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1. The XXL Survey L. Active galactic nucleus contamination in galaxy clusters: Detection and cosmological impact

Author: Sunayana Bhargava, Christian Garrel, Elias Koulouridis, Marguerite Pierre, Ivan Valtchanov, Nicolas Cerardi, Ben J. Maughan, Michel Aguena, Christophe Benoist, Cale Baguley, Miriam E. Ramos-Ceja, Christophe Adami, Lucio Chiappetti, Cristian Vignali, and Jon P. Willis
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: X-ray observations of galaxy clusters are impacted by the presence of active galactic nuclei (AGNs) in a manner that is challenging to quantify, leading to biases in the detection and measurement of cluster properties for both astrophysics and cosmological applications. We detect and characterise clusters contaminated by central AGNs within the XXL survey footprint and provide a systematic assessment of the cosmological impact of such systems in X-ray cluster samples. We introduce a new automated class for AGN-contaminated (AC) clusters in the XXL source detection pipeline. The majority of these systems are otherwise missed by current X-ray cluster-detection methods. The AC selection is also effective in distinguishing AGN and cool-core presence using supplementary optical and infrared information. We present 33 AC objects, including 25 clusters in the redshift range, $0.14 \leq z \leq 1.03$, and eight other sources with significantly peaked central profiles. Six of these are new confirmed clusters. We computed the missed fraction of the XXL survey, which is defined as the fraction of genuine clusters that are undetected due to their centrally peaked X-ray profiles. We report seven undetected AC clusters above $z > 0.6$, in the range where X-ray cluster detection efficiency drops significantly. The missed fraction is estimated to be at the level of $5\%$ for the 50 square-degree XXL area. The impact on cosmological estimates from missed clusters is negligible for XXL, but it produces a tension of $\sim 3σ$ with the fiducial cosmology when considering larger survey areas. Looking towards surveys such as eROSITA and \textit{Athena}, larger areas and increased sensitivity will significantly enhance cluster detection, and therefore robust methods for characterising AGN contamination will be crucial for precise cluster cosmology, particularly in the redshift $z > 1$ regime., 26 pages, 11 figures (33 images of AC objects presented in the appendix), 3 tables. Accepted for publication in A&A
Published: 2023
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2. Dark energy survey year 3 results: weak lensing shape catalogue

Author: Peter Doel, Alexandra Amon, Joe Zuntz, Jack Elvin-Poole, M. Smith, Daniel Gruen, V. Scarpine, J. Carretero, Tamara M. Davis, H. T. Diehl, David Bacon, Niall MacCrann, I. Tutusaus, Tesla E. Jeltema, A. Navarro-Alsina, J. De Vicente, D. W. Gerdes, J. Gschwend, Daniel Thomas, Gary Bernstein, Marcos Lima, E. M. Huff, M. Gatti, W. C. Wester, Josh Frieman, R. Chen, Michel Aguena, Samuel Hinton, G. Gutierrez, David J. Brooks, R. P. Rollins, Matthew R. Becker, J. Prat, Ami Choi, Ben Hoyle, S. Samuroff, F. Paz-Chinchón, Santiago Avila, Chihway Chang, Antonella Palmese, M. A. G. Maia, E. Bertin, M. E. C. Swanson, S. Serrano, S. Pandey, S. Desai, Michael Schubnell, J. McCullough, M. Costanzi, D. L. Burke, J. P. Dietrich, Juan Garcia-Bellido, E. Suchyta, W. G. Hartley, Carlos Solans Sanchez, Christopher J. Conselice, S. Allam, Robert A. Gruendl, Ramon Miquel, Eli S. Rykoff, Jochen Weller, F. J. Castander, Richard G. Kron, T. Shin, D. L. Hollowood, T. M. C. Abbott, Elisabeth Krause, C. Doux, Chun-Hao To, E. J. Sanchez, A. A. Plazas, I. Ferrero, Matt J. Jarvis, K. Honscheid, S. Everett, L. F. Secco, M. Carrasco Kind, Martin Crocce, R. D. Wilkