Author: "Plazas, A.A." - Searchworks@Jio Institute Digital Library Search Results

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30 results on '"Plazas, A.A."'

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

Author: Herner, K., Annis, J., Brout, D., Soares-Santos, M., Kessler, R., Sako, M., Butler, R., Doctor, Z., Palmese, A., Allam, S., Tucker, D.L., Sobreira, F., Yanny, B., Diehl, H.T., Frieman, J., Glaeser, N., Garcia, A., Sherman, N.F., Bechtol, K., Berger, E., Chen, H.Y., Conselice, C.J., Cook, E., Cowperthwaite, P.S., Davis, T.M., Drlica-Wagner, A., Farr, B., Finley, D., Foley, R.J., Garcia-Bellido, J., Gill, M.S.S., Gruendl, R.A., Holz, D.E., Kuropatkin, N., Lin, H., Marriner, J., Marshall, J.L., Matheson, T., Neilsen, E., Paz-Chinchón, F., Sauseda, M., Scolnic, D., Williams, P.K.G., Avila, S., Bertin, E., Buckley-Geer, E., Burke, D.L., Rosell, A. Carnero, Carrasco-Kind, M., Carretero, J., da Costa, L.N., De Vicente, J., Desai, S., Doel, P., Eifler, T.F., Everett, S., Fosalba, P., Gaztanaga, E., Gerdes, D.W., Gschwend, J., Gutierrez, G., Hartley, W.G., Hollowood, D.L., Honscheid, K., James, D.J., Krause, E., Kuehn, K., Lahav, O., Li, T.S., Lima, M., Maia, M.A.G., March, M., Menanteau, F., Miquel, R., Plazas, A.A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Wester, W., and Zhang, Y.
Published: 2020
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2. Reprint of "Evidence for color dichotomy in the primordial Neptunian Trojan population"

Author: Lin (林省文), Hsing Wen, W. Gerdes, David, J. Hamilton, Stephanie, C. Adams, Fred, M. Bernstein, Gary, Sako, Masao, Bernadinelli, Pedro, Tucker, Douglas, Allam, Sahar, C. Becker, Juliette, Khain, Tali, Markwardt, Larissa, Franson, Kyle, Abbott, T.M.C., Annis, J., Avila, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., De Vicente, J., Doel, P., Eifler, T.F., Flaugher, B., García-Bellido, J., Hollowood, D.L., Honscheid, Klaus, James, D.J., Kuehn, K., Kuropatkin, N., Maia, M.A.G., Marshall, J.L., Miquel, R., Plazas, A.A., Romer, A.K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., Walker, A.R., and Wester, W.
Published: 2019
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3. DES science portal: Computing photometric redshifts

Author: Gschwend, J., Rossel, A.C., Ogando, R.L.C., Neto, A.F., Maia, M.A.G., da Costa, L.N., Lima, M., Pellegrini, P., Campisano, R., Singulani, C., Adean, C., Benoist, C., Aguena, M., Carrasco Kind, M., Davis, T.M., de Vicente, J., Hartley, W.G., Hoyle, B., Palmese, A., Sadeh, I., Abbott, T.M.C., Abdalla, F.B., Allam, S., Annis, J., Asorey, J., Brooks, D., Calcino, J., Carollo, D., Castander, F.J., D’Andrea, C.B., Desai, S., Evrard, A.E., Fosalba, P., Frieman, J., García-Bellido, J., Glazebrook, K., Gerdes, D.W., Gruendl, R.A., Gutierrez, G., Hinton, S., Hollowood, D.L., Honscheid, K., Hoormann, J.K., James, D.J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G., Lidman, C., Lin, H., Macaulay, E., Marshall, J., Melchior, P., Miquel, R., Möller, A., Plazas, A.A., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R.H., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Sommer, N.E., Suchyta, E., Swanson, M.E.C., Tarle, G., Tucker, B.E., Tucker, D.L., Uddin, S., and Walker, A.R.
Published: 2018
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4. Crowdsourcing quality control for Dark Energy Survey images

Author: Melchior, P., Sheldon, E., Drlica-Wagner, A., Rykoff, E.S., Abbott, T.M.C., Abdalla, F.B., Allam, S., Benoit-Lévy, A., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Crocce, M., D’Andrea, C.B., da Costa, L.N., Desai, S., Doel, P., Evrard, A.E., Finley, D.A., Flaugher, B., Frieman, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gruendl, R.A., Honscheid, K., James, D.J., Jarvis, M., Kuehn, K., Li, T.S., Maia, M.A.G., March, M., Marshall, J.L., Nord, B., Ogando, R., Plazas, A.A., Romer, A.K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, R.C., Soares-Santos, M., Suchyta, E., Swanson, M.E.C., Tarle, G., Vikram, V., Walker, A.R., Wester, W., and Zhang, Y.
Published: 2016
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5. Skip Nav Destination The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Author: Kelsey, L., Sullivan, M., Smith, M., Wiseman, P., Brout, D., Davis, T.M., Frohmaier, C., Galbany, L., Grayling, M., Gutiérrez, C.P., Hinton, S.R., Kessler, R., Lidman, C., Möller, A., Sako, M., Scolnic, D., Uddin, S.A., Vincenzi, M., Abbott, T.M.C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Brooks, D., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Costanzi, M., Da Costa, L.N., Desai, S., Diehl, H.T., Doel, P., Everett, S., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., García-Bellido, J., Gerdes, D.W., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Hollowood, D.L., Honscheid, K., James, D.J., Kim, A.G., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Marshall, J.L., Martini, P., Menanteau, F., Miquel, R., Morgan, R., Ogando, R.L.C., Palmese, A., Paz-Chinchón, F., Plazas, A.A., Romer, A.K., Sánchez, C., Sanchez, E., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T.N., Walker, A.R., Wilkinson, R.D., Laboratoire de Physique de Clermont (LPC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS)
Subjects: surveys, supernovae: general, cosmology: observations, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract: International audience; Analyses of Type Ia supernovae (SNe Ia) have found puzzling correlations between their standardized luminosities and host galaxy properties: SNe Ia in high-mass, passive hosts appear brighter than those in lower mass, star-forming hosts. We examine the host galaxies of SNe Ia in the Dark Energy Survey 3-yr spectroscopically confirmed cosmological sample, obtaining photometry in a series of ‘local’ apertures centred on the SN, and for the global host galaxy. We study the differences in these host galaxy properties, such as stellar mass and rest-frame U − R colours, and their correlations with SN Ia parameters including Hubble residuals. We find all Hubble residual steps to be >3σ in significance, both for splitting at the traditional environmental property sample median and for the step of maximum significance. For stellar mass, we find a maximal local step of 0.098 ± 0.018 mag; ∼0.03 mag greater than the largest global stellar mass step in our sample (0.070 ± 0.017 mag). When splitting at the sample median, differences between local and global U − R steps are small, both ∼0.08 mag, but are more significant than the global stellar mass step (0.057 ± 0.017 mag). We split the data into sub-samples based on SN Ia light-curve parameters: stretch (x_1) and colour (c), finding that redder objects (c > 0) have larger Hubble residual steps, for both stellar mass and U − R, for both local and global measurements, of ∼0.14 mag. Additionally, the bluer (star-forming) local environments host a more homogeneous SN Ia sample, with local U − R rms scatter as low as 0.084 ± 0.017 mag for blue (c < 0) SNe Ia in locally blue U − R environments.
Published: 2021

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

Author: Nadler, E.O., Wechsler, R.H., Bechtol, K., Mao, Y.-Y., Green, G., Drlica-Wagner, A., McNanna, M., Mau, S., Pace, A.B., Simon, J.D., Kravtsov, A., Dodelson, S., Li, T.S., Riley, A.H., Wang, M.Y., Abbott, T.M.C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G.M., Bertin, E., Brooks, D., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L.N., De Vicente, J., Desai, S., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W.G., Hinton, S.R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M.A.G., Marshall, J.L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A.A., Romer, A.K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T.N., Walker, A.R., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Kavli Institute for Particle Astrophysics and Cosmology, National Aeronautics and Space Administration (US), Department of Energy (US), Ministerio de Ciencia e Innovación (España), Science and Technology Facilities Council (UK), University of Illinois, University of Chicago, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional das Fundaçôes Estaduais de Amparo à Pesquisa (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Generalitat de Catalunya, Nadler, E. O., Wechsler, R. H., Bechtol, K., Mao, Y. -Y., Green, G., Drlica-Wagner, A., Mcnanna, M., Mau, S., Pace, A. B., Simon, J. D., Kravtsov, A., Dodelson, S., T. S., Li, Riley, A. H., Wang, M. Y., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Da Costa, L. N., De Vicente, J., Desai, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Varga, T. N., and Walker, A. R.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Milky Way, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Virial theorem, Galactic halo, Galaxy abundances, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, Milky Way dark matter halo, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, Physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The population of Milky Way (MW) satellites contains the faintest known galaxies and thus provides essential insight into galaxy formation and dark matter microphysics. Here we combine a model of the galaxy-halo connection with newly derived observational selection functions based on searches for satellites in photometric surveys over nearly the entire high Galactic latitude sky. In particular, we use cosmological zoom-in simulations of MW-like halos that include realistic Large Magellanic Cloud (LMC) analogs to fit the position-dependent MW satellite luminosity function. We report decisive evidence for the statistical impact of the LMC on the MW satellite population due to an estimated 6 ± 2 observed LMC-associated satellites, consistent with the number of LMC satellites inferred from Gaia proper-motion measurements, confirming the predictions of cold dark matter models for the existence of satellites within satellite halos. Moreover, we infer that the LMC fell into the MW within the last 2 Gyr at high confidence. Based on our detailed full-sky modeling, we find that the faintest observed satellites inhabit halos with peak virial masses below 3.2× 10 M· at 95% confidence, and we place the first robust constraints on the fraction of halos that host galaxies in this regime. We predict that the faintest detectable satellites occupy halos with peak virial masses above 10 M·, highlighting the potential for powerful galaxy formation and dark matter constraints from future dwarf galaxy searches., This research received support from the National Science Foundation (NSF) under grant No. NSF AST-1517422, grant No. NSF PHY17-48958 through the Kavli Institute for Theoretical Physics program “The Small-Scale Structure of Cold(?) Dark Matter,” and grant No. NSF DGE-1656518 through the NSF Graduate Research Fellowship received by E.O.N. Support for Y.-Y.M. was provided by the Pittsburgh Particle Physics, Astrophysics and Cosmology Center through the Samuel P. Langley PITT PACC Postdoctoral Fellowship and NASA through NASA Hubble Fellowship grant No. HST-HF2-51441.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Part of this work was performed at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1607611. This research made use of computational resources at SLAC National Accelerator Laboratory, a U.S. Department of Energy Office; the authors are thankful for the support of the SLAC computational team. This research made use of the Sherlock cluster at the Stanford Research Computing Center (SRCC); the authors are thankful for the support of the SRCC team. This research made use of https://arXiv.org and NASA’s Astrophysics Data System for bibliographic information. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the NSFʼs National Optical-Infrared Astronomy Laboratory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This work is based in part on observations at Cerro Tololo Inter-American Observatory, NSFʼs National Optical-Infrared Astronomy Laboratory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. The IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/ 2007-2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by the Fermi Research Alliance, LLC, under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2019

7. Dark Energy Survey Year 1 Results: Cross-correlation between Dark Energy Survey Y1 galaxy weak lensing and South Pole Telescope +Planck CMB weak lensing

Author: Omori, Y., Baxter, E.J., Kirk, D., Alarcon, A., Bernstein, G.M., Bleem, L.E., Cawthon, R., Choi, A., Chown, R., Crawford, T.M., Davis, C., De Vicente, J., DeRose, J., Dodelson, S., Eifler, T.F., Fosalba, P., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Gruen, D., Hartley, W.G., Holder, G.P., Hoyle, B., Huterer, D., Jain, B., Jarvis, M., Krause, E., MacCrann, N., Miquel, R., Prat, J., Rau, M.M., Reichardt, C.L., ROZO, E., Samuroff, S., Sánchez, C., Secco, L.F., Sheldon, E., Simard, G., Troxel, M.A., Vielzeuf, P., Wechsler, R.H., Zuntz, J., Abbott, T.M.C., Abdalla, F.B., Allam, S., Annis, J., Avila, S., Aylor, K., Benson, B.A., Bertin, E., Bridle, S.L., Brooks, D., Burke, D.L., Carlstrom, J.E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Chang, C.L., Cho, H-M., Crites, A.T., Crocce, M., Cunha, C.E., Da Costa, L.N., De Haan, T., Desai, S., Diehl, H.T., Dietrich, J.P., Dobbs, M.A., Everett, W.B., Fernandez, E., Flaugher, B., Frieman, J., García-Bellido, J., George, E.M., Gruendl, R.A., Gutierrez, G., Halverson, N.W., Harrington, N.L., Hollowood, D.L., Honscheid, K., Holzapfel, W.L., Hou, Z., Hrubes, J.D., James, D.J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Lee, A.T., Leitch, E.M., Luong-Van, D., Maia, M.A.G., Manzotti, A., Marrone, D.P., Marshall, J.L., Martini, P., McMahon, J.J., Melchior, P., Menanteau, F., Meyer, S.S., Mocanu, L.M., Mohr, J.J., Natoli, T., Ogando, R.L.C., Padin, S., Plazas, A.A., Pryke, C., Romer, A.K., Roodman, A., Ruhl, J.E., Rykoff, E.S., Sanchez, E., Scarpine, V., Schaffer, K.K., Schindler, R., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Smith, R.C., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A.A., Story, K.T., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Vanderlinde, K., Vieira, J.D., Vikram, V., Walker, A.R., Weller, J., Williamson, R., Wu, W.L.K., Zahn, O., 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: Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmology
Abstract: International audience; We cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg2. With the combined measurements from four source galaxy redshift bins, we obtain a detection significance of 5.8σ. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial ΛCDM model, finding A=0.99±0.17. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the ΛCDM model, we obtain the marginalized constraints of Ωm=0.261-0.051+0.070 and S8≡σ8Ωm/0.3=0.660-0.100+0.085. These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT, and Planck data.
Published: 2019

