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1. Reprint of 'Evidence for color dichotomy in the primordial Neptunian Trojan population'

Author

Peter Doel, V. Scarpine, Kyle Franson, Larissa Markwardt, Pedro Bernadinelli, Carlos E. Cunha, Tim Eifler, E. Suchyta, Douglas L. Tucker, Tali Khain, I. Sevilla-Noarbe, Kyler Kuehn, Salcedo Romero de Ávila, J. Annis, L. N. da Costa, Fred C. Adams, Alistair R. Walker, Marcelle Soares-Santos, T. M. C. Abbott, David J. Brooks, K. Honscheid, E. J. Sanchez, Jennifer L. Marshall, W. C. Wester, B. Flaugher, Juan Garcia-Bellido, Juliette C. Becker, D. L. Hollowood, A. A. Plazas, Ramon Miquel, S. Allam, R. C. Smith, M. A. G. Maia, C. B. D'Andrea, S. Hamilton, M. Carrasco Kind, Masao Sako, G. Tarle, A. Carnero Rosell, Flavia Sobreira, David J. James, J. De Vicente, Hsing Wen Lin, Gary Bernstein, M. Smith, A. K. Romer, D. W. Gerdes, and N. P. Kuropatkin

Subjects
Physics, Solar System, education.field_of_study, Planetesimal, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Population, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Jovian, Space and Planetary Science, Trojan, Planet, 0103 physical sciences, Trans-Neptunian object, Eccentricity (behavior), education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, media_common
Abstract

In the current model of early Solar System evolution, the stable members of the Jovian and Neptunian Trojan populations were captured into resonance from the leftover reservoir of planetesimals during the outward migration of the giant planets. As a result, both Jovian and Neptunian Trojans share a common origin with the primordial disk population, whose other surviving members constitute today’s trans-Neptunian object (TNO) populations. The cold (low inclination and small eccentricity) classical TNOs are ultra-red, while the dynamically excited “hot” (high inclination and larger eccentricity) population of TNOs contains a mixture of ultra-red and blue objects. In contrast, Jovian and Neptunian Trojans are observed to be blue. While the absence of ultra-red Jovian Trojans can be readily explained by the sublimation of volatile material from their surfaces due to the high flux of solar radiation at 5 AU, the lack of ultra-red Neptunian Trojans presents both a puzzle and a challenge to formation models. In this work we report the discovery by the Dark Energy Survey (DES) of two new dynamically stable L4 Neptunian Trojans, 2013 VX30 and 2014 UU240, both with inclinations i > 30°, making them the highest-inclination known stable Neptunian Trojans. We have measured the colors of these and three other dynamically stable Neptunian Trojans previously observed by DES, and find that 2013 VX30 is ultra-red, the first such Neptunian Trojan in its class. As such, 2013 VX30 may be a “missing link” between the Trojan and TNO populations. Using a simulation of the DES TNO detection efficiency, we find that there are 162 ± 73 Trojans with Hr

Published
2019

2. Erratum: Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 13 quadruply+ imaged quasars

Author

Santiago Avila, Carlos E. Cunha, Anupreeta More, Issha Kayo, David J. Brooks, S. Desai, Philip J. Marshall, Peter Doel, Simon Birrer, Josh Frieman, E. Suchyta, Kyler Kuehn, M. Smith, Ofer Lahav, Daniel Gruen, F. Ostrovski, G. Tarle, Matthew W. Auger, Sherry H. Suyu, E. Bertin, Juan Garcia-Bellido, T. M. C. Abbott, Veronica Motta, M. Carrasco Kind, Cristian E. Rusu, D. W. Gerdes, Christopher D. Fassnacht, J. Carretero, James H. H. Chan, E. J. Sanchez, Adriano Agnello, B. Flaugher, I. Sevilla-Noarbe, Richard G. McMahon, Flavia Sobreira, A. Carnero Rosell, Anowar J. Shajib, B. Hoyle, Marcos Lima, Jennifer L. Marshall, D. L. Hollowood, Peter Melchior, N. Kuropatkin, Frederic Courbin, G. Gutierrez, G. Meylan, M. March, M. E. C. Swanson, A. R. Walker, E. Buckley-Geer, David J. James, Tom Shanks, Timo Anguita, L. N. da Costa, Felipe Menanteau, M. A. G. Maia, J. De Vicente, Pablo Fosalba, Ramon Miquel, Tommaso Treu, Paul L. Schechter, Thomas E. Collett, J. Annis, N. D. Morgan, Marcelle Soares-Santos, S. Allam, Robert A. Gruendl, Huan Lin, C. Lemon, W. G. Hartley, Masamune Oguri, A. A. Plazas, and V. Scarpine

Subjects
Physics, QUASARES, Space and Planetary Science, Lens (geology), Astronomy, Astronomy and Astrophysics, Quasar, Sample (graphics)
Abstract

The paper ‘Is every strong lens model unhappy in its own way? Uniform modelling of a sample of 13 quadruply+ imaged quasars’ was published in MNRAS, 483, 4, 5649–5671 (2019). The coordinate values of the image positions in table 4 were wrongly printed due to a clerical error. At a later stage of writing the manuscript, we have changed the zero-point definition of the lens coordinate systems, but the relative image positions were not accounted for this change of definition while printing out table 4. We provide the updated Table 4 below. This error does not impact any other results of the paper in any way, except for the table itself. We thank Collin Werner and Paul Schechter for helping us identify this error.

Published
2021

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

Author

F. J. Castander, Geraint F. Lewis, W. G. Hartley, Alex Drlica-Wagner, T. M. C. Abbott, C. B. D'Andrea, Tesla E. Jeltema, Dragan Huterer, E. J. Sanchez, D. A. Finley, M. Carrasco Kind, Tenglin Li, Santiago Avila, Carlos E. Cunha, Robert C. Nichol, N. E. Sommer, Vinu Vikram, J. Carretero, Santiago González-Gaitán, R. H. Schindler, K. Bechtol, Tamara M. Davis, E. Swann, D. L. Burke, A. Carnero Rosell, Samuel Hinton, Ben Hoyle, J. Annis, Edward Macaulay, David Brooks, M. E. C. Swanson, Peter Nugent, Martin Crocce, G. Gutierrez, Daniel Thomas, Mark Sullivan, Joshua A. Frieman, P. Wiseman, E. Suchyta, August E. Evrard, Antonella Palmese, Ryan J. Foley, N. Kuropatkin, Daniel Scolnic, A. G. Kim, V. Scarpine, S. Allam, Robert A. Gruendl, E. Kasai, R. C. Thomas, M. A. G. Maia, Mathew Smith, C. Lidman, Peter de Nully Brown, Alistair R. Walker, Lluís Galbany, D. Brout, Jacobo Asorey, S. Serrano, Marcelle Soares-Santos, Jennifer L. Marshall, Enrique Gaztanaga, L. N. da Costa, Rob Sharp, M. Sako, Brad E. Tucker, J. Calcino, David J. James, Daniela Carollo, Bruce A. Bassett, D. L. Hollowood, Anais Möller, A. A. Plazas, Pablo Fosalba, Bonnie Zhang, Richard Kessler, Bhuvnesh Jain, J. De Vicente, K. Honscheid, S. A. Uddin, Karl Glazebrook, Marcos Lima, Flavia Sobreira, M. S. Schubnell, Ofer Lahav, I. Sevilla-Noarbe, J. Lasker, Juan Garcia-Bellido, A. Roodman, Juan Estrada, B. Flaugher, H. T. Diehl, C. Davis, Kyler Kuehn, Daniel Gruen, David Bacon, Alexei V. Filippenko, J. Gschwend, Gregory Tarle, P. Martini, Tim Eifler, Elisabeth Krause, Ramon Miquel, P. Doel, Thomas E. Collett, Huan Lin, J. K. Hoormann, A. K. Romer, and Yen-Chen Pan

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cepheid variable, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, STFC, media_common, Physics, 010308 nuclear & particles physics, Cosmic distance ladder, RCUK, SATÉLITES ARTIFICIAIS, Astronomy and Astrophysics, Universe, Redshift, Space and Planetary Science, astro-ph.CO, Dark energy, symbols, ST/N000668/1, Baryon acoustic oscillations, Astrophysics - Cosmology and Nongalactic Astrophysics, Hubble's law
Abstract

We present an improved measurement of the Hubble constant (H_0) using the 'inverse distance ladder' method, which adds the information from 207 Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) at redshift 0.018 < z < 0.85 to existing distance measurements of 122 low redshift (z < 0.07) SNe Ia (Low-z) and measurements of Baryon Acoustic Oscillations (BAOs). Whereas traditional measurements of H_0 with SNe Ia use a distance ladder of parallax and Cepheid variable stars, the inverse distance ladder relies on absolute distance measurements from the BAOs to calibrate the intrinsic magnitude of the SNe Ia. We find H_0 = 67.8 +/- 1.3 km s-1 Mpc-1 (statistical and systematic uncertainties, 68% confidence). Our measurement makes minimal assumptions about the underlying cosmological model, and our analysis was blinded to reduce confirmation bias. We examine possible systematic uncertainties and all are below the statistical uncertainties. Our H_0 value is consistent with estimates derived from the Cosmic Microwave Background assuming a LCDM universe (Planck Collaboration et al. 2018)., 15 pages, 5 figures, updated to match accepted version

Published
2019

4. Discovery of a Candidate Binary Supermassive Black Hole in a Periodic Quasar from Circumbinary Accretion Variability

Author

David J. James, Yu Ching Chen, Pablo Fosalba, David J. Brooks, Keith Bechtol, G. Gutierrez, Karl Glazebrook, Tim Eifler, V. Scarpine, Santiago Serrano, Flavia Sobreira, H. Thomas Diehl, Josh Frieman, Santiago Avila, Xin Liu, Carlos E. Cunha, Juan de Vicente, Shantanu Desai, Peter Doel, Jennifer L. Marshall, Juan Garcia-Bellido, Felipe Menanteau, Aurelio Carnero Rosell, Daniel Gruen, Emmanuel Bertin, Enrique Gaztanaga, Gregory Tarle, Richard Kessler, Mathew Smith, Ramon Miquel, B. Flaugher, J. Carretero, Matias Carrasco Kind, Devon L. Hollowood, Tamara M. Davis, K. Honscheid, Vinu Vikram, Marcos Lima, Richard G. McMahon, Hengxiao Guo, E. J. Sanchez, Molly E. C. Swanson, E. Suchyta, J. Gschwend, Elisabeth Krause, August E. Evrard, Yue Shen, Francisco J. Castander, Manda Banerji, Luiz N. da Costa, Paul Martini, Marcio A. G. Maia, R. Chris Smith, Christopher R. Davis, A. Miguel Holgado, Will Hartley, Eric Morganson, Ben Hoyle, S. Allam, Robert A. Gruendl, Andres Plazas Malagon, Kyler Kuehn, Chris B. D'Andrea, Alistair R. Walker, Marcelle Soares-Santos, Michael Schubnell, Wei-Ting Liao, E. Buckley-Geer, James Annis, A. Roodman, UAM. Departamento de Física Teórica, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Australian Research Council, and Instituto Nacional de Ciência e Tecnologia (Brasil)

Subjects
Astrophysics, Surveys, 7. Clean energy, 01 natural sciences, high-redshift [Galaxies], Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Data Release, Galaxies: Active, Dark Energy, nuclei [Galaxies], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Galaxy Mergers, Digital Sky Survey, Galaxies: Nuclei, Oscillations, active [Galaxies], QUASARES, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational-Waves, 0103 physical sciences, Galaxy formation and evolution, Quasars: General, Astrophysics::Galaxy Astrophysics, Supermassive black hole, 010308 nuclear & particles physics, Gravitational wave, Spectral Energy-Distributions, Física, Astronomy and Astrophysics, Quasar, general [Quasars], Black hole physics, Mass, Light curve, Galaxies: High-Redshift, Astrophysics - Astrophysics of Galaxies, Redshift, Black Hole Physics, 13. Climate action, Space and Planetary Science, Variable Quasars, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Galactic Nuclei, Circumbinary planet, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Binary supermassive black holes (BSBHs) are expected to be a generic byproduct from hierarchical galaxy formation. The final coalescence of BSBHs is thought to be the loudest gravitational wave (GW) siren, yet no confirmed BSBH is known in the GW-dominated regime. While periodic quasars have been proposed as BSBH candidates, the physical origin of the periodicity has been largely uncertain. Here, we report discovery of a periodicity (p = 1607 ± 7 d) at 99.95 per cent significance (with a global p value of ∼10-3 accounting for the look elsewhere effect) in the optical light curves of a redshift 1.53 quasar, SDSS J025214.67-002813.7. Combining archival Sloan Digital Sky Survey data with new, sensitive imaging from the Dark Energy Survey, the total ∼20-yr time baseline spans ∼4.6 cycles of the observed 4.4-yr (rest frame 1.7-yr) periodicity. The light curves are best fit by a bursty model predicted by hydrodynamic simulations of circumbinary accretion discs. The periodicity is likely caused by accretion rate modulation by a milli-parsec BSBH emitting GWs, dynamically coupled to the circumbinary accretion disc. A bursty hydrodynamic variability model is statistically preferred over a smooth, sinusoidal model expected from relativistic Doppler boost, a kinematic effect proposed for PG1302-102. Furthermore, the frequency dependence of the variability amplitudes disfavours Doppler boost, lending independent support to the circumbinary accretion variability hypothesis. Given our detection rate of one BSBH candidate from circumbinary accretion variability out of 625 quasars, it suggests that future large, sensitive synoptic surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time may be able to detect hundreds to thousands of candidate BSBHs from circumbinary accretion with direct implications for Laser Interferometer Space Antenna., Liao, Wei-Ting, et al. DES Collaboration, The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciênciae Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).

Published
2020

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

Author

M. Smith, Daniel Gruen, V. Scarpine, A. K. Romer, Felipe Menanteau, M. E. C. Swanson, Eli S. Rykoff, E. Suchyta, Enrique Gaztanaga, August E. Evrard, J. Carretero, Marco A. P. Lima, Juan Garcia-Bellido, Brian Nord, Michael Schubnell, Adriano Agnello, C. Davis, Keith Bechtol, Flavia Sobreira, Santiago Avila, M. Carrasco Kind, A. Carnero Rosell, I. Sevilla-Noarbe, Carlos E. Cunha, Yanxi Zhang, Douglas L. Tucker, Kyler Kuehn, Tim Eifler, G. Gutierrez, G. Tarle, A. A. Plazas, N. Kuropatkin, Enrique Fernández, L. N. da Costa, Huan Lin, Josh Frieman, M. March, K. Honscheid, David J. James, David J. Brooks, R. H. Schindler, Pablo Fosalba, T. M. C. Abbott, D. L. Burke, Ofer Lahav, Peter Doel, E. J. Sanchez, S. Allam, Robert A. Gruendl, Marcelle Soares-Santos, H. T. Diehl, J. Annis, D. L. Hollowood, J. De Vicente, W. G. Hartley, Jennifer L. Marshall, Daniel Thomas, E. Buckley-Geer, Adam Amara, Ramon Miquel, Thomas E. Collett, A. Roodman, B. Flaugher, Ben Hoyle, M. A. G. Maia, Peter Melchior, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), and German Research Foundation

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, Gravitational lensing: strong, DES [surveys], astro-ph.GA, Library science, Techniques: spectroscopic, FOS: Physical sciences, clusters [gravitational lensing], Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, survey [gravitational lensing], Galaxies: individual, 0103 physical sciences, media_common.cataloged_instance, Astrophysics::Solar and Stellar Astrophysics, European union, general [gravitational lenses], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, STFC, media_common, Physics, 010308 nuclear & particles physics, business.industry, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, gravitational lensing individual, Alliance, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), strong [gravitational lensing], Fundamental physics, astro-ph.CO, Christian ministry, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

We describe the observation and confirmation of nine new strong gravitational lenses discovered in Year 1 data from the Dark Energy Survey (DES). We created candidate lists based on (i) galaxy group and cluster samples, and (ii) photometrically selected galaxy samples. We selected 46 candidates through visual inspection and then used the Gemini Multi-Object Spectrograph (GMOS) at the Gemini South telescope to acquire a spectroscopic follow-up of 21 of these candidates. Through an analysis of these spectroscopic follow-up data, we confirmed nine new lensing systems and rejected two candidates, and the analysis was inconclusive on 10 candidates. For each of the confirmed systems, our report measured spectroscopic properties, estimated source image-lens separations, and estimated enclosed masses as well. The sources that we targeted have an i-band surface brightness range of i ∼ 22-24 mag arcsec and a spectroscopic redshift range of z ∼ 0.8−2.6. The lens galaxies have a photometric redshift range of z ∼ 0.3−0.7. The lensing systems range in source image-lens separation from 2 to 9 arcsec and in enclosed mass from 10 to 10 M, Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ão Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência e Tecnologia, the Deutsche Forschungsge-meinschaft, and the Collaborating Institutions in the DES. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some of which include ERDF funds from the European Union. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2020

6. First Cosmology Results using Supernovae Ia from the Dark Energy Survey: Survey Overview, Performance, and Supernova Spectroscopy

Author

J. Calcino, David J. James, Bruce A. Bassett, R. L. C. Ogando, C. B. D'Andrea, Christopher J. Miller, R. R. Gupta, Tim Eifler, Juan Garcia-Bellido, Jennifer L. Marshall, Karl Glazebrook, Lluís Galbany, M. D. Johnson, Douglas L. Tucker, Kyler Kuehn, WeiKang Zheng, Daniel Scolnic, H. T. Diehl, Robert P. Kirshner, W. G. Hartley, Ramon Miquel, Felipe Menanteau, B. P. Thomas, Tenglin Li, R. C. Wolf, J. Lasker, Ryan J. Foley, Santiago Avila, Geraint F. Lewis, E. Bertin, Santiago González-Gaitán, J. K. Hoormann, E. Kasai, Mark Sullivan, Melissa L. Graham, C. Davis, M. Pursiainen, G. Tarle, Carlos E. Cunha, W. C. Wester, Eric H. Neilsen, J. Gschwend, Daniel Muthukrishna, Gary Bernstein, N. E. Sommer, Peter Nugent, C. Frohmaier, David Goldstein, Samuel Hinton, Alejandro Clocchiatti, Bonnie Zhang, A. K. Romer, Daniela Carollo, M. Carrasco Kind, J. Annis, G. Gutierrez, Edward Macaulay, R. C. Thomas, Paul Martini, J. De Vicente, Robert C. Nichol, Kaisey S. Mandel, Flavia Sobreira, Anais Möller, Alexei V. Filippenko, M. W. G. Johnson, Yen-Chen Pan, F. J. Castander, D. J. Brout, Enrique Gaztanaga, K. Honscheid, A. Carnero Rosell, T. M. C. Abbott, M. March, V. Scarpine, E. J. Sanchez, A. A. Plazas, P. Challis, Keith Bechtol, C. Lidman, B. E. Tucker, Eric Morganson, E. Swann, Jacobo Asorey, I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, L. N. da Costa, Ricard Casas, Juan Estrada, Michael Schubnell, M. Childress, S. A. Uddin, J. Carretero, Tamara M. Davis, Rob Sharp, M. Sako, D. L. Hollowood, S. Serrano, Richard Kessler, Marcos Lima, Josh Frieman, P. Wiseman, D. L. Burke, Robert A. Gruendl, Arturo Avelino, E. Suchyta, A. G. Kim, David J. Brooks, Ben Hoyle, Steven M. Crawford, M. A. G. Maia, M. Smith, Daniel Gruen, D. W. Gerdes, Australian Astronomical Observatory, Comisión Nacional de Investigación Científica y Tecnológica (Chile), University of California, National Aeronautics and Space Administration (US), W. M. Keck Foundation, Smithsonian Institution, University of Arizona, South African Astronomical Observatory, European Commission, Google, University of Southampton, Department of Energy (US), National Science Foundation (US), National Energy Research Scientific Computing Center (US), Gordon and Betty Moore Foundation, Heising Simons Foundation, David and Lucile Packard Foundation, Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Educación y Ciencia (España), Science and Technology Facilities Council (UK), Higher Education Funding Council for England, University of Illinois, University of Chicago, The Ohio State University, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), Deutsches Krebsforschungszentrum, University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (España), University College London, University of Edinburgh, CSIC - Instituto de Ciencias del Espacio (ICE), Ministerio de Ciencia e Innovación (España), University of Pennsylvania, University of Portsmouth, Stanford University, University of Sussex, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Institut 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
Observational cosmology, 010504 meteorology & atmospheric sciences, Cosmological parameters, Astrophysics, Sky surveys, 01 natural sciences, Cosmology, 0103 physical sciences, Binary star, 010303 astronomy & astrophysics, STFC, 0105 earth and related environmental sciences, Physics, Type Ia supernovae, RCUK, Astronomy and Astrophysics, Redshift, ESPECTROSCOPIA, Stars, Supernova, Supernovae, 13. Climate action, Space and Planetary Science, Dark energy, Variable star, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present details on the observing strategy, data-processing techniques, and spectroscopic targeting algorithms for the first three years of operation for the Dark Energy Survey Supernova Program (DES-SN). This five-year program using the Dark Energy Camera mounted on the 4 m Blanco telescope in Chile was designed to discover and follow supernovae (SNe) Ia over a wide redshift range (0.05 < z < 1.2) to measure the equation-of-state parameter of dark energy. We describe the SN program in full: Strategy, observations, data reduction, spectroscopic follow-up observations, and classification. From three seasons of data, we have discovered 12,015 likely SNe, 308 of which have been spectroscopically confirmed, including 251 SNe Ia over a redshift range of 0.017 < z < 0.85. We determine the effective spectroscopic selection function for our sample and use it to investigate the redshiftdependent bias on the distance moduli of SNe Ia we have classified. The data presented here are used for the first cosmology analysis by DES-SN ("DES-SN3YR"), the results of which are given in Dark Energy Survey Collaboration et al. The 489 spectra that are used to define the DES-SN3YR sample are publicly available at https://des.ncsa.illinois.edu/releases/sn., Based in part on data acquired through the Australian Astronomical Observatory under program ATAC A/2013B/12. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina), and Ministério da Ciência, Tecnologia e Inovação (Brazil). Observations with Gemini were obtained under NOAO programs 2013A-0373 and 2015B0197, corresponding to GN-2013B-Q-55, GS-2013B-Q-45, GS-2015B-Q-7, GN-2015B-Q-10, as well as GS-2015B-Q-8 under a Chilean program. Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. Observations with GTC were made under programs GTC77-13B, GTC70-14B, and GTC101-15B. Some of the data presented herein were obtained at the W. M. Keck Observatory, which isoperated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Observations with Keck were made under programs U063-2013B, U021-2014B, U048-2015B, and U038-2016A. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile, partially through program CN2015B-89. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona, under programs 2014c-SAO-4, 2015a-SAO-12, 2015c-SAO-21. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT) under programs 2013-1-RSA_OTH-023, 2013-2-RSA_OTH-018, 2014-1-RSA_OTH016, 2014-2-SCI-070, 2015-1-SCI-063, and 2015-2-SCI-061. Based on observations collected at the European Southern Observatory under ESO programmes 093.A-0749(A), 094.A0310(B), 095.A-0316(A), 096.A-0536(A), 095.D-0797(A). Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, Inovações e Comunicações (MCTIC) do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). SOAR observations obtained under program 2014B-0205. Research at Lick Observatory is partially supported by a generous gift from Google. The Southampton group acknowledges support from EUFP7/ERC grant [615929]. MS acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 759194—USNAC). The Penn group was supported by DOE grant DE-FOA-0001358 and NSF grant AST-1517742. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. A.V.F.ʼs group at U.C. Berkeley is grateful for financial assistance from NSF grant AST-1211916, the Christopher R. Redlich Fund, Gary and Cynthia Bengier, the TABASGO Foundation, and the Miller Institute for Basic Research in Science. The UCSC team is supported in part by NASA grants 14-WPS14-0048, NNG16PJ34G, NNG17PX03C, NSF grants AST-1518052 and AST-1815935, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and by fellowships from the Alfred P. Sloan Foundation and the David and Lucile Packard Foundation to R.J.F. SGG acknowledges support by FCT under Project CRISP PTDC/FIS-AST31546 and UIDB/00099/2020. L.G. was funded by the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). Support for AC was provided by ANID, through the Millennium Science Initiative grant ICN12_009 (MAS) and by grant Basal CATA PFB 06/09. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo InterAmerican Observatory at NSF?s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/ 2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).

Published
2020

7. Measuring linear and non-linear galaxy bias using counts-in-cells in the Dark Energy Survey Science Verification data

Author

Flavia Sobreira, Alistair R. Walker, D. L. Hollowood, Gruendl, R, A, Marcelle Soares-Santos, M. Smith, Sánchez, F, J, Santiago Avila, Carlos E. Cunha, H. T. Diehl, Rafe Schindler, Daniel Gruen, A. Pujol, Marcos Lima, M. March, Jennifer L. Marshall, A. E. Evrard, M. E.C. Swanson, I. Sevilla-Noarbe, David Brooks, Ofer Lahav, W. G. Hartley, A. I. Salvador, N. Kuropatkin, Juan Garcia-Bellido, E. Bertin, F. J. Castander, Ramon Miquel, P. Doel, T. M. C. Abbott, A. Roodman, J. Annis, J. De Vicente, David J. James, J. Carretero, Ashley J. Ross, E. J. Sanchez, Vikram, Pablo Fosalba, A. Carnero Rosell, Felipe Menanteau, G. Gutierrez, M. Carrasco Kind, Daniel Thomas, J. Gschwend, Gregory Tarle, Kyler Kuehn, Enrique Gaztanaga, A Pagul, E. Suchyta, Joshua A. Frieman, Scarpine, A. K. Romer, D. L. Burke, S. Allam, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, 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), and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Cosmological parameters, Dark matter, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Dark energy, 0103 physical sciences, cosmological parameters, observations [Cosmology], dark energy, Cluster analysis, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, STFC, ComputingMilieux_MISCELLANEOUS, QC, Physics, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Galaxy, Redshift, Nonlinear system, Density distribution, Space and Planetary Science, cosmology: observations, ESTRUTURA DO UNIVERSO, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Non-linear bias measurements require a great level of control of potential systematic effects in galaxy redshift surveys. Our goal is to demonstrate the viability of using Counts-in-Cells (CiC), a statistical measure of the galaxy distribution, as a competitive method to determine linear and higher-order galaxy bias and assess clustering systematics. We measure the galaxy bias by comparing the first four moments of the galaxy density distribution with those of the dark matter distribution. We use data from the MICE simulation to evaluate the performance of this method, and subsequently perform measurements on the public Science Verification (SV) data from the Dark Energy Survey (DES). We find that the linear bias obtained with CiC is consistent with measurements of the bias performed using galaxy-galaxy clustering, galaxy-galaxy lensing, CMB lensing, and shear+clustering measurements. Furthermore, we compute the projected (2D) non-linear bias using the expansion $\delta_{g} = \sum_{k=0}^{3} (b_{k}/k!) \delta^{k}$, finding a non-zero value for $b_2$ at the $3\sigma$ level. We also check a non-local bias model and show that the linear bias measurements are robust to the addition of new parameters. We compare our 2D results to the 3D prediction and find compatibility in the large scale regime ($>30$ Mpc $h^{-1}$), Comment: Accepted for publication in MNRAS

Published
2018

8. Dark energy survey year-1 results

Author

A. Benoit-Lévy, A. A. Plazas, Ramon Miquel, Will J. Percival, G. Gutierrez, F. J. Castander, Nilanjan Banik, I. Sevilla-Noarbe, O. Friedrich, N. Kuropatkin, Flavia Sobreira, N. Kokron, J. Carretero, Martin Crocce, E. J. Sanchez, Robert A. Gruendl, David Brooks, Peter Doel, L. N. da Costa, Michael Schubnell, Kyler Kuehn, W. G. Hartley, J. Annis, M. Smith, Ashley J. Ross, Daniel Gruen, Filipe B. Abdalla, D. L. Hollowood, Santiago Avila, Carlos E. Cunha, G. Tarle, K. Honscheid, M. E. C. Swanson, J. De Vicente, C. Davis, David J. James, Daniel Thomas, V. Scarpine, Marcos Lima, A. I. Salvador, H. Camacho, Pablo Fosalba, D. W. Gerdes, Juan Garcia-Bellido, D. Gomes, Kwan Chuen Chan, Joshua A. Frieman, E. Suchyta, M. Carrasco Kind, F. Andrade-Oliveira, Alistair R. Walker, R. Gomes, E. Bertin, Rafe Schindler, Rogerio Rosenfeld, 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, Univ Portsmouth, Univ Autonoma Madrid, CSIC, Ohio State Univ, Univ Florida, Fermilab Natl Accelerator Lab, Univ Amsterdam, Leiden Univ, Universidade de São Paulo (USP), Lab Interinst e Astron, Universidade Estadual Paulista (Unesp), Stanford Univ, Sun Yat Sen Univ, Max Planck Inst Extraterrestrial Phys, Ludwig Maximilians Univ Munchen, UCL, Rhodes Univ, CNRS, UPMC Univ Paris 06, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, Observatorio Nacl, Ctr Invest Energet Medioambientales & Tecnol CIEM, Univ Chicago, Univ Michigan, SLAC Natl Accelerator Lab, Swiss Fed Inst Technol, Santa Cruz Inst Particle Phys, Univ Washington, Australian Astron Observ, Inst Catalana Recerca & Estudis Avancats, CALTECH, Univ Southampton, Universidade Estadual de Campinas (UNICAMP), Oak Ridge Natl Lab, Natl Opt Astron Observ, GRAPPA (ITFA, IoP, FNWI), and IoP (FNWI)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, methods: numerical, cosmology: theory, 0103 physical sciences, Halo effect, ST/K0090X/1, Cluster analysis, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, theory [cosmology], 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, RCUK, Astronomy and Astrophysics, numerical [methods], Redshift, Galaxy, observations [cosmology], ST/K00283X/1, Space and Planetary Science, cosmology: observations, Dark energy, Halo, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Mock catalogues are a crucial tool in the analysis of galaxy surveys data, both for the accurate computation of covariance matrices, and for the optimisation of analysis methodology and validation of data sets. In this paper, we present a set of 1800 galaxy mock catalogues designed to match the Dark Energy Survey Year-1 BAO sample (Crocce et al. 2017) in abundance, observational volume, redshift distribution and uncertainty, and redshift dependent clustering. The simulated samples were built upon HALOGEN (Avila et al. 2015) halo catalogues, based on a $2LPT$ density field with an exponential bias. For each of them, a lightcone is constructed by the superposition of snapshots in the redshift range $0.45, Comment: 18 pages, 15 figures, 1 table, published in MNRAS

Published
2018

9. UV-luminous, star-forming hosts of z ∼ 2 reddened quasars in the Dark Energy Survey

Author

David J. James, Pablo Fosalba, V. Scarpine, A. Benoit-Lévy, R. C. Smith, J. Gschwend, J. Carretero, M. Carrasco-Kind, Flavia Sobreira, G. Gutierrez, Shantanu Desai, S. L. Reed, Paul C. Hewett, Richard G. McMahon, David Brooks, Daniel Gruen, Brian Nord, M. Banerji, Joshua A. Frieman, Peter Doel, A. K. Romer, Juan Garcia-Bellido, Jennifer L. Marshall, E. J. Sanchez, Robert A. Gruendl, E. Buckley-Geer, Paul Martini, E. Suchyta, F. B. Abdalla, D. W. Gerdes, B. Flaugher, Alistair R. Walker, Ramon Miquel, Marcelle Soares-Santos, Carlos E. Cunha, Robert C. Nichol, Rafe Schindler, Kyler Kuehn, C. F. Wethers, Tesla E. Jeltema, Matthew Smith, Marcos Lima, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, M. A. G. Maia, A. A. Plazas, K. Honscheid, C. Lemon, C. B. D'Andrea, Diego Capozzi, S. E. Kuhlmann, Michael Schubnell, Darren L. DePoy, A. Carnero Rosell, Yue Shen, Felipe Menanteau, Gregory Tarle, 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, Banerji, Manda [0000-0002-0639-5141], Hewett, Paul [0000-0002-6528-1937], Lemon, Cameron [0000-0003-2456-9317], McMahon, Richard [0000-0001-8447-8869], and Apollo - University of Cambridge Repository

Subjects
Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Photometry (optics), galaxies: high-redshift, quasars: general, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, Star formation, RCUK, Astronomy and Astrophysics, Quasar, Astrophysics - Astrophysics of Galaxies, Galaxy, Wavelength, 13. Climate action, Space and Planetary Science, galaxies: star formation, Astrophysics of Galaxies (astro-ph.GA), ultraviolet: galaxies, Dark energy, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present the first rest-frame UV population study of 17 heavily reddened, high-luminosity (E(B-V)$_{\rm{QSO}}\gtrsim$ 0.5; L$_{\rm{bol}}>$ 10$^{46}$ergs$^{-1}$) broad-line quasars at $1.5 < z < 2.7$. We combine the first year of deep, optical, ground-based observations from the Dark Energy Survey (DES) with the near infrared VISTA Hemisphere Survey (VHS) and UKIDSS Large Area Survey (ULAS) data, from which the reddened quasars were initially identified. We demonstrate that the significant dust reddening towards the quasar in our sample allows host galaxy emission to be detected at the rest-frame UV wavelengths probed by the DES photometry. By exploiting this reddening effect, we disentangle the quasar emission from that of the host galaxy via spectral energy distribution (SED) fitting. We find evidence for a relatively unobscured, star-forming host galaxy in at least ten quasars, with a further three quasars exhibiting emission consistent with either star formation or scattered light. From the rest-frame UV emission, we derive instantaneous, dust-corrected star formation rates (SFRs) in the range 25 < SFR$_{\rm{UV}}$ < 365 M$_{\odot}$yr$^{-1}$, with an average SFR$_{\rm{UV}}$ = 130 $\pm$ 95 M$_{\odot}$yr$^{-1}$. We find a broad correlation between SFR$_{\rm{UV}}$ and the bolometric quasar luminosity. Overall, our results show evidence for coeval star formation and black hole accretion occurring in luminous, reddened quasars at the peak epoch of galaxy formation., 21 pages, 8 figures, MNRAS Accepted

Published
2018

11. Dark Energy Survey Year 1 Results:Constraints on Intrinsic Alignments and their Colour Dependence from Galaxy Clustering and Weak Lensing

Author

Juan Garcia-Bellido, J. Carretero, Elisabeth Krause, I. Sevilla-Noarbe, Erin Sheldon, David Brooks, J. P. Dietrich, Daniel Gruen, N. Kuropatkin, D. W. Gerdes, J. De Vicente, R. H. Schindler, R. L. C. Ogando, L. N. da Costa, E. Suchyta, Ramon Miquel, Marcos Lima, S. Serrano, Peter Doel, Peter Melchior, Francisco J. Castander, D. L. DePoy, Michael Troxel, M. A. G. Maia, Vinu Vikram, A. Carnero Rosell, M. March, A. A. Plazas, T. M. C. Abbott, Kyler Kuehn, Joshua A. Frieman, M. Carrasco Kind, Michael Schubnell, P. Larsen, Christopher J. Miller, Daniel Thomas, S. Samuroff, V. Scarpine, Tim Eifler, Flavia Sobreira, E. J. Sanchez, Jonathan Blazek, David J. James, W. G. Hartley, M. Gatti, Niall MacCrann, Enrique Gaztanaga, Devon L. Hollowood, C. D. Leonard, J. Prat, Sarah Bridle, Scott Dodelson, Pablo Fosalba, B. Flaugher, Carlos E. Cunha, Ben Hoyle, G. Gutierrez, Joe Zuntz, Shantanu Desai, H. T. Diehl, Mathew Smith, E. Bertin, C. Davis, J. Gschwend, Gary Bernstein, S. Allam, Robert A. Gruendl, Paul Martini, Felipe Menanteau, Gregory Tarle, K. Honscheid, J. Annis, Jennifer L. Marshall, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
luminous red galaxies, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmological parameters, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, contamination, gravitational lensing: weak, statistics [Galaxies], TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, 0103 physical sciences, cosmological parameters, observations [Cosmology], 010303 astronomy & astrophysics, Weak gravitational lensing, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, cosmological parameter constraints, model, Series (mathematics), 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Galaxy, Amplitude, kids-450, Space and Planetary Science, cosmology: observations, Dark energy, impact, astro-ph.CO, High Energy Physics::Experiment, digital sky survey, Astrophysics::Earth and Planetary Astrophysics, weak [Gravitational lensing], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform a joint analysis of intrinsic alignments and cosmology using tomographic weak lensing, galaxy clustering and galaxy-galaxy lensing measurements from Year 1 (Y1) of the Dark Energy Survey. We define early- and late-type subsamples, which are found to pass a series of systematics tests, including for spurious photometric redshift error and point spread function correlations. We analyse these split data alongside the fiducial mixed Y1 sample using a range of intrinsic alignment models. In a fiducial Nonlinear Alignment Model (NLA) analysis, assuming a flat \lcdm~cosmology, we find a significant difference in intrinsic alignment amplitude, with early-type galaxies favouring $A_\mathrm{IA} = 2.38^{+0.32}_{-0.31}$ and late-type galaxies consistent with no intrinsic alignments at $0.05^{+0.10}_{-0.09}$. We find weak evidence of a diminishing alignment amplitude at higher redshifts in the early-type sample. The analysis is repeated using a number of extended model spaces, including a physically motivated model that includes both tidal torquing and tidal alignment mechanisms. In multiprobe likelihood chains in which cosmology, intrinsic alignments in both galaxy samples and all other relevant systematics are varied simultaneously, we find the tidal alignment and tidal torquing parts of the intrinsic alignment signal have amplitudes $A_1 = 2.66 ^{+0.67}_{-0.66}$, $A_2=-2.94^{+1.94}_{-1.83}$, respectively, for early-type galaxies and $A_1 = 0.62 ^{+0.41}_{-0.41}$, $A_2 = -2.26^{+1.30}_{-1.16}$ for late-type galaxies. In the full (mixed) Y1 sample the best constraints are $A_1 = 0.70 ^{+0.41}_{-0.38}$, $A_2 = -1.36 ^{+1.08}_{-1.41}$. For all galaxy splits and IA models considered, we report cosmological parameter constraints that are consistent with the results of Troxel et al. (2017) and Dark Energy Survey Collaboration (2017)., 31 pages, 23 figures; accepted by MNRAS

Published
2019

12. Density split statistics: Cosmological constraints from counts and lensing in cells in des Y1 and SDSS data

Author

C. Sánchez, J. Carretero, R. P. Rollins, Peter Melchior, Joshua A. Frieman, G. Tarle, Alex Drlica-Wagner, Joe Zuntz, Michael Schubnell, C. B. D'Andrea, A. Benoit-Lévy, A. A. Plazas, A. Roodman, I. Sevilla-Noarbe, Tommaso Giannantonio, Keith Bechtol, David J. James, Michael Troxel, Felipe Menanteau, J. DeRose, N. Kuropatkin, A. Alarcon, Flavia Sobreira, Vinu Vikram, O. Lahav, L. N. da Costa, Matt J. Jarvis, Jochen Weller, P. Martini, Jennifer L. Marshall, Alistair R. Walker, T. M. C. Abbott, Filipe B. Abdalla, E. Krause, Yanxi Zhang, Kyler Kuehn, David J. Brooks, J. P. Dietrich, Juan Garcia-Bellido, Marcos Lima, M. Crocce, Marcelle Soares-Santos, E. S. Rykoff, M. March, M. Gatti, M. Carrasco Kind, A. J. Ross, Ben Hoyle, J. Elvin-Poole, C. L. Davis, J. Clampitt, A. Carnero Rosell, B. Jain, W. G. Hartley, R. C. Smith, B. Flaugher, E. J. Sanchez, J. de Vicente, S. Samuroff, Mathew Smith, M. E. C. Swanson, S. Desai, Jonathan Blazek, Risa H. Wechsler, Enrique Gaztanaga, R. Cawthon, Joseph J. Mohr, Stefan Hilbert, Daniel Gruen, K. Honscheid, Sarah Bridle, E. Sheldon, T. McClintock, Oliver Friedrich, Carlos E. Cunha, E. Rozo, Daniel Thomas, E. Buckley-Geer, Ramon Miquel, S. Allam, Robert A. Gruendl, Tesla E. Jeltema, Enrique J. Fernández, Peter Doel, J. Annis, J. Prat, P. Fosalba, H. T. Diehl, M. S. S. Gill, G. Gutierrez, J. Gschwend, C. Chang, Gary Bernstein, N. MacCrann, V. Scarpine, E. Bertin, 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, Giannantonio, Tommaso [0000-0002-9865-0436], and Apollo - University of Cambridge Repository

Subjects
cosmological model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), media_common.quotation_subject, sloan digital sky survey, Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gravitation: lens, Excellence, 0103 physical sciences, media_common.cataloged_instance, European union, distribution function, Astronomy observatory, dark energy, 010303 astronomy & astrophysics, matter: density, Astrophysics::Galaxy Astrophysics, media_common, perturbation theory, Physics, 010308 nuclear & particles physics, European research, matter: density: fluctuation, Astronomy, statistical analysis: Bayesian, two-point function, Research council, Fundamental physics, many-body problem, astro-ph.CO, Christian ministry, galaxy, National laboratory, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We derive cosmological constraints from the probability distribution function (PDF) of evolved large-scale matter density fluctuations. We do this by splitting lines of sight by density based on their count of tracer galaxies, and by measuring both gravitational shear around and counts-in-cells in overdense and underdense lines of sight, in Dark Energy Survey (DES) First Year and Sloan Digital Sky Survey (SDSS) data. Our analysis uses a perturbation theory model (see companion paper Friedrich at al.) and is validated using N-body simulation realizations and log-normal mocks. It allows us to constrain cosmology, bias and stochasticity of galaxies w.r.t. matter density and, in addition, the skewness of the matter density field. From a Bayesian model comparison, we find that the data weakly prefer a connection of galaxies and matter that is stochastic beyond Poisson fluctuations on, Comment: 33 pages, 22 figures; matches published version

Published
2019
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13. Dark Energy Survey Year 1 results: the effect of intracluster light on photometric redshifts for weak gravitational lensing

Author

Flavia Sobreira, V. Scarpine, Ramon Miquel, Martin Crocce, Ofer Lahav, Elisabeth Krause, C. Davis, J. Gschwend, Filipe B. Abdalla, J. P. Dietrich, Juan Garcia-Bellido, Eduardo Rozo, Felipe Menanteau, David J. James, Yanxi Zhang, Alex Drlica-Wagner, Alistair R. Walker, Pablo Fosalba, Marcelle Soares-Santos, D. L. Burke, Vinu Vikram, J. Annis, K. Honscheid, Peter Melchior, Santiago Avila, Carlos E. Cunha, Brian Yanny, A. A. Plazas, Shantanu Desai, R. Cawthon, Daniel Thomas, Ben Hoyle, H. T. Diehl, Eli S. Rykoff, S. Allam, Robert A. Gruendl, Antonella Palmese, Jennifer L. Marshall, M. A. G. Maia, Enrique Gaztanaga, A. Carnero Rosell, J. Carretero, M. Carrasco Kind, I. Sevilla-Noarbe, A. K. Romer, B. Flaugher, N. Kuropatkin, T. N. Varga, L. N. da Costa, R. L. C. Ogando, Tesla E. Jeltema, Joshua A. Frieman, J. De Vicente, Huan Lin, V. C. Busti, M. Smith, Daniel Gruen, D. W. Gerdes, M. E. C. Swanson, G. Tarle, C. J. Miller, Kyler Kuehn, E. Suchyta, David J. Brooks, D. L. Hollowood, Richard G. Kron, and Marcos Lima

Subjects
High energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, 0103 physical sciences, media_common.cataloged_instance, European union, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, media_common, Physics, 010308 nuclear & particles physics, business.industry, European research, Astronomy and Astrophysics, Space and Planetary Science, Research council, Fundamental physics, Christian ministry, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the effect of diffuse intracluster light on the critical surface mass density estimated from photometric redshifts of lensing source galaxies, and the resulting bias in a weak lensing measurement of galaxy cluster mass. Under conservative assumptions, we find the bias to be negligible for imaging surveys like the Dark Energy Survey (DES) with a recommended scale cut of >=200 kpc distance from cluster centers. For significantly deeper source catalogs from present and future surveys like the Large Synoptic Survey Telescope (LSST) program, more conservative scale and source magnitude cuts or a correction of the effect may be necessary to achieve per-cent level lensing measurement accuracy, especially at the massive end of the cluster population., 11 pages, 4 figures, matches version published in MNRAS

Published
2019

14. Galaxies in X-ray selected clusters and groups in dark energy survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Author

A. A. Plazas, J. Gschwend, B. Flaugher, E. Suchyta, Martin Sahlén, Chris A. Collins, Matt Hilton, Flavia Sobreira, Daniel Gruen, M. A. G. Maia, Felipe Menanteau, Martin Crocce, Gregory Tarle, Michael Schubnell, Robert G. Mann, D. W. Gerdes, John P. Stott, J. Carretero, G. Gutierrez, K. Honscheid, M. March, Mathew Smith, H. T. Diehl, J. P. Dietrich, David Bacon, Risa H. Wechsler, N. Kuropatkin, C. B. D'Andrea, Eli S. Rykoff, C. J. Miller, P. Rooney, Rituparna Das, A. Benoit-Lévy, David J. James, David J. Brooks, Enrique Gaztanaga, Ramon Miquel, Pablo Fosalba, A. Bermeo, Juan Garcia-Bellido, Julian A. Mayers, A. Carnero Rosell, Francisco J. Castander, Filipe B. Abdalla, M. Carrasco Kind, Robert C. Nichol, J. Song, E. Buckley-Geer, C. Vergara Cervantes, Marcos Lima, Alistair R. Walker, Marcelle Soares-Santos, I. Sevilla-Noarbe, L. N. da Costa, R. L. C. Ogando, C. Hennig, M. E. C. Swanson, Timothy A. McKay, Yanxi Zhang, Tim Eifler, H. Wilcox, Jennifer L. Marshall, Ben Hoyle, Nicola Mehrtens, Peter Melchior, Kyler Kuehn, A. K. Romer, Andrew R. Liddle, Sarah Bridle, Carlos E. Cunha, Pedro T. P. Viana, T. M. C. Abbott, E. J. Sanchez, Scott T. Kay, Han Lin, D. L. Burke, S. Allam, Robert A. Gruendl, Tesla E. Jeltema, C. J. Conselice, 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), Evolution, Astrophysics::High Energy Astrophysical Phenomena, astro-ph.GA, General – galaxies, Bayesian probability, AST-1138766, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Clusters, Astronomi, astrofysik och kosmologi, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics and Cosmology, clusters: general [galaxies], AST-1536171, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, evolution [galaxies], STFC, Luminosity function (astronomy), QB, Physics, Sequence, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Function (mathematics), Galaxies, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), Dark energy, astro-ph.CO, Survey data collection, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using $\sim 100$ X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the luminosity function simultaneously in redshift ($0.1, Comment: Updated to match the accepted version

Published
2019

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

Author

R. L. C. Ogando, Enrique Gaztanaga, Vinu Vikram, Douglas L. Tucker, Kyler Kuehn, Jennifer L. Marshall, David J. James, Michael Rauch, George D. Becker, Paul C. Hewett, V. Scarpine, G. Tarle, G. Gutierrez, A. Roodman, R. C. Smith, A. Carnero Rosell, J. De Vicente, M. Carrasco Kind, Daniel Thomas, Ofer Lahav, E. Buckley-Geer, J. Annis, C. B. D'Andrea, B. Flaugher, Salcedo Romero de Ávila, Flavia Sobreira, Michael Schubnell, E. Pons, Shantanu Desai, Ben Hoyle, A. A. Plazas, Carlos E. Cunha, K. Honscheid, S. L. Reed, F. J. Castander, S. Allam, T. M. C. Abbott, J. Gschwend, E. J. Sanchez, Paul Martini, M. A. G. Maia, Ramon Miquel, E. Bertin, Peter Doel, H. T. Diehl, M. Smith, Daniel Gruen, I. Sevilla-Noarbe, L. N. da Costa, M. Banerji, David J. Brooks, M. E. C. Swanson, J. Carretero, E. Suchyta, August E. Evrard, Richard G. McMahon, Josh Frieman, Juan Garcia-Bellido, D. L. Hollowood, S. Serrano, and Marcos Lima

Subjects
formation [galaxies], first stars, Astrophysics, 01 natural sciences, Virial theorem, Luminosity, 0103 physical sciences, individual: VDES J0020-3653 [quasars], Emission spectrum, dark ages, 010303 astronomy & astrophysics, Reionization, STFC, Line (formation), Physics, biology, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Quasar, biology.organism_classification, Galaxias, individual: VDES J0246-5219 [quasars], 13. Climate action, Space and Planetary Science, indiviual: VDES J0244-5008 [quasars], active [galaxies], Dark Ages, reionization, individual: VDES J0224-4711 [quasars], high-redshift [galaxies]
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.

Published
2019

16. Characterization and in silico Mutagenic Assessment of a New Betahistine Degradation Impurity

Author

Tiago C. Lourenço, Caroline L. de Oliveira, Miller N. de Freitas, C.R.W. Guimaraes, João Luis Callegari Lopes, Murilo B. M. de Mello, Gama Fernando Henrique De Souza, Alessandra Mascarello, Mariah A. Ultramari, Fernanda P. Ferreira, Carlos E. Cunha, Antonio A. F. de Oliveira, and Giuliano C. Clososki

Subjects
Active ingredient, Electrospray, Chromatography, Chemistry, forced-degradation studies, General Chemistry, Tandem mass spectrometry, Mass spectrometry, Impurity, MEDICAMENTO, betahistine, Forced degradation, medicine, Betahistine, drug stability, drug impurities, Two-dimensional nuclear magnetic resonance spectroscopy, medicine.drug
Abstract

Currently, the pharmaceutical industry devotes great attention to drug degradation products because these compounds can offer risks to patients. A previous degradation study of betahistine (N-α-methyl-2-pyridylethylamine) conducted under different stress conditions detected three main impurities named A, B and C. Degradation products were analyzed by high-resolution mass spectrometry in electrospray source and time of flight analyzer (ESI-TOF) and nuclear magnetic resonance (NMR). Impurity mutagenicity was evaluated by Derek Nexus and Sarah Nexus softwares. Liquid chromatography hyphenate with tandem mass spectrometry (LC-MS/MS) analysis of the betahistine forced degradation sample indicated the presence of a new impurity, which was named impurity C1. 2D NMR experiments allowed the complete structural characterization of the new entity. The active pharmaceutical ingredient and degradation impurities were classified as inactive in the in silico mutagenic studies. Systematic investigation of a forced degradation sample led to the characterization of a new betahistine impurity. The in silico mutagenicity study of the betahistine degradation impurities may be useful in the risk assessment of the drug products.

Published
2019

17. Cosmological Constraints from Multiple Probes in the Dark Energy Survey

Author

Eric H. Neilsen, Martin Crocce, A. Carnero Rosell, J. Carretero, Tamara M. Davis, Martin Becker, J. P. Dietrich, J. Gschwend, Richard G. McMahon, J. DeRose, L. F. Secco, D. J. Brout, Darren L. DePoy, W. G. Hartley, F. J. Castander, Richard G. Kron, P. Andersen, Lluís Galbany, A. Roodman, Tommaso Giannantonio, C. Davis, Gary Bernstein, Daniel Gruen, S. A. Uddin, Ofer Lahav, J. Lasker, Elisabeth Krause, J. Muir, Enrique Gaztanaga, N. E. Sommer, Rob Sharp, D. L. Hollowood, Risa H. Wechsler, D. W. Gerdes, A. G. Kim, V. Scarpine, S. Serrano, Richard Kessler, A. Campos, Eli S. Rykoff, Erin Sheldon, David Brooks, D. L. Burke, Geraint F. Lewis, David Goldstein, Carlos Solans Sanchez, Bonnie Zhang, Alex Drlica-Wagner, Marcos Lima, I. Sevilla-Noarbe, H. T. Diehl, P. Martini, M. Gatti, David Bacon, J. Calcino, David J. James, Joseph J. Mohr, J. Prat, Samuel Hinton, Bruce A. Bassett, J. P. Marriner, M. Carrasco Kind, Eric J. Baxter, G. Gutierrez, Dragan Huterer, Niall MacCrann, M. H.L.S. Wang, Bhuvnesh Jain, B. Flaugher, F. Andrade-Oliveira, Alistair R. Walker, Robert C. Nichol, Joe Zuntz, S. Kent, Pablo Fosalba, S. Allam, Ryan J. Foley, Robert A. Gruendl, Anais Möller, N. Kokron, E. Bertin, R. Cawthon, Ramon Miquel, Ashley J. Ross, Juan Estrada, M. S. Schubnell, P. Doel, Marcelle Soares-Santos, J. Annis, H. Camacho, Will J. Percival, N. Weaverdyck, A. Porredon, Karl Glazebrook, Enrique Fernández, Juan Garcia-Bellido, P. Challis, Huan Lin, Daniela Carollo, Jennifer L. Marshall, Brad E. Tucker, K. Honscheid, Brian Yanny, Shantanu Desai, N. Kuropatkin, E. Kasai, Rafe Schindler, Mathew Smith, A. Alarcon, M. Childress, C. Lidman, Felipe Menanteau, Daniel Scolnic, Gregory Tarle, L. N. da Costa, Tesla E. Jeltema, August E. Evrard, E. Swann, K. C. Chan, J. De Vicente, P. Lemos, Daniel Thomas, Brian Nord, Flavia Sobreira, Michael Troxel, Joshua A. Frieman, M. March, M. E. C. Swanson, Matt J. Jarvis, Kyler Kuehn, P. Vielzeuf, Yanxi Zhang, Tim Eifler, Keith Bechtol, Antonella Palmese, Rogerio Rosenfeld, M. A. G. Maia, J. K. Hoormann, Ricardo L. C. Ogando, Ben Hoyle, A. A. Plazas, A. K. Romer, C. B. D'Andrea, Edward Macaulay, Jack Elvin-Poole, S. Samuroff, R. C. Thomas, Eric Morganson, Jacobo Asorey, Yen-Chen Pan, Peter Melchior, N. Banik, Jonathan Blazek, Tenglin Li, Sarah Bridle, Scott Dodelson, Santiago Avila, Chihway Chang, Carlos E. Cunha, Jochen Weller, T. M. C. Abbott, Hiranya V. Peiris, E. J. Sanchez, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, National Optical Astronomy Observatory, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Fermi National Accelerator Laboratory, University of Queensland, Dark Cosmology Centre, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de E-Astronomia - LIneA, Korea Astronomy and Space Science Institute, University of Portsmouth, African Institute for Mathematical Sciences, South African Astronomical Observatory, University of Pennsylvania, LSST, University of Wisconsin-Madison, Argonne National Laboratory, Institut d'Astrophysique de Paris, Ohio State University, Observatoire de Sauverny, University of Manchester, University College London, Stanford University, SLAC National Accelerator Laboratory, Universidade de São Paulo (USP), Carnegie Mellon University, Medioambientales y Tecnológicas (CIEMAT), Astrophysical Observatory of Turin, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, Harvard-Smithsonian Center for Astrophysics, University of Chicago, University of Southampton, Observatório Nacional, Texas A and M University, 382 Via Pueblo Mall, IIT Hyderabad, Excellence Cluster Universe, Ludwig-Maximilians-Universität, Steward Observatory, California Institute of Technology, University of Michigan, Santa Cruz Institute for Particle Physics, University of Pittsburgh, Universidad Autonoma de Madrid, University of Cambridge, Ludwig-Maximilians Universität München, Swinburne University of Technology, ETH Zurich, Max Planck Institute for Extraterrestrial Physics, University of Namibia, Lawrence Berkeley National Laboratory, Macquarie University, University of Sydney, Australian National University, Peyton Hall, Institució Catalana de Recerca i Estudis Avançats, ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), National Astronomical Observatory of Japan, Academia Sinica, University of Waterloo, Perimeter Institute for Theoretical Physics, University of Sussex, Brookhaven National Laboratory, Physics Department, Universidade Estadual de Campinas (UNICAMP), Duke University, Observatories of the Carnegie Institution for Science, University of Edinburgh, Natl Opt Astron Observ, IEEC, CSIC, Fermilab Natl Accelerator Lab, Univ Queensland, Univ Copenhagen, Universidade Estadual Paulista (Unesp), Lab Interinst E Astron LIneA, Korea Astron & Space Sci Inst, Univ Portsmouth, African Inst Math Sci, South African Astron Observ, Univ Penn, Univ Wisconsin, Argonne Natl Lab, CNRS, UPMC Univ Paris 06, Ohio State Univ, Ecole Polytech Fed Lausanne, Univ Manchester, UCL, Stanford Univ, SLAC Natl Accelerator Lab, Carnegie Mellon Univ, Ctr Invest Energet Medioambientales & Tecnol CIEM, Astrophys Observ Turin, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, Harvard Smithsonian Ctr Astrophys, Univ Chicago, Univ Southampton, Observ Nacl, Texas A&M Univ, Ludwig Maximilians Univ Munchen, Steward Observ, CALTECH, Univ Michigan, Santa Cruz Inst Particle Phys, Univ Pittsburgh, Univ Autonoma Madrid, Univ Cambridge, Swinburne Univ Technol, Swiss Fed Inst Technol, Max Planck Inst Extraterr Phys, Univ Namibia, Lawrence Berkeley Natl Lab, Macquarie Univ, Univ Sydney, Australian Natl Univ, Princeton Univ, Inst Catalana Recerca & Estudis Avancats, ARC Ctr Excellence All Sky Astrophys CAASTRO, Natl Astron Observ Japan, Acad Sinica, Univ Waterloo, Perimeter Inst Theoret Phys, Univ Sussex, Brookhaven Natl Lab, Brandeis Univ, Duke Univ, Observ Carnegie Inst Sci, and Univ Edinburgh

Subjects
bao, Cosmology and Nongalactic Astrophysics (astro-ph.CO), MATÉRIA ESCURA, media_common.quotation_subject, Cosmic microwave background, Dark matter, FOS: Physical sciences, General Physics and Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, des, Gravitation and Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, supernova, galaxies, 0103 physical sciences, redshift distributions, 010306 general physics, QC, STFC, Weak gravitational lensing, media_common, Physics, Equation of state (cosmology), RCUK, Shape of the universe, Universe, 13. Climate action, astro-ph.CO, Dark energy, baryon acoustic-oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The combination of multiple observational probes has long been advocated as a powerful technique to constrain cosmological parameters, in particular dark energy. The Dark Energy Survey has measured 207 spectroscopically--confirmed Type Ia supernova lightcurves; the baryon acoustic oscillation feature; weak gravitational lensing; and galaxy clustering. Here we present combined results from these probes, deriving constraints on the equation of state, $w$, of dark energy and its energy density in the Universe. Independently of other experiments, such as those that measure the cosmic microwave background, the probes from this single photometric survey rule out a Universe with no dark energy, finding $w=-0.80^{+0.09}_{-0.11}$. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of $\Omega_b=0.069^{+0.009}_{-0.012}$ that is independent of early Universe measurements. These results demonstrate the potential power of large multi-probe photometric surveys and pave the way for order of magnitude advances in our constraints on properties of dark energy and cosmology over the next decade., Comment: 8 pages, 2 figures; v3 matches version accepted by PRL

Published
2019

18. Multimodal Single-Cell Analysis Reveals Physiological Maturation in the Developing Human Neocortex

Author

Diane Jung, Carlos E. Cunha, Georgia Panagiotakos, Nils Lovegren, Andreas Mayer, Anne A. Leyrat, Jay A. A. West, Michael L. Gonzales, Arturo Alvarez-Buylla, Lukasz Szpankowski, Tomasz J. Nowakowski, Beatriz Alvarado, Dmitry Velmeshev, Jiadong Chen, Simone Mayer, Ugomma C. Eze, Arnold R. Kriegstein, Emmy Li, Mercedes F. Paredes, Shaohui Wang, Aparna Bhaduri, Arpana Arjun, and Alex A. Pollen

Subjects
0301 basic medicine, radial glia, Neocortex, Transcriptome, Mice, radial glia scaffold, Substance Misuse, 0302 clinical medicine, Single-cell analysis, 5-HT2A, Psychology, Receptor, Serotonin, 5-HT2A, Developmental, Pediatric, General Neuroscience, Neurogenesis, Gene Expression Regulation, Developmental, Brain, differentiation, Cell biology, calcium imaging, medicine.anatomical_structure, Stem Cell Research - Nonembryonic - Non-Human, Cognitive Sciences, Single-Cell Analysis, Sequence Analysis, Receptor, neurotransmitter, Cell type, Serotonin, human neocortical development, 1.1 Normal biological development and functioning, Ependymoglial Cells, Biology, Article, single-cell RNA sequencing, 03 medical and health sciences, Calcium imaging, Neurotransmitter receptor, Underpinning research, medicine, Animals, Humans, Cell Lineage, Progenitor cell, Neurology & Neurosurgery, Sequence Analysis, RNA, Gene Expression Profiling, intermediate progenitor cells, Neurosciences, Stem Cell Research, 030104 developmental biology, Gene Expression Regulation, RNA, Calcium, 030217 neurology & neurosurgery
Abstract

In the developing human neocortex, progenitor cells generate diverse cell types prenatally. Progenitor cells and newborn neurons respond to signaling cues, including neurotransmitters. While single-cell RNA sequencing has revealed cellular diversity, physiological heterogeneity has yet to be mapped onto these developing and diverse cell types. By combining measurements of intracellular Ca2+ elevations in response to neurotransmitter receptor agonists and RNA sequencing of the same single cells, we show that Ca2+ responses are cell-type-specific and change dynamically with lineage progression. Physiological response properties predict molecular cell identity and additionally reveal diversitynot captured by single-cell transcriptomics. We find that the serotonin receptor HTR2A selectively activates radial glia cells in the developing human, butnot mouse, neocortex, and inhibiting HTR2A receptorsin human radial glia disrupts the radial glial scaffold. We show highly specific neurotransmittersignaling during neurogenesis in the developing human neocortex and highlight evolutionarilydivergent mechanisms of physiological signaling.

Published
2019

19. Mass calibration of optically selected DES clusters using a measurement of CMB-cluster lensing with SPTpol data

Author

John E. Carlstrom, D. L. Burke, A. E. Evrard, Juan Garcia-Bellido, E. Bertin, T. L. Chou, J. Hubmayr, D. Rapetti, G. Gutierrez, Robert I. Citron, M. E.C. Swanson, Jeff McMahon, J. Gschwend, Flavia Sobreira, J. D. Hrubes, N. Huang, Jason W. Henning, S. Serrano, N. L. Harrington, S. Allam, Robert A. Gruendl, K. Honscheid, Joaquin Vieira, Adrian T. Lee, Lloyd Knox, Daniel Gruen, A. A. Plazas, I. Sevilla-Noarbe, Yanxi Zhang, Michael Schubnell, Peter Melchior, T. de Haan, Tianjun Li, J. Carretero, Peter A. R. Ade, Bradford Benson, Amy N. Bender, B. Flaugher, K. T. Story, C. L. Davis, V. Scarpine, L. E. Bleem, Srinivasan Raghunathan, H. C. Chiang, Keith Bechtol, Christian L. Reichardt, K. K. Schaffer, Felipe Menanteau, Valentine Novosad, Graeme Smecher, Ramon Miquel, P. Doel, Gregory Tarle, T. Jeltema, C. L. Chang, David J. James, J. P. Dietrich, Benjamin Saliwanchik, R. C. Smith, W. G. Hartley, Federico Bianchini, Gensheng Wang, Ben Hoyle, Gilbert Holder, Nathan Whitehorn, D. L. Hollowood, Pablo Fosalba, John P. Nibarger, Andrew Nadolski, Gene C. Hilton, K. Vanderlinde, David Brooks, Elizabeth George, M. A. G. Maia, C. J. Miller, A. K. Romer, Jason Gallicchio, T. Natoli, T. M. Crawford, E. J. Baxter, A. Carnero Rosell, J. E. Ruhl, Carole Tucker, Enrique Gaztanaga, Joshua Montgomery, H-M. Cho, N. W. Halverson, András Kovács, J. De Vicente, A. G. Kim, E. Suchyta, Antony A. Stark, M. A. Dobbs, Salcedo Romero de Ávila, C. Pryke, Stephen Padin, Marcos Lima, J. A. Beall, S. S. Meyer, M. Carrasco Kind, Nikhel Gupta, T. McClintock, N. Kuropatkin, J. T. Sayre, T. N. Varga, L. N. da Costa, E. Rozo, J. Annis, J. E. Austermann, Joshua A. Frieman, Z. Hou, Kyler Kuehn, Jennifer L. Marshall, Daniel Thomas, Marcelle Soares-Santos, W. B. Everett, S. Patil, Carlos E. Cunha, A. T. Crites, S. Desai, T. F. Eifler, T. M. C. Abbott, E. J. Sanchez, Kent D. Irwin, Lindsey Bleem, L. M. Mocanu, H. T. Diehl, W. L. K. Wu, W. L. Holzapfel, Gary Bernstein, A. J. Gilbert, Adam Anderson, 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), 010504 meteorology & atmospheric sciences, Cosmic microwave background, FOS: Physical sciences, Flux, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), gravitational lensing: weak, weak [gravitational lensing], 0103 physical sciences, Cluster (physics), clusters: general [galaxies], 010303 astronomy & astrophysics, STFC, Galaxy cluster, QC, 0105 earth and related environmental sciences, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Estimator, Astronomy and Astrophysics, Galaxy, Space and Planetary Science, galaxies: clusters: general, astro-ph.CO, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use cosmic microwave background (CMB) temperature maps from the 500 deg$^{2}$ SPTpol survey to measure the stacked lensing convergence of galaxy clusters from the Dark Energy Survey (DES) Year-3 redMaPPer (RM) cluster catalog. The lensing signal is extracted through a modified quadratic estimator designed to be unbiased by the thermal Sunyaev-Zel{'}dovich (tSZ) effect. The modified estimator uses a tSZ-free map, constructed from the SPTpol 95 and 150 GHz datasets, to estimate the background CMB gradient. For lensing reconstruction, we employ two versions of the RM catalog: a flux-limited sample containing 4003 clusters and a volume-limited sample with 1741 clusters. We detect lensing at a significance of 8.7$\sigma$(6.7$\sigma$) with the flux(volume)-limited sample. By modeling the reconstructed convergence using the Navarro-Frenk-White profile, we find the average lensing masses to be $M_{200m}$ = ($1.62^{+0.32}_{-0.25}$ [stat.] $\pm$ 0.04 [sys.]) and ($1.28^{+0.14}_{-0.18}$ [stat.] $\pm$ 0.03 [sys.]) $\times\ 10^{14}\ M_{\odot}$ for the volume- and flux-limited samples respectively. The systematic error budget is much smaller than the statistical uncertainty and is dominated by the uncertainties in the RM cluster centroids. We use the volume-limited sample to calibrate the normalization of the mass-richness scaling relation, and find a result consistent with the galaxy weak-lensing measurements from DES (Mcclintock et al. 2018)., Comment: 19 pages, 6 figures, published in ApJ

Published
2019

20. Astrometry and Occultation predictions to Trans-Neptunian and Centaur Objects observed within the Dark Energy Survey

Author

V. Scarpine, Juan de Vicente, Marcelo Assafin, J. Carretero, Flavia Sobreira, Alex Drlica Wagner, S. Serrano, Nikolay Kuropatkin, E. Suchyta, Tim Abbot, Mathew Smith, I. Sevilla, Aurelio Carnero Rossell, Rodney S. Gomes, Josh Frieman, A. A. Plazas, G. Gutierrez, Josselin Desmars, Julio Camargo, Enrique Gaztanaga, Roberto Vieira-Martins, M. A. G. Maia, Juan Garcia-Bellido, Matias Carrasco Kind, Ramon Miquel, E. Buckley-Geer, Luiz N. da Costa, Emmanuel Bertin, Ricardo L. C. Ogando, D. L. Burke, Michael Schubnell, David J. James, David J. Brooks, J. Gschwend, S. Avila, Gary Bernstein, S. Allam, Robert A. Gruendl, Matheus Gysi, Felipe Menanteau, Pablo Fosalba, Molly E. C. Swanson, Christopher J. Davis, Will G. Hartley, Marcelle Soares-Santos, Devon L. Hollowood, Martin Banda-Huarca, Filipe B. Abdalla, Gregory Tarle, Daniel Gruen, Felipe Braga Ribas, D. W. Gerdes, Peter Doel, Thomas Diehl, K. Honscheid, Christopher J. Miller, S. Hamilton, William Wester, Kyler Kuehn, Carlos E. Cunha, E. J. Sanchez, K. Romer, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Solar System, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Large Synoptic Survey Telescope, 01 natural sciences, Occultation, surveys, 0103 physical sciences, occultations, ephemerides, 010303 astronomy & astrophysics, QC, STFC, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy, RCUK, Astronomy and Astrophysics, Centaur, Astrometry, Albedo, Photometry (astronomy), Space and Planetary Science, Sky, astro-ph.EP, astrometry, Kuiper belt: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

Transneptunian objects (TNOs) are a source of invaluable information to access the history and evolution of the outer solar system. However, observing these faint objects is a difficult task. As a consequence, important properties such as size and albedo are known for only a small fraction of them. Now, with the results from deep sky surveys and the Gaia space mission, a new exciting era is within reach as accurate predictions of stellar occultations by numerous distant small solar system bodies become available. From them, diameters with kilometer accuracies can be determined. Albedos, in turn, can be obtained from diameters and absolute magnitudes. We use observations from the Dark Energy Survey (DES) from November 2012 until February 2016, amounting to 4292847 CCD frames. We searched them for all known small solar system bodies and recovered a total of 202 TNOs and Centaurs, 63 of which have been discovered by the DES collaboration until the date of this writing. Their positions were determined using the Gaia Data Release 2 as reference and their orbits were refined. Stellar occultations were then predicted using these refined orbits plus stellar positions from Gaia. These predictions are maintained, and updated, in a dedicated web service. The techniques developed here are also part of an ambitious preparation to use the data from the Large Synoptic Survey Telescope (LSST), that expects to obtain accurate positions and multifilter photometry for tens of thousands of TNOs., 25 pages, submitted to Astronomical Journal

Published
2019

21. Dark Energy Survey Year 1 results: Validation of weak lensing cluster member contamination estimates from P(z) decomposition

Author

M. Carrasco Kind, Marcos Lima, Enrique Gaztanaga, Joshua A. Frieman, Douglas L. Tucker, J. DeRose, Kyler Kuehn, D. L. Burke, Peter Doel, A. Carnero Rosell, I. Sevilla-Noarbe, H. T. Diehl, N. Kuropatkin, Daniel Thomas, E. Buckley-Geer, Robert A. Gruendl, Michael Schubnell, Melanie Simet, T. N. Varga, L. N. da Costa, A. K. Romer, David Brooks, M. E. C. Swanson, A. A. Plazas, K. Honscheid, J. Carretero, E. J. Sanchez, J. P. Dietrich, Juan Garcia-Bellido, David J. James, B. Flaugher, Pablo Fosalba, G. Gutierrez, Eli S. Rykoff, Eduardo Rozo, J. Annis, Thomas McClintock, Stella Seitz, Daniel Gruen, A. von der Linden, Tesla E. Jeltema, W. G. Hartley, J. De Vicente, V. Scarpine, Devon L. Hollowood, S. Serrano, E. Suchyta, August E. Evrard, Jennifer L. Marshall, C. B. D'Andrea, Shantanu Desai, D. W. Gerdes, Mathew Smith, Felipe Menanteau, Gregory Tarle, Christopher J. Miller, Yanxi Zhang, M. Costanzi, Ramon Miquel, Santiago Avila, Carlos E. Cunha, M. A. G. Maia, Risa H. Wechsler, Niall MacCrann, E. Bertin, J. Gschwend, Flavia Sobreira, M. March, R. L. C. Ogando, Peter Melchior, Ben Hoyle, 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, Varga, T. N., Derose, J., Gruen, D., Mcclintock, T., Seitz, S., Rozo, E., Costanzi, M., Hoyle, B., Maccrann, N., Plazas, A. A., Rykoff, E. S., Simet, M., Von Der Linden, A., Wechsler, R. H., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cunha, C. E., D'Andrea, C. B., Da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Romer, A. K., 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., and Zhang, Y.

Subjects
High energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, gravitational lensing: weak, Clusters: General [Galaxies], 0103 physical sciences, media_common.cataloged_instance, European union, Observation [Cosmology], 010303 astronomy & astrophysics, STFC, QC, media_common, Physics, 010308 nuclear & particles physics, business.industry, European research, RCUK, Astronomy and Astrophysics, observations [cosmology], Cosmology: Observations, Galaxies: Clusters: General, Gravitational lensing: weak, 13. Climate action, Space and Planetary Science, Research council, galaxies: clusters: general, cosmology: observations, Fundamental physics, Christian ministry, CLUSTERS, weak [Gravitational lensing], business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Weak lensing source galaxy catalogs used in estimating the masses of galaxy clusters can be heavily contaminated by cluster members, prohibiting accurate mass calibration. In this study we test the performance of an estimator for the extent of cluster member contamination based on decomposing the photometric redshift $P(z)$ of source galaxies into contaminating and background components. We perform a full scale mock analysis on a simulated sky survey approximately mirroring the observational properties of the Dark Energy Survey Year One observations (DES Y1), and find excellent agreement between the true number profile of contaminating cluster member galaxies in the simulation and the estimated one. We further apply the method to estimate the cluster member contamination for the DES Y1 redMaPPer cluster mass calibration analysis, and compare the results to an alternative approach based on the angular correlation of weak lensing source galaxies. We find indications that the correlation based estimates are biased by the selection of the weak lensing sources in the cluster vicinity, which does not strongly impact the $P(z)$ decomposition method. Collectively, these benchmarks demonstrate the strength of the $P(z)$ decomposition method in alleviating membership contamination and enabling highly accurate cluster weak lensing studies without broad exclusion of source galaxies, thereby improving the total constraining power of cluster mass calibration via weak lensing., Comment: 14 pages, 8 figures; submitted to MNNRAS

Published
2019

22. First Cosmology Results Using SNe Ia from the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation

Author

Samuel Hinton, Antonella Palmese, K. Kuehn, G. Gutierrez, Vinu Vikram, M. A. G. Maia, Bonnie Zhang, Daniel B. Thomas, Felipe Menanteau, R. G. Sharp, Marcos Lima, B. Flaugher, Daniel Muthukrishna, Geraint F. Lewis, Alexei V. Filippenko, M. N. K. Smith, Alex Drlica-Wagner, P. Challis, J. Calcino, David J. James, Jacobo Asorey, R. C. Smith, A. G. Kim, A. Clocchiatti, A. Roodman, P. Fosalba, K. Honscheid, T. Jeltema, Michael Schubnell, C. B. D'Andrea, S. E. Kuhlmann, V. Scarpine, Daniel Scolnic, Per Kragh Andersen, Karl Glazebrook, Josh Frieman, E. S. Rykoff, J. Annis, P. E. Nugent, W. C. Wester, P. Martini, Douglas L. Tucker, Y.-H. Zhang, Lluís Galbany, David J. Brooks, Kaisey S. Mandel, Ben Hoyle, Carlos E. Cunha, Edward Macaulay, Vivian Miranda, Bruce A. Bassett, Elisabeth Krause, R. P. Kirshner, G. Tarle, Ryan J. Foley, Jennifer L. Marshall, C. L. Davis, O. Lahav, A. Carnero Rosell, S. Desai, E. Kasai, Ramon Miquel, D. J. Brout, Tianjun Li, D. L. Burke, J. Carretero, Daniel Gruen, H. T. Diehl, Tamara M. Davis, J. P. Marriner, Darren L. DePoy, Matt J. Jarvis, R. R. Gupta, Juan Garcia-Bellido, T. F. Eifler, W. G. Hartley, F. J. Castander, S. Allam, Robert A. Gruendl, A. A. Plazas, Daniela Carollo, T. M. C. Abbott, Gary Bernstein, E. Morganson, Arturo Avelino, E. Suchyta, N. E. Sommer, B. E. Tucker, Enrique J. Fernández, E. J. Sanchez, C. Lidman, P. Doel, M. Sako, C. J. Miller, E. Swann, D. L. Hollowood, S. Serrano, M. E. C. Swanson, M. J. Childress, Richard Kessler, Anais Möller, E. Bertin, Troxel, I. Sevilla-Noarbe, L. N. da Costa, Flavia Sobreira, Salcedo Romero de Ávila, Juan Estrada, Alistair R. Walker, R. C. Thomas, Marcelle Soares-Santos, M. March, Basilio X. Santiago, Mark Sullivan, J. De Vicente, M. Carrasco Kind, Robert C. Nichol, S. A. Uddin, J. Lasker, R. L. C. Ogando, Keith Bechtol, J. K. Hoormann, A. K. Romer, Peter Brown, and Yen-Chen Pan

Subjects
010504 meteorology & atmospheric sciences, Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Cosmology, symbols.namesake, 0103 physical sciences, cosmological parameters, Planck, dark energy, 010303 astronomy & astrophysics, QC, STFC, 0105 earth and related environmental sciences, Physics, Organic Chemistry, RCUK, Astronomy and Astrophysics, Redshift, Galaxy, Supernova, 13. Climate action, Space and Planetary Science, astro-ph.CO, Dark energy, symbols, Supernova Legacy Survey, CLUSTERS, general [supernovae], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

© 2019. The American Astronomical Society. All rights reserved.. We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017 < z < 0.849. We combine the DES-SN sample with an external sample of 122 low-redshift (z < 0.1) SNe Ia, resulting in a "DES-SN3YR" sample of 329 SNe Ia. Our cosmological analyses are blinded: after combining our DES-SN3YR distances with constraints from the Cosmic Microwave Background, our uncertainties in the measurement of the dark energy equation-of-state parameter, w, are 0.042 (stat) and 0.059 (stat+syst) at 68% confidence. We provide a detailed systematic uncertainty budget, which has nearly equal contributions from photometric calibration, astrophysical bias corrections, and instrumental bias corrections. We also include several new sources of systematic uncertainty. While our sample is less than one-third the size of the Pantheon sample, our constraints on w are only larger by 1.4×, showing the impact of the DES-SN Ia light-curve quality. We find that the traditional stretch and color standardization parameters of the DES-SNe Ia are in agreement with earlier SN Ia samples such as Pan-STARRS1 and the Supernova Legacy Survey. However, we find smaller intrinsic scatter about the Hubble diagram (0.077 mag). Interestingly, we find no evidence for a Hubble residual step (0.007 ± 0.018 mag) as a function of host-galaxy mass for the DES subset, in 2.4σ tension with previous measurements. We also present novel validation methods of our sample using simulated SNe Ia inserted in DECam images and using large catalog-level simulations to test for biases in our analysis pipelines.

Published
2019

23. Measurement of the splashback feature around SZ-selected Galaxy clusters with DES, SPT, and ACT

Author

Ofer Lahav, J. Carretero, David Brooks, M. Smith, R. C. Smith, B. Flaugher, Risa H. Wechsler, J. Gschwend, Daniel Gruen, Marcelle Soares-Santos, A. E. Evrard, T. N. Varga, Marcos Lima, Lindsey Bleem, J. P. Dietrich, L. N. da Costa, T. M. Crawford, Laura Newburgh, Jeff McMahon, D. W. Gerdes, David J. James, M. E.C. Swanson, Edward J. Wollack, K. Honscheid, V. Scarpine, L. A. Page, J. C. Hill, Z. Zhang, Antony A. Stark, Pablo Fosalba, Michael D. Niemack, K. Bechtol, Eli S. Rykoff, Federico Nati, Chihway Chang, A. K. Romer, Sebastian Bocquet, Carlos E. Cunha, G. Gutierrez, Eric J. Baxter, Simone Aiola, M. A. G. Maia, George Stein, Suzanne T. Staggs, Jennifer L. Marshall, C. J. Miller, Nick Battaglia, Ramon Miquel, P. Doel, John E. Carlstrom, R. H. Schindler, Mathew S. Madhavacheril, Tim Eifler, Mark J. Devlin, Patricio A. Gallardo, Shantanu Desai, F. J. Castander, S. Patil, Zhilei Xu, Felipe Menanteau, Andrey V. Kravtsov, A. G. Kim, Steve K. Choi, Sigurd Naess, Loïc Maurin, Megan Gralla, Ricardo L. C. Ogando, Thomas McClintock, Gregory Tarle, Nikhel Gupta, A. Carnero Rosell, Ben Hoyle, E. J. Sanchez, S. P. Ho, Kevin M. Huffenberger, Flavia Sobreira, Elisabeth Krause, B. Partridge, S. Adhikari, Tesla E. Jeltema, Christian L. Reichardt, Juan Garcia-Bellido, E. Bertin, Bradford Benson, J. DeRose, E. Suchyta, Eduardo Rozo, Matt Hilton, D. L. Hollowood, S. Serrano, D. L. Burke, A. van Engelen, J. De Vicente, Kyler Kuehn, S. Allam, Robert A. Gruendl, Daniel Thomas, E. Buckley-Geer, Jo Dunkley, Joseph J. Mohr, John P. Hughes, A. A. Plazas, W. G. Hartley, T. Shin, Bhuvnesh Jain, J. R. Bond, M. Carrasco Kind, David Rapetti, Enrique Gaztanaga, Hao-Yi Wu, Mark Brodwin, Shin, T, Adhikari, S, Baxter, E, Chang, C, Jain, B, Battaglia, N, Bleem, L, Bocquet, S, Derose, J, Gruen, D, Hilton, M, Kravtsov, A, Mcclintock, T, Rozo, E, Rykoff, E, Varga, T, Wechsler, R, Wu, H, Zhang, Z, Aiola, S, Allam, S, Bechtol, K, Benson, B, Bertin, E, Bond, J, Brodwin, M, Brooks, D, Buckley-Geer, E, Burke, D, Carlstrom, J, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, S, Cunha, C, Crawford, T, Da Costa, L, De Vicente, J, Desai, S, Devlin, M, Dietrich, J, Doel, P, Dunkley, J, Eifler, T, Evrard, A, Flaugher, B, Fosalba, P, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Gerdes, D, Gralla, M, Gruendl, R, Gschwend, J, Gupta, N, Gutierrez, G, Hartley, W, Hill, J, Ho, S, Hollowood, D, Honscheid, K, Hoyle, B, Huffenberger, K, Hughes, J, James, D, Jeltema, T, Kim, A, Krause, E, Kuehn, K, Lahav, O, Lima, M, Madhavacheril, M, Maia, M, Marshall, J, Maurin, L, Mcmahon, J, Menanteau, F, Miller, C, Miquel, R, Mohr, J, Naess, S, Nati, F, Newburgh, L, Niemack, M, Ogando, R, Page, L, Partridge, B, Patil, S, Plazas, A, Rapetti, D, Reichardt, C, Romer, A, Sanchez, E, Scarpine, V, Schindler, R, Serrano, S, Smith, M, Smith, R, Soares-Santos, M, Sobreira, F, Staggs, S, Stark, A, Stein, G, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, Van Engelen, A, Wollack, E, Xu, Z, 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, ACT, and SPT

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, Cosmology: observation, Cosmology, 0103 physical sciences, Cluster (physics), observations [Cosmology], 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, STFC, QB, Physics, 010308 nuclear & particles physics, RCUK, Galaxies: evolution, Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, South Pole Telescope, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, Atacama Cosmology Telescope, Halo, Galaxies: clusters: general, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a detection of the splashback feature around galaxy clusters selected using their Sunyaev-Zel'dovich (SZ) signal. Recent measurements of the splashback feature around optically selected galaxy clusters have found that the splashback radius, $r_{\rm sp}$, is smaller than predicted by N-body simulations. A possible explanation for this discrepancy is that $r_{\rm sp}$ inferred from the observed radial distribution of galaxies is affected by selection effects related to the optical cluster-finding algorithms. We test this possibility by measuring the splashback feature in clusters selected via the SZ effect in data from the South Pole Telescope SZ survey and the Atacama Cosmology Telescope Polarimeter survey. The measurement is accomplished by correlating these clusters with galaxies detected in the Dark Energy Survey Year 3 data. The SZ observable used to select clusters in this analysis is expected to have a tighter correlation with halo mass and to be more immune to projection effects and aperture-induced biases than optically selected clusters. We find that the measured $r_{\rm sp}$ for SZ-selected clusters is consistent with the expectations from simulations, although the small number of SZ-selected clusters makes a precise comparison difficult. In agreement with previous work, when using optically selected redMaPPer clusters, $r_{\rm sp}$ is $\sim$ $2\sigma$ smaller than in the simulations. These results motivate detailed investigations of selection biases in optically selected cluster catalogs and exploration of the splashback feature around larger samples of SZ-selected clusters. Additionally, we investigate trends in the galaxy profile and splashback feature as a function of galaxy color, finding that blue galaxies have profiles close to a power law with no discernible splashback feature, which is consistent with them being on their first infall into the cluster., Comment: 17 pages, 13 figures, published in MNRAS

Published
2019

24. Methods for cluster cosmology and application to the SDSS in preparation for DES Year 1 release

Author

G. Gutierrez, Melanie Simet, Marcos Lima, Xi Chen, A. Roodman, David J. James, Sunayana Bhargava, Tommaso Giannantonio, Pablo Fosalba, K. Bechtol, Eli S. Rykoff, M. Smith, Jennifer L. Marshall, A. A. Plazas, Christopher J. Miller, Daniel Gruen, A. Bermeo-Hernandez, Yanxi Zhang, M. E. C. Swanson, Tim Eifler, Arya Farahi, Huan Lin, Martin Crocce, J. Carretero, Santiago Avila, Filipe B. Abdalla, J. De Vicente, Marcelle Soares-Santos, Carlos E. Cunha, Peter Doel, Elisabeth Krause, J. P. Dietrich, Juan Garcia-Bellido, A. von der Linden, A. Carnero Rosell, J. DeRose, Flavia Sobreira, H. T. Diehl, Rafe Schindler, David J. Brooks, Joshua A. Frieman, Tesla E. Jeltema, D. W. Gerdes, Eduardo Rozo, I. Sevilla-Noarbe, R. L. C. Ogando, Ramon Miquel, V. Scarpine, W. G. Hartley, T. McClintock, C. Davis, N. Kuropatkin, T. N. Varga, J. Gschwend, M. March, Devon L. Hollowood, S. Serrano, Adam Mantz, L. N. da Costa, Daniel Thomas, E. Buckley-Geer, Enrique Gaztanaga, E. Suchyta, S. W. Allen, Risa H. Wechsler, D. L. Burke, Jochen Weller, M. Carrasco Kind, Kyler Kuehn, T. M. C. Abbott, Robert A. Gruendl, E. J. Sanchez, Ben Hoyle, Paul Giles, M. A. G. Maia, M. Costanzi, B. Flaugher, A. K. Romer, Paul Martini, Joseph J. Mohr, Juan Estrada, Michael Schubnell, K. Honscheid, Erin Sheldon, Felipe Menanteau, G. Tarle, August E. Evrard, Costanzi, M., Rozo, E., Simet, M., Zhang, Y., Evrard, A. E., Mantz, A., Rykoff, E. S., Jeltema, T., Gruen, D., Allen, S., Mcclintock, T., Romer, A. K., von der Linden, A., Farahi, A., Derose, J., Varga, T. N., Weller, J., Giles, P., Hollowood, D. L., Bhargava, S., Bermeo-Hernandez, A., Chen, X., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., de Vicente, J., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., Hoyle, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Wechsler, R. H.

Subjects
Cosmological parameter, Large-scale structure of Universe, Cosmological parameters, Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, clusters: general [Galaxies], 01 natural sciences, 7. Clean energy, Cosmology, symbols.namesake, Nucleosynthesis, 0103 physical sciences, Planck, 010303 astronomy & astrophysics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, QC, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies: clusters: general, Redshift, Baryon, 13. Climate action, Space and Planetary Science, symbols, Dark energy, Neutrino, CLUSTERS
Abstract

We perform the first blind analysis of cluster abundance data. Specifically, we derive cosmological constraints from the abundance and weak-lensing signal of \redmapper\ clusters of richness $\lambda\geq 20$ in the redshift range $z\in[0.1,0.3]$ as measured in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness--mass relation of the clusters. For a flat $\Lambda$CDM cosmological model with massive neutrinos, we find $S_8 \equiv \sigma_{8}(\Omega_m/0.3)^{0.5}=0.79^{+0.05}_{-0.04}$. This value is both consistent and competitive with that derived from cluster catalogues selected in different wavelengths. Our result is also consistent with the combined probes analyses by the Dark Energy Survey (DES) and the Kilo-Degree Survey (KiDS), and with the Cosmic Microwave Background (CMB) anisotropies as measured by \planck. We demonstrate that the cosmological posteriors are robust against variation of the richness--mass relation model and to systematics associated with the calibration of the selection function. In combination with Baryon Acoustic Oscillation (BAO) data and Big-Bang Nucleosynthesis (BBN) data, we constrain the Hubble rate to be $h=0.66\pm 0.02$, independent of the CMB. Future work aimed at improving our understanding of the scatter of the richness--mass relation has the potential to significantly improve the precision of our cosmological posteriors. The methods described in this work were developed for use in the forthcoming analysis of cluster abundances in the DES. Our SDSS analysis constitutes the first part of a staged-unblinding analysis of the full DES data set.

Published
2019

25. Identification of RR Lyrae stars in multiband, sparsely-sampled data from the Dark Energy Survey using template fitting and Random Forest classification

Author

A. H. Riley, P. S. Ferguson, J. L. Myron, B. Yanny, I. Sevilla-Noarbe, G. Gutierrez, N. Kuropatkin, A. K. Vivas, E. S. Rykoff, P. Doel, L. N. da Costa, Juan Garcia-Bellido, Michael Schubnell, Jennifer L. Marshall, L. Plybon, Daniel Thomas, E. Buckley-Geer, J. F. Maner, M. E. C. Swanson, James P. Long, Peter Melchior, Alex Drlica-Wagner, Alistair R. Walker, Marcelle Soares-Santos, R. C. Smith, Joshua A. Frieman, E. Morganson, S. A. Cantu, D. L. Hollowood, J. Annis, S. Serrano, K. Bechtol, Ricardo L. C. Ogando, Flavia Sobreira, David J. James, Ben Hoyle, Eric H. Neilsen, A. Carnero Rosell, A. A. Plazas, Basilio X. Santiago, C. E. Martínez-Vázquez, J. De Vicente, Louis E. Strigari, Vinu Vikram, C. B. D'Andrea, Douglas L. Tucker, Kyler Kuehn, W. G. Hartley, Douglas Burke, E. Suchyta, V. Scarpine, K. M. Stringer, Ramon Miquel, Z. Lin, Lucas M. Macri, Dylan Hatt, David J. Brooks, G. Tarle, T. F. Eifler, Daniel Gruen, T. M. C. Abbott, Arya Farahi, Enrique Gaztanaga, F. Paz-Chinchón, S. Allam, Christopher Nielsen, Andrew B. Pace, J. Gschwend, E. J. Sanchez, Ethan O. Nadler, M. Carrasco Kind, Tenglin Li, E. Bertin, Carlos E. Cunha, B. Flaugher, M. N. K. Smith, S. Desai, J. Carretero, 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
stars: variables: RR Lyrae, Milky Way, FOS: Physical sciences, Astrophysics, RR Lyrae variable, 01 natural sciences, Galactic halo, 0103 physical sciences, structure [galaxy], Satellite galaxy, 010303 astronomy & astrophysics, Galaxy: structure, Solar and Stellar Astrophysics (astro-ph.SR), Physics, methods: statistical, 010308 nuclear & particles physics, variable stars: RR Lyrae [stars], Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy: halo, Stars, halo [galaxy], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, Variable star, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract

Many studies have shown that RR Lyrae variable stars (RRL) are powerful stellar tracers of Galactic halo structure and satellite galaxies. The Dark Energy Survey (DES), with its deep and wide coverage (g ~ 23.5 mag) in a single exposure; over 5000 deg$^{2}$) provides a rich opportunity to search for substructures out to the edge of the Milky Way halo. However, the sparse and unevenly sampled multiband light curves from the DES wide-field survey (median 4 observations in each of grizY over the first three years) pose a challenge for traditional techniques used to detect RRL. We present an empirically motivated and computationally efficient template fitting method to identify these variable stars using three years of DES data. When tested on DES light curves of previously classified objects in SDSS stripe 82, our algorithm recovers 89% of RRL periods to within 1% of their true value with 85% purity and 76% completeness. Using this method, we identify 5783 RRL candidates, ~31% of which are previously undiscovered. This method will be useful for identifying RRL in other sparse multiband data sets., 34 pages, 21 figures. Accepted for publication in AJ. Data products are available at https://des.ncsa.illinois.edu/releases/other/y3-rrl

Published
2019

26. Cosmological lensing ratios with DES Y1, SPT and Planck

Author

M. A. G. Maia, Shantanu Desai, C. L. Chang, J. D. Hrubes, J. De Vicente, Erik Shirokoff, Antony A. Stark, A. Alarcon, H. T. Diehl, Erin Sheldon, David Brooks, David Bacon, M. E. C. Swanson, Andrina Nicola, Alistair R. Walker, Markus Rau, Marcelle Soares-Santos, T. Natoli, N. W. Halverson, Niall MacCrann, Y. Omori, J. E. Ruhl, Flavia Sobreira, David J. James, H-M. Cho, Pablo Fosalba, K. Vanderlinde, Marcos Lima, Kyler Kuehn, Ben Hoyle, Joseph J. Mohr, M. A. Dobbs, E. Suchyta, E. M. Leitch, O. Friedrich, M. Smith, Adrian T. Lee, Lloyd Knox, Daniel Gruen, Vinu Vikram, August E. Evrard, Jennifer L. Marshall, Filipe B. Abdalla, M. Gatti, Richard G. Kron, J. Prat, J. P. Dietrich, Juan Garcia-Bellido, I. Sevilla-Noarbe, S. S. Meyer, Peter Melchior, R. Cawthon, K. T. Story, N. L. Harrington, Robert A. Gruendl, G. Gutierrez, C. Pryke, B. Flaugher, L. M. Mocanu, G. Simard, D. W. Gerdes, Tesla E. Jeltema, G. P. Holder, Daniel Thomas, Bhuvnesh Jain, Michael Troxel, Christian L. Reichardt, J. Carretero, Matt J. Jarvis, T. de Haan, Z. Hou, P. Vielzeuf, Bradford Benson, Tim Eifler, V. Scarpine, T. M. Crawford, J. Annis, C. J. Miller, Daniel P. Marrone, E. Bertin, R. Williamson, C. Davis, N. Kuropatkin, J. T. Sayre, M. Carrasco Kind, L. N. da Costa, R. Chown, A. Pujol, Ofer Lahav, K. Aylor, K. K. Schaffer, J. Gschwend, Gary Bernstein, A. K. Romer, D. Luong-Van, W. B. Everett, Enrique Gaztanaga, Elisabeth Krause, Ramon Miquel, P. Doel, S. Serrano, Jochen Weller, W. L. Holzapfel, C. Sánchez, T. M. C. Abbott, E. J. Sanchez, Scott Dodelson, Santiago Avila, Chihway Chang, Carlos E. Cunha, A. T. Crites, Joe Zuntz, B. Mawdsley, Lindsey Bleem, A. Manzotti, Z. K. Staniszewski, W. G. Hartley, S. Samuroff, T. Shin, Stephen Padin, A. Roodman, Tommaso Giannantonio, Felipe Menanteau, A. A. Plazas, Oliver Zahn, Gregory Tarle, Joaquin Vieira, Eli S. Rykoff, D. L. Burke, John E. Carlstrom, Eric J. Baxter, Jeff McMahon, K. Honscheid, Elizabeth George, 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, gravitational lensing: weak, 0103 physical sciences, LENTES GRAVITACIONAIS, Planck, cosmological parameters, 010303 astronomy & astrophysics, QC, Photometric redshift, Physics, 010308 nuclear & particles physics, Matter power spectrum, Astronomy and Astrophysics, Galaxy, South Pole Telescope, Gravitational lens, Space and Planetary Science, cosmology: observations, Dark energy, symbols, astro-ph.CO, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Correlations between tracers of the matter density field and gravitational lensing are sensitive to the evolution of the matter power spectrum and the expansion rate across cosmic time. Appropriately defined ratios of such correlation functions, on the other hand, depend only on the angular diameter distances to the tracer objects and to the gravitational lensing source planes. Because of their simple cosmological dependence, such ratios can exploit available signal-to-noise down to small angular scales, even where directly modeling the correlation functions is difficult. We present a measurement of lensing ratios using galaxy position and lensing data from the Dark Energy Survey, and CMB lensing data from the South Pole Telescope and Planck, obtaining the highest precision lensing ratio measurements to date. Relative to the concordance $\Lambda$CDM model, we find a best fit lensing ratio amplitude of $A = 1.1 \pm 0.1$. We use the ratio measurements to generate cosmological constraints, focusing on the curvature parameter. We demonstrate that photometrically selected galaxies can be used to measure lensing ratios, and argue that future lensing ratio measurements with data from a combination of LSST and Stage-4 CMB experiments can be used to place interesting cosmological constraints, even after considering the systematic uncertainties associated with photometric redshift and galaxy shear estimation., Comment: 17 pages, 11 figures

Published
2019

27. A new RASS galaxy cluster catalogue with low contamination extending to $z\sim1$ in the DES overlap region

Author

M. A. G. Maia, Kyler Kuehn, J. Annis, Paul Giles, Ben Hoyle, G. Tarle, August E. Evrard, Marcos Lima, E. Suchyta, F. J. Castander, Jennifer L. Marshall, Matthias Klein, J. Carretero, W. G. Hartley, T. M. C. Abbott, Devon L. Hollowood, J. Gschwend, David J. Brooks, C. B. D'Andrea, V. Scarpine, Daniel Thomas, E. Buckley-Geer, E. J. Sanchez, Enrique Gaztanaga, G. Gutierrez, Robert A. Gruendl, Tesla E. Jeltema, A. A. Plazas, E. Bertin, Marcelle Soares-Santos, A. Roodman, Flavia Sobreira, Rafe Schindler, S. Serrano, R. C. Smith, Peter Doel, Vinu Vikram, Joshua A. Frieman, H. T. Diehl, M. Paulus, M. March, Santiago Avila, Carlos E. Cunha, A. K. Romer, M. E. C. Swanson, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, J. De Vicente, M. Carrasco Kind, Shantanu Desai, Ramon Miquel, David J. James, Pablo Fosalba, Felipe Menanteau, Sebastian Grandis, A. Carnero Rosell, Joseph J. Mohr, K. Honscheid, R. L. C. Ogando, B. Flaugher, M. Smith, Daniel Gruen, J. P. Dietrich, Juan Garcia-Bellido, 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), Active galactic nucleus, galaxies: clusters: intracluster medium, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, ROSAT, Cluster (physics), education, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, QC, Physics, education.field_of_study, 010308 nuclear & particles physics, Halo mass function, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), galaxies: distances and redshifts, CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the MARD-Y3 catalog of between 1086 and 2171 galaxy clusters (52\% and 65\% new) produced using multi-component matched filter (MCMF) followup in 5000\,deg$^2$ of DES-Y3 optical data of the $\sim$20000 overlapping 2RXS X-ray sources. Optical counterparts are identified as peaks in galaxy richness as a function of redshift along the line of sight toward each 2RXS source within a search region informed by an X-ray prior. All peaks are assigned a probability \fcont\ of being a random superposition. The clusters lie at $0.020.5$. Residual contamination is 2.6\% and 9.6\% for the cuts adopted here. For each cluster we present the optical center, redshift, rest frame X-ray luminosity, $M_{500}$ mass, coincidence with NWAY infrared sources and estimators of dynamical state. About 2\% of MARD-Y3 clusters have multiple possible counterparts, the photo-z's are high quality with $\sigma_{\Delta z/(1+z)}=0.0046$, and $\sim$1\% of clusters exhibit evidence of X-ray luminosity boosting from emission by cluster AGN. Comparison with other catalogs (MCXC, RM, SPT-SZ, Planck) is performed to test consistency of richness, luminosity and mass estimates. We measure the MARD-Y3 X-ray luminosity function and compare it to the expectation from a fiducial cosmology and externally calibrated luminosity- and richness-mass relations. Agreement is good, providing evidence that MARD-Y3 has low contamination and can be understood as a simple two step selection-- X-ray and then optical-- of an underlying cluster population described by the halo mass function., Comment: Version accepted for publication

Published
2019

28. Dark Energy Survey Year 1 results: measurement of the galaxy angular power spectrum

Author

C. B. D'Andrea, A. K. Romer, J. Carretero, D. L. Hollowood, J. Gschwend, Rogerio Rosenfeld, I. Sevilla-Noarbe, Douglas L. Tucker, M. Smith, Kyler Kuehn, Shantanu Desai, F. Lacasa, S. Kent, Ramon Miquel, N. Kuropatkin, Marcos Lima, David J. Brooks, Donnacha Kirk, Michael Schubnell, R. C. Smith, Sarah Bridle, A. Roodman, Tommaso Giannantonio, B. Flaugher, Alistair R. Walker, Filipe B. Abdalla, Carlos E. Cunha, L. N. da Costa, Marcelle Soares-Santos, A. A. Plazas, Jennifer L. Marshall, Will J. Percival, N. Kokron, G. Tarle, D. W. Gerdes, A. Troja, E. Suchyta, August E. Evrard, K. Honscheid, F. J. Castander, David J. James, T. M. C. Abbott, M. Carrasco Kind, F. Andrade-Oliveira, Elisabeth Krause, Pablo Fosalba, K. C. Chan, E. J. Sanchez, M. E. C. Swanson, J. De Vicente, Martin Crocce, J. Annis, Ben Hoyle, R. Cawthon, Juan Garcia-Bellido, R. A. Bernstein, Joe Zuntz, Flavia Sobreira, M. W. G. Johnson, A. Carnero Rosell, Joshua A. Frieman, Daniel Thomas, E. Buckley-Geer, Salcedo Romero de Ávila, Juan Estrada, Ashley J. Ross, D. L. Burke, S. Allam, Robert A. Gruendl, Huan Lin, H. Camacho, M. D. Johnson, G. Gutierrez, E. Bertin, Peter Doel, H. T. Diehl, 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, Universidade de São Paulo (USP), Lab Interinst E Astron LIneA, Universidade Estadual Paulista (Unesp), Univ Geneva, Universidade Estadual de Campinas (UNICAMP), Observ Nacl, Univ Portsmouth, IEEC, CSIC, Ohio State Univ, Univ Autonoma Madrid, Natl Opt Astron Observ, UCL, Rhodes Univ, Fermilab Natl Accelerator Lab, Observ Carnegie Inst Washington, CNRS, UPMC Univ Paris 06, Univ Manchester, Stanford Univ, SLAC Natl Accelerator Lab, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, Univ Chicago, Univ Penn, Ctr Invest Energet Medioambientales & Tecnol CIEM, IIT Hyderabad, Univ Michigan, Univ Cambridge, Ludwig Maximilians Univ Munchen, Santa Cruz Inst Particle Phys, Max Planck Inst Extraterr Phys, Harvard Smithsonian Ctr Astrophys, Steward Observ, CALTECH, Australian Astron Observ, Texas A&M Univ, Inst Catalana Recerca & Estudis Avancats, Univ Waterloo, Perimeter Inst Theoret Phys, Univ Sussex, Univ Southampton, Brandeis Univ, Oak Ridge Natl Lab, and Univ Edinburgh

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), symbols.namesake, Goodness of fit, Robustness (computer science), 0103 physical sciences, LENTES GRAVITACIONAIS, Statistical physics, 010303 astronomy & astrophysics, STFC, QB, Physics, 010308 nuclear & particles physics, Covariance matrix, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, RCUK, Astronomy and Astrophysics, Markov chain Monte Carlo, cosmology: observations, large-scale structure of Universe, Galaxy, observations [cosmology], Space and Planetary Science, Dark energy, symbols, astro-ph.CO, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use data from the first-year (Y1) observations of the DES collaboration to measure the galaxy angular power spectrum (APS), and search for its BAO feature using a template-fitting method. We test our methodology in a sample of 1800 DES Y1-like mock catalogs. The APS is measured with the pseudo-$C_\ell$ method, using pixelized maps constructed from the mock catalogs and the DES mask. The covariance matrix of the $C_\ell$'s in these tests are also obtained from the mock catalogs. We use templates to model the measured spectra and estimate template parameters firstly from the $C_\ell$'s of the mocks using two different methods, a maximum likelihood estimator and a MCMC, finding consistent results with a good reduced $\chi^2$. Robustness tests are performed to estimate the impact of different choices of settings used in our analysis. After these tests on mocks, we apply our method to a galaxy sample constructed from DES Y1 data specifically for LSS studies. This catalog comprises galaxies within an effective area of 1318 deg$^2$ and $0.6, Comment: 13 pages, 14 figures

Published
2019

29. Dark Energy Survey Year 1 results: Detection of Intra-cluster Light at Redshift $\sim$ 0.25

Author

Chris A. Collins, Peter Doel, Marcos Lima, B. Flaugher, H. T. Diehl, Antonella Palmese, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, Michael Schubnell, M. A. G. Maia, V. Scarpine, David J. James, Felipe Menanteau, Joshua A. Frieman, Pablo Fosalba, J. P. Dietrich, Juan Garcia-Bellido, D. L. Hollowood, W. G. Hartley, J. Gschwend, S. Serrano, Flavia Sobreira, M. E. C. Swanson, Yanxi Zhang, Kyler Kuehn, C. J. Miller, Tim Eifler, Peter Melchior, K. Honscheid, W. C. Wester, Joseph J. Mohr, Brian Yanny, M. March, Shantanu Desai, M. Smith, Enrique Gaztanaga, J. Carretero, E. Bertin, Eli S. Rykoff, C. B. D'Andrea, Daniel Gruen, G. Gutierrez, A. A. Plazas, Marcelle Soares-Santos, G. Tarle, A. Carnero Rosell, Ricardo L. C. Ogando, E. Suchyta, August E. Evrard, D. W. Gerdes, T. M. C. Abbott, Ben Hoyle, M. Carrasco Kind, J. De Vicente, Chun-Hao To, E. J. Sanchez, Daniel Thomas, Matt Hilton, Tenglin Li, Santiago Avila, Carlos E. Cunha, Y. Leung, David J. Brooks, Ramon Miquel, D. L. Burke, A. K. Romer, Alex Drlica-Wagner, Robert A. Gruendl, J. Annis, Tesla E. Jeltema, Jennifer L. Marshall, 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
Brightness, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Luminosity, 0103 physical sciences, Cluster (physics), Surface brightness, 010303 astronomy & astrophysics, Galaxy cluster, STFC, QC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Computer Science::Computers and Society, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Cluster sampling, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using data collected by the Dark Energy Survey (DES), we report the detection of intracluster light (ICL) with $\sim300$ galaxy clusters in the redshift range of 0.2-0.3. We design methods to mask detected galaxies and stars in the images and stack the cluster light profiles, while accounting for several systematic effects (sky subtraction, instrumental point-spread function, cluster selection effects and residual light in the ICL raw detection from background and cluster galaxies). The methods allow us to acquire high signal-to-noise measurements of the ICL and central galaxies (CGs), which we separate with radial cuts. The ICL appears as faint and diffuse light extending to at least 1 Mpc from the cluster center, reaching a surface brightness level of 30 mag arcsec$^{-2}$. The ICL and the cluster CG contribute to $44\%\pm17$\% of the total cluster stellar luminosity within 1 Mpc. The ICL color is overall consistent with that of the cluster red sequence galaxies, but displays the trend of becoming bluer with increasing radius. The ICL demonstrates an interesting self-similarity feature -- for clusters in different richness ranges, their ICL radial profiles are similar after scaling with cluster $R_\mathrm{200m}$, and the ICL brightness appears to be a good tracer of the cluster radial mass distribution. These analyses are based on the DES redMaPPer cluster sample identified in the first year of observations., Revised to match the published version. Paper data available from https://des.ncsa.illinois.edu/releases/other/paper-data

Published
2019

30. Transfer learning for galaxy morphology from one survey to another

Author

V. Scarpine, Michael Schubnell, Mariangela Bernardi, E. Suchyta, August E. Evrard, T. M. C. Abbott, N. Kuropatkin, L. N. da Costa, A. Carnero Rosell, M. E. C. Swanson, E. J. Sanchez, Peter Doel, Kyler Kuehn, R. H. Schindler, Ben Hoyle, Santiago Avila, Sugata Kaviraj, Carlos E. Cunha, K. Honscheid, Ofer Lahav, Joshua A. Frieman, G. Tarle, Joe Zuntz, J. Annis, Peter Melchior, Brian Nord, David J. Brooks, David J. James, Felipe Menanteau, Pablo Fosalba, Marc Huertas-Company, M. Carrasco Kind, Alistair R. Walker, H. Doḿinguez Sanchez, Marcelle Soares-Santos, Filipe B. Abdalla, Ramon Miquel, M. A. G. Maia, A. A. Plazas, G. Gutierrez, D. L. Hollowood, C. Davis, C. B. D'Andrea, J. Gschwend, Enrique Gaztanaga, W. G. Hartley, Flavia Sobreira, Robert A. Gruendl, M. Smith, D. W. Gerdes, J. L. Fischer, Daniel Gruen, M. March, Daniel Thomas, E. Buckley-Geer, J. De Vicente, Juan Garcia-Bellido, J. Carretero, R. C. Smith, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris Diderot - Paris 7 (UPD7), DES, Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)

Subjects
structure [Galaxies], astro-ph.GA, FOS: Physical sciences, Morphology (biology), photometric [Methods], Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, surveys, methods: photometric, 0103 physical sciences, observational [Methods], 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Methods observational, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: structure, methods: observational, Transfer of learning, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Deep Learning (DL) algorithms for morphological classification of galaxies have proven very successful, mimicking (or even improving) visual classifications. However, these algorithms rely on large training samples of labelled galaxies (typically thousands of them). A key question for using DL classifications in future Big Data surveys is how much of the knowledge acquired from an existing survey can be exported to a new dataset, i.e. if the features learned by the machines are meaningful for different data. We test the performance of DL models, trained with Sloan Digital Sky Survey (SDSS) data, on Dark Energy survey (DES) using images for a sample of $\sim$5000 galaxies with a similar redshift distribution to SDSS. Applying the models directly to DES data provides a reasonable global accuracy ($\sim$ 90%), but small completeness and purity values. A fast domain adaptation step, consisting in a further training with a small DES sample of galaxies ($\sim$500-300), is enough for obtaining an accuracy > 95% and a significant improvement in the completeness and purity values. This demonstrates that, once trained with a particular dataset, machines can quickly adapt to new instrument characteristics (e.g., PSF, seeing, depth), reducing by almost one order of magnitude the necessary training sample for morphological classification. Redshift evolution effects or significant depth differences are not taken into account in this study., Accepted for publication in MNRAS

Published
2019

31. Dark Energy Survey Year 1 Results: Galaxy Sample for BAO Measurement

Author

F. J. Castander, Filipe B. Abdalla, T. M. C. Abbott, A. Benoit-Lévy, M. Smith, Alex Drlica-Wagner, Daniel Gruen, E. J. Sanchez, R. A. Bernstein, C. B. D'Andrea, K. Honscheid, Ofer Lahav, D. W. Gerdes, Elisabeth Krause, M. Garcia-Fernandez, Flavia Sobreira, Daniel Scolnic, Santiago Avila, S. E. Kuhlmann, Carlos E. Cunha, J. Carretero, Douglas L. Tucker, Kyler Kuehn, Jack Elvin-Poole, G. Gutierrez, B. Jain, Vinu Vikram, Peter Doel, M. E. C. Swanson, R. Cawthon, Marcos Lima, Martin Crocce, Jennifer L. Marshall, R. C. Smith, Yanxi Zhang, Tim Eifler, H. T. Diehl, Felipe Menanteau, Daniel Thomas, J. Annis, V. Scarpine, Kwan Chuen Chan, Masao Sako, W. G. Hartley, Ramon Miquel, C. Sánchez, Paul Martini, E. Buckley-Geer, Will J. Percival, Brian Yanny, Shantanu Desai, Enrique Gaztanaga, K. Bechtol, C. J. Miller, M. A. G. Maia, Alistair R. Walker, Joshua A. Frieman, A. Alarcon, Tommaso Giannantonio, A. Carnero Rosell, David J. James, N. Banik, I. Sevilla-Noarbe, Marcelle Soares-Santos, Rafe Schindler, Pablo Fosalba, J. De Vicente, N. Kuropatkin, E. Suchyta, D. L. Hollowood, L. N. da Costa, Erin Sheldon, David Brooks, Rogerio Rosenfeld, E. Bertin, A. A. Plazas, C. Davis, Ana Salvador, J. Gschwend, Gary Bernstein, Ashley J. Ross, G. Tarle, S. Allam, Robert A. Gruendl, M. Carrasco Kind, Robert C. Nichol, Juan Garcia-Bellido, 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, CSIC, Ohio State Univ, Ctr Invest Energet Medioambientales & Tecnol CIEM, Univ Manchester, Univ Portsmouth, Univ Autonoma Madrid, Sun Yat Sen Univ, Fermilab Natl Accelerator Lab, Barcelona Inst Sci & Technol, Swiss Fed Inst Technol, UCL, Univ Cambridge, Ludwig Maximilians Univ Munchen, Universidade Estadual Paulista (Unesp), Lab Interinst E Astron LIneA, Natl Opt Astron Observ, Rhodes Univ, LSST, CNRS, UPMC Univ Paris 06, Univ Penn, Observ Carnegie Inst Washington, Observ Nacl, Univ Illinois, Natl Ctr Supercomp Applicat, Univ Chicago, Stanford Univ, IIT Hyderabad, CALTECH, Steward Observ, Univ Michigan, SLAC Natl Accelerator Lab, Santa Cruz Inst Particle Phys, Harvard Smithsonian Ctr Astrophys, Australian Astron Observ, Argonne Natl Lab, Universidade de São Paulo (USP), Texas A&M Univ, Inst Catalana Recerca & Estudis Avancats, Brookhaven Natl Lab, Univ Southampton, Brandeis Univ, Universidade Estadual de Campinas (UNICAMP), and Oak Ridge Natl Lab

