science and Technology, India Science & Engineering Research Board (SERB), India Ministry of Human Resource Development, India Spanish Ministerio de Economia y Competitividad Conselleria d'Economia i Competitivitat and Conselleria d'Educacio Cultura i Universitats of the Govern de les Illes Balears National Science Centre of Poland European Commission Royal Society Scottish Funding Council Scottish Universities Physics Alliance Hungarian Scientific Research Fund (OTKA) Lyon Institute of Origins (LIO) National Research Foundation of Korea Industry Canada Province of Ontario through Ministry of Economic Development and Innovation National Science and Engineering Research Council Canada Canadian Institute for Advanced Research Brazilian Ministry of Science, Technology, and Innovation Russian Foundation for Basic Research Leverhulme Trust Research Corporation Ministry of Science and Technology (MOST), Taiwan Kavli Foundation Australian Government National Collaborative Research Infrastructure Strategy Government of Western Australia United States Department of Energy United States National Science Foundation Ministry of Science and Education of Spain Science and Technology Facilities Council of the United Kingdom Higher Education Funding Council for England National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign Kavli Institute of Cosmological Physics at the University of Chicago Center for Cosmology and Astro-Particle Physics at the Ohio State University Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University Financiadora de Estudos e Projetos Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ) Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) Ministerio da Ciencia, Tecnologia e Inovacao Deutsche Forschungsgemeinschaft Collaborating Institutions in the Dark Energy Survey National Science Foundation MINECO Centro de Excelencia Severo Ochoa European Research Council under European Union's Seventh Framework Programme ERC NASA (United States) DOE (United States) IN2P3/CNRS (France) CEA/Irfu (France) ASI (Italy) INFN (Italy) MEXT (Japan) KEK (Japan) JAXA (Japan) Wallenberg Foundation Swedish Research Council National Space Board (Sweden) NASA in the United States DRL in Germany INAF for the project Gravitational Wave Astronomy with the first detections of adLIGO and adVIRGO experiments ESA (Denmark) ESA (France) ESA (Germany) ESA (Italy) ESA (Switzerland) ESA (Spain) German INTEGRAL through DLR grant US under NASA Grant National Science Foundation PIRE program grant Hubble Fellowship KAKENHI of MEXT Japan JSPS Optical and Near-Infrared Astronomy Inter-University Cooperation Program - MEXT UK Science and Technology Facilities Council ERC Advanced Investigator Grant Lomonosov Moscow State University Development programm Moscow Union OPTICA Russian Science Foundation National Research Foundation of South Africa Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS) NVIDIA at Harvard University University of Hawaii National Aeronautics and Space Administration's Planetary Defense Office Queen's University Belfast National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate European Research Council under European Union's Seventh Framework Programme/ERC STFC grants European Union FP7 programme through ERC STFC through an Ernest Rutherford Fellowship FONDECYT Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) NASA in the US This Supplement provides supporting material for Abbott et al. (2016a). 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. UK Space Agency in the UK Agenzia Spaziale Italiana (ASI) in Italy Ministerio de Ciencia y Tecnologia (MinCyT) Consejo Nacional de Investigaciones Cientificas y Tecnologicas (CONICET) from Argentina USA NSF PHYS NSF ICREA Science and Technology Facilities Council UK Space Agency CALTECH, LIGO, Pasadena, CA 91125 USA Louisiana State Univ, Baton Rouge, LA 70803 USA Univ Salerno, I-84084 Salerno, Italy Ist Nazl Fis Nucl, Sez Napoli, Complesso Univ Monte S Angelo, I-80126 Naples, Italy Univ Florida, Gainesville, FL 32611 USA LIGO Livingston Observ, Livingston, LA 70754 USA Univ Savoie Mt Blanc, CNRS IN2P3, Lab Annecy le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA Leibniz Univ Hannover, D-30167 Hannover, Germany Univ Pisa, I-56127 Pisa, Italy Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia Univ Mississippi, University, MS 38677 USA Calif State Univ Fullerton, Fullerton, CA 92831 USA Univ Paris 11, Univ Paris Saclay, CNRS, LAL,IN2P3, Orsay, France Chennai Math Inst, Chennai, Tamil Nadu, India Univ Roma Tor Vergata, I-00133 Rome, Italy Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England Univ Hamburg, D-22761 Hamburg, Germany INFN, Sez Roma, I-00185 Rome, Italy Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS,IN2P3,CEA,Irfu, F-75205 Paris 13, France Montana State Univ, Bozeman, MT 59717 USA Univ Perugia, I-06123 Perugia, Italy Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy EGO, I-56021 Pisa, Italy Syracuse Univ, Syracuse, NY 13244 USA Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland LIGO Hanford Observ, Richland, WA 99352 USA Wigner RCP, RMKI, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA Columbia Univ, New York, NY 10027 USA Stanford Univ, Stanford, CA 94305 USA Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy INFN, Sez Padova, I-35131 Padua, Italy CAMK PAN, PL-00716 Warsaw, Poland Univ Birmingham, Birmingham B15 2TT, W Midlands, England Univ Genoa, I-16146 Genoa, Italy INFN, Sez Genova, I-16146 Genoa, Italy RRCAT, Indore 