8. Three new VHS–DES quasars at 6.7 < z < 6.9 and emission line properties at z > 6.5

Author: Reed, S.L., Banerji, M., Becker, G.D., Hewett, P.C., Martini, P., Mcmahon, R.G., Pons, E., Rauch, M., Abbott, T.M.C., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Cunha, C.E., D'Andrea, C.B., Da Costa, L.N., De Vicente, J., Desai, S., Diehl, H.T., Doel, P., Evrard, A.E., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gschwend, J., Gutierrez, G., Hollowood, D.L., Honscheid, K., Hoyle, B., James, D.J., Kuehn, K., Lahav, O., Lima, M., Maia, M.A.G., Marshall, J.L., Miquel, R., Ogando, R.L.C., Plazas, A.A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Tucker, D.L., Vikram, V., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: galaxies: high-redshift, quasars: individual: VDES J0224−4711, quasars: individual: VDES J0244−5008, first stars, galaxies: active, quasars: individual: VDES J0020−3653, reionization, galaxies: formation, quasars: individual: VDES J0246−5219, dark ages, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the results from a search for z > 6.5 quasars using the Dark Energy Survey (DES) Year 3 dataset combined with the VISTA Hemisphere Survey (VHS) and WISE All-Sky Survey. Our photometric selection method is shown to be highly efficient in identifying clean samples of high-redshift quasars leading to spectroscopic confirmation of three new quasars - VDESJ 0244-5008 (z=6.724), VDESJ 0020-3653 (z=6.834) and VDESJ 0246-5219 (z=6.90) - which were selected as the highest priority candidates in the survey data without any need for additional follow-up observations. The new quasars span the full range in luminosity covered by other z>6.5 quasar samples (J AB = 20.2 to 21.3; M1450 = -25.6 to -26.6). We have obtained spectroscopic observations in the near infrared for VDESJ 0244-5008 and VDESJ 0020-3653 as well as our previously identified quasar, VDESJ 0224-4711 at z=6.50 from Reed et al. (2017). We use the near infrared spectra to derive virial black-hole masses from the full-width-half-maximum of the MgII line. These black-hole masses are ~ 1 - 2 x 10$^9$M$_\odot$. Combining with the bolometric luminosities of these quasars of L$_{\rm{bol}}\simeq$ 1 - 3 x 10$^{47}$implies that the Eddington ratios are high - $\simeq$0.6-1.1. We consider the C\textrm{\textsc{IV}} emission line properties of the sample and demonstrate that our high-redshift quasars do not have unusual C\textrm{\textsc{IV}} line properties when compared to carefully matched low-redshift samples. Our new DES+VHS $z>6.5$ quasars now add to the growing census of luminous, rapidly accreting supermassive black-holes seen well into the epoch of reionisation., Comment: 12 pages, 9 figures
Published: 2019

9. The Future Landscape of High-Redshift Galaxy Cluster Science

Author: Mantz, A., Allen, S.W., Battaglia, N., Benson, B., Canning, R., Ettori, S., Evrard, A., Linden, A., McDonald, M., Abidi, M., Ahmed, Z., Amin, Mustafa.A., Ansarinejad, B., Armstrong, R., Avestruz, C., Baccigalupi, C., Bandura, K., Barkhouse, W., Basu, K., Bavdhankar, C., Bender, A.N., Bernardis, P., Bischoff, C., Biviano, A., Bleem, L., Bocquet, S., Bond, J., Borgani, S., Borrill, J., Boutigny, D., Frye, B., Bruggen, M., Cai, Z., Carlstrom, J.E., Castander, F.J., Challinor, A., Clowe, D., Cohn, J.D., Comparat, J., Cooray, A., Coulton, W., Cyr-Racine, F., Daddi, E., Delabrouille, J., Dell'antonio, I., Demarteau, M., Donahue, M., Dunkley, J., Escoffier, S., Essinger-Hileman, T., Fabbian, G., Fabjan, D., Farahi, A., Foreman, S., Fraisse, A.A., Garcia, L., Gaspari, M., Gerbino, M., Gitti, M., Gluscevic, V., Gonzalez, A., Górski, K.M., Gruen, D., Gudmundsson, J.E., Gupta, N., Haan, T., Hernquist, L., Hirata, C.M., Hlozek, R., Jeltema, T., Cohen-Tanugi, J., Johnson, B., Kadota, K., Kamionkowski, M., Khatri, R., Kisner, T., Kneib, J., Knox, L., Kovetz, E.D., Krause, E., Lattanzi, M., Lau, Erwin.T., Liguori, M., Lovisari, L., Macorra, A., Masi, S., Masui, K., Maughan, B., Maurogordato, S., McMahon, J., McNamara, B., Melchior, P., Mertens, J., Meyers, J., Mirbabayi, M., More, S., Motloch, P., Moustakas, J., Mroczkowski, T., Mukherjee, S., Nagai, D., Nagy, J., Naselsky, P., Nati, F., Newburgh, L., Niemack, M.D., Nomerotski, A., Noordeh, E., Ntampaka, M., Ota, N., Page, L., Palmese, A., Penna-Lima, M., Piacentni, F., Pierpaoli, E., Plazas, A.A., Pogosian, L., Pointecouteau, E., Prakash, A., Pratt, G., Prescod-Weinstein, C., Pryke, C., Puglisi, G., Rapetti, D., Raveri, M., Reichardt, C.L., Reiprich, Thomas.H., Remazeilles, M., Rhodes, J., Ricci, M., Rocha, G., Rose, B., Rozo, E., Ruhl, J., Sadun, A., Saliwanchik, B., Schaan, E., Schmidt, R., Fromenteau, S., Sehgal, N., Senatore, L., Seo, H., Sereno, M., Shafieloo, A., Shan, H., Shandera, S., Sherwin, B.D., Simon, S., Sridhar, S., Staggs, S., Stern, D., Suzuki, A., Tsai, Y., Turriziani, S., Umilta, C., Vazza, F., Vieregg, A., Vikhlinin, A., Walker, S.A., Watson, S., Weeren, R.J. van, Weller, J., Werner, N., Whitehorn, N., Wong, K., Wright, A., Wu, W.L.K., Xu, Z., Yasini, S., Zemcov, M., Zhang, Y., Zhao, G., Zheng, Y., Zhu, N., Zhuravleva, I., Zuntz, J., Hickox, R., Churazov, E., Nulsen, P., Jones, W.C., Wang, L., and Desai, S.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We describe the opportunities for galaxy cluster science in the high- redshift regime where massive, virialized halos first formed and where star formation and AGN activity peaked. New observing facilities from radio to X-ray wavelengths, combining high spatial/spectral resolution with large collecting areas, are poised to uncover this population.
Published: 2019

10. Dark Energy Survey Year 1 Results: Tomographic cross-correlations between Dark Energy Survey galaxies and CMB lensing from South Pole Telescope+Planck

Author: Omori, Y., Giannantonio, T., Porredon, A., Baxter, E.J., Crocce, M., Fosalba, P., Alarcon, A., Banik, N., Blazek, J., Bleem, L.E., Bridle, S.L., Cawthon, R., Choi, A., Chown, R., Crawford, T., Dodelson, S., Drlica-Wagner, A., Eifler, T.F., Elvin-Poole, J., Friedrich, O., Gruen, D., Holder, G.P., Huterer, D., Jain, B., Jarvis, M., Kirk, D., Kokron, N., Krause, E., MacCrann, N., Muir, J., Prat, J., Reichardt, C.L., Ross, A.J., ROZO, E., Rykoff, E.S., Sánchez, C., Secco, L.F., Simard, G., Wechsler, R.H., Zuntz, J., Abbott, T.M.C., Abdalla, F.B., Allam, S., Avila, S., Aylor, K., Benson, B.A., Bernstein, G.M., Bertin, E., Bianchini, F., Brooks, D., Buckley-Geer, E., Burke, D.L., Carlstrom, J.E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., Chang, C.L., Cho, H-M., Crites, A.T., Cunha, C.E., Da Costa, L.N., De Haan, T., Davis, C., De Vicente, J., Desai, S., Diehl, H.T., Dietrich, J.P., Dobbs, M.A., Everett, W.B., Doel, P., Estrada, J., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., George, E.M., Gruendl, R.A., Gschwend, J., Gutierrez, G., Halverson, N.W., Harrington, N.L., Hartley, W.G., Hollowood, D.L., Holzapfel, W.L., Honscheid, K., Hou, Z., Hoyle, B., Hrubes, J.D., James, D.J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lee, A.T., Leitch, E.M., Lima, M., Luong-Van, D., Manzotti, A., Marrone, D.P., Marshall, J.L., McMahon, J.J., Melchior, P., Menanteau, F., Meyer, S.S., Miller, C.J., Miquel, R., Mocanu, L.M., Mohr, J.J., Natoli, T., Padin, S., Plazas, A.A., Pryke, C., Romer, A.K., Roodman, A., Ruhl, J.E., Sanchez, E., Scarpine, V., Schaffer, K.K., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shirokoff, E., Smith, M., Soares-Santos, M., Sobreira, F., Staniszewski, Z., Stark, A.A., Story, K.T., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Troxel, M.A., Vanderlinde, K., Vieira, J.D., Walker, A.R., Wu, W.L.K., Zahn, O., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, SPT, and UAM. Departamento de Física Teórica
Subjects: Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, 0103 physical sciences, media_common.cataloged_instance, European union, 010306 general physics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), STFC, ComputingMilieux_MISCELLANEOUS, QC, media_common, Physics, 010308 nuclear & particles physics, European research, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Física, GALÁXIAS, Cosmology, South Pole Telescope, 13. Climate action, Research council, Fundamental physics, Christian ministry, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Kavli Foundation; Natural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Canada Research Chairs program; U.S. Department of Energy [DE-SC0007901]; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-1125897]; Australian Research Council Future Fellowship [FT150100074]; Fermi Research Alliance, LLC [De-AC02-07CH11359]; United States Department of Energy; National Science Foundation [OCI-0725070, ACI-1238993]; NSF Physics Frontier Center [PHY-0114422]; Kavli Institute of Cosmological Physics at the University of Chicago; Gordon and Betty Moore Foundation; GBMF [947]; National Aeronautics and Space Administration; U.S. 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; 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; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the Dark Energy Survey; University of California at Santa Cruz; University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Ludwig-Maximilians Universitat Munchen; University of Portsmouth; OzDES Membership Consortium; Association of Universities for Research in Astronomy (AURA); MINECO [AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509]; ERDF; European Union - CERCA program of the Generalitat de Catalunya; European Research Council under the European Union [240672, 291329, 306478]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq) [De-AC02-07CH11359, 465376/2014-2]; U.S. Department of Energy, Office of Science, Office of High Energy Physics - Canada Foundation for Innovation (CFI); ministere de l'Economie, de la science et de l'innovation du Quebec (MESI); Fonds de recherche du Quebec-Nature et technologies (FRQ-NT); state of Illinois; University of Illinois at Urbana-Champaign [49,70, MATPLOTLIB [75], 76,77]
Published: 2019