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Magnitude (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Measure (mathematics), 0103 physical sciences, Cluster analysis, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Galaxy, Redshift, observations [cosmology], Space and Planetary Science, cosmology: observations, astro-ph.CO, Dark energy, ESTRUTURA DO UNIVERSO, Baryon acoustic oscillations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We define and characterise a sample of 1.3 million galaxies extracted from the first year of Dark Energy Survey data, optimised to measure Baryon Acoustic Oscillations in the presence of significant redshift uncertainties. The sample is dominated by luminous red galaxies located at redshifts $z \gtrsim 0.6$. We define the exact selection using color and magnitude cuts that balance the need of high number densities and small photometric redshift uncertainties, using the corresponding forecasted BAO distance error as a figure-of-merit in the process. The typical photo-$z$ uncertainty varies from $2.3\%$ to $3.6\%$ (in units of 1+$z$) from $z=0.6$ to $1$, with number densities from $200$ to $130$ galaxies per deg$^2$ in tomographic bins of width $\Delta z = 0.1$. Next we summarise the validation of the photometric redshift estimation. We characterise and mitigate observational systematics including stellar contamination, and show that the clustering on large scales is robust in front of those contaminants. We show that the clustering signal in the auto-correlations and cross-correlations is generally consistent with theoretical models, which serves as an additional test of the redshift distributions., Comment: 15 pages, 12 figures. Added discussion on photo-z validation and other tests added based on referee's comments. Matches published version in MNRAS

Published
2019

32. Chemical Abundance Analysis of Tucana III, the Second $r$-process Enhanced Ultra-Faint Dwarf Galaxy

Author

Ben Hoyle, Michael Schubnell, Shantanu Desai, J. Carretero, Antonella Palmese, David Brooks, Felipe Menanteau, M. E. C. Swanson, M. A. G. Maia, J. De Vicente, Kyler Kuehn, Tenglin Li, Carlos E. Cunha, Peter Doel, Jennifer L. Marshall, K. Honscheid, Ramon Miquel, E. Suchyta, G. Tarle, R. A. Bernstein, A. A. Plazas, David J. James, Juan Garcia-Bellido, E. Bertin, V. Scarpine, Pablo Fosalba, C. J. Miller, Terese T. Hansen, C. Lidman, W. C. Wester, B. Flaugher, Enrique Gaztanaga, M. Smith, C. B. D'Andrea, Andrew B. Pace, D. L. Burke, W. G. Hartley, D. L. Hollowood, G. Gutierrez, T. F. Eifler, E. Buckley-Geer, A. Carnero Rosell, S. Serrano, M. Carrasco Kind, Robert A. Gruendl, Alex Drlica-Wagner, Adriano Pieres, J. D. Simon, D. Q. Nagasawa, E. J. Sanchez, D. W. Gerdes, Louis E. Strigari, Basilio X. Santiago, J. Gschwend, Marcelle Soares-Santos, D. L. DePoy, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, Joshua A. Frieman, and Keith Bechtol

Subjects
Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Abundance (ecology), Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, r-process, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract

We present a chemical abundance analysis of four additional confirmed member stars of Tucana III, a Milky Way satellite galaxy candidate in the process of being tidally disrupted as it is accreted by the Galaxy. Two of these stars are centrally located in the core of the galaxy while the other two stars are located in the eastern and western tidal tails. The four stars have chemical abundance patterns consistent with the one previously studied star in Tucana III: they are moderately enhanced in $r$-process elements, i.e. they have $ \approx +$0.4 dex. The non-neutron-capture elements generally follow trends seen in other dwarf galaxies, including a metallicity range of 0.44 dex and the expected trend in $\alpha$-elements, i.e., the lower metallicity stars have higher Ca and Ti abundance. Overall, the chemical abundance patterns of these stars suggest that Tucana III was an ultra-faint dwarf galaxy, and not a globular cluster, before being tidally disturbed. As is the case for the one other galaxy dominated by $r$-process enhanced stars, Reticulum II, Tucana III's stellar chemical abundances are consistent with pollution from ejecta produced by a binary neutron star merger, although a different $r$-process element or dilution gas mass is required to explain the abundances in these two galaxies if a neutron star merger is the sole source of $r$-process enhancement., Comment: 18 pages, 10 figures; accepted by ApJ

Published
2018

33. SPOKES: An end-to-end simulation facility for spectroscopic cosmological surveys

Author

La. Gamper, Jaime E. Forero-Romero, Lukas Gamper, Donnacha Kirk, Adam Amara, Brian Nord, Chihway Chang, Carlos E. Cunha, B. Hambrecht, A. H. Bauer, Stephanie Jouvel, Michael T. Busha, Alexandre Refregier, Andrina Nicola, O. Coles, Will Saunders, Risa H. Wechsler, and Santiago Serrano

Subjects
Flexibility (engineering), Computer science, Group method of data handling, business.industry, Astronomy and Astrophysics, Usability, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Pipeline (software), Computer Science Applications, 010309 optics, Data access, Space and Planetary Science, Component (UML), 0103 physical sciences, Systems engineering, Dark energy, Benchmark (computing), business, 010303 astronomy & astrophysics
Abstract

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

Published
2016

34. Choreography of molecular movements during ribosome progression along mRNA

Author

Carlos E. Cunha, Neva Caliskan, Frank Peske, Wolfgang Wintermeyer, Heena Sharma, Riccardo Belardinelli, and Marina V. Rodnina

Subjects
0301 basic medicine, Ribosome Subunits, Small, Bacterial, Ribosome Subunits, Large, Bacterial, Molecular Dynamics Simulation, Ribosome, 03 medical and health sciences, RNA, Transfer, Structural Biology, parasitic diseases, Escherichia coli, Peptide Elongation Factor G, Initiation factor, RNA, Messenger, Molecular Biology, Chemistry, Escherichia coli Proteins, Hydrolysis, RNA, Ribosomal RNA, Cell biology, Elongation factor, RNA, Bacterial, 030104 developmental biology, Ribosome Subunits, Transfer RNA, Guanosine Triphosphate
Abstract

During translation elongation, ribosome translocation along an mRNA entails rotations of the ribosomal subunits, swiveling motions of the small subunit (SSU) head and stepwise movements of the tRNAs together with the mRNA. Here, we reconstructed the choreography of the collective motions of the Escherichia coli ribosome during translocation promoted by elongation factor EF-G, by recording the fluorescence signatures of nine different reporters placed on both ribosomal subunits, tRNA and mRNA. We captured an early forward swiveling of the SSU head taking place while the SSU body rotates in the opposite, clockwise direction. Backward swiveling of the SSU head starts upon tRNA translocation and continues until the post-translocation state is reached. This work places structures of translocation intermediates along a time axis and unravels principles of the motions of macromolecular machines.

Published
2016

35. Rapidly evolving transients in the Dark Energy Survey

Author

Flavia Sobreira, F. J. Castander, Mark Sullivan, S. A. Uddin, Chris Curtin, David Brooks, Tesla E. Jeltema, T. F. Eifler, Ryan J. Foley, E. Suchyta, M. Carrasco Kind, Robert C. Nichol, M. Pursiainen, J. Carretero, Juan Garcia-Bellido, K. Honscheid, Brad E. Tucker, Edward Macaulay, Tamara M. Davis, W. G. Hartley, M. E. C. Swanson, E. Swann, M. A. G. Maia, Daniel Gruen, B. Flaugher, J. K. Hoormann, P. Wiseman, Geraint F. Lewis, Anais Möller, N. Kuropatkin, Daniela Carollo, E. Buckley-Geer, J. De Vicente, N. E. Sommer, Claudia P. Gutiérrez, C. Davis, T. M. C. Abbott, S. Prajs, Felipe Menanteau, J. Annis, C. B. D'Andrea, Gregory Tarle, D. L. Burke, Alistair R. Walker, A. A. Plazas, Marcelle Soares-Santos, P. Doel, E. J. Sanchez, Rafe Schindler, H. T. Diehl, Filipe B. Abdalla, M. Childress, C. Lidman, A. Carnero Rosell, S. Allam, Robert A. Gruendl, M. Sako, Tenglin Li, Santiago Avila, R. C. Smith, Cosimo Inserra, P. Martini, Carlos E. Cunha, D. L. Hollowood, Bonnie Zhang, Jacobo Asorey, A. L. King, Richard Kessler, A. Roodman, Marcos Lima, Ricardo L. C. Ogando, V. Scarpine, Samuel Hinton, G. Gutierrez, J. Calcino, David J. James, Pablo Fosalba, Joshua A. Frieman, Karl Glazebrook, Mathew Smith, Douglas L. Tucker, and Kyler Kuehn

Subjects
general [Supernovae], Supernovae: general, FOS: Physical sciences, Astrophysics, 01 natural sciences, 0103 physical sciences, Exponential decay, Ejecta, 010303 astronomy & astrophysics, STFC, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Photosphere, 010308 nuclear & particles physics, ST/P000398/1, Física, RCUK, Astronomy and Astrophysics, Light curve, Redshift, Galaxy, Supernova, 13. Climate action, Space and Planetary Science, Dark energy, Astrophysics - High Energy Astrophysical Phenomena
Abstract

This article has been accepted for publication in Monthly Notices of Royal Astronomical Society © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved., We present the results of a search for rapidly evolving transients in the Dark Energy Survey Supernova Programme. These events are characterized by fast light-curve evolution (rise to peak in≲10 d and exponential decline in≲30 d after peak).We discovered 72 events, including 37 transients with a spectroscopic redshift from host galaxy spectral features. The 37 events increase the total number of rapid optical transients by more than a factor of two. They are found at a wide range of redshifts (0.05 < z < 1.56) and peak brightnesses (-15.75 > Mg > -22.25). The multiband photometry is well fit by a blackbody up to few weeks after peak. The events appear to be hot (T ≈ 10 000-30 000 K) and large (R ≈ 1014 - 2 × 1015 cm) at peak, and generally expand and cool in time, though some events show evidence for a receding photosphere with roughly constant temperature. Spectra taken around peak are dominated by a blue featureless continuum consistent with hot, optically thick ejecta. We compare our events with a previously suggested physical scenario involving shock breakout in an optically thick wind surrounding a core-collapse supernova, we conclude that current models for such a scenario might need an additional power source to describe the exponential decline. We find that these transients tend to favour star-forming host galaxies, which could be consistent with a core-collapse origin. However, more detailed modelling of the light curves is necessary to determine their physical origin., We acknowledge support from EU/FP7-ERC grant no [615929]. Based in part on data obtained from the ESO Science Archive Facility under program 097.D-0709. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020 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, Fundacâo 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 Inovaçâo, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey

Published
2018

36. Dark Energy Survey year 1 results: Galaxy-galaxy lensing

Author

Keith Bechtol, B. Flaugher, David Thomas, H. T. Diehl, A. K. Romer, David Bacon, Paul Martini, Elisabeth Krause, Eli S. Rykoff, J. Prat, Joe Zuntz, Niall MacCrann, Marcos Lima, Masao Sako, W. G. Hartley, G. Gutierrez, C. Davis, A. Roodman, J. Gschwend, R. P. Rollins, M. D. Johnson, Gary Bernstein, R. H. Schindler, Tommaso Giannantonio, R. C. Smith, L. F. Secco, R. Cawthon, G. Tarle, Ramon Miquel, A. Carnero Rosell, Tesla E. Jeltema, F. J. Castander, I. Sevilla-Noarbe, E. Rozo, C. Sánchez, Douglas L. Tucker, Kyler Kuehn, Brian Yanny, Enrique Fernández, Michael Schubnell, Daniel Gruen, Shantanu Desai, A. A. Plazas, T. M. C. Abbott, J. Carretero, E. Buckley-Geer, Alex Drlica-Wagner, Daniel A. Goldstein, Juan Garcia-Bellido, Y. Fang, A. Benoit-Lévy, E. J. Sanchez, T. N. Varga, E. M. Huff, E. Bertin, Jonathan Blazek, L. N. da Costa, D. W. Gerdes, Mathew Smith, Oliver Friedrich, J. P. Dietrich, Donnacha Kirk, Tenglin Li, Scott Dodelson, D. L. Burke, Chihway Chang, Alistair R. Walker, A. Alarcon, Carlos E. Cunha, M. Gatti, Marcelle Soares-Santos, C. B. D'Andrea, S. E. Kuhlmann, Erin Sheldon, Felipe Menanteau, Joseph J. Mohr, Michael Troxel, David J. James, M. E. C. Swanson, S. Allam, Robert A. Gruendl, Martin Crocce, Jennifer L. Marshall, Pablo Fosalba, J. Annis, Ashley J. Ross, K. Honscheid, Joshua A. Frieman, Brian Nord, Risa H. Wechsler, J. De Vicente, Flavia Sobreira, S. Samuroff, M. W. G. Johnson, M. March, Markus Michael Rau, Matt J. Jarvis, P. Vielzeuf, Yanxi Zhang, Tim Eifler, M. Carrasco Kind, Robert C. Nichol, Ofer Lahav, Enrique Gaztanaga, Vinu Vikram, Filipe B. Abdalla, V. Scarpine, David J. Brooks, Bhuvnesh Jain, Jack Elvin-Poole, Peter Melchior, E. Suchyta, Ben Hoyle, N. Kokron, M. A. G. Maia, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, cosmic rays, Consistency (statistics), 0103 physical sciences, Experiments in gravity, 010303 astronomy & astrophysics, STFC, QC, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, COSMIC cancer database, 010308 nuclear & particles physics, RCUK, Astronomy, Redshift, Galaxy, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, Jackknife resampling, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present galaxy-galaxy lensing measurements from 1321 sq. deg. of the Dark Energy Survey (DES) Year 1 (Y1) data. The lens sample consists of a selection of 660,000 red galaxies with high-precision photometric redshifts, known as redMaGiC, split into five tomographic bins in the redshift range $0.15 < z < 0.9$. We use two different source samples, obtained from the Metacalibration (26 million galaxies) and Im3shape (18 million galaxies) shear estimation codes, which are split into four photometric redshift bins in the range $0.2 < z < 1.3$. We perform extensive testing of potential systematic effects that can bias the galaxy-galaxy lensing signal, including those from shear estimation, photometric redshifts, and observational properties. Covariances are obtained from jackknife subsamples of the data and validated with a suite of log-normal simulations. We use the shear-ratio geometric test to obtain independent constraints on the mean of the source redshift distributions, providing validation of those obtained from other photo-$z$ studies with the same data. We find consistency between the galaxy bias estimates obtained from our galaxy-galaxy lensing measurements and from galaxy clustering, therefore showing the galaxy-matter cross-correlation coefficient $r$ to be consistent with one, measured over the scales used for the cosmological analysis. The results in this work present one of the three two-point correlation functions, along with galaxy clustering and cosmic shear, used in the DES cosmological analysis of Y1 data, and hence the methodology and the systematics tests presented here provide a critical input for that study as well as for future cosmological analyses in DES and other photometric galaxy surveys., 26 pages, 19 figures. Matches the version accepted by PRD

Published
2018

37. The Dark Energy Survey Data Release 1

Author

M. W. G. Johnson, M. Baumer, Tesla E. Jeltema, Eric H. Neilsen, Peter Nugent, Martin Crocce, S. Hamilton, M. Smith, Antonella Palmese, Nora Shipp, Eli S. Rykoff, F. Nogueira, L. Baruah, Daniel Gruen, Daniel Scolnic, Brian Nord, M. A. G. Maia, Brian Yanny, Matthias Klein, J. Song, R. R. Gupta, Yanxi Zhang, Arya Farahi, J. Carretero, M. March, Basilio X. Santiago, Tamara M. Davis, Shantanu Desai, Gary S. Da Costa, Jochen Weller, T. F. Eifler, Daniel A. Goldstein, J. M. Hislop, Joseph J. Mohr, R. C. Thomas, Erin Sheldon, David Brooks, M. E. C. Swanson, A. Porredon, A. Carnero Rosell, A. Saro, D. W. Gerdes, Xi Chen, Attila Kovács, Eric Morganson, R. C. Wolf, J. P. Dietrich, A. Kremin, T. M. C. Abbott, Richard G. McMahon, Jeremy Mould, J. D. Maloney, Jacobo Asorey, A. Benoit-Lévy, Hiranya V. Peiris, Ofer Lahav, Vinu Vikram, J. Lasker, E. J. Sanchez, B. Flaugher, S. Juneau, Risa H. Wechsler, Ricardo L. C. Ogando, Alistair R. Walker, A. A. Plazas, Ryan J. Foley, M. Carrasco Kind, W. C. Wester, Jennifer L. Marshall, D. L. Burke, Adam Amara, A. Scott, M.L. Sánchez, Jonathan Blazek, C. B. D'Andrea, Marcelle Soares-Santos, R. C. Smith, S. E. Kuhlmann, Ashley J. Ross, Robert C. Nichol, Ben Hoyle, G. Daues, M. Gower, C. J. Miller, M. D. Johnson, Wayne A. Barkhouse, Samuel Hinton, Felipe Menanteau, Kevin Reil, L. Nunes, F. Paz-Chinchón, David J. James, Tenglin Li, Scott Dodelson, Santiago Avila, Ann Elliott, Chihway Chang, T. Kacprzak, G. Tarle, Knut Olsen, R. Das, Ramon Miquel, Lyndsay Old, Juan Garcia-Bellido, E. Bertin, A. Roodman, Tommaso Giannantonio, Carlos E. Cunha, J. Poh, Pablo Fosalba, Enrique Gaztanaga, G. Gutierrez, J. DeRose, J. J. Thaler, Enrique Fernández, Will J. Percival, S. Allam, Paul M. Ricker, A. Pujol, Robert A. Gruendl, V. Scarpine, Andrew B. Pace, R. P. Rollins, K. Honscheid, Timothy A. McKay, Darren L. DePoy, G. Khullar, R. T. Li, Joe Zuntz, Alex Drlica-Wagner, R. Nikutta, Francisco J. Castander, C. Pond, Douglas L. Tucker, Don Petravick, W. G. Hartley, A. K. Vivas, R. Cawthon, Riccardo Campisano, D. A. Finley, D. Brout, Karl Glazebrook, Dragan Huterer, Peter Melchior, Elisabeth Krause, Mark Sullivan, Kyler Kuehn, V. C. Busti, P. Rooney, C. J. Conselice, Huan Lin, Marc Manera, J. Annis, Sebastian Bocquet, A. M. G. Koziol, M. L. Silveira, M. Fitzpatrick, Andrew R. Liddle, Alfredo Zenteno, O. Ballester, Steve Kent, Daniel Thomas, E. Buckley-Geer, Michael Troxel, A. K. Romer, Paul Martini, A. Fausti Neto, Keith Bechtol, C. Davis, J. Gschwend, Gary Bernstein, Hao-Yi Wu, Peter Doel, H. T. Diehl, J. De Vicente, J. P. Marriner, M. S. S. Gill, E. Suchyta, Niall MacCrann, August E. Evrard, Alexandre Refregier, Douglas N. Friedel, Albert Stebbins, M. Banerji, Joshua A. Frieman, I. Sevilla-Noarbe, J. A. Smith, T. McClintock, N. Kuropatkin, L. N. da Costa, Laia Cardiel-Sas, M. Sako, D. L. Hollowood, S. Serrano, David L. Nidever, Marcos Lima, Richard G. Kron, P. Lopez-Reyes, Filipe B. Abdalla, Bhuvnesh Jain, Matthew R. Becker, Flavia Sobreira, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), DES, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), NOAO Data Lab, Abbott, T. M. C., Abdalla, F. B., Allam, S., Amara, A., Annis, J., Asorey, J., Avila, S., Ballester, O., Banerji, M., Barkhouse, W., Baruah, L., Baumer, M., Bechtol, K., Becker, M. R., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Blazek, J., Bocquet, S., Brooks, D., Brout, Buckley-Geer, E., Burke, D. L., Busti, V., Campisano, R., Cardiel-Sas, L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, X., Conselice, C., Costa, G., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Das, R., Daues, G., Davis, T. M., Davis, C., De Vicente, J., Depoy, D. L., Derose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elliott, A. E., Evrard, A. E., Farahi, A., Fausti Neto, A., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fosalba, P., Friedel, D. N., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gill, M. S. S., Glazebrook, K., Goldstein, D. A., Gower, M., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hamilton, S., Hartley, W. G., Hinton, S. R., Hislop, J. M., Hollowood, D., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kacprzak, T., Kent, S., Khullar, G., Klein, M., Kovacs, A., Koziol, A. M. G., Krause, E., Kremin, A., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lasker, J., Li, T. S., Li, R. T., Liddle, A. R., Lima, M., Lin, H., López-Reyes, P., Maccrann, N., Maia, M. A. G., Maloney, J. D., Manera, M., March, M., Marriner, J., Marshall, J. L., Martini, P., Mcclintock, T., Mckay, T., Mcmahon, R. G., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Mohr, J. J., Morganson, E., Mould, J., Neilsen, E., Nichol, R. C., Nogueira, F., Nord, B., Nugent, P., Nunes, L., Ogando, R. L. C., Old, L., Pace, A. B., Palmese, A., Paz-Chinchón, F., Peiris, H. V., Percival, W. J., Petravick, D., Plazas, A. A., Poh, J., Pond, C., Porredon, A., Pujol, A., Refregier, A., Reil, K., Ricker, P. M., Rollins, R. P., Romer, A. K., Roodman, A., Rooney, P., Ross, A. J., Rykoff, E. S., Sako, M., Sanchez, M. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Shipp, N., Silveira, M. L., Smith, M., Smith, R. C., Smith, J. A., Soares-Santos, M., Sobreira, F., Song, J., Stebbins, A., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Vivas, A. K., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wolf, R. C., Wu, H., Yanny, B., Zenteno, A., Zhang, Y., Zuntz, J., Des, Collaboration, Juneau, S., Fitzpatrick, M., Nikutta, R., Nidever, D., Olsen, K., Scott, A., and NOAO Data, Lab

Subjects
Astronomical Objects, catalog, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], techniques: image processing, Astrophysics, astronomical databases: miscellaneous, 01 natural sciences, law.invention, photometric [techniques], techniques: photometric, law, Observatory, Astrophysics - Cosmology and Nongalactic Astrophysic, 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics, image processing [techniques], observations [cosmology], sky survey, Astrophysics - Solar and Stellar Astrophysics, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, sextractor, Data release, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.SR, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, astro-ph.GA, FOS: Physical sciences, Astronomy & Astrophysics, miscellaneou [astronomical databases], Telescope, surveys, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, survey, Astronomical And Space Sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Physical Chemistry (Incl. Structural), 010308 nuclear & particles physics, Organic Chemistry, representations, Astronomy and Astrophysics, miscellaneous [astronomical databases], angular masks, Astrophysics - Astrophysics of Galaxies, Galaxy, Data set, catalogs, cosmology: observations, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM
Abstract

We describe the first public data release of the Dark Energy Survey, DES DR1, consisting of reduced single epoch images, coadded images, coadded source catalogs, and associated products and services assembled over the first three years of DES science operations. DES DR1 is based on optical/near-infrared imaging from 345 distinct nights (August 2013 to February 2016) by the Dark Energy Camera mounted on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. We release data from the DES wide-area survey covering ~5,000 sq. deg. of the southern Galactic cap in five broad photometric bands, grizY. DES DR1 has a median delivered point-spread function of g = 1.12, r = 0.96, i = 0.88, z = 0.84, and Y = 0.90 arcsec FWHM, a photometric precision of < 1% in all bands, and an astrometric precision of 151 mas. The median coadded catalog depth for a 1.95" diameter aperture at S/N = 10 is g = 24.33, r = 24.08, i = 23.44, z = 22.69, and Y = 21.44 mag. DES DR1 includes nearly 400M distinct astronomical objects detected in ~10,000 coadd tiles of size 0.534 sq. deg. produced from ~39,000 individual exposures. Benchmark galaxy and stellar samples contain ~310M and ~ 80M objects, respectively, following a basic object quality selection. These data are accessible through a range of interfaces, including query web clients, image cutout servers, jupyter notebooks, and an interactive coadd image visualization tool. DES DR1 constitutes the largest photometric data set to date at the achieved depth and photometric precision., 30 pages, 20 Figures. Release page found at this url https://des.ncsa.illinois.edu/releases/dr1

Published
2018

38. Dynamical Analysis of Three Distant Trans-Neptunian Objects with Similar Orbits

Author

H. T. Diehl, J. Annis, Vinu Vikram, Ramon Miquel, L. Zullo, Robert A. Gruendl, K. Honscheid, T. F. Eifler, Kevin Napier, E. Bertin, Juan Garcia-Bellido, T. M. C. Abbott, Pedro H. Bernardinelli, Tali Khain, I. Sevilla-Noarbe, V. Scarpine, W. G. Hartley, N. Kuropatkin, Kyler Kuehn, Michael Schubnell, E. J. Sanchez, L. N. da Costa, J. Carretero, E. Suchyta, Marcelle Soares-Santos, R. H. Schindler, Elisabeth Krause, David J. James, B. Flaugher, P. Doel, Filipe B. Abdalla, Felipe Menanteau, Juliette C. Becker, M. E. C. Swanson, O. Lahav, M. N. K. Smith, M. Sako, Kyle Franson, Fred C. Adams, Carlos E. Cunha, W. C. Wester, Larissa Markwardt, D. L. Hollowood, S. Desai, S. Hamilton, Joshua A. Frieman, G. Gutierrez, G. Tarle, A. A. Plazas, A. K. Romer, C. L. Davis, Salcedo Romero de Ávila, A. Carnero Rosell, M. Carrasco Kind, Yanxi Zhang, Brian Nord, Daniel Gruen, D. W. Gerdes, Flavia Sobreira, M. A. G. Maia, A. R. Walker, J. De Vicente, Hsing Wen Lin, Ricardo L. C. Ogando, D. Brooks, 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
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Solar System, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Phase plane, Orbital mechanics, 01 natural sciences, Omega, 13. Climate action, Space and Planetary Science, Planet, Neptune, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Trans-Neptunian object, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Order of magnitude, QC, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

This paper reports the discovery and orbital characterization of two extreme trans-Neptunian objects (ETNOs), 2016 QV$_{89}$ and 2016 QU$_{89}$, which have orbits that appear similar to that of a previously known object, 2013 UH$_{15}$. All three ETNOs have semi-major axes $a\approx 172$ AU and eccentricities $e\approx0.77$. The angular elements $(i,\omega,\Omega)$ vary by 6, 15, and 49 deg, respectively between the three objects. The two new objects add to the small number of TNOs currently known to have semi-major axes between 150 and 250 AU, and serve as an interesting dynamical laboratory to study the outer realm of our Solar System. Using a large ensemble of numerical integrations, we find that the orbits are expected to reside in close proximity in the $(a,e)$ phase plane for roughly 100 Myr before diffusing to more separated values. We then explore other scenarios that could influence their orbits. With aphelion distances over 300 AU, the orbits of these ETNOs extend far beyond the classical Kuiper Belt, and an order of magnitude beyond Neptune. As a result, their orbital dynamics can be affected by the proposed new Solar System member, referred to as Planet Nine in this work. With perihelion distances of 35-40 AU, these orbits are also influenced by resonant interactions with Neptune. A full assessment of any possible, new Solar System planets must thus take into account this emerging class of TNOs., Comment: accepted to AJ

Published
2018

39. Chemical Abundance Analysis of Three α-poor, Metal-poor Stars in the Ultrafaint Dwarf Galaxy Horologium I

Author

R. H. Schindler, E. Balbinot, David J. James, A. Roodman, B. Yanny, E. Suchyta, Darren L. DePoy, T. Jeltema, D. Q. Nagasawa, A. Benoit-Lévy, Alistair R. Walker, W. G. Hartley, M. Carrasco Kind, Marcelle Soares-Santos, R. C. Wolf, Keith Bechtol, G. Gutierrez, Josh Frieman, Risa H. Wechsler, Terese T. Hansen, Jennifer L. Marshall, Elisabeth Krause, J. D. Simon, Enrique Gaztanaga, P. Fosalba, Tianjun Li, Juan Garcia-Bellido, Andrew B. Pace, C. M. Pellegrino, C. B. D'Andrea, S. E. Kuhlmann, Rebecca A. Bernstein, E. Bertin, A. Carnero Rosell, T. F. Eifler, K. Kuehn, F. B. Abdalla, Daniel Thomas, C. J. Davis, David J. Brooks, N. B. Suntzeff, B. Flaugher, Alex Drlica-Wagner, J. Carretero, M. N. K. Smith, T. M. C. Abbott, G. Tarle, J. Gschwend, S. Allam, Robert A. Gruendl, Michael Schubnell, E. J. Sanchez, J. Annis, K. Honscheid, Carlos E. Cunha, Ramon Miquel, B. Nord, S. Desai, R. C. Smith, Flavia Sobreira, Daniel Gruen, M. March, Basilio X. Santiago, D. W. Gerdes, I. Sevilla-Noarbe, N. Kuropatkin, Douglas L. Tucker, L. N. da Costa, V. Scarpine, P. Doel, Louis E. Strigari, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, UAM. Departamento de Física Teórica, 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
astro-ph.SR, stars: abundances, 010504 meteorology & atmospheric sciences, dwarf [galaxies], astro-ph.GA, Milky Way, Metallicity, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Galactic halo, chemically peculiar [stars], 0103 physical sciences, abundances [galaxies], Astrophysics::Solar and Stellar Astrophysics, Large Magellanic Cloud, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, Physics, Star formation, RCUK, Física, Astronomy and Astrophysics, galaxies: dwarf, Astrophysics - Astrophysics of Galaxies, stars: chemically peculiar, abundances [stars], Supernova, Stars, Astrophysics - Solar and Stellar Astrophysics, AST-1560223, 13. Climate action, Space and Planetary Science, galaxies: abundances, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Reproduced with permission of AAS, We present chemical abundance measurements of three stars in the ultrafaint dwarf galaxy Horologium I, a Milky Way satellite discovered by the Dark Energy Survey. Using high-resolution spectroscopic observations, we measure the metallicity of the three stars, as well as abundance ratios of several α-elements, iron-peak elements, and neutron-capture elements. The abundance pattern is relatively consistent among all three stars, which have a low average metallicity of [Fe/H] ∼ -2.6 and are not α-enhanced ([α/Fe] ∼ 0.0). This result is unexpected when compared to other low-metallicity stars in the Galactic halo and other ultrafaint dwarfs and suggests the possibility of a different mechanism for the enrichment of Hor I compared to other satellites. We discuss possible scenarios that could lead to this observed nucleosynthetic signature, including extended star formation, enrichment by a Population III supernova, and or an association with the Large Magellanic Cloud, Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under grant nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-88861, FPA2015-68048, SEV- 2012-0234, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007- 2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project no. CE110001020

Published
2018

40. DES meets Gaia: discovery of strongly lensed quasars from a multiplet search

Author

David J. James, B. Flaugher, V. Scarpine, Adriano Agnello, N. D. Morgan, Karl Glazebrook, A. Carnero Rosell, T. M. C. Abbott, Veronica Motta, Matthew W. Auger, Nikolay Kuropatkin, R. H. Schindler, Michael Schubnell, Enrique Gaztanaga, E. Buckley-Geer, Shantanu Desai, E. J. Sanchez, Tommaso Treu, J. Gschwend, David Brooks, M. E. C. Swanson, Ofer Lahav, Paul L. Schechter, D. L. Burke, Marcos Lima, R. A. Bernstein, Flavia Sobreira, Timo Anguita, G. Gutierrez, I. Sevilla-Noarbe, Ricardo L. C. Ogando, Anupreeta More, E. Bertin, L. N. da Costa, A. A. Plazas, Philip J. Marshall, Brian Nord, K. Honscheid, Juan Garcia-Bellido, Alex Drlica-Wagner, Ramon Miquel, Christopher D. Fassnacht, C. B. D'Andrea, E. Suchyta, Marcelle Soares-Santos, Risa H. Wechsler, Douglas L. Tucker, Kyler Kuehn, Joshua A. Frieman, Robert A. Gruendl, M. March, J. Annis, Sherry H. Suyu, Filipe B. Abdalla, Felipe Menanteau, Gregory Tarle, Adam Amara, Carlos E. Cunha, Tim Eifler, Frederic Courbin, Takahiro Morishita, Huan Lin, K. Benoit-Lévy, K. Bechtol, K. Rojas, Georges Meylan, J. Carretero, Richard G. McMahon, M. Smith, Daniel Gruen, D. W. Gerdes, Marcio A. G. Maia, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FOS: Physical sciences, techniques: image processing, Astrophysics, Surveys, strong [Gravitational lensing], 01 natural sciences, law.invention, Einstein radius, surveys, law, 0103 physical sciences, image processing [Techniques], 010303 astronomy & astrophysics, Multiplet, Physics, methods: statistical, Simple lens, 010308 nuclear & particles physics, Astronomy, gravitational lensing: strong, Astronomy and Astrophysics, Quasar, Radius, Astrophysics - Astrophysics of Galaxies, Redshift, Lens (optics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery, spectroscopic confirmation and first lens models of the first two, strongly lensed quasars from a combined search in WISE and Gaia over the DES footprint. The four-image lensWGD2038-4008 (r.a.=20:38:02.65, dec.=-40:08:14.64) has source- and lens-redshifts $z_{s}=0.777 \pm 0.001$ and $z_l = 0.230 \pm 0.002$ respectively. Its deflector has effective radius $R_{\rm eff} \approx 3.4^{\prime\prime}$, stellar mass $\log(M_{\star}/M_{\odot}) = 11.64^{+0.20}_{-0.43}$, and shows extended isophotal shape variation. Simple lens models yield Einstein radii $R_{\rm E}=(1.30\pm0.04)^{\prime\prime},$ axis ratio $q=0.75\pm0.1$ (compatible with that of the starlight) and considerable shear-ellipticity degeneracies. The two-image lensWGD2021-4115 (r.a.=20:21:39.45, dec.=--41:15:57.11) has $z_{s}=1.390\pm0.001$ and $z_l = 0.335 \pm 0.002$, and Einstein radius $R_{\rm E} = (1.1\pm0.1)^{\prime\prime},$ but higher-resolution imaging is needed to accurately separate the deflector and faint quasar image. We also show high-rank candidate doubles selected this way, some of which have been independently identified with different techniques, and discuss a DES+WISE quasar multiplet selection., Comment: MNRAS subm. 21/10/2017, awaiting reviewer selection. This paper has been approved by DES Collaboration-Wide Review

Published
2018

41. Evidence for Color Dichotomy in the Primordial Neptunian Trojan Population

Author

Marcelle Soares-Santos, David J. James, Pedro Bernadinelli, M. Smith, Douglas L. Tucker, Kyler Kuehn, Tim Eifler, Jennifer L. Marshall, Flavia Sobreira, Larissa Markwardt, D. W. Gerdes, V. Scarpine, B. Flaugher, P. Doel, Tali Khain, I. Sevilla-Noarbe, Juliette C. Becker, A. A. Plazas, L. N. da Costa, Masao Sako, D. L. Hollowood, M. Carrasco Kind, A. K. Romer, Fred C. Adams, W. C. Wester, E. Suchyta, S. Allam, Juan Garcia-Bellido, S. Hamilton, J. Annis, A. R. Walker, T. M. C. Abbott, C. B. D'Andrea, J. De Vicente, Hsing Wen Lin, E. J. Sanchez, M. A. G. Maia, A. Carnero Rosell, D. Brooks, Santiago Avila, Carlos E. Cunha, N. P. Kuropatkin, K. Honscheid, Kyle Franson, Ramon Miquel, Gary Bernstein, G. Tarle, and R. C. Smith

Subjects
Solar System, Planetesimal, Trans-Neptunian objects, 010504 meteorology & atmospheric sciences, Population, FOS: Physical sciences, 01 natural sciences, Jovian, Orbital, Planet, 0103 physical sciences, Trans-Neptunian object, education, 010303 astronomy & astrophysics, STFC, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, RCUK, Astronomy, Astronomy and Astrophysics, High flux, Space and Planetary Science, Trojan, Resonances, Trojan asteroids, Astrophysics - Earth and Planetary Astrophysics
Abstract

In the current model of early Solar System evolution, the stable members of the Jovian and Neptunian Trojan populations were captured into resonance from the leftover reservoir of planetesimals during the outward migration of the giant planets. As a result, both Jovian and Neptunian Trojans share a common origin with the primordial disk population, whose other surviving members constitute today's trans-Neptunian object (TNO) populations. The cold (low inclination and small eccentricity) classical TNOs are ultra-red, while the dynamically excited “hot” (high inclination and larger eccentricity) population of TNOs contains a mixture of ultra-red and blue objects. In contrast, Jovian and Neptunian Trojans are observed to be blue. While the absence of ultra-red Jovian Trojans can be readily explained by the sublimation of volatile material from their surfaces due to the high flux of solar radiation at 5 AU, the lack of ultra-red Neptunian Trojans presents both a puzzle and a challenge to formation models. In this work we report the discovery by the Dark Energy Survey (DES) of two new dynamically stable L4 Neptunian Trojans, 2013 VX30 and 2014 UU240, both with inclinations i > 30° making them the highest-inclination known stable Neptunian Trojans. We have measured the colors of these and three other dynamically stable Neptunian Trojans previously observed by DES, and find that 2013 VX30 is ultra-red, the first such Neptunian Trojan in its class. As such, 2013 VX30 may be a “missing link” between the Trojan and TNO populations. Using a simulation of the DES TNO detection efficiency, we find that there are 162 ± 73 Trojans with Hr < 10 at the L4 Lagrange point of Neptune. Moreover, the blue-to-red Neptunian Trojan population ratio should be higher than 17:1. Based on this result, we discuss the possible origin of the ultra-red Neptunian Trojan population and its implications for the formation history of Neptunian Trojans.

Published
2018
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42. Dark Energy Survey Year 1 results: curved-sky weak lensing mass map

Author

Peter Doel, H. T. Diehl, David Bacon, Niall MacCrann, C. Davis, J. Gschwend, C. B. D'Andrea, S. E. Kuhlmann, Gary Bernstein, David J. James, Daniel B. Thomas, S. Samuroff, J. Prat, Pablo Fosalba, Tesla E. Jeltema, E. Suchyta, Elisabeth Krause, K. Honscheid, T. Kacprzak, G. Gutierrez, Alex Drlica-Wagner, C. Bonnett, A. Benoit-Lévy, M. A. G. Maia, Michael Troxel, R. Cawthon, R. P. Rollins, A. A. Plazas, Daniel Gruen, E. M. Huff, Vinu Vikram, Shantanu Desai, J. Annis, Felipe Menanteau, E. Buckley-Geer, R. C. Smith, Douglas L. Tucker, Kyler Kuehn, M. D. Johnson, J. De Vicente, J. Carretero, Eli S. Rykoff, A. Alarcon, Eric H. Neilsen, I. Sevilla-Noarbe, Martin Crocce, Matt J. Jarvis, Ramon Miquel, Matthew Smith, Jack Elvin-Poole, Donnacha Kirk, B. Flaugher, A. Pujol, T. S. Li, C. Sánchez, Alistair R. Walker, J. P. Dietrich, Huan Lin, Eric J. Baxter, M. T. Busha, P. Vielzeuf, M. W. G. Johnson, A. Carnero Rosell, Don Petravick, Marcelle Soares-Santos, M. Gatti, Yanxi Zhang, Erin Sheldon, W. G. Hartley, T. N. Varga, David Brooks, W. C. Wester, Steve Kent, L. N. da Costa, Peter Melchior, Juan Garcia-Bellido, Attila Kovács, V. Scarpine, A. K. Romer, Eduardo Rozo, A. Roodman, D. L. Burke, Tommaso Giannantonio, Matthew R. Becker, Flavia Sobreira, Paul Martini, S. Allam, Robert A. Gruendl, Ricardo L. C. Ogando, Joshua A. Frieman, J. DeRose, A. Fausti Neto, Ben Hoyle, G. Tarle, Enrique Fernández, Marcos Lima, M. Sako, Markus Michael Rau, Keith Bechtol, M. March, Risa H. Wechsler, E. Bertin, Chihway Chang, Carlos E. Cunha, F. J. Castander, Enrique Gaztanaga, T. M. C. Abbott, Joseph J. Mohr, E. J. Sanchez, Juan Estrada, Joe Zuntz, B. Mawdsley, Michael Schubnell, M. Carrasco Kind, Robert C. Nichol, Filipe B. Abdalla, Bhuvnesh Jain, Ofer Lahav, Boris Leistedt, Niall Jeffrey, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, gravitational lensing: weak, surveys, 0103 physical sciences, media_common.cataloged_instance, European union, Astronomy observatory, 010303 astronomy & astrophysics, STFC, media_common, QB, Physics, 010308 nuclear & particles physics, European research, Astronomy, RCUK, Astronomy and Astrophysics, Space and Planetary Science, Research council, Fundamental physics, astro-ph.CO, Christian ministry, National laboratory, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We construct the largest curved-sky galaxy weak lensing mass map to date from the DES first-year (DES Y1) data. The map, about 10 times larger than previous work, is constructed over a contiguous $\approx1,500 $deg$^2$, covering a comoving volume of $\approx10 $Gpc$^3$. The effects of masking, sampling, and noise are tested using simulations. We generate weak lensing maps from two DES Y1 shear catalogs, Metacalibration and Im3shape, with sources at redshift $0.2, Comment: 25 pages, 19 figures, 1 table; revision with changes implemented according to journal referee

Published
2018
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43. Survey geometry and the internal consistency of recent cosmic shear measurements

Author

O. Friedrich, Marcos Lima, E. Suchyta, I. Sevilla-Noarbe, D. L. Hollowood, August E. Evrard, N. Kuropatkin, Juan Garcia-Bellido, L. N. da Costa, Daniel Thomas, Hiranya V. Peiris, Enrique Gaztanaga, Martin Crocce, Erin Sheldon, B. Flaugher, E. J. Sanchez, D. L. Burke, F. Lacasa, Ramon Miquel, Joseph J. Mohr, A. Roodman, K. Honscheid, C. B. D'Andrea, Donnacha Kirk, Alistair R. Walker, M. Gatti, David J. Brooks, Ofer Lahav, M. Carrasco Kind, J. Prat, J. De Vicente, Michael Troxel, C. Sánchez, V. Scarpine, Joshua A. Frieman, Marcelle Soares-Santos, J. Carretero, G. Gutierrez, S. Allam, Robert A. Gruendl, Flavia Sobreira, Ricardo L. C. Ogando, Matt J. Jarvis, Rafe Schindler, Risa H. Wechsler, Felipe Menanteau, P. Vielzeuf, Ben Hoyle, Tim Eifler, Meng Wang, Dragan Huterer, Kyler Kuehn, M. E. C. Swanson, Filipe B. Abdalla, J. Annis, P. Lemos, Elisabeth Krause, M. March, A. Carnero Rosell, S. Samuroff, Peter Doel, H. T. Diehl, David J. James, Pablo Fosalba, Niall MacCrann, A. A. Plazas, Joe Zuntz, J. DeRose, Tenglin Li, Scott Dodelson, Santiago Avila, Chihway Chang, Carlos E. Cunha, W. G. Hartley, E. Bertin, C. Davis, J. Gschwend, A. Chen, M. Smith, Daniel Gruen, D. W. Gerdes, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, gravitational lensing: weak, 0103 physical sciences, Statistical physics, Planck, 010303 astronomy & astrophysics, Physics, methods: statistical, COSMIC cancer database, 010308 nuclear & particles physics, Covariance matrix, Multiplicative function, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Covariance, methods: data analysis, Amplitude, Shear (geology), Space and Planetary Science, symbols, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We explore the impact of an update to the typical approximation for the shape noise term in the analytic covariance matrix for cosmic shear experiments that assumes the absence of survey boundary and mask effects. We present an exact expression for the number of galaxy pairs in this term based on the the survey mask, which leads to more than a factor of three increase in the shape noise on the largest measured scales for the Kilo-Degree Survey (KIDS-450) real-space cosmic shear data. We compare the result of this analytic expression to several alternative methods for measuring the shape noise from the data and find excellent agreement. This update to the covariance resolves any internal model tension evidenced by the previously large cosmological best-fit $\chi^2$ for the KiDS-450 cosmic shear data. The best-fit $\chi^2$ is reduced from 161 to 121 for 118 degrees of freedom. We also apply a correction to how the multiplicative shear calibration uncertainty is included in the covariance. This change, along with a previously known update to the reported effective angular values of the data vector, jointly shift the inferred amplitude of the correlation function to higher values. We find that this improves agreement of the KiDS-450 cosmic shear results with Dark Energy Survey Year 1 and Planck results., Comment: 7 pages, 2 figures; matches accepted version

Published
2018
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44. BAO from Angular Clustering: Optimization and Mitigation of Theoretical Systematics

Author

Elisabeth Krause, Daniel Thomas, Juan Garcia-Bellido, Martin Crocce, G. Gutierrez, Alistair R. Walker, Marcelle Soares-Santos, Kyler Kuehn, W. G. Hartley, E. Suchyta, Santiago Avila, Ashley J. Ross, Carlos E. Cunha, D. L. Burke, G. Tarle, C. Davis, J. Carretero, David J. James, Jack Elvin-Poole, Juan Estrada, J. Gschwend, Kevin Reil, Pablo Fosalba, V. Scarpine, Marcos Lima, Ramon Miquel, S. Allam, Robert A. Gruendl, Kwan Chuen Chan, Joshua A. Frieman, Ofer Lahav, Will J. Percival, A. A. Plazas, B. Flaugher, E. Bertin, A. Roodman, C. J. Miller, M. Manera, M. E. C. Swanson, A. Carnero Rosell, David J. Brooks, I. Sevilla-Noarbe, M. Smith, Rogerio Rosenfeld, Daniel Gruen, Ben Hoyle, L. N. da Costa, F. J. Castander, C. B. D'Andrea, D. W. Gerdes, Felipe Menanteau, T. M. C. Abbott, E. J. Sanchez, K. Honscheid, J. De Vicente, Flavia Sobreira, M. March, Tim Eifler, Filipe B. Abdalla, M. Carrasco Kind, Enrique Gaztanaga, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, UAM. Departamento de Física Teórica, Instituto de Física Teórica (IFT), Sun Yat Sen Univ, IEEC, CSIC, Ohio State Univ, Univ Portsmouth, Univ Autonoma Madrid, Univ Manchester, UCL, Universidade Estadual Paulista (Unesp), Lab Interinstituc & Astron LIneA, Natl Opt Astron Observ, Rhodes Univ, Fermilab Natl Accelerator Lab, Inst Astrophys Paris, UPMC Univ Paris 06, Stanford Univ, SLAC Natl Accelerator Lab, Observ Nacl, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, Univ Penn, CIEMAT, Steward Observ, CALTECH, Univ Chicago, Univ Michigan, Swiss Fed Inst Technol, Max Planck Inst Extraterrestrial Phys, Ludwig Maximilians Univ Munchen, Harvard Smithsonian Ctr Astrophys, Australian Astron Observ, Universidade de São Paulo (USP), Inst Catalana Recerca & Estudis Avancats, Univ Southampton, Universidade Estadual de Campinas (UNICAMP), and Oak Ridge Natl Lab

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, Gaussian, AST-1138766, Eigenmode expansion, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Statistical fluctuations, 01 natural sciences, symbols.namesake, 0103 physical sciences, Statistical physics, observations [Cosmology], 010303 astronomy & astrophysics, STFC, Physics, 010308 nuclear & particles physics, Covariance matrix, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Estimator, Física, Astronomy and Astrophysics, Markov chain Monte Carlo, Covariance, Space and Planetary Science, cosmology: observations, astro-ph.CO, symbols, Baryon acoustic oscillations, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the methodology and potential theoretical systematics of measuring Baryon Acoustic Oscillations (BAO) using the angular correlation functions in tomographic bins. We calibrate and optimize the pipeline for the Dark Energy Survey Year 1 dataset using 1800 mocks. We compare the BAO fitting results obtained with three estimators: the Maximum Likelihood Estimator (MLE), Profile Likelihood, and Markov Chain Monte Carlo. The fit results from the MLE are the least biased and their derived 1-$\sigma$ error bar are closest to the Gaussian distribution value after removing the extreme mocks with non-detected BAO signal. We show that incorrect assumptions in constructing the template, such as mismatches from the cosmology of the mocks or the underlying photo-$z$ errors, can lead to BAO angular shifts. We find that MLE is the method that best traces this systematic biases, allowing to recover the true angular distance values. In a real survey analysis, it may happen that the final data sample properties are slightly different from those of the mock catalog. We show that the effect on the mock covariance due to the sample differences can be corrected with the help of the Gaussian covariance matrix or more effectively using the eigenmode expansion of the mock covariance. In the eigenmode expansion, the eigenmodes are provided by some proxy covariance matrix. The eigenmode expansion is significantly less susceptible to statistical fluctuations relative to the direct measurements of the covariance matrix because of the number of free parameters is substantially reduced, Comment: 23 pages, 23 figs, match to the published version

Published
2018

45. Baryon Content in a Sample of 91 Galaxy Clusters Selected by the South Pole Telescope at 0.2 < z < 1.25

Author

R. C. Smith, N. Kuropatkin, J. Carretero, L. N. da Costa, Michael McDonald, Elisabeth Krause, J. P. Dietrich, H. Israel, C. B. D'Andrea, S. E. Kuhlmann, David J. James, G. Tarle, Brian Nord, G. Gutierrez, Vinu Vikram, Carlos E. Cunha, Joseph J. Mohr, A. Saro, F. B. Abdalla, Esra Bulbul, Juan Garcia-Bellido, B. Flaugher, Felipe Menanteau, S. S. Murray, Sebastian Bocquet, J. Hlavacek-L., Matthias Klein, V. Strazzullo, Jochen Weller, F. J. Castander, E. Buckley-Geer, Flavia Sobreira, R. Capasso, T. M. C. Abbott, V. Scarpine, D. Rapetti, Shantanu Desai, A. A. Plazas, Nikhel Gupta, Ramon Miquel, B. Stalder, Mark Brodwin, S. Allam, Robert A. Gruendl, M. A. G. Maia, M. L. N. Ashby, E. J. Sanchez, K. Honscheid, Jennifer L. Marshall, Anthony H. Gonzalez, Gordon P. Garmire, Enrique Gaztanaga, Tesla E. Jeltema, John E. Carlstrom, R. H. Schindler, Matthew B. Bayliss, A. Stanford, M. E. C. Swanson, Michael Schubnell, I-Non Chiu, Alistair R. Walker, Bradford Benson, Lindsey Bleem, Yanxi Zhang, Marcelle Soares-Santos, Keren Sharon, Christian L. Reichardt, Tim Eifler, M. Smith, A. Carnero Rosell, Daniel Gruen, Peter Melchior, C. Stern, Alex Drlica-Wagner, D. W. Gerdes, David J. Brooks, J. Annis, E. Suchyta, August E. Evrard, Ofer Lahav, R. L. C. Ogando, A. Benoit-Lévy, A. K. Romer, Ralph P. Kraft, Marcos Lima, A. Roodman, Peter Doel, H. T. Diehl, E. Bertin, C. Davis, J. Gschwend, Kyler Kuehn, 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, Chiu, I., Mohr, J. J., Mcdonald, M., Bocquet, S., Desai, S., Klein, M., Israel, H., Ashby, M. L. N., Stanford, A., Benson, B. A., Brodwin, M., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Bayliss, M., Benoit-Lévy, A., Bertin, E., Bleem, L., Brooks, D., Buckley-Geer, Bulbul, E., Capasso, R., Carlstrom, J. E., Rosell, A. Carnero, Carretero, J., Castander, F. J., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., García-Bellido, J., Garmire, G., Gaztanaga, E., Gerdes, D. W., Gonzalez, A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, N., Gutierrez, G., Hlavacek-L, J., Honscheid, K., James, D. J., Jeltema, T., Kraft, R., Krause, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Murray, S., Nord, B., Ogando, R. L. C., Plazas, A. A., Rapetti, D., Reichardt, C. L., Romer, A. K., Roodman, A., Sanchez, E., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Sharon, K., Smith, R. C., Smith, M., Soares-Santos, M., Sobreira, F., Stalder, B., Stern, C., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., Walker, A. R., Weller, J., and Zhang, Y.

Subjects
galaxies: clusters: individual, galaxies: clusters: intracluster medium, Stellar mass, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Virial theorem, Intracluster medium, 0103 physical sciences, galaxies: clusters: general, Astrophysics - Cosmology and Nongalactic Astrophysics, clusters: general [galaxies], 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, QB, Physics, clusters: individual [galaxies], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Redshift, Baryon, South Pole Telescope, clusters: intracluster medium [galaxies], 13. Climate action, Space and Planetary Science, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We estimate total mass ($M_{500}$), intracluster medium (ICM) mass ($M_{\mathrm{ICM}}$) and stellar mass ($M_{\star}$) in a Sunyaev-Zel'dovich effect (SZE) selected sample of 91 galaxy clusters with masses $M_{500}\gtrsim2.5\times10^{14}M_{\odot}$ and redshift $0.2 < z < 1.25$ from the 2500 deg$^2$ South Pole Telescope SPT-SZ survey. The total masses $M_{500}$ are estimated from the SZE observable, the ICM masses $M_{\mathrm{ICM}}$ are obtained from the analysis of $Chandra$ X-ray observations, and the stellar masses $M_{\star}$ are derived by fitting spectral energy distribution templates to Dark Energy Survey (DES) $griz$ optical photometry and $WISE$ or $Spitzer$ near-infrared photometry. We study trends in the stellar mass, the ICM mass, the total baryonic mass and the cold baryonic fraction with cluster mass and redshift. We find significant departures from self-similarity in the mass scaling for all quantities, while the redshift trends are all statistically consistent with zero, indicating that the baryon content of clusters at fixed mass has changed remarkably little over the past $\approx9$ Gyr. We compare our results to the mean baryon fraction (and the stellar mass fraction) in the field, finding that these values lie above (below) those in cluster virial regions in all but the most massive clusters at low redshift. Using a simple model of the matter assembly of clusters from infalling groups with lower masses and from infalling material from the low density environment or field surrounding the parent halos, we show that the measured mass trends without strong redshift trends in the stellar mass scaling relation could be explained by a mass and redshift dependent fractional contribution from field material. Similar analyses of the ICM and baryon mass scaling relations provide evidence for the so-called "missing baryons" outside cluster virial regions., Comment: Accepted by MNRAS with further clarification and discussion of the mass calibration added

Published
2018

46. The STRong lensing Insights into the Dark Energy Survey (STRIDES) 2016 follow-up campaign. II. New quasar lenses from double component fitting

Author

N. D. Morgan, E. Bertin, Timo Anguita, Cristian E. Rusu, B. Flaugher, Darren L. DePoy, C. B. D'Andrea, Peter Doel, W. G. Hartley, V. Scarpine, Nikolay Kuropatkin, H. T. Diehl, E. Buckley-Geer, M. Carrasco Kind, R. A. Bernstein, Shantanu Desai, J. De Vicente, J. H. Hsueh, A. A. Plazas, E. Suchyta, J. Gschwend, Tommaso Treu, Marcio A. G. Maia, D. L. Burke, P. Williams, Paul L. Schechter, Alistair R. Walker, Marcelle Soares-Santos, Gregory Tarle, J. Annis, S. Allam, Robert A. Gruendl, D. L. Hollowood, David Brooks, Flavia Sobreira, Ramon Miquel, Huan Lin, Marcos Lima, F. Ostrovski, Kyler Kuehn, Matthew W. Auger, Carlos E. Cunha, Adriano Agnello, Daniel Gruen, Yordanka Apostolovski, A. Carnero Rosell, T. M. C. Abbott, Veronica Motta, Louis E. Abramson, D. W. Gerdes, E. J. Sanchez, Matthew Smith, Juan Garcia-Bellido, K. Honscheid, Christopher D. Fassnacht, David J. James, K. Rojas, J. Carretero, Richard G. McMahon, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), UAM. Departamento de Física Teórica, and Instituto de Física Teórica (IFT)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Library science, FOS: Physical sciences, techniques: image processing, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, surveys, quasars: general, 0103 physical sciences, 010306 general physics, Astronomy observatory, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, business.industry, Física, gravitational lensing: strong, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Fundamental physics, Christian ministry, National laboratory, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report upon the follow up of 34 candidate lensed quasars found in the Dark Energy Survey using NTT-EFOSC, Magellan-IMACS, KECK-ESI and SOAR-SAMI. These candidates were selected by a combination of double component fitting, morphological assessment and color analysis. Most systems followed up are indeed composed of at least one quasar image and 13 with two or more quasar images: two lenses, four projected binaries and seven Nearly Identical Quasar Pairs (NIQs). The two systems confirmed as genuine gravitationally lensed quasars are one quadruple at zs=1.713 and one double at zs=1.515. Lens modeling of these two systems reveals that both systems require very little contribution from the environment to reproduce the image configuration. Nevertheless, small flux anomalies can be observed in one of the images of the quad. Further observations of 9 inconclusive systems (including 7 NIQs) will allow to confirm (or not) their gravitational lens nature., T. A. acknowledges support by proyecto FONDECYT 11130630 and by the Ministry for the Economy, Development, and Tourism's Programa Inicativa Científica Milenio through grant IC 12009, awarded to The Millennium Institute of Astrophysics (MAS). T.T. and V.M. acknowledge support by the Packard Foundation through a Packard Research Fellowship to T.T. T.T. acknowledges support by the National Science Foundation through grant AST-1450141. 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, Fundacâo Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministerio da Ciência, Tecnologia e Inovacâo, 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 Eidgen össische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig- Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium

Published
2018
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47. A catalogue of structural and morphological measurements for DES Y1

Author

Peter Doel, David J. Brooks, A. A. Plazas, Devon L. Hollowood, Tesla E. Jeltema, Asa F. L. Bluck, Adam Amara, Clare Davis, Alistair R. Walker, Claudio Bruderer, Robert Chris Smith, David J. James, E. J. Sanchez, Bruno Moraes, Marcelle Soares-Santos, Marcella Carollo, E. Suchyta, Aurelio Carnero Rosell, D. L. Burke, Rafe Schindler, Elisabeth Krause, Alexandre Refregier, Joanna Woo, Juan Garcia-Bellido, Molly E. C. Swanson, K. Honscheid, Christopher J. Conselice, Kyler Kuehn, Flavia Sobreira, Shantanu Desai, Ofer Lahav, J. Carretero, S. Allam, Robert A. Gruendl, M. Banerji, Mathew Smith, Joshua A. Frieman, Santiago Javier Avila Perez, Daniel Thomas, Ramon Miquel, Emmanuel Bertin, C. B. D'Andrea, Vinu Vikram, Carlos E. Cunha, Timothy M. C. Abbott, I. Sevilla-Noarbe, Matias Carrasco Kind, Basilio X. Santiago, Felipe Menanteau, Juan De Vincente, A. Kathy Romer, Gregory Tarle, L. N. da Costa, N. P. Kuropatkin, F. Tarsitano, G. Gutierrez, Peter Melchior, A. Roodman, William G. Hartley, Daniel Gruen, Marcio A. G. Maia, James Annis, Juan Estrada, 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
Galaxy structure, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Magnitude (mathematics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, Cosmology, surveys, Galaxy evolution, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, QC, STFC, Astrophysics::Galaxy Astrophysics, catalogues, QB, Parametric statistics, Physics, 010308 nuclear & particles physics, Estimator, RCUK, Astronomy and Astrophysics, Position angle, Astrophysics - Astrophysics of Galaxies, galaxies: general, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a structural and morphological catalogue for 45 million objects selected from the first year of data from 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, Sersic 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 the measurements as a function of magnitude, 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% below this threshold, for a total of 25 million 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 Dark Energy Survey collaboration Y1 cosmology data products at the following URL: https://des.ncsa.illinois.edu/releases/y1a1/gold/morphology., Accepted for publication in MNRAS. 26 pages, 16 figures. Catalogue data are available at https://des.ncsa.illinois.edu/releases/y1a1/gold/morphology

Published
2018

48. Extreme variability quasars from the Sloan Digital Sky Survey and the Dark Energy Survey

Author

Darren L. DePoy, Yue Shen, K. Honscheid, Carlos E. Cunha, Chris B. D'Andrea, J. Gschwend, Alistair R. Walker, Kevin Reil, A. Benoit-Lévy, Marcelle Soares-Santos, Felipe Menanteau, Marcio A. G. Maia, William Wester, J. Carretero, Nikolay Kuropatkin, Kyler Kuehn, David J. Brooks, Rafe Schindler, Shantanu Desai, Luiz N. da Costa, Eric Morganson, Aurelio Carnero Rosell, Richard G. McMahon, Mathew Smith, G. Gutierrez, Jennifer L. Marshall, Robert A. Gruendl, Juan Garcia-Bellido, Diego Capozzi, Manda Banerji, Michael Schubnell, V. Scarpine, David J. James, E. Buckley-Geer, Emmanuel Bertin, Marcos Lima, A. Roodman, Paul Martini, Molly E. C. Swanson, Erin S. Sheldon, Filipe B. Abdalla, Xin Liu, Andres Plazas Malagon, E. Suchyta, Peter Doel, E. J. Sanchez, Joshua A. Frieman, Steve Kuhlmann, Flavia Sobreira, Nick Rumbaugh, Daniel Gruen, M. Carrasco Kind, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Population, black hole physics, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, surveys, quasars: general, 0103 physical sciences, Emission spectrum, education, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, media_common, Physics, education.field_of_study, Accretion (meteorology), 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Quasar, line: profiles, Light curve, Astrophysics - Astrophysics of Galaxies, Redshift, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We perform a systematic search for long-term extreme variability quasars (EVQs) in the overlapping Sloan Digital Sky Survey (SDSS) and 3-Year Dark Energy Survey (DES) imaging, which provide light curves spanning more than 15 years. We identified ~1000 EVQs with a maximum g band magnitude change of more than 1 mag over this period, about 10% of all quasars searched. The EVQs have L_bol~10^45-10^47 erg/s and L/L_Edd~0.01-1. Accounting for selection effects, we estimate an intrinsic EVQ fraction of ~30-50% among all g, Comment: submitted to ApJ; comments welcome

Published
2018

49. On the relative bias of void tracers in the Dark Energy Survey

Author

Shantanu Desai, David J. James, Pablo Fosalba, Ramon Miquel, Jennifer L. Marshall, B. Flaugher, K. Honscheid, G. Gutierrez, Eli S. Rykoff, W. C. Wester, G. Pollina, Alistair R. Walker, Marcelle Soares-Santos, C. Sánchez, V. Scarpine, A. Carnero Rosell, Rafe Schindler, J. De Vicente, Flavia Sobreira, Joshua A. Frieman, Peter Doel, J. Carretero, Felipe Menanteau, I. Sevilla-Noarbe, M. March, H. T. Diehl, Gregory Tarle, N. Kuropatkin, Peter Melchior, Kyler Kuehn, J. Gschwend, L. N. da Costa, M. Smith, Tommaso Giannantonio, D. L. Burke, Daniel Gruen, Juan Garcia-Bellido, Ben Hoyle, S. Allam, D. W. Gerdes, E. Bertin, Klaus Dolag, A. K. Romer, Tesla E. Jeltema, K. Paech, Marcos Lima, D. L. DePoy, D. L. Hollowood, E. Suchyta, August E. Evrard, David J. Brooks, Jochen Weller, T. M. C. Abbott, E. J. Sanchez, R. A. Bernstein, Santiago Avila, Carlos E. Cunha, A. A. Plazas, W. G. Hartley, Nico Hamaus, C. B. D'Andrea, Michael Schubnell, M. Carrasco Kind, Bhuvnesh Jain, 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
Void (astronomy), Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spatial distribution, 01 natural sciences, 0103 physical sciences, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, QB, media_common, Physics, COSMIC cancer database, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, Universe, Amplitude, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, Dark energy, large-scale structure of Universe, CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Luminous tracers of large-scale structure are not entirely representative of the distribution of mass in our Universe. As they arise from the highest peaks in the matter density field, the spatial distribution of luminous objects is biased towards those peaks. On large scales, where density fluctuations are mild, this bias simply amounts to a constant offset in the clustering amplitude of the tracer, known as linear bias. In this work we focus on the relative bias between galaxies and galaxy clusters that are located inside and in the vicinity of cosmic voids, extended regions of relatively low density in the large-scale structure of the Universe. With the help of hydro-dynamical simulations we verify that the relation between galaxy and cluster overdensity around voids remains linear. Hence, the void-centric density profiles of different tracers can be linked by a single multiplicative constant. This amounts to the same value as the relative linear bias between tracers for the largest voids in the sample. For voids of small sizes, which typically arise in higher density regions, this constant has a higher value, possibly showing an environmental dependence similar to that observed for the linear bias itself. We confirm our findings by analysing mocks and data obtained during the first year of observations by the Dark Energy Survey. As a side product, we present the first catalogue of three-dimensional voids extracted from a photometric survey with a controlled photo-z uncertainty. Our results will be relevant in forthcoming analyses that attempt to use voids as cosmological probes., Comment: 17 pages, 13 figures, MNRAS submitted

Published
2018
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50. A multicomponent matched filter cluster confirmation tool for eROSITA: initial application to the RASS and DES-SV data sets

Author

Michael Schubnell, Kevin Reil, A. Benoit-Lévy, V. Scarpine, David J. James, J. P. Dietrich, Ramon Miquel, Daniel Gruen, Joseph J. Mohr, Peter Melchior, A. Carnero Rosell, G. Gutierrez, Shantanu Desai, H. Israel, Mathew Smith, Kyler Kuehn, K. Honscheid, M. Carrasco Kind, E. Suchyta, August E. Evrard, M. A. G. Maia, Felipe Menanteau, M. Klein, A. A. Plazas, Flavia Sobreira, M. March, Basilio X. Santiago, M. E. C. Swanson, E. Buckley-Geer, Marcos Lima, G. Tarle, Marcelle Soares-Santos, Tim Eifler, David Brooks, Joshua A. Frieman, I. Sevilla-Noarbe, L. N. da Costa, E. J. Sanchez, S. Allam, Robert A. Gruendl, Carlos E. Cunha, A. K. Romer, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Institut 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, ROSAT, 010303 astronomy & astrophysics, Luminosity function, QC, Remote sensing, Photometric redshift, Physics, 010308 nuclear & particles physics, Matched filter, Astronomy and Astrophysics, Redshift, South Pole Telescope, Space and Planetary Science, galaxies: clusters: general, X-rays: galaxies: clusters, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe a multi-component matched filter cluster confirmation tool (MCMF) designed for the study of large X-ray source catalogs produced by the upcoming X-ray all-sky survey mission eROSITA. We apply the method to confirm a sample of 88 clusters with redshifts $0.05, Comment: 20 pages, 19 figures

Published
2018

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