452013, MP, India Lomonosov Moscow State Univ, Fac Phys, Moscow 119991, Russia Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland Univ Western Australia, Crawley, 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Spain Acad Sci Czech Republ, Inst Astron, CS-25165 Ondrejov, Czech Republic Acad Sci Czech Republ, Inst Phys, Slovance 1999-2, Prague 18221 8, Czech Republic Nikolaev Natl Univ, Nikolska Str 24, UA-54030 Nikolayev, Ukraine Univ Malaga, Fac Ciencias, Blvd Louis Pasteur, E-29010 Malaga, Spain Univ Malaga, Ensenanza Virtual & Labs Tecnol, Jimenez Fraud 10, E-29071 Malaga, Spain ISDEFE SMOS FOS ESA ESAC, E-28692 Villanueva De La Canada, Madrid, Spain Czech Tech Univ, Fac Elect Engn, Dept Radioelect, Tech 2, Prague 16627, Czech Republic Acad Sci Czech Republ, Inst Astron, Bocni 2 1401, CZ-14100 Prague 4, Czech Republic Estn Sondeos Atmosfer ESAt) El Arenosillo CEDEA I, E-21130 Mazagon, Huelva, Spain Univ Huelva, ETSI La Rabida, Dept Ingn Elect Sistemas Informat & Automat, E-21819 Palos De La Frontera, Huelva, Spain IHSM UMA CSIC, Inst Hortofruticultura Subtrop & Mediterranea La, E-29750 Algarrobo Costa, Malaga, Spain Univ Auckland, Dept Phys, Private Bag 92019, Auckland 1, New Zealand Vintage Lane Observ, RD3, Blenheim 7273, New Zealand Natl Inst Water & Atmospher Res NIWA, Lauder, New Zealand Sungkyunkwan Univ SKKU, Dept Phys, Suwon, South Korea Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70-264, Mexico City 04510, DF, Mexico Aryabhatta Res Inst Observat Sci, Manora Peak 263002, Nainital, India Univ Cadiz, Escuela Politecn Super, Avda Ramon Puyol, E-11202 Algeciras, Cadiz, Spain INTA, Div Ciencias Espacio, E-28850 Torrejon De Ardoz, Madrid, Spain Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain Ohio Univ, Inst Astrophys, Dept Phys & Astron, Clippinger Lab 251B, Athens, OH 45701 USA Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany Univ Munich, Fac Phys, 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CIEMAT, Madrid, Spain Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA Argonne Natl Lab, 9700 South Cass Ave, Argonne, IL 60439 USA Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35806 USA Univ Alabama, Dept Phys, 320 Sparkman Dr, Huntsville, AL 35899 USA NASA, Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA Univ Alabama, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35899 USA Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35899 USA Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy Jacobs Technol Inc, Huntsville, AL USA Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany Los Alamos Natl Lab, Los Alamos, NM 87545 USA Univ Coll Dublin, Sch Phys, Stillorgan Rd, Dublin 4, Ireland NASA Headquarters, Washington, DC USA Tech Univ Munich, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany Deutsch 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Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy Univ Torino, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy CNRS IN2P3, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA CRESST, Greenbelt, MD 20771 USA CIFS, I-10133 Turin, Italy Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy ASI, Sci Data Ctr, I-00133 Rome, Italy George Mason Univ, Coll Sci, Fairfax, VA 22030 USA Naval Res Lab, Washington, DC 20375 USA Univ Montpellier, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA INAF Ist Radioastron, I-40129 Bologna, Italy Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy Univ Udine, I-33100 Udine, Italy Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile Univ Maryland, Dept Phys, College Pk, MD 20742 USA Univ Maryland, Dept Astron, College Pk, MD 20742 USA Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France Naval Res Lab, Div Space Sci, Washington, DC 20375 USA Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria Univ North Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland IEEC CSIC, Inst Space Sci, Campus UAB, E-08193 Barcelona, Spain Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China Univ Hong Kong, Lab Space Res, Hong Kong, Hong Kong, Peoples R China NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan Max Planck Inst Kernphys, D-69029 Heidelberg, Germany ICREA, Barcelona, Spain Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, RM, Italy INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy INAF Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy INAF Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy Univ Naples Federico II, CU Monte St Angelo, Dip Fis Ettore Pancini, Via Cinthia, I-80126 Naples, Italy INAF ORA Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy INAF Osservatorio Astron Torino, Str Osservatorio 20, I-10025 Pino Torinese, To, Italy INAF Inst Space Astrophys & Planetol, Via Fosso del Cavaliere 100, I-00133 Rome, Italy Univ Geneva, Dept Astron, ISDC, Chemin Ecogia 16, CH-1290 Versoix, Switzerland Natl Space Inst Elektrovej, DTU Space, Bldg 327, DK-2800 Lyngby, Denmark Univ Coll Dublin, Sch Phys, Space Sci Grp, Dublin 4, Ireland ESAC, ESA, Sci Operat Dept, E-28691 Madrid, Spain Univ Paris Diderot, CNRS IN2P3, Sorbonne Paris Cite, APC,CEA Irfu,Observ Paris, 10 Rue Alice Domont & Leonie Duquet, F-75205 Paris 13, France INAF, IASF Milano, Via E Bassini 15, I-20133 Milan, Italy Univ Toulouse, 9 Ave Roche,BP 44346, F-31028 Toulouse, France UPS OMP, 9 Ave Roche,BP 44346, F-31028 Toulouse, France CNRS, 9 Ave Roche,BP 44346, F-31028 Toulouse, France IRAP, 9 Ave Roche,BP 44346, F-31028 Toulouse, France Univ Paris Diderot, CNRS IN2P3, Sorbonne Paris