11. A catalogue of structural and morphological measurements for DES Y1

Author: Tarsitano, F., Hartley, W.G., Amara, A., Bluck, A., Bruderer, C., Carollo, M., Conselice, C, Melchior, P., Moraes, B., Refregier, A., Sevilla-Noarbe, I., Woo, J., Abbott, T.M.C., Allam, S., Annis, J., Avila, S., Banerji, M., Bertin, E., Brooks, D., Burke, D.L., Carretero, J., Cunha, C.E., Davis, C., Desai, S., Doel, P., Estrada, J., Frieman, J., Gruen, D., Gruendl, R.A., Gutierrez, G., Hollowood, D., Honscheid, K., James, D.J., Jeltema, T., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M.A.G., Menanteau, F., Miquel, R., Plazas, A.A., Romer, A.K., Roodman, A., Sanchez, E., Santiago, B., Schindler, R., Smith, M., Smith, R.C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Vikram, V., and Walker, A.R.
Subjects: Galaxy structure, Astronomy and astrophysics, Galaxy evolution, Space and planetary science, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Astrophysics::Galaxy Astrophysics
Abstract: We present a structural and morphological catalogue for 45 million objects selected from the first year data of the Dark Energy Survey (DES). Single Sersic fits and non-parametric measurements are produced for g, r, and i filters. The parameters from the best-fitting Sersic model (total magnitude, half-light radius, S´ersic index, axis ratio, and position angle) are measured with GALFIT; the non-parametric coefficients (concentration, asymmetry, clumpiness, Gini, M20) are provided using the Zurich Estimator of Structural Types (ZEST+). To study the statistical uncertainties, we consider a sample of state-of-the-art image simulations with a realistic distribution in the input parameter space and then process and analyse them as we do with real data: this enables us to quantify the observational biases due to PSF blurring and magnitude effects and correct themeasurements as a function ofmagnitude, galaxy size, Sersic index (concentration for the analysis of the non-parametric measurements) and ellipticity. We present the largest structural catalogue to date: we find that accurate and complete measurements for all the structural parameters are typically obtained for galaxies with SEXTRACTOR MAG AUTO I ≤ 21. Indeed, the parameters in the filters i and r can be overall well recovered up to MAG AUTO ≤ 21.5, corresponding to a fitting completeness of ∼90 per cent below this threshold, for a total of 25million galaxies. The combination of parametric and non-parametric structural measurements makes this catalogue an important instrument to explore and understand how galaxies form and evolve. The catalogue described in this paper will be publicly released alongside the DES collaboration Y1 cosmology data products at the following URL:https://des.ncsa.illinois.edu/releases.
Published: 2018

12. Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters

Author: Farahi, A., Chen, X., Evrard, A.E., Hollowood, D.L., Wilkinson, R., Bhargava, S., Giles, P., Romer, A.K., Jeltema, T., Hilton, M., Bermeo, A., Mayers, J., Vergara Cervantes, C., Rozo, E., Rykoff, E.S., Collins, C., Costanzi, M., Everett, S., Liddle, A.R., Mann, R.G., Mantz, A., Rooney, P., Sahlen, M., Stott, J., Viana, P.T.P., Zhang, Y., Annis, J., Avila, S., Brooks, D., Buckley-Geer, E., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., da Costa, L.N., de Vicente, J., Desai, S., Diehl, H.T., Dietrich, J.P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D.J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M.A.G., Marshall, J.L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R.L.C., Plazas, A.A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Tucker, D.L., Vikram, V., Walker, A.R., Weller, J., Farahi, A., Chen, X., Evrard, A.E., Hollowood, D.L., Wilkinson, R., Bhargava, S., Giles, P., Romer, A.K., Jeltema, T., Hilton, M., Bermeo, A., Mayers, J., Vergara Cervantes, C., Rozo, E., Rykoff, E.S., Collins, C., Costanzi, M., Everett, S., Liddle, A.R., Mann, R.G., Mantz, A., Rooney, P., Sahlen, M., Stott, J., Viana, P.T.P., Zhang, Y., Annis, J., Avila, S., Brooks, D., Buckley-Geer, E., Burke, D.L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F.J., da Costa, L.N., de Vicente, J., Desai, S., Diehl, H.T., Dietrich, J.P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D.J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M.A.G., Marshall, J.L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R.L.C., Plazas, A.A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Tucker, D.L., Vikram, V., Walker, A.R., and Weller, J.
Abstract: Using archival X-ray observations and a lognormal population model, we estimate constraints on the intrinsic scatter in halo mass at fixed optical richness for a galaxy cluster sample identified in Dark Energy Survey Year-One (DES-Y1) data with the redMaPPer algorithm. We examine the scaling behaviour of X-ray temperatures, T-X, with optical richness, lambda(RM), for clusters in the redshift range 0.2 50 per cent complete for clusters with lambda(RM) > 130. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, sigma(ln) (T) (vertical bar) (lambda) = 0.275 +/- 0.019. Joined with constraints for T-X scaling with halo mass from the Weighing the Giants program and richness-temperature covariance estimates from the LoCuSS sample, we derive the richness-conditioned scatter in mass, sigma(ln) (M) (vertical bar) (lambda) = 0.30 +/- 0.04((stat)) +/- 0.09((sys)), at an optical richness of approximately 100. Uncertainties in external parameters, particularly the slope and variance of the T-X-mass relation and the covariance of T-X and lambda(RM) at fixed mass, dominate the systematic error. The 95 per cent confidence region from joint sample analysis is relatively broad, sigma(ln) (M) (vertical bar) (lambda) is an element of [0.14, 0.55], or a factor 10 in variance.
Published: 2019

13. Improving Weak Lensing Mass Map Reconstructions using Gaussian and Sparsity Priors: Application to DES SV

Author: Jeffrey, N., Abdalla, F.B., Lahav, O., Lanusse, F., Starck, J.-L., Leonard, A., Kirk, D., Chang, C., Baxter, E., Kacprzak, T., Seitz, S., Vikram, V., Whiteway, L., Abbott, T.M.C., Allam, S., Avila, S., Bertin, E., Brooks, 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., Davis, C., De Vicente, J., Desai, S., Doel, P., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D.W., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Hartley, W.G., Honscheid, K., Hoyle, B., James, D.J., Jarvis, M., Kuehn, K., Lima, M., Lin, H., March, M., Melchior, P., Menanteau, F., Miquel, R., Plazas, A.A., Reil, K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Walker, A.R., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: methods: statistical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational lensing: weak, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Mapping the underlying density field, including non-visible dark matter, using weak gravitational lensing measurements is now a standard tool in cosmology. Due to its importance to the science results of current and upcoming surveys, the quality of the convergence reconstruction methods should be well understood. We compare three methods: Kaiser-Squires (KS), Wiener filter, and GLIMPSE. KS is a direct inversion, not accounting for survey masks or noise. The Wiener filter is well-motivated for Gaussian density fields in a Bayesian framework. GLIMPSE uses sparsity, aiming to reconstruct non-linearities in the density field. We compare these methods with several tests using public Dark Energy Survey (DES) Science Verification (SV) data and realistic DES simulations. The Wiener filter and GLIMPSE offer substantial improvements over smoothed KS with a range of metrics. Both the Wiener filter and GLIMPSE convergence reconstructions show a 12 per cent improvement in Pearson correlation with the underlying truth from simulations. To compare the mapping methods' abilities to find mass peaks, we measure the difference between peak counts from simulated {\Lambda}CDM shear catalogues and catalogues with no mass fluctuations (a standard data vector when inferring cosmology from peak statistics); the maximum signal-to-noise of these peak statistics is increased by a factor of 3.5 for the Wiener filter and 9 for GLIMPSE. With simulations we measure the reconstruction of the harmonic phases; the phase residuals' concentration is improved 17 per cent by GLIMPSE and 18 per cent by the Wiener filter. The correlation between reconstructions from data and foreground redMaPPer clusters is increased 18 per cent by the Wiener filter and 32 per cent by GLIMPSE., Comment: 19 pages, 10 figures, MNRAS published: 15 May 2018
Published: 2018

14. The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles

Author: Chang, Chihway, Baxter, E., Jain, B., Sánchez, C., Adhikari, S., Varga, T.N., Fang, Y., Rozo, Eduardo, Rykoff, E.S., Kravtsov, Andrey, Gruen, D., Hartley, W., Huff, E.M., Jarvis, M., Kim, A.G., Prat, J., MacCrann, N., McClintock, T., Palmese, A., Rapetti, D., Rollins, R.P., Samuroff, S., Sheldon, E., Troxel, M.A., Wechsler, R.H., Zhang, Y., Zuntz, J., Abbott, T.M.C., Abdalla, F.B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bernstein, G.M., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., D'Andrea, C.B., Da Costa, L.N., Davis, C., Desai, S., Diehl, H.T., Dietrich, J.P., Drlica-Wagner, A., Eifler, T.F., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D.J., Jeltema, T., Krause, E., Kuehn, K., Lahav, O., Lima, M., March, M., Marshall, J.L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J.J., Nord, B., Ogando, R.L.C., Plazas, A.A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Weller, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: halos, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Physical Chemistry, Atomic, 01 natural sciences, Particle and Plasma Physics, gravitational lensing: weak, 0103 physical sciences, Cluster (physics), Nuclear, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Molecular, Astronomy and Astrophysics, Redshift, Galaxy, Dark matter halo, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, Dark energy, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The cluster-centric radius at which this process occurs, r_sp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near r_sp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first year Dark Energy Survey (DES) data. For a cluster sample with mean M_200m mass ~2.5 x 10^14 M_sun, we find strong evidence of a splashback-like steepening of the galaxy density profile and measure r_sp=1.13 +/- 0.07 Mpc/h, consistent with earlier SDSS measurements of More et al. (2016) and Baxter et al. (2017). Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure r_sp=1.34 +/- 0.21 Mpc/h from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that consistent with LCDM simulations, r_sp scales with R_200m and does not evolve with redshift over the redshift range of 0.3--0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of r_sp. We discuss progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples., Comment: 25 pages, 15 figures; update to journal accepted version
Published: 2018

15. Evidence for color dichotomy in the primordial Neptunian Trojan population

Author: Lin (林省文), Hsing Wen, primary, W. Gerdes, David, additional, J. Hamilton, Stephanie, additional, C. Adams, Fred, additional, M. Bernstein, Gary, additional, Sako, Masao, additional, Bernadinelli, Pedro, additional, Tucker, Douglas, additional, Allam, Sahar, additional, C. Becker, Juliette, additional, Khain, Tali, additional, Markwardt, Larissa, additional, Franson, Kyle, additional, Abbott, T.M.C., additional, Annis, J., additional, Avila, S., additional, Brooks, D., additional, Carnero Rosell, A., additional, Carrasco Kind, M., additional, Cunha, C.E., additional, D’Andrea, C.B., additional, da Costa, L.N., additional, De Vicente, J., additional, Doel, P., additional, Eifler, T.F., additional, Flaugher, B., additional, García-Bellido, J., additional, Hollowood, D.L., additional, Honscheid, Klaus, additional, James, D.J., additional, Kuehn, K., additional, Kuropatkin, N., additional, Maia, M.A.G., additional, Marshall, J.L., additional, Miquel, R., additional, Plazas, A.A., additional, Romer, A.K., additional, Sanchez, E., additional, Scarpine, V., additional, Sevilla-Noarbe, I., additional, Smith, M., additional, Smith, R.C., additional, Soares-Santos, M., additional, Sobreira, F., additional, Suchyta, E., additional, Tarle, G., additional, Walker, A.R., additional, and Wester, W., additional
Published: 2019
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16. Evidence for Dynamically Driven Formation of the GW170817 Neutron Star Binary in NGC 4993

Author: Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., and Zuntz, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, galaxies: structure – gravitational waves, galaxies: individual (NGC 4993), Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: We present a study of NGC 4993, the host galaxy of the GW170817 gravitational-wave event, the GRB 170817A short gamma-ray burst (sGRB), and the AT 2017gfo kilonova. We use Dark Energy Camera imaging, AAT spectra, and publicly available data, relating our findings to binary neutron star (BNS) formation scenarios and merger delay timescales. NGC 4993 is a nearby early-type galaxy, with an i-band Sérsic index n = 4.0 and low asymmetry (A = 0.04 ± 0.01). These properties are unusual for sGRB hosts. However, NGC 4993 presents shell-like structures and dust lanes indicative of a recent galaxy merger, with the optical transient located close to a shell. We constrain the star formation history (SFH) of the galaxy assuming that the galaxy merger produced a star formation burst, but find little to no ongoing star formation in either spatially resolved broadband SED or spectral fitting. We use the best-fit SFH to estimate the BNS merger rate in this type of galaxy, as ${R}_{\mathrm{NSM}}^{\mathrm{gal}}={5.7}_{-3.3}^{+0.57}\times {10}^{-6}{\mathrm{yr}}^{-1}$. If star formation is the only considered BNS formation scenario, the expected number of BNS mergers from early-type galaxies detectable with LIGO during its first two observing seasons is ${0.038}_{-0.022}^{+0.004}$, as opposed to ~0.5 from all galaxy types. Hypothesizing that the binary formed due to dynamical interactions during the galaxy merger, the subsequent time elapsed can constrain the delay time of the BNS coalescence. By using velocity dispersion estimates and the position of the shells, we find that the galaxy merger occurred t mer lesssim 200 Myr prior to the BNS coalescence.
Published: 2017

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

Author: Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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., Alexander, K.D., Balbinot, E., Blanchard, P., Brown, D.A., Carlin, J.L., Conselice, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., Finley, D.A., Foley, R.J., Fong, W., Fryer, C.L., Gill, M.S.S., Gruendl, R.A., Hanna, C., Kasen, D., Li, T.S., Lopes, P.A.A., Margutti, R., Marshall, J.L., Matheson, T., Medina, G.E., Metzger, B.D., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D.J., Secco, L.F., Sobreira, F., Stebbins, A., Villar, V.A., Vivas, K., Walker, A.R., Wester, W., Williams, P.K.G., Zenteno, A., Zhang, Y., Abbott, T.M.C., Abdalla, F.B., Banerji, M., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D.L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., Costa, L.N. da, 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: binaries: close— catalogs— gravitational waves — stars: neutron— surveys
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 deg2 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 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -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 NGC4993 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 NGC4993 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.
Published: 2017

18. The DES bright arcs survey: hundreds of candidate strongly lensed galaxy systems from the Dark Energy Survey Science Verification and Year 1 observations

