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1. DES science portal: Computing photometric redshifts

Author

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

Published
2018
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2. Velocity dispersions of clusters in the Dark Energy Survey Y3 redMaPPer catalogue

Author

A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, UAM. Departamento de Física Teórica, A Wetzell, V., Jeltema, T. E., Hegland, B., Everett, S., Giles, P. A., Wilkinson, R., Farahi, A., Costanzi, M., Hollowood, D. L., Upsdell, E., Saro, A., Myles, J., Bermeo, A., Bhargava, S., Collins, C. A., Cross, D., Eiger, O., Gardner, G., Hilton, M., Jobel, J., Kelly, P., Laubner, D., Liddle, A. R., Mann, R. G., Martinez, V., Mayers, J., Mcdaniel, A., Romer, A. K., Rooney, P., Sahlen, M., Stott, J., Swart, A., Turner, D. J., Viana, P. T. P., Abbott, T. M. C., Aguena, M., Allam, S., Andrade- Oliveira, F., Annis, J., Asorey, J., Bertin, E., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Evrard, A. E., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lewis, G. F., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., Tucker, B. E., Tucker, D. L., Varga, T. N., Weller, J., Des, Collaboration, Department of Energy (US), European Commission, European Research Council, Ministero dell'Istruzione, dell'Università e della Ricerca, Ministerio de Ciencia, Innovación y Universidades (España), Fundação para a Ciência e a Tecnologia (Portugal), Agencia Estatal de Investigación (España), National Science Foundation (US), Generalitat de Catalunya, and Ministerio de Economía y Competitividad (España)

Subjects
X-Rays: Galaxies: Clusters, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Física, Astronomy and Astrophysics, galaxies: clusters: general, X-rays: galaxies: clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Space and Planetary Science, clusters: general [galaxies], galaxies: clusters [X-rays], CLUSTERS, QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB, Galaxies: Clusters: General
Abstract

DES Collaboration: V. Wetzell et al., We measure the velocity dispersions of clusters of galaxies selected by the red-sequence Matched-filter Probabilistic Percolation (redMaPPer) algorithm in the first three years of data from the Dark Energy Survey (DES), allowing us to probe cluster selection and richness estimation, λ, in light of cluster dynamics. Our sample consists of 126 clusters with sufficient spectroscopy for individual velocity dispersion estimates. We examine the correlations between cluster velocity dispersion, richness, X-ray temperature, and luminosity, as well as central galaxy velocity offsets. The velocity dispersion–richness relation exhibits a bimodal distribution. The majority of clusters follow scaling relations between velocity dispersion, richness, and X-ray properties similar to those found for previous samples; however, there is a significant population of clusters with velocity dispersions that are high for their richness. These clusters account for roughly 22 per cent of the λ < 70 systems in our sample, but more than half (55 per cent) of λ < 70 clusters at z > 0.5. A couple of these systems are hot and X-ray bright as expected for massive clusters with richnesses that appear to have been underestimated, but most appear to have high velocity dispersions for their X-ray properties likely due to line-of-sight structure. These results suggest that projection effects contribute significantly to redMaPPer selection, particularly at higher redshifts and lower richnesses. The redMaPPer determined richnesses for the velocity dispersion outliers are consistent with their X-ray properties, but several are X-ray undetected and deeper data are needed to understand their nature., This work was supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Numbers DE-SC0010107 and A00-1465-001. AS is supported by the ERC-StG ‘ClustersXCosmo’ grant agreement 716762, by the FARE-MIUR grant ’ClustersXEuclid’ R165SBKTMA, and by INFN InDark Grant. PTPV was supported by Fundação para a Ciência e a Tecnologia (FCT) through research grants UIDB/04434/2020andUIDP/04434/2020. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the University of Illinois at Urbana-Champaign - National Center for Supercomputing Applications, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California, Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas – Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians-Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This study is based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the EU Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under contract no. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2022

3. Kinematic and thermal signatures of the directly imaged protoplanet candidate around Elias 2−24.

Author

Pinte, C, Hammond, I, Price, D J, Christiaens, V, Andrews, S M, Chauvin, G, Pérez, L M, Jorquera, S, Garg, H, Norfolk, B J, Calcino, J, and Bonnefoy, M

Subjects
PLANETARY mass, GAS giants, NATURAL satellites, PROTOPLANETARY disks, HEATING
Abstract

We report kinematic and thermal signatures associated with the directly imaged protoplanet candidate in the Elias 2–24 disc. Using the DSHARP (Disc Substructures at High Angular Resolution Project) ALMA (Atacama Large Millimetre/submillimetre Array) observations of the 12CO J = 2 − 1 line, we show that the disc kinematics are perturbed, with a detached CO emission spot at the location of the planet candidate and traces of spiral wakes, and also that the observed CO emission intensities require local heating. While the foreground extinction hides the velocity channels associated with the planet, preventing a planet mass estimate, the level of gas heating implied by the CO emission indicates the presence of a warm, embedded giant planet. Comparison with models shows that this could either be a ≳5 MJup or a lower mass (≳2 MJup) but accreting protoplanet. [ABSTRACT FROM AUTHOR]

Published
2023
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4. kinematic excess in the annular gap and gas-depleted cavity in the disc around HD 169142.

Author

Garg, H, Pinte, C, Hammond, I, Teague, R, Hilder, T, Price, D J, Calcino, J, Christiaens, V, and Poblete, P P

Subjects
ORIGIN of planets, CIRCUMSTELLAR matter, SPATIAL resolution, SURFACE reconstruction, ORBITS (Astronomy)
Abstract

We present ALMA band 6 images of the 12CO, 13CO, and C18O J  = 2-1 line emissions for the circumstellar disc around HD 169142, at ∼8 au spatial resolution. We resolve a central gas-depleted cavity, along with two independent near-symmetric ring-like structures in line emission: a well-defined inner gas ring [∼25 au] and a second relatively fainter and diffuse outer gas ring [∼65 au]. We identify a localized super-Keplerian feature or vertical flow with a magnitude of ∼75 ms−1 in the 12CO map. This feature has the shape of an arc that spans azimuthally across a position angle range of −60° to 45° and radially in between the B1[26au] and B2[59au] dust rings. Through reconstruction of the gas surface density profile, we find that the magnitude of the background perturbations by the pressure support and self-gravity terms are not significant enough to account for the kinematic excess. If of planetary origin, the relative depletion in the gas-density profile would suggest a 1 MJ planet. In contrast, the central cavity displays relatively smooth kinematics, suggesting either a low-mass companion and/or a binary orbit with a minimal vertical velocity component. [ABSTRACT FROM AUTHOR]

Published
2022
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5. protoplanetary disc around HD 169142: circumstellar or circumbinary?

Author

Poblete, P P, Cuello, N, Pérez, S, Marino, S, Calcino, J, Macías, E, Ribas, Á, Zurlo, A, Cuadra, J, Montesinos, M, Zúñiga-Fernández, S, Bayo, A, Pinte, C, Ménard, F, and Price, D J

Subjects
PROTOPLANETARY disks, GAS distribution, PLANETARY orbits
Abstract

Stellar binaries represent a substantial fraction of stellar systems, especially among young stellar objects. Accordingly, binaries play an important role in setting the architecture of a large number of protoplanetary discs. Binaries in coplanar and polar orientations with respect to the circumbinary disc are stable configurations and could induce non-axisymmetric structures in the dust and gas distributions. In this work, we suggest that the structures shown in the central region of the protoplanetary disc HD 169142 are produced by the presence of an inner stellar binary and a circumbinary (P-type) planet. We find that a companion with a mass ratio of 0.1, semimajor axis of 9.9 au, eccentricity of 0.2, and inclination of 90°, together with a 2  M J coplanar planet on a circular orbit at 45 au reproduce the structures at the innermost ring observed at 1.3 mm and the shape of spiral features in scattered light observations. The model predicts changes in the disc's dust structure, and star's astrometric parameters, which would allow testing its veracity by monitoring this system over the next 20 yr. [ABSTRACT FROM AUTHOR]

Published
2022
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6. First Cosmology Results Using Type Ia Supernovae From the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation

Author

Brout, D., Scolnic, D., Kessler, R., D'Andrea, C. B., Davis, T. M., Gupta, R. R., Hinton, S. R., Kim, A. G., Lasker, J., Lidman, C., Macaulay, E., M��ller, A., Nichol, R. C., Sako, M., Smith, M., Sullivan, M., Zhang, B., Andersen, P., Asorey, J., Avelino, A., Bassett, B. A., Brown, P., Calcino, J., Carollo, D., Challis, P., Childress, M., Clocchiatti, A., Filippenko, A. V., Foley, R. J., Galbany, L., Glazebrook, K., Hoormann, J. K., Kasai, E., Kirshner, R. P., Kuehn, K., Kuhlmann, S., Lewis, G. F., Mandel, K. S., March, M., Miranda, V., Morganson, E., Muthukrishna, D., Nugent, P., Palmese, A., Pan, Y. -C., Sharp, R., Sommer, N. E., Swann, E., Thomas, R. C., Tucker, B. E., Uddin, S. A., Wester, W., Abbott, T. M. C., Allam, S., Annis, J., Avila, S., Bechtol, K., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DePoy, D. L., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Estrada, J., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jarvis, M., Jeltema, T., Krause, E., Lahav, O., Li, T. S., Lima, M., Maia, M. A. G., Marriner, J., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Zhang, Y., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified type Ia supernovae (SNe Ia) from the first three years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017, Comment: 30 Pages, 18 Figures, 12 Tables. Submitted to ApJ. Comments welcome

Published
2019

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

Author

D'Andrea, C. B., Smith, M., Sullivan, M., Nichol, R. C., Thomas, R. C., Kim, A. G., Möller, A., Sako, M., Castander, F. J., Filippenko, A. V., Foley, R. J., Galbany, L., González-Gaitán, S., Kasai, E., Kirshner, R. P., Lidman, C., Scolnic, D., Brout, D., Davis, T. M., Gupta, R. R., Hinton, S. R., Kessler, R., Lasker, J., Macaulay, E., Wolf, R. C., Zhang, B., Asorey, J., Avelino, A., Bassett, B. A., Calcino, J., Carollo, D., Casas, R., Challis, P., Childress, M., Clocchiatti, A., Crawford, S., Glazebrook, K., Goldstein, D. A., Graham, M. L., Hoormann, J. K., Kuehn, K., Lewis, G. F., Mandel, K. S., Morganson, E., Muthukrishna, D., Nugent, P., Pan, Y. -C., Pursiainen, M., Sharp, R., Sommer, N. E., Swann, E., Tucker, B. E., Uddin, S. A., Wiseman, P., Zheng, W., Abbott, T. M. C., Annis, J., Avila, S., Bechtol, K., Bernstein, G. M., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Eifler, T. F., Estrada, J., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Johnson, M. W. G., Johnson, M. D., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Sobreira, F., Suchyta, E., Tarle, G., Tucker, D. L., Wester, W., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present spectroscopy from the first three seasons of the Dark Energy Survey Supernova Program (DES-SN). We describe the supernova spectroscopic program in full: strategy, observations, data reduction, and classification. We have spectroscopically confirmed 307 supernovae, including 251 type Ia supernovae (SNe Ia) over a redshift range of $0.017 < z < 0.85$. We determine the effective spectroscopic selection function for our sample, and use it to investigate the redshift-dependent bias on the distance moduli of SNe Ia we have classified. We also provide a full overview of the strategy, observations, and data products of DES-SN, which has discovered 12,015 likely supernovae during these first three seasons. The data presented here are used for the first cosmology analysis by DES-SN ('DES-SN3YR'), the results of which are given in DES Collaboration (2018a)., 25 pages, 14 figures, 8 tables. Submitted to AJ

Published
2018

8. OzDES Reverberation Mapping Programme: the first Mg ii lags from 5 yr of monitoring.

Author

Yu, Zhefu, Martini, Paul, Penton, A, Davis, T M, Malik, U, Lidman, C, Tucker, B E, Sharp, R, Kochanek, C S, Peterson, B M, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Asorey, J, Bertin, E, Brooks, D, Burke, D L, Calcino, J, and Carnero Rosell, A

Subjects
QUASARS, SUPERMASSIVE black holes, DARK energy
Abstract

Reverberation mapping is a robust method to measure the masses of supermassive black holes outside of the local Universe. Measurements of the radius–luminosity (R − L) relation using the Mg  ii emission line are critical for determining these masses near the peak of quasar activity at z ≈ 1−2, and for calibrating secondary mass estimators based on Mg  ii that can be applied to large samples with only single-epoch spectroscopy. We present the first nine Mg  ii lags from our 5-yr Australian Dark Energy Survey reverberation mapping programme, which substantially improves the number and quality of Mg  ii lag measurements. As the Mg  ii feature is somewhat blended with iron emission, we model and subtract both the continuum and iron contamination from the multiepoch spectra before analysing the Mg  ii line. We also develop a new method of quantifying correlated spectroscopic calibration errors based on our numerous, contemporaneous observations of F-stars. The lag measurements for seven of our nine sources are consistent with both the H β and Mg  ii   R − L relations reported by previous studies. Our simulations verify the lag reliability of our nine measurements, and we estimate that the median false positive rate of the lag measurements is |$4{{\ \rm per\ cent}}$|⁠. [ABSTRACT FROM AUTHOR]

Published
2021
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9. OzDES multi-object fibre spectroscopy for the Dark Energy Survey: results and second data release.

Author

Lidman, C, Tucker, B E, Davis, T M, Uddin, S A, Asorey, J, Bolejko, K, Brout, D, Calcino, J, Carollo, D, Carr, A, Childress, M, Hoormann, J K, Foley, R J, Galbany, L, Glazebrook, K, Hinton, S R, Kessler, R, Kim, A G, King, A, and Kremin, A

Abstract

We present a description of the Australian Dark Energy Survey (OzDES) and summarize the results from its 6 years of operations. Using the 2dF fibre positioner and AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope, OzDES has monitored 771 active galactic nuclei, classified hundreds of supernovae, and obtained redshifts for thousands of galaxies that hosted a transient within the 10 deep fields of the Dark Energy Survey. We also present the second OzDES data release, containing the redshifts of almost 30 000 sources, some as faint as r AB = 24 mag, and 375 000 individual spectra. These data, in combination with the time-series photometry from the Dark Energy Survey, will be used to measure the expansion history of the Universe out to z ∼ 1.2 and the masses of hundreds of black holes out to z ∼ 4. OzDES is a template for future surveys that combine simultaneous monitoring of targets with wide-field imaging cameras and wide-field multi-object spectrographs. [ABSTRACT FROM AUTHOR]

Published
2020
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10. C  iv black hole mass measurements with the Australian Dark Energy Survey (OzDES).

Author

Hoormann, J K, Martini, P, Davis, T M, King, A, Lidman, C, Mudd, D, Sharp, R, Sommer, N E, Tucker, B E, Yu, Z, Allam, S, Asorey, J, Avila, S, Banerji, M, Brooks, D, Buckley-Geer, E, Burke, D L, Calcino, J, Carnero Rosell, A, and Carollo, D

Subjects
DARK energy, BLACK holes, QUASARS, SUPERMASSIVE black holes, MASS measurement, GALACTIC evolution
Abstract

Black hole mass measurements outside the local Universe are critically important to derive the growth of supermassive black holes over cosmic time, and to study the interplay between black hole growth and galaxy evolution. In this paper, we present two measurements of supermassive black hole masses from reverberation mapping (RM) of the broad C  iv emission line. These measurements are based on multiyear photometry and spectroscopy from the Dark Energy Survey Supernova Program (DES-SN) and the Australian Dark Energy Survey (OzDES), which together constitute the OzDES RM Program. The observed reverberation lag between the DES continuum photometry and the OzDES emission line fluxes is measured to be |$358^{+126}_{-123}$| and |$343^{+58}_{-84}$| d for two quasars at redshifts of 1.905 and 2.593, respectively. The corresponding masses of the two supermassive black holes are 4.4 × 109 and 3.3 × 109 M⊙, which are among the highest redshift and highest mass black holes measured to date with RM studies. We use these new measurements to better determine the C  iv radius−luminosity relationship for high-luminosity quasars, which is fundamental to many quasar black hole mass estimates and demographic studies. [ABSTRACT FROM AUTHOR]

Published
2019
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11. First cosmology results using Type Ia supernova from the Dark Energy Survey: simulations to correct supernova distance biases.

Author

Kessler, R, Brout, D, D'Andrea, C B, Davis, T M, Hinton, S R, Kim, A G, Lasker, J, Lidman, C, Macaulay, E, Möller, A, Sako, M, Scolnic, D, Smith, M, Sullivan, M, Zhang, B, Andersen, P, Asorey, J, Avelino, A, Calcino, J, and Carollo, D

Subjects
TYPE I supernovae, DARK energy, LIGHT curves, DISTANCES, PHYSICAL cosmology, SUPERNOVAE
Abstract

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

Published
2019
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12. Rapidly evolving transients in the Dark Energy Survey.

Author

Pursiainen, M, Childress, M, Smith, M, Prajs, S, Sullivan, M, Davis, T M, Foley, R J, Asorey, J, Calcino, J, and Carollo, D

Subjects
DARK energy, SUPERNOVAE, STELLAR evolution, GALACTIC redshift, GALAXIES
Abstract

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 > M g > −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. [ABSTRACT FROM AUTHOR]

Published
2018
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13. OzDES Reverberation Mapping Program: Lag recovery reliability for 6-year CIV analysis

Author

G. Tarle, Maria E. S. Pereira, E. Suchyta, R. D. Wilkinson, Daniela Carollo, I. Ferrero, A. Carnero Rosell, Samuel Hinton, J. Gschwend, Tim Eifler, Kyler Kuehn, M. E. C. Swanson, G. Gutierrez, Juan Garcia-Bellido, J. Carretero, Tamara M. Davis, Rob Sharp, Sunayana Bhargava, David J. Brooks, Antonella Palmese, M. A. G. Maia, M. Smith, D. L. Hollowood, Daniel Gruen, J. K. Hoormann, C. Lidman, B. E. Tucker, S. Serrano, Jennifer L. Marshall, A. K. Romer, Daniel Scolnic, Paul Martini, Josh Frieman, Enrique Gaztanaga, Anais Möller, E. Bertin, S. A. Uddin, D. W. Gerdes, J. Calcino, David J. James, A. A. Plazas, H. T. Diehl, David Bacon, A. Penton, A. G. Kim, Pablo Fosalba, M. Carrasco Kind, Ramon Miquel, M. Costanzi, K. Honscheid, J. Annis, J. De Vicente, W. C. Wester, S. Everett, S. Allam, Robert A. Gruendl, F. Paz-Chinchón, Felipe Menanteau, V. Scarpine, U. Malik, Chun-Hao To, Michel Aguena, E. J. Sanchez, Jacobo Asorey, N. Kuropatkin, Zhefu Yu, T. N. Varga, L. N. da Costa, Robert Morgan, 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), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), DES, Penton, A, Malik, U, Davis, T M, Martini, P, Yu, Z, Sharp, R, Lidman, C, Tucker, B E, Hoormann, J K, Aguena, M, Allam, S, Annis, J, Asorey, J, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Calcino, J, Carnero&nbsp, Rosell, A, Carollo, D, Carrasco&nbsp, Kind, M, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, De&nbsp, Vicente, J, Diehl, H T, Eifler, T F, Everett, S, Ferrero, I, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hinton, S R, Hollowood, D L, Honscheid, K, James, D J, Kim, A G, Kuehn, K, Kuropatkin, N, Maia, M A G, Marshall, J L, Menanteau, F, Miquel, R, Morgan, R, Möller, A, Palmese, A, Paz-Chinchón, F, Plazas, A A, Romer, A K, Sanchez, E, Scarpine, V, Scolnic, D, Serrano, S, Smith, M, Suchyta, E, Swanson, M E C, Tarle, G, To, C, Uddin, S A, Varga, T N, Wester, W, Wilkinson, R D, Lewis, G, National Science Foundation (US), Ministerio de Ciencia e Innovación (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), and UAM. Departamento de Física Teórica

Subjects
galaxies: active, quasars: emission lines, quasars: general, Astrophysics - Astrophysics of Galaxies, Lag, FOS: Physical sciences, 01 natural sciences, emission lines [Quasars], statistical analysis, (Galaxies:) Quasars: Emission Lines, 0103 physical sciences, quasar, silver, AGN, 010303 astronomy & astrophysics, Reliability (statistics), Physics, [PHYS]Physics [physics], general [quasars], 010308 nuclear & particles physics, ) Quasars: Emission Lines [(Galaxies], Física, Astronomy and Astrophysics, gold, (Galaxies:) Quasars: Supermassive Black Holes, Nuclei, Reliability engineering, emission line [quasars], Space and Planetary Science, quality, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], slope, Reverberation mapping, dispersion, galaxy, statistical, ) Quasars: Supermassive Black Holes [(Galaxies]
Abstract

Penton, A. et al (DES Collaboration), We present the statistical methods that have been developed to analyse the OzDES reverberation mapping sample. To perform this statistical analysis we have created a suite of customizable simulations that mimic the characteristics of each source in the OzDES sample. These characteristics include: the variability in the photometric and spectroscopic light curves, the measurement uncertainties, and the observational cadence. By simulating the sources in the OzDES sample that contain the C iv emission line, we developed a set of criteria that rank the reliability of a recovered time-lag depending on the agreement between different recovery methods, the magnitude of the uncertainties, and the rate at which false positives were found in the simulations. These criteria were applied to simulated light curves and these results used to estimate the quality of the resulting Radius-Luminosity relation. We grade the results using three quality levels (gold, silver, and bronze). The input slope of the R-L relation was recovered within 1σ for each of the three quality samples, with the gold standard having the lowest dispersion with a recovered a R-L relation slope of 0.454 ± 0.016 with an input slope of 0.47. Future work will apply these methods to the entire OzDES sample of 771 AGN., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).

Published
2021

14. OzDES Reverberation Mapping Programme: The first Mg ii lags from 5 yr of monitoring

Author

I. Ferrero, Antonella Palmese, I. Sevilla-Noarbe, M. Soares-Santos, Paul Martini, N. Kuropatkin, Zhefu Yu, M. A. G. Maia, J. Calcino, B. Flaugher, Josh Frieman, David J. James, A. Penton, L. N. da Costa, Anais Möller, M. March, A. G. Kim, Bradley M. Peterson, Ramon Miquel, A. A. Plazas, E. Bertin, Tamara M. Davis, Geraint F. Lewis, Juan Garcia-Bellido, Douglas L. Tucker, Kyler Kuehn, Rob Sharp, H. T. Diehl, Jacobo Asorey, C. Lidman, B. E. Tucker, J. Annis, D. L. Burke, D. L. Hollowood, S. Serrano, M.E. da Silva Pereira, M. Smith, M. Costanzi, Robert Morgan, Daniel Gruen, Enrique Gaztanaga, S. Allam, Robert A. Gruendl, D. W. Gerdes, G. Tarle, Jennifer L. Marshall, J. Gschwend, V. Scarpine, Daniel Thomas, S. Everett, Michel Aguena, Christopher S. Kochanek, Daniela Carollo, F. Paz-Chinchón, U. Malik, M. Carrasco Kind, F. Andrade-Oliveira, Samuel Hinton, G. Gutierrez, Richard G. Kron, Felipe Menanteau, E. Suchyta, David J. Brooks, A. Carnero Rosell, Chun-Hao To, E. J. Sanchez, Yu, Z., Martini, P., Penton, A., Davis, T. M., Malik, U., Lidman, C., Tucker, B. E., Sharp, R., Kochanek, C. S., Peterson, B. M., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Asorey, J., Bertin, E., Brooks, D., Burke, D. L., Calcino, J., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Costanzi, M., Da Costa, L. N., Da Silva Pereira, M. E. S., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kim, A. G., Kron, R., Kuehn, K., Kuropatkin, N., Lewis, G. F., Maia, M. A. G., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Moller, A., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Tucker, D. L., The Ohio State University, Harvard University, University of Queensland, ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australian National University, Australian Astronomical Observatory, 3700 San Martin Drive, Universidade de São Paulo (USP), LineA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Medioambientales y Tecnológicas (CIEMAT), Institut D'Astrophysique DeParis, Institutd'Astrophysique de Paris, Gower Street, SLAC National Accelerator Laboratory, Stanford University, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, Astrophysical Observatory of Turin, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, University of Trieste, Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Santa Cruz Institute for Particle Physics, University of Oslo, University of Chicago, Universidad Autonoma de Madrid, CSIC), Institut D'Estudis Espacials de Catalunya (IEEC), Harvard & Smithsonian, Lawrence Berkeley National Laboratory, Lowell Observatory, the University of Sydney, University of Pennsylvania, Texas A&M University, Institució Catalana de Recerca i Estudis Avancats, The Barcelona Institute of Science and Technology Campus UAB, University of Wisconsin- Madison, LPC, University of Cambridge, Peyton Hall, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, National Science Foundation (US), Department of Energy (US), Australian Government, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), and OzDES

Subjects
Physics, Supermassive black hole, general [quasars], 010308 nuclear & particles physics, Lag, nuclei [galaxies], Astronomy and Astrophysics, Quasar, Astrophysics, galaxies: nuclei, quasars: general, 01 natural sciences, Spectral line, Space and Planetary Science, 0103 physical sciences, Reverberation mapping, Emission spectrum, Continuum (set theory), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Line (formation)
Abstract

Yu, Zhefu, et al., Reverberation mapping is a robust method to measure the masses of supermassive black holes outside of the local Universe. Measurements of the radius–luminosity (R−L) relation using the Mg II emission line are critical for determining these masses near the peak of quasar activity at z ≈ 1−2, and for calibrating secondary mass estimators based on Mg II that can be applied to large samples with only single-epoch spectroscopy. We present the first nine Mg II lags from our 5-yr Australian Dark Energy Survey reverberation mapping programme, which substantially improves the number and quality of Mg II lag measurements. As the Mg II feature is somewhat blended with iron emission, we model and subtract both the continuum and iron contamination from the multiepoch spectra before analysing the Mg II line. We also develop a new method of quantifying correlated spectroscopic calibration errors based on our numerous, contemporaneous observations of F-stars. The lag measurements for seven of our nine sources are consistent with both the H β and Mg II R−L relations reported by previous studies. Our simulations verify the lag reliability of our nine measurements, and we estimate that the median false positive rate of the lag measurements is 4 per cent⁠., We thank the anonymous referee for the careful review and comments. We thank Dr. Yue Shen for the constructive comments. ZY was supported in part by the United States National Science Foundation under Grant No. 161553 to PM. PM is grateful for support from the Radcliffe Institute for Advanced Study at Harvard University. PM also acknowledges support from the United States Department of Energy, Office of High Energy Physics under Award Number DE-SC-0011726. AP and UM are supported by the Australian Government Research Training Programme (RTP) Scholarship. This research was supported in part by the Australian Government through the Australian Research Council Laureate Fellowship funding scheme (project FL180100168). Based in part on data acquired at the Anglo-Australian Telescope, under programme A/2013B/012]. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaroi people, and pay our respects to elders past and present. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2021

15. OzDES multi-object fibre spectroscopy for the Dark Energy Survey: Results and second data release

Author

Enrique Gaztanaga, C. Lidman, J. Carretero, Tim Eifler, B. E. Tucker, E. Swann, Tamara M. Davis, Lluís Galbany, Sara Webb, J. Gschwend, S. Allam, Robert A. Gruendl, Samuel Hinton, Eli S. Rykoff, J. K. Hoormann, Krzysztof Bolejko, W. G. Hartley, G. Gutierrez, M. E. C. Swanson, Mark Sullivan, Edward Macaulay, Anais Möller, Paul Martini, Michael Schubnell, A. Carnero Rosell, Douglas L. Tucker, Kyler Kuehn, Ryan J. Foley, R. D. Wilkinson, Peter Doel, I. Sevilla-Noarbe, Daniel Scolnic, Andrew J. King, N. Kuropatkin, N. E. Sommer, Bonnie Zhang, Felipe Menanteau, M. Pursiainen, G. Tarle, Zhefu Yu, A. Kremin, Fang Yuan, V. Scarpine, Anthony Carr, M. Carrasco Kind, Sunayana Bhargava, David Parkinson, T. N. Varga, L. N. da Costa, S. A. Uddin, A. R. Walker, Robert C. Nichol, A. Roodman, M. Childress, Daniela Carollo, M. Costanzi, K. Honscheid, Juan Garcia-Bellido, E. Bertin, D. Lagattuta, Antonella Palmese, Jennifer L. Marshall, J. De Vicente, Joshua A. Frieman, M. A. G. Maia, D. Mudd, W. C. Wester, Fiona H. Panther, U. Malik, M. March, Basilio X. Santiago, Geraint F. Lewis, Peter Melchior, Richard Scalzo, J. Annis, Rob Sharp, M. Sako, D. L. Hollowood, S. Serrano, Richard Kessler, P. Wiseman, S. Everett, David J. Brooks, Marcos Lima, E. Suchyta, A. A. Plazas, F. J. Castander, Jacobo Asorey, T. M. C. Abbott, D. J. Brout, Michel Aguena, Huan Lin, J. Calcino, David J. James, Pablo Fosalba, E. J. Sanchez, Karl Glazebrook, Ramon Miquel, F. Paz-Chinchón, M. Smith, Daniel Gruen, Tenglin Li, Santiago Avila, A. G. Kim, Lidman, C., Tucker, B. E., Davis, T. M., Uddin, S. A., Asorey, J., Bolejko, K., Brout, D., Calcino, J., Carollo, D., Carr, A., Childress, M., Hoormann, J. K., Foley, R. J., Galbany, L., Glazebrook, K., Hinton, S. R., Kessler, R., Kim, A. G., King, A., Kremin, A., Kuehn, K., Lagattuta, D., Lewis, G. F., Macaulay, E., Malik, U., March, M., Martini, P., Moller, A., Mudd, D., Nichol, R. C., Panther, F., Parkinson, D., Pursiainen, M., Sako, M., Swann, E., Scalzo, R., Scolnic, D., Sharp, R., Smith, M., Sommer, N. E., Sullivan, M., Webb, S., Wiseman, P., Yu, Z., Yuan, F., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., Da Costa, L. N., De Vicente, J., Doel, P., Eifler, T. F., Everett, S., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., T. S., Li, Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Laboratoire de Physique de Clermont (LPC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Department of Energy (US), National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Science and Technology Facilities Council (UK), University of Illinois, Kavli Institute for Theoretical Physics, University of Chicago, The Ohio State University, Texas A&M University, Financiadora de Estudos e Projetos (Brasil), Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Ministério da Ciência, Tecnologia e Inovação (Brasil), German Research Foundation, European Commission, Australian Research Council, and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS)

Subjects
transients: supernovae, Astrophysics, dark energy [cosmology], 01 natural sciences, 7. Clean energy, law.invention, cosmology: dark energy, supermassive black hole [quasars], law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010303 astronomy & astrophysics, catalogues, Physics, quasars: supermassive black holes, Astrophysics::Instrumentation and Methods for Astrophysics, GALÁXIAS, Supernova, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, surveys, techniques: spectroscopic, catalogue, Astrophysics - Cosmology and Nongalactic Astrophysics, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, supermassive black holessurveys [Quasars], 0103 physical sciences, survey, Spectrograph, Astrophysics::Galaxy Astrophysics, STFC, 010308 nuclear & particles physics, supermassive black holes [quasars], RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Photometry (astronomy), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Quasars: supermassive black holessurveys, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], supernovae [transients]
Abstract

We present a description of the Australian Dark Energy Survey (OzDES) and summarize the results from its 6 years of operations. Using the 2dF fibre positioner and AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope, OzDES has monitored 771 active galactic nuclei, classified hundreds of supernovae, and obtained redshifts for thousands of galaxies that hosted a transient within the 10 deep fields of the Dark Energy Survey. We also present the second OzDES data release, containing the redshifts of almost 30 000 sources, some as faint as r = 24 mag, and 375 000 individual spectra. These data, in combination with the time-series photometry from the Dark Energy Survey, will be used to measure the expansion history of the Universe out to z ∼1.2 and the masses of hundreds of black holes out to z ∼4. OzDES is a template for future surveys that combine simultaneous monitoring of targets with wide-field imaging cameras and wide-field multi-object spectrographs., 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, Fi-nanciadora 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, Tecnologia e Inovação, the Deutsche Forschungsgemein-schaft, and the Collaborating Institutions in the DES. LG was funded by the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement no. 839090. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). Parts of this research were supported by the Australian Research Council under grants DP160100930, FL180100168, and FT140101270.

Published
2020

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

Author

Abbott TMC, Alarcon A, Allam S, Andersen P, Andrade-Oliveira F, Annis J, Asorey J, Avila S, Bacon D, Banik N, Bassett BA, Baxter E, Bechtol K, Becker MR, Bernstein GM, Bertin E, Blazek J, Bridle SL, Brooks D, Brout D, Burke DL, Calcino J, Camacho H, Campos A, Carnero Rosell A, Carollo D, Carrasco Kind M, Carretero J, Castander FJ, Cawthon R, Challis P, Chan KC, Chang C, Childress M, Crocce M, Cunha CE, D'Andrea CB, da Costa LN, Davis C, Davis TM, De Vicente J, DePoy DL, DeRose J, Desai S, Diehl HT, Dietrich JP, Dodelson S, Doel P, Drlica-Wagner A, Eifler TF, Elvin-Poole J, Estrada J, Evrard AE, Fernandez E, Flaugher B, Foley RJ, Fosalba P, Frieman J, Galbany L, García-Bellido J, Gatti M, Gaztanaga E, Gerdes DW, Giannantonio T, Glazebrook K, Goldstein DA, Gruen D, Gruendl RA, Gschwend J, Gutierrez G, Hartley WG, Hinton SR, Hollowood DL, Honscheid K, Hoormann JK, Hoyle B, Huterer D, Jain B, James DJ, Jarvis M, Jeltema T, Kasai E, Kent S, Kessler R, Kim AG, Kokron N, Krause E, Kron R, Kuehn K, Kuropatkin N, Lahav O, Lasker J, Lemos P, Lewis GF, Li TS, Lidman C, Lima M, Lin H, Macaulay E, MacCrann N, Maia MAG, March M, Marriner J, Marshall JL, Martini P, McMahon RG, Melchior P, Menanteau F, Miquel R, Mohr JJ, Morganson E, Muir J, Möller A, Neilsen E, Nichol RC, Nord B, Ogando RLC, Palmese A, Pan YC, Peiris HV, Percival WJ, Plazas AA, Porredon A, Prat J, Romer AK, Roodman A, Rosenfeld R, Ross AJ, Rykoff ES, Samuroff S, Sánchez C, Sanchez E, Scarpine V, Schindler R, Schubnell M, Scolnic D, Secco LF, Serrano S, Sevilla-Noarbe I, Sharp R, Sheldon E, Smith M, Soares-Santos M, Sobreira F, Sommer NE, Swann E, Swanson MEC, Tarle G, Thomas D, Thomas RC, Troxel MA, Tucker BE, Uddin SA, Vielzeuf P, Walker AR, Wang M, Weaverdyck N, Wechsler RH, Weller J, Yanny B, Zhang B, Zhang Y, and Zuntz J

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 light curves, 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&#95;{-0.11}^{+0.09}. The geometry is shown to be consistent with a spatially flat Universe, and we obtain a constraint on the baryon density of Ω&#95;{b}=0.069&#95;{-0.012}^{+0.009} that is independent of early Universe measurements. These results demonstrate the potential power of large multiprobe 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.

Published
2019
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