Cite, Francois Arago Ctr,APC,CEA Irfu,Observ Paris, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden Lockheed Martin Space Syst Co, Palo Alto, CA 94304 USA Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA Ioffe Phys Tech Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA Nagoya Univ, Inst Space Earth Environm Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan Yamaguchi Univ, Res Inst Time Studies, Yamaguchi, Yamaguchi 7538511, Japan Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan Kyoto Univ, Dept Astron, Kyoto, Kyoto 6068502, Japan Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan Yale Univ, Dept Phys, New Haven, CT 06520 USA Liverpool JMU, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia Univ Nova Gorica, Vipavska 13, Nova Gorica 5000, Slovenia Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands Univ Oxford, Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands Lomonosov Moscow State Univ, Sternberg Astron Inst, 13 Univ Skiy Prospekt, Moscow 119234, Russia South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa Inst Astrofis Canarias, Calle Via Lactea S-N, E-38200 Tenerife, Spain Irkutsk State Univ, Inst Appl Phys, 20 Gagarin Blvd, Irkutsk 664003, Russia RAS, Kislovodsk Solar Stn Main Pulkovo Observ, POB 45,Ul Gagarina 100, Kislovodsk 357700, Russia Blagoveschensk State Pedag Univ, Lenin Str 104, Blagoveshchensk 675000, Amur Region, Russia Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528851, Japan RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan Nihon Univ, Dept Phys, Chiyoda Ku, 1-8-14 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Manoa, Inst Astron, Honolulu, HI 96822 USA Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA Harvard Univ, Dept Phys, Cambridge, MA 02138 USA Millennium Inst Astrophys, Casilla 36-D, Santiago, Chile Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France Univ Paris 06, 98 Bis Blvd Arago, F-75014 Paris, France European Southern Observ, Alonso de Cordova 3107, Santiago, Chile Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaialantie 20, FI-21500 Piikkio, Finland Univ Chile, Dept Astron, Camino El Observ 1515, Santiago, Chile Univ Paris 06, Sorbonne Univ, UMR 7585, LPNHE, F-75005 Paris, France CNRS, UMR 7585, Lab Phys Nucl & Hautes Energies, 4 Pl Jussieu, F-75005 Paris, France Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel Univ Warsaw, Fac Phys, PL-02093 Warsaw, Poland Polish Acad Sci, Ctr Theoret Phys, PL-02668 Warsaw, Poland Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA Los Alamos Natl Lab, B244, Los Alamos, NM 87545 USA CNRS UMR 5277 UPS, Inst Rech Astrophys & Planetol, 14 Ave Edouard Belin, F-31400 Toulouse, France Univ Texas San Antonio, San Antonio, TX USA Univ Munich, Fac Phys, Schellingstr 4, D-80799 Munich, Germany Texas A&M Univ, Dept Phys & Astron, Mitchell Inst Fundamental Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA Univ Nacl Cordoba, IATE, Laprida 854, Cordoba, Argentina Pontificia Univ Catolica Chile, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago, Chile CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil National Science Foundation: AST-1138766 National Science Foundation: AST-1238877 MINECO: AYA2012-39559 MINECO: ESP2013-48274 MINECO: FPA2013-47986 Centro de Excelencia Severo Ochoa: SEV-2012-0234 ERC: 240672 ERC: 291329 ERC: 306478 German INTEGRAL through DLR grant: 50 OG 1101 US under NASA Grant: NNX15AU74G National Science Foundation PIRE program grant: 1545949 Hubble Fellowship: HST-HF-51325.01 KAKENHI of MEXT Japan: 24103003 KAKENHI of MEXT Japan: 15H00774 KAKENHI of MEXT Japan: 15H00788 JSPS: 15H02069 JSPS: 15H02075 ERC Advanced Investigator Grant: 267697 Russian Science Foundation: 16-12-00085 Russian Science Foundation: RFBR15-02-07875 National Aeronautics and Space Administration's Planetary Defense Office: NNX14AM74G National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate: NNX08AR22G European Research Council under European Union's Seventh Framework Programme/ERC: 291222 STFC grants: ST/I001123/1 STFC grants: ST/L000709/1 European Union FP7 programme through ERC: 320360 FONDECYT: 3140326 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO): CE110001020 USA NSF PHYS: 1156600 NSF: 1242090 Science and Technology Facilities Council: Gravitational Waves Science and Technology Facilities Council: ST/L000946/1 Science and Technology Facilities Council: ST/K005014/1 Science and Technology Facilities Council: ST/N000668/1 Science and Technology Facilities Council: ST/M000966/1 Science and Technology Facilities Council: ST/I006269/1 Science and Technology Facilities Council: ST/L000709/1 Science and Technology Facilities Council: ST/J00166X/1 Science and Technology Facilities Council: ST/K000845/1 Science and Technology Facilities Council: ST/K00090X/1 Science and Technology Facilities Council: ST/N000633/1 Science and Technology Facilities Council: ST/H001972/1 Science and Technology Facilities Council: ST/L000733/1 Science and Technology Facilities Council: ST/N000757/1 Science and Technology Facilities Council: ST/M001334/1 Science and Technology Facilities Council: ST/J000019/1 Science and Technology Facilities Council: ST/M003035/1 Science and Technology Facilities Council: ST/I001123/1 Science and Technology Facilities Council: ST/N00003X/1 Science and Technology Facilities Council: ST/I006269/1 Gravitational Waves Science and Technology Facilities Council: ST/N000072/1 Science and Technology Facilities Council: ST/L003465/1 UK Space Agency: ST/P002196/1

35. 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

37. DES J0454$-$4448: Discovery of the First Luminous z $\ge$ 6 Quasar from the Dark Energy Survey

Author

Reed, S. L., Mcmahon, R. G., Banerji, M., Becker, G. D., Gonzalez-Solares, E., Martini, P., Ostrovski, F., Rauch, M., Abbott, T., Abdalla, F. B., Allam, S., Benoit-Levy, A., Bertin, E., Buckley-Geer, E., Burke, D., Carnero Rosell, A., Da Costa, L. N., Ďandrea, C., Depoy, D. L., Desai, S., Diehl, H. T., Doel, P., Cunha, C. E., Estrada, J., Evrard, A. E., Fausti Neto, A., Finley, D. A., Fosalba, P., Frieman, J., Gruen, D., Honscheid, K., James, D., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Makler, M., Marshall, J., Merritt, K., Miquel, R., Mohr, J., Nord, B., Ogando, R., Plazas, A., Romer, K., Roodman, A., Rykoff, E., Sako, M., Sanchez, E., Santiago, B., Schubnell, M., Sevilla, I., Smith, C., Soares-Santos, M., Eric Suchyta, Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D., Walker, A., and Wechsler, R. H.

38. Extreme magnification of an individual star at redshift 1.5 by a galaxy-cluster lens

Author

Agnello, A, Lin, H, Kuropatkin, N, Buckley-Geer, E, Anguita, T, Schechter, P L, Morishita, T, Motta, V, Rojas, K, Treu, T, Amara, A, Auger, M W, Courbin, F, Fassnacht, C D, Frieman, J, More, A, Marshall, P J, McMahon, R G, Meylan, G, Suyu, S H, Glazebrook, K, Morgan, N, Nord, B, Abbott, T M C, Abdalla, F B, Annis, J, Bechtol, K, Benoit-Lévy, A, Bertin, E, Bernstein, R A, Brooks, D, Burke, D L, Rosell, A Carnero, Carretero, J, Cunha, C E, D’Andrea, C B, da Costa, L N, Desai, S, Drlica-Wagner, A, Eifler, T F, Flaugher, B, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Honscheid, K, James, D J, Kuehn, K, Lahav, O, Lima, M, Maia, M A G, March, M, Menanteau, F, Miquel, R, Ogando, R L C, Plazas, A A, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, M E C, Tarle, G, Tucker, D, Wechsler, R, Kelly, Patrick L., Diego, Jose M., Rodney, Steven, Kaiser, Nick, Broadhurst, Tom, Zitrin, Adi, Treu, Tommaso, Pérez-González, Pablo G., Morishita, Takahiro, Jauzac, Mathilde, Selsing, Jonatan, Oguri, Masamune, Pueyo, Laurent, Ross, Timothy W., Filippenko, Alexei V., Smith, Nathan, Hjorth, Jens, Cenko, S. Bradley, Wang, Xin, Howell, D. Andrew, Richard, Johan, Frye, Brenda L., Jha, Saurabh W., Foley, Ryan J., Norman, Colin, Bradac, Marusa, Zheng, Weikang, Brammer, Gabriel, Benito, Alberto Molino, Cava, Antonio, Christensen, Lise, de Mink, Selma E., Graur, Or, Grillo, Claudio, Kawamata, Ryota, Kneib, Jean-Paul, Matheson, Thomas, McCully, Curtis, Nonino, Mario, Pérez-Fournon, Ismael, Riess, Adam G., Rosati, Piero, Schmidt, Kasper Borello, Sharon, Keren, and Weiner, Benjamin J.

39. 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.

40. 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

41. Discovery of the Lensed Quasar System DES J0408-5354

Author

Lin, H., Buckley-Geer, E., Agnello, A., Ostrovski, F., Mcmahon, R. G., Nord, B., Kuropatkin, N., Tucker, D. L., Treu, T., Chan, J. H. H., Suyu, S. H., Diehl, H. T., Collett, T., Gill, M. S. S., More, A., Amara, A., Auger, M. W., Courbin, F., Fassnacht, C. D., Frieman, J., Marshall, P. J., Meylan, G., Rusu, C. E., Abbott, T. M. C., Abdalla, F. B., Allam, S., Banerji, M., Bechtol, K., Benoit-Levy, A., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., D'Andrea, C. B., Da Costa, L. N., Desai, S., Dietrich, J. P., Eifler, T. F., Finley, D. A., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Sanchez, E., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Walker, A. R., and DES Collaboration

Subjects
surveys, quasars: general, Astrophysics::Solar and Stellar Astrophysics, gravitational lensing: strong, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the discovery and spectroscopic confirmation of the quad-like lensed quasar system DES J0408-5354 found in the Dark Energy Survey (DES) Year 1 (Y1) data. This system was discovered during a search for DES Y1 strong lensing systems using a method that identified candidates as red galaxies with multiple blue neighbors. DES J0408-5354 consists of a central red galaxy surrounded by three bright (i < 20) blue objects and a fourth red object. Subsequent spectroscopic observations using the Gemini South telescope confirmed that the three blue objects are indeed the lensed images of a quasar with redshift z = 2.375, and that the central red object is an early-type lensing galaxy with redshift z = 0.597. DES J0408-5354 is the first quad lensed quasar system to be found in DES and begins to demonstrate the potential of DES to discover and dramatically increase the sample size of these very rare objects.

42. Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing

Author

Abbott, T. M. C., Abdalla, F. B., Alarcon, A., Aleksic, J., Allam, S., Allen, S., Amara, A., Annis, J., Asorey, J., Avila, S., Bacon, D., Balbinot, E., Banerji, M., Banik, N., Barkhouse, W., Baumer, M., Baxter, E., Bechtol, K., Becker, M. R., Benoit-Levy, A., Benson, B. A., Bernstein, G. M., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Buckley-Geer, E., Burke, D. L., Busha, M. T., Campos, A. [UNESP], Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, N., Childress, M., Choi, A., Conselice, C., Crittenden, R., Crocce, M., Cunha, C. E., D'Andrea, C. B., Costa, L. N. da, Das, R., Davis, T. M., Davis, C., De Vicente, J., DePoy, D. L., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elliott, A. E., Elsner, F., Elvin-Poole, J., Estrada, J., Evrard, A. E., Fang, Y., Fernandez, E., Ferte, A., Finley, D. A., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Garcia-Bellido, J., Garcia-Fernandez, M., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. D., Johnson, M. W. G., Kacprzak, T., Kent, S., Kim, A. G., King, A., Kirk, D., Kokron, N., Kovacs, A., Krause, E., Krawiec, C., Kremin, A., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lacasa, F. [UNESP], Lahav, O., Li, T. S., Liddle, A. R., Lidman, C., Lima, M., Lin, H., MacCrann, N., Maia, M. A. G., Makler, M., Manera, M., March, M., Marshall, J. L., Martini, P., McMahon, R. G., Melchior, P., Menanteau, F., Miquel, R., Miranda, V., Mudd, D., Muir, J., Moller, A., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R. L. C., Palmese, A., Peacock, J., Peiris, H. V., Peoples, J., Percival, W. J., Petravick, D., Plazas, A. A., Porredon, A., Prat, J., Pujol, A., Rau, M. M., Refregier, A., Ricker, P. M., Roe, N., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R. [UNESP], Ross, A. J., Rozo, E., Rykoff, E. S., Sako, M., Salvador, A. I., Samuroff, S., Sanchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, R. C., Smith, M., Smith, J., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Tucker, B. E., Uddin, S. A., Varga, T. N., Vielzeuf, P., Vikram, V., Vivas, A. K., Walker, A. R., Wang, M., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Yanny, B., Yuan, F., Zenteno, A., Zhang, B., Zhang, Y., Zuntz, J., Dark Energy Survey 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 Optical Astronomy Observatory, Rhodes University, University College London, IEEC-CSIC, Barcelona Institute of Science and Technology, Fermi National Accelerator Laboratory, Stanford University, ETH Zurich, University of Queensland, ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), University of Portsmouth, Universidad Autonoma de Madrid, University of Surrey, University of Cambridge, Witmer Hall, SLAC National Accelerator Laboratory, University of Pennsylvania, LSST, Institut d'Astrophysique de Paris, University of Chicago, Observatoire de Sauverny, Ohio State University, University of Manchester, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, Observatório Nacional, National Center for Supercomputing Applications, University of Illinois, University of Southampton, School of Physics and Astronomy, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), Texas A and M University, IIT Hyderabad, Excellence Cluster Universe, Ludwig-Maximilians-Universität, California Institute of Technology, University of Edinburgh, Ludwig-Maximilians Universität München, Max Planck Institute for Extraterrestrial Physics, Swinburne University of Technology, 501 Campbell Hall, Lawrence Berkeley National Laboratory, University of Washington, Santa Cruz Institute for Particle Physics, Universidade de São Paulo (USP), Australian Astronomical Observatory, Argonne National Laboratory, Centro Brasileiro de Pesquisas Físicas, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, Australian National University, University of Sussex, University of Arizona, UFRGS, Brookhaven National Laboratory, Dept. Physics-Astronomy, Universidade Estadual de Campinas (UNICAMP), Oak Ridge National Laboratory, Chinese Academy of Sciences, Cerro Tololo Interamer Observ, Rhodes Univ, UCL, CSIC, Barcelona Inst Sci & Technol, Fermilab Natl Accelerator Lab, Stanford Univ, Swiss Fed Inst Technol, Univ Queensland, ARC Ctr Excellence All Sky Astrophys CAASTRO, Univ Portsmouth, UAM, Univ Surrey, Univ Cambridge, Univ North Dakota, SLAC Natl Accelerator Lab, Univ Penn, CNRS, UPMC Univ Paris 06, Univ Chicago, EPFL, Ohio State Univ, Univ Manchester, Universidade Estadual Paulista (Unesp), Lab Interinst Astron LIneA, Observ Nacl, Natl Ctr Supercomp Applicat, Univ Illinois, Univ Southampton, Univ Nottingham, Univ Michigan, Ctr Invest Energet Medioambient & Tecnol CIEMAT, Texas A&M Univ, Ludwig Maximilians Univ Munchen, CALTECH, Univ Edinburgh, Max Planck Inst Extraterr Phys, Swinburne Univ Technol, Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Univ Washington, Santa Cruz Inst Particle Phys, Australian Astron Observ, Argonne Natl Lab, Ctrt Brasileiro Pesquisas Fisicas, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, Australian Natl Univ, Univ Sussex, Univ Arizona, Univ Fed Rio Grande do Sul, Brookhaven Natl Lab, Austin Peay State Univ, Oak Ridge Natl Lab, and Chinese Acad Sci

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, symbols.namesake, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, Weak gravitational lensing, STFC, ResearchInstitutes_Networks_Beacons/MERI, QC, Physics, 010308 nuclear & particles physics, Astronomy, RCUK, Manchester Environmental Research Institute, Redshift, Galaxy, symbols, Dark energy, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present cosmological results from a combined analysis of galaxy clustering and weak gravitational lensing, using 1321 deg$^2$ of $griz$ imaging data from the first year of the Dark Energy Survey (DES Y1). We combine three two-point functions: (i) the cosmic shear correlation function of 26 million source galaxies in four redshift bins, (ii) the galaxy angular autocorrelation function of 650,000 luminous red galaxies in five redshift bins, and (iii) the galaxy-shear cross-correlation of luminous red galaxy positions and source galaxy shears. To demonstrate the robustness of these results, we use independent pairs of galaxy shape, photometric redshift estimation and validation, and likelihood analysis pipelines. To prevent confirmation bias, the bulk of the analysis was carried out while blind to the true results; we describe an extensive suite of systematics checks performed and passed during this blinded phase. The data are modeled in flat $\Lambda$CDM and $w$CDM cosmologies, marginalizing over 20 nuisance parameters, varying 6 (for $\Lambda$CDM) or 7 (for $w$CDM) cosmological parameters including the neutrino mass density and including the 457 $\times$ 457 element analytic covariance matrix. We find consistent cosmological results from these three two-point functions, and from their combination obtain $S_8 \equiv \sigma_8 (\Omega_m/0.3)^{0.5} = 0.783^{+0.021}_{-0.025}$ and $\Omega_m = 0.264^{+0.032}_{-0.019}$ for $\Lambda$CDM for $w$CDM, we find $S_8 = 0.794^{+0.029}_{-0.027}$, $\Omega_m = 0.279^{+0.043}_{-0.022}$, and $w=-0.80^{+0.20}_{-0.22}$ at 68% CL. The precision of these DES Y1 results rivals that from the Planck cosmic microwave background measurements, allowing a comparison of structure in the very early and late Universe on equal terms. Although the DES Y1 best-fit values for $S_8$ and $\Omega_m$ are lower than the central values from Planck ..., Comment: Matches published version. Results essentially unchanged, except updated covariance matrix leads to improved chi^2 (colored text removed)

43. Eight Ultra-faint Galaxy Candidates Discovered in Year Two of the Dark Energy Survey

Author

Des, The Collaboration, Drlica-Wagner, A., Bechtol, K., Rykoff, E. S., Luque, E., Queiroz, A., Mao, Y. -Y, Risa Wechsler, Simon, J. D., Santiago, B., Yanny, B., Balbinot, E., Dodelson, S., Fausti Neto, A., James, D. J., Li, T. S., Maia, M. A. G., Marshall, J. L., Pieres, A., Stringer, K., Walker, A. R., Abbott, T. M. C., Abdalla, F. B., Allam, S., Benoit-Levy, A., Bernstein, G. M., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Crocce, M., Da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Evrard, A. E., Finley, D. A., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Kuehn, K., Kuropatkin, N., Lahav, O., Martini, P., Miquel, R., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D., Vikram, V., Wester, W., Zhang, Y., and Zuntz, J.

44. The DES Science Verification Weak Lensing Shear Catalogs

Author

Jarvis, M., Sheldon, E., Zuntz, J., Kacprzak, T., Bridle, S. L., Amara, A., Armstrong, R., Becker, M. R., Bernstein, G. M., Bonnett, C., Chang, C., Das, R., Jörg Dietrich, Drlica-Wagner, A., Eifler, T. F., Gangkofner, C., Gruen, D., Hirsch, M., Huff, E. M., Jain, B., Kent, S., Kirk, D., Maccrann, N., Melchior, P., Plazas, A. A., Refregier, A., Rowe, B., Rykoff, E. S., Samuroff, S., Sánchez, C., Suchyta, E., Troxel, M. A., Vikram, V., Abbott, T., Abdalla, F. B., Allam, S., Annis, J., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D Andrea, C. B., Da Costa, L. N., Depoy, D. L., Desai, S., Diehl, H. T., Doel, P., Fausti Neto, A., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., March, M., Martini, P., Miquel, R., Mohr, J. J., Neilsen, E., Nord, B., Ogando, R., Reil, K., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Walker, A. R., and Wechsler, R. H.

46. Wide-Field Lensing Mass Maps from DES Science Verification Data: Methodology and Detailed Analysis

Author

Vikram, V., Chang, C., Jain, B., Bacon, D., Amara, A., Becker, M. R., Bernstein, G., Bonnett, C., Bridle, S., Brout, D., Busha, M., Frieman, J., Gaztanaga, E., Hartley, W., Jarvis, M., Kacprzak, T., Kovacs, A., Lahav, O., Leistedt, B., Lin, H., Melchior, P., Peiris, H., Rozo, E., Rykoff, E., Sanchez, C., Sheldon, E., Troxel, M. A., Wechsler, R., Zuntz, J., Abbott, T., Abdalla, F. B., Armstrong, R., Banerji, M., Bauer, A. H., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carnero Rosell, A., Carrasco Kind, M., Castander, F. J., Crocce, M., Cunha, C. E., D Andrea, C. B., Da Costa, L. N., Depoy, D. L., Desai, S., Diehl, H. T., Dietrich, J. P., Estrada, J., August Evrard, Fausti Neto, A., Fernandez, E., Flaugher, B., Fosalba, P., Gerdes, D., Gruen, D., Gruendl, R. A., Honscheid, K., James, D., Kent, S., Kuehn, K., Kuropatkin, N., Li, T. S., Maia, M. A. G., Makler, M., March, M., Marshall, J., Martini, P., Merritt, K. W., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Sevilla, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Walker, A. R., and Weller, 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

Weak gravitational lensing allows one to reconstruct the spatial distribution of the projected mass density across the sky. These "mass maps" provide a powerful tool for studying cosmology as they probe both luminous and dark matter. In this paper, we present a weak lensing mass map reconstructed from shear measurements in a 139 sq. deg area from the Dark Energy Survey (DES) Science Verification (SV) data. We compare the distribution of mass with that of the foreground distribution of galaxies and clusters. The overdensities in the reconstructed map correlate well with the distribution of optically detected clusters. We demonstrate that candidate superclusters and voids along the line of sight can be identified, exploiting the tight scatter of the cluster photometric redshifts. We cross-correlate the mass map with a foreground magnitude-limited galaxy sample from the same data. Our measurement gives results consistent with mock catalogs from N-body simulations that include the primary sources of statistical uncertainties in the galaxy, lensing, and photo-z catalogs. The statistical significance of the cross-correlation is at the 6.8-sigma level with 20 arcminute smoothing. A major goal of this study is to investigate systematic effects arising from a variety of sources, including PSF and photo-z uncertainties. We make maps derived from twenty variables that may characterize systematics and find the principal components. We find that the contribution of systematics to the lensing mass maps is generally within measurement uncertainties. In this work, we analyze less than 3% of the final area that will be mapped by the DES; the tools and analysis techniques developed in this paper can be applied to forthcoming larger datasets from the survey., Comment: 21 pages, 14 figures, 2 tables; accepted to PRD

47. VizieR Online Data Catalog: OzDES DR1 (Childress+, 2017)

Author

Childress, M. J., Lidman, C., Davis, T. M., Tucker, B. E., Asorey, J., Yuan, F., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Banerji, M., Benoit-Levy, A., Stephanie Bernard, Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Cunha, C. E., Costa, L. N. Da, D Andrea, C. B., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Foley, R. J., Fosalba, P., Frieman, J., Garcia-Bellido, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hinton, S. R., Hoormann, J. K., James, D. J., Kessler, R., Kim, A. G., King, A. L., Kovacs, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lagattuta, D. J., Lewis, G. F., Li, T. S., Lima, M., Lin, H., Macaulay, E., Maia, M. A. G., Marriner, J., March, M., Marshall, J. L., Martini, P., Mcmahon, R. G., Menanteau, F., Miquel, R., Moller, A., Morganson, E., Mould, J., Mudd, D., Muthukrishna, D., Nichol, R. C., Nord, B., Ogando, R. L. C., Ostrovski, F., Parkinson, D., Plazas, A. A., Reed, S. L., Reil, K., Rome, R. A. K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, I. D., Sevilla-Noarbe, N., Seymour, R., Sharp, M., Smith, M., Soares-Santos, F., Sobreira, Sommer, N. E., Spinka, H., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Uddin, S. A., Walker, A. R., Wester, W., and Zhang, B. R.

48. COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

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., García-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., McMahon, R. G., 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
strong [gravitational lensing], astro-ph.GA, Astrophysics::Instrumentation and Methods for Astrophysics, data analysis [methods], Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmological parameters, Astronomy & Astrophysics, Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences, astro-ph.IM
Abstract

We present time-delay measurements for the new quadruple imaged quasar DES J04085354, the first quadruple 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 2.2 m 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, and hence making the time delay measurement very robust against microlensing. In only seven months we very accurately measured one of the time delays in DES J04085354: - "t(AB) = 112.1 ± 2.1 days (1.8%) using only the MPIA 2.2 m data. In combination with data taken with the 1.2 m Euler Swiss telescope, we also measured two delays involving the D component of the system - "t(AD) = ± 12.8 days (8.2%) and - "t(BD) = 42.4 ± 17.6 days (41%), where all the error bars include systematics. Turning these time delays into cosmological constraints will require deep Hubble Space Telescope (HST) imaging or ground-based adaptive optics (AO), and information on the velocity field of the lensing galaxy.

49. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Dark Energy Camera Discovery of the Optical Counterpart

Author

Soares-Santos, M., Holz, D. E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H., Kessler, R., Sako, M., Allam, S., Tucker, D. L., Butler, R. E., Palmese, A., Doctor, Z., Diehl, H. T., Frieman, J., Yanny, B., Lin, H., Scolnic, D., Cowperthwaite, P., Neilsen, E., Marriner, J., Kuropatkin, N., Hartley, W. G., Paz-Chinchón, F., Alexander, K. D., Balbinot, E., Blanchard, P., Brown, D. A., Carlin, J. L., Conselice, C., Cook, E. R., Drlica-Wagner, A., Drout, M. R., Durret, F., Eftekhari, T., Ben Farr, Finley, D. A., Foley, R. J., Fong, W., Fryer, C. L., García-Bellido, J., Gill, M. S. S., Gruendl, R. A., Hanna, C., Kasen, D., Li, T. S., Lopes, P. A. A., Lourenço, A. C. C., Margutti, R., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muñoz, R. R., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D. J., Secco, L. F., Sobreira, F., Stebbins, A., Villar, V. A., Walker, A. R., Wester, W., Williams, P. K. G., Zenteno, A., Zhang, Y., Abbott, T. M. C., Abdalla, F. B., Banerji, M., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D Andrea, C. B., Da Costa, L. N., Davis, C., Desai, S., Dietrich, J. P., Doel, P., Eifler, T. F., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M. A. G., March, M., Mcmahon, R. G., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Vikram, V., Wechsler, R. H., and Weller, J.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the Dark Energy Camera (DECam) discovery of the optical counterpart of the first binary neutron star merger detected through gravitational wave emission, GW170817. Our observations commenced 10.5 hours post-merger, as soon as the localization region became accessible from Chile. We imaged 70 deg$^2$ in the $i$ and $z$ bands, covering 93\% of the initial integrated localization probability, to a depth necessary to identify likely optical counterparts (e.g., a kilonova). At 11.4 hours post-merger we detected a bright optical transient located $10.6''$ from the nucleus of NGC\,4993 at redshift $z=0.0098$, consistent (for $H_0 = 70$\, km s$^{-1}$ Mpc$^{-1}$) with the distance of $40 \pm 8$\, Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes $i\approx 17.30$ and $z\approx 17.45$, and thus an absolute magnitude of $M_i = -15.7$, in the luminosity range expected for a kilonova. We identified 1,500 potential transient candidates. Applying simple selection criteria aimed at rejecting background events such as supernovae, we find the transient associated with NGC\,4993 as the only remaining plausible counterpart, and reject chance coincidence at the 99.5\% confidence level. We therefore conclude that the optical counterpart we have identified near NGC\,4993 is associated with GW170817. This discovery ushers in the era of multi-messenger astronomy with gravitational waves, and demonstrates the power of DECam to identify the optical counterparts of gravitational-wave sources., 9 Pages, 3 Figures, 2 Tables. ApJL, In Press. Keywords: GW170817, LVC

50. First SN Discoveries from the Dark Energy Survey

Author

Abbott, T., Abdalla, F., Achitouv, I., Ahn, E., Aldering, G., Allam, S., Alonso, D., Amara, A., Annis, J., Antonik, M., Aragon-Salamanca, A., Armstrong, R., Ashall, C., Asorey, J., Bacon, D., Balbinot, E., Banerji, M., Barbary, K., Barkhouse, W., Baruah, L., Bauer, A., Bechtol, K., Becker, M., Bender, R., Benoist, C., Benoit-Levy, A., Bernardi, M., Bernstein, G., Bernstein, J. P., Bernstein, R., Bertin, E., Beynon, E., Bhattacharya, S., Biesiadzinski, T., Biswas, R., Blake, C., Bloom, J. S., Bocquet, S., Brandt, C., Bridle, S., Brooks, D., Brown, P. J., Brunner, R., Buckley-Geer, E., Burke, D., Burkert, A., Busha, M., Campa, J., Campbell, H., Cane, R., Capozzi, D., Carlstrom, J., Rosell, A. Carnero, Carollo, M., Carrasco-Kind, M., Carretero, J., Carter, M., Casas, R., Castander, F. J., Chen, Y., Chiu, I., Chue, C., Clampitt, J., Clerkin, L., Cohn, J., Colless, M., Copeland, E., Covarrubias, R. A., Crittenden, R., Crocce, M., Cunha, C., Costa, L. Da, D, C., Andrea, Das, S., Das, R., Davis, T. M., Deb, S., Depoy, D., Derylo, G., Desai, S., Simoni, F., Devlin, M., Diehl, H. T., Dietrich, J., Dodelson, S., Doel, P., Dolag, K., Efstathiou, G., Eifler, T., Erickson, B., Eriksen, M., Estrada, J., Etherington, J., August Evrard, Farrens, S., Neto, A. Fausti, Fernandez, E., Ferreira, P. C., Finley, D., Fischer, J. A., Flaugher, B., Fosalba, P., Frieman, J., Furlanetto, C., Garcia-Bellido, J., Gaztanaga, E., Gelman, M., Gerdes, D., Giannantonio, T., Gilhool, S., Gill, M., Gladders, M., Gladney, L., Glazebrook, K., Gray, M., Gruen, D., Gruendl, R., Gupta, R., Gutierrez, G., Habib, S., Hall, E., Hansen, S., Hao, J., Heitmann, K., Helsby, J., Henderson, R., Hennig, C., High, W., Hirsch, M., Hoffmann, K., Holhjem, K., Honscheid, K., Host, O., Hoyle, B., Hu, W., Huff, E., Huterer, D., Jain, B., James, D., Jarvis, M., Jarvis, M. J., Jeltema, T., Johnson, M., Jouvel, S., Kacprzak, T., Karliner, I., Katsaros, J., Kent, S., Kessler, R., Kim, A., Kim-Vy, T., King, L., Kirk, D., Kochanek, C., Kopp, M., Koppenhoefer, J., Kovacs, E., Krause, E., Kravtsov, A., Kron, R., Kuehn, K., Kuemmel, M., Kuhlmann, S., Kunder, A., Kuropatkin, N., Kwan, J., Lahav, O., Leistedt, B., Levi, M., Lewis, P., Liddle, A., Lidman, C., Lilly, S., Lin, H., Liu, J., Lopez-Arenillas, C., Lorenzon, W., Loverde, M., Ma, Z., Maartens, R., Maccrann, N., Macri, L., Maia, M., Makler, M., Manera, M., Maraston, C., March, M., Markovic, K., Marriner, J., Marshall, J., Marshall, S., Martini, P., Sanahuja, P. Marti, Mayers, J., Mckay, T., Mcmahon, R., Melchior, P., Merritt, K. W., Merson, A., Miller, C., Miquel, R., Mohr, J., Moore, T., Mortonson, M., Mosher, J., Mould, J., Mukherjee, P., Neilsen, E., Ngeow, C., Nichol, R., Nidever, D., Nord, B., Nugent, P., Ogando, R., Old, L., Olsen, J., Ostrovski, F., Paech, K., Papadopoulos, A., Papovich, C., Patton, K., Peacock, J., Pellegrini, P. S. S., Peoples, J., Percival, W., Perlmutter, S., Petravick, D., Plazas, A., Ponce, R., Poole, G., Pope, A., Refregier, A., Reyes, R., Ricker, P., Roe, N., Romer, K., Roodman, A., Rooney, P., Ross, A., Rowe, B., Rozo, E., Rykoff, E., Sabiu, C., Saglia, R., Sako, M., Sanchez, A., Sanchez, C., Sanchez, E., Sanchez, J., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schmidt, B. P., Schmitt, R. L., Schubnell, M., Seitz, S., Senger, R., Sevilla, I., Sharp, R., Sheldon, E., Sheth, R., Smith, R. C., Smith, M., Snigula, J., Soares-Santos, M., Sobreira, F., Song, J., Soumagnac, M., Spinka, H., Stebbins, A., Stoughton, C., Suchyta, E., Suhada, R., Sullivan, M., Sun, F., Suntzeff, N., Sutherland, W., Swanson, M. E. C., Sypniewski, A. J., Szepietowski, R., Talaga, R., Tarle, G., Tarrant, E., Balan, S. Thaithara, Thaler, J., Thomas, D., Thomas, R. C., Tucker, D., Uddin, S. A., Ural, S., Vikram, V., Voigt, L., Walker, A. R., Walker, T., Wechsler, R., Weinberg, D., Weller, J., Wester, W., Wetzstein, M., White, M., Wilcox, H., Wilman, D., Yanny, B., Young, J., Zablocki, A., Zenteno, A., Zhang, Y., and Zuntz, J.

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