Author: Diehl, H.T., Buckley-Geer, E.J., Lindgren, K.A., Nord, B., Gaitsch, H., Gaitsch, S., Lin, H., Allam, S., Collett, T.E., Furlanetto, C., Gill, M.S.S., More, A., Nightingale, J., Odden, C., Pellico, A., Tucker, D.L., Costa, L.N. da, Neto, A.Fausti, Kuropatkin, N., Soares-Santos, M., Welch, B., Zhang, Y., Frieman, J.A., Abdalla, F.B., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Rosell, A.Carnero, Kind, M.Carrasco, Carretero, J., Cunha, C.E., Desai, S., Dietrich, J.P., Drlica-Wagner, A., Evrard, A.E., Finley, D.A., Flaugher, B., Gerdes, D.W., Goldstein, D.A., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., James, D.J., Kuehn, K., Kuhlmann, S., Lahav, O., Li, T.S., Lima, M., Maia, M.A.G., Marshall, J.L., Menanteau, F., Miquel, R., Nichol, R.C., Nugent, P., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sako, M., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., and Walker, A.R.
Subjects: galaxies: high-redshift – gravitational lensing: strong
Abstract: We report the results of searches for strong gravitational lens systems in the Dark Energy Survey (DES) Science Verification and Year 1 observations. The Science Verification data span approximately 250 sq. deg. with a median i-band limiting magnitude for extended objects (10?) of 23.0. The Year 1 data span approximately 2000 sq. deg. and have anti-band limiting magnitude for extended objects (10?) of 22.9. As these data sets are both wide and deep, they are particularly useful for identifying strong gravitational lens candidates. Potential strong gravitational lens candidate systems were initially identified based on a color and magnitude selection in the DES object catalogs or because the system is at the location of a previously identified galaxy cluster. Cutout images of potential candidates were then visually scanned using an object viewer and numerically ranked according to whether or not we judged them to be likely strong gravitational lens systems. Having scanned nearly 400,000 cutouts, we present 374 candidate strong lens systems, of which 348 are identified for the first time. We provide the R.A. and decl., the magnitudes and photometric properties of the lens and source objects, and the distance (radius) of the source(s) from the lens center for each system.
Published: 2017

19. Nonlinearity and pixel shifting effects in HXRG infrared detectors

Author: Plazas, A.A., primary, Shapiro, C., additional, Smith, R., additional, Rhodes, J., additional, and Huff, E., additional
Published: 2017
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20. Spurious shear induced by the tree rings of the LSST CCDs

Author: Okura, Y., primary, Plazas, A.A., additional, May, M., additional, and Tamagawa, T., additional
Published: 2015
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21. Characterization and correction of charge-induced pixel shifts in DECam

Author: Gruen, D., primary, Bernstein, G.M., additional, Jarvis, M., additional, Rowe, B., additional, Vikram, V., additional, Plazas, A.A., additional, and Seitz, S., additional
Published: 2015
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22. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

Author: Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., Zuntz, J., Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., and Zuntz, J.
Abstract: We present a study of NGC 4993, the host galaxy of the GW170817 gravitational-wave event, the GRB 170817A short gamma-ray burst (sGRB), and the AT 2017gfo kilonova. We use Dark Energy Camera imaging, AAT spectra, and publicly available data, relating our findings to binary neutron star (BNS) formation scenarios and merger delay timescales. NGC 4993 is a nearby early-type galaxy, with an i-band Sérsic index n = 4.0 and low asymmetry (A = 0.04 ± 0.01). These properties are unusual for sGRB hosts. However, NGC 4993 presents shell-like structures and dust lanes indicative of a recent galaxy merger, with the optical transient located close to a shell. We constrain the star formation history (SFH) of the galaxy assuming that the galaxy merger produced a star formation burst, but find little to no ongoing star formation in either spatially resolved broadband SED or spectral fitting. We use the best-fit SFH to estimate the BNS merger rate in this type of galaxy, as ${R}_{\mathrm{NSM}}^{\mathrm{gal}}={5.7}_{-3.3}^{+0.57}\times {10}^{-6}{\mathrm{yr}}^{-1}$. If star formation is the only considered BNS formation scenario, the expected number of BNS mergers from early-type galaxies detectable with LIGO during its first two observing seasons is ${0.038}_{-0.022}^{+0.004}$, as opposed to ~0.5 from all galaxy types. Hypothesizing that the binary formed due to dynamical interactions during the galaxy merger, the subsequent time elapsed can constrain the delay time of the BNS coalescence. By using velocity dispersion estimates and the position of the shells, we find that the galaxy merger occurred t mer lesssim 200 Myr prior to the BNS coalescence.
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23. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

Author: Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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., Weller, J., Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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.
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 deg2 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 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -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 NGC4993 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 NGC4993 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.
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24. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

Author: Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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., Weller, J., Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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.
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 deg2 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 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -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 NGC4993 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 NGC4993 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.
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25. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

Author: Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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., Weller, J., Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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.
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 deg2 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 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -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 NGC4993 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 NGC4993 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.
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26. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

Author: Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., Zuntz, J., Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., and Zuntz, J.
Abstract: We present a study of NGC 4993, the host galaxy of the GW170817 gravitational-wave event, the GRB 170817A short gamma-ray burst (sGRB), and the AT 2017gfo kilonova. We use Dark Energy Camera imaging, AAT spectra, and publicly available data, relating our findings to binary neutron star (BNS) formation scenarios and merger delay timescales. NGC 4993 is a nearby early-type galaxy, with an i-band Sérsic index n = 4.0 and low asymmetry (A = 0.04 ± 0.01). These properties are unusual for sGRB hosts. However, NGC 4993 presents shell-like structures and dust lanes indicative of a recent galaxy merger, with the optical transient located close to a shell. We constrain the star formation history (SFH) of the galaxy assuming that the galaxy merger produced a star formation burst, but find little to no ongoing star formation in either spatially resolved broadband SED or spectral fitting. We use the best-fit SFH to estimate the BNS merger rate in this type of galaxy, as ${R}_{\mathrm{NSM}}^{\mathrm{gal}}={5.7}_{-3.3}^{+0.57}\times {10}^{-6}{\mathrm{yr}}^{-1}$. If star formation is the only considered BNS formation scenario, the expected number of BNS mergers from early-type galaxies detectable with LIGO during its first two observing seasons is ${0.038}_{-0.022}^{+0.004}$, as opposed to ~0.5 from all galaxy types. Hypothesizing that the binary formed due to dynamical interactions during the galaxy merger, the subsequent time elapsed can constrain the delay time of the BNS coalescence. By using velocity dispersion estimates and the position of the shells, we find that the galaxy merger occurred t mer lesssim 200 Myr prior to the BNS coalescence.
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27. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

Author: Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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., Weller, J., Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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.
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 deg2 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 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -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 NGC4993 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 NGC4993 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.
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28. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

Author: Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., Zuntz, J., Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., and Zuntz, J.
Abstract: We present a study of NGC 4993, the host galaxy of the GW170817 gravitational-wave event, the GRB 170817A short gamma-ray burst (sGRB), and the AT 2017gfo kilonova. We use Dark Energy Camera imaging, AAT spectra, and publicly available data, relating our findings to binary neutron star (BNS) formation scenarios and merger delay timescales. NGC 4993 is a nearby early-type galaxy, with an i-band Sérsic index n = 4.0 and low asymmetry (A = 0.04 ± 0.01). These properties are unusual for sGRB hosts. However, NGC 4993 presents shell-like structures and dust lanes indicative of a recent galaxy merger, with the optical transient located close to a shell. We constrain the star formation history (SFH) of the galaxy assuming that the galaxy merger produced a star formation burst, but find little to no ongoing star formation in either spatially resolved broadband SED or spectral fitting. We use the best-fit SFH to estimate the BNS merger rate in this type of galaxy, as ${R}_{\mathrm{NSM}}^{\mathrm{gal}}={5.7}_{-3.3}^{+0.57}\times {10}^{-6}{\mathrm{yr}}^{-1}$. If star formation is the only considered BNS formation scenario, the expected number of BNS mergers from early-type galaxies detectable with LIGO during its first two observing seasons is ${0.038}_{-0.022}^{+0.004}$, as opposed to ~0.5 from all galaxy types. Hypothesizing that the binary formed due to dynamical interactions during the galaxy merger, the subsequent time elapsed can constrain the delay time of the BNS coalescence. By using velocity dispersion estimates and the position of the shells, we find that the galaxy merger occurred t mer lesssim 200 Myr prior to the BNS coalescence.
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29. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

Author: Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., Zuntz, J., Palmese, A., Hartley, W., Tarsitano, F., Conselice, Christopher J., Lahav, O., Allam, S., Annis, J., Lin, H., Soares-Santos, M., Tucker, D., Brout, D., Banerji, M., Bechtol, K., Diehl, H.T., Fruchter, A., García-Bellido, J., Herner, K., Levan, A.J., Li, T.S., Lidman, C., Misra, K., Sako, M., Scolnic, D., Smith, M., Abbott, T.M.C., Abdalla, F.B., Benoit-Lévy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Cunha, C.E., D’Andrea, C.B., da Costa, L.N., Davis, C., DePoy, D.L., Desai, S., Dietrich, J.P., Doel, P., Drlica-Wagner, A., Eifler, T.F., Evrard, A.E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lima, M., Maia, M.A.G., March, M., Marshall, J.L., McMahon, R.G., Menanteau, F., Miller, C.J., Miquel, R., Neilsen, E., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sanchez, E., Schindler, R., Smith, R.C., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Walker, A.R., Weller, J., Zhang, Y., and Zuntz, J.
Abstract: We present a study of NGC 4993, the host galaxy of the GW170817 gravitational-wave event, the GRB 170817A short gamma-ray burst (sGRB), and the AT 2017gfo kilonova. We use Dark Energy Camera imaging, AAT spectra, and publicly available data, relating our findings to binary neutron star (BNS) formation scenarios and merger delay timescales. NGC 4993 is a nearby early-type galaxy, with an i-band Sérsic index n = 4.0 and low asymmetry (A = 0.04 ± 0.01). These properties are unusual for sGRB hosts. However, NGC 4993 presents shell-like structures and dust lanes indicative of a recent galaxy merger, with the optical transient located close to a shell. We constrain the star formation history (SFH) of the galaxy assuming that the galaxy merger produced a star formation burst, but find little to no ongoing star formation in either spatially resolved broadband SED or spectral fitting. We use the best-fit SFH to estimate the BNS merger rate in this type of galaxy, as ${R}_{\mathrm{NSM}}^{\mathrm{gal}}={5.7}_{-3.3}^{+0.57}\times {10}^{-6}{\mathrm{yr}}^{-1}$. If star formation is the only considered BNS formation scenario, the expected number of BNS mergers from early-type galaxies detectable with LIGO during its first two observing seasons is ${0.038}_{-0.022}^{+0.004}$, as opposed to ~0.5 from all galaxy types. Hypothesizing that the binary formed due to dynamical interactions during the galaxy merger, the subsequent time elapsed can constrain the delay time of the BNS coalescence. By using velocity dispersion estimates and the position of the shells, we find that the galaxy merger occurred t mer lesssim 200 Myr prior to the BNS coalescence.
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30. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

Author: Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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., Weller, J., Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., 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, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., 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., Vivas, K., 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., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., D’Andrea, C.B., Costa, L.N. da, Davis, C., Desai, S., 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.
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 deg2 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 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -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 NGC4993 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 NGC4993 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.
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30 results on '"Plazas, A.A."'

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

2. Reprint of "Evidence for color dichotomy in the primordial Neptunian Trojan population"

3. DES science portal: Computing photometric redshifts

4. Crowdsourcing quality control for Dark Energy Survey images

5. Skip Nav Destination The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

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

7. Dark Energy Survey Year 1 Results: Cross-correlation between Dark Energy Survey Y1 galaxy weak lensing and South Pole Telescope +Planck CMB weak lensing

8. Three new VHS–DES quasars at 6.7 < z < 6.9 and emission line properties at z > 6.5

9. The Future Landscape of High-Redshift Galaxy Cluster Science

10. Dark Energy Survey Year 1 Results: Tomographic cross-correlations between Dark Energy Survey galaxies and CMB lensing from South Pole Telescope+Planck

11. A catalogue of structural and morphological measurements for DES Y1

12. Mass variance from archival X-ray properties of Dark Energy Survey Year-1 galaxy clusters

13. Improving Weak Lensing Mass Map Reconstructions using Gaussian and Sparsity Priors: Application to DES SV

14. The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles

15. Evidence for color dichotomy in the primordial Neptunian Trojan population

16. Evidence for Dynamically Driven Formation of the GW170817 Neutron Star Binary in NGC 4993

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

18. The DES bright arcs survey: hundreds of candidate strongly lensed galaxy systems from the Dark Energy Survey Science Verification and Year 1 observations

19. Nonlinearity and pixel shifting effects in HXRG infrared detectors

20. Spurious shear induced by the tree rings of the LSST CCDs

21. Characterization and correction of charge-induced pixel shifts in DECam

22. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

23. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

24. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

25. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

26. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

27. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

28. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

29. Evidence for dynamically driven formation of the GW170817 neutron star binary in NGC 4993

30. The electromagnetic counterpart of the binary neutron star merger LIGO/Virgo GW170817. I. Discovery of the optical counterpart using the Dark Energy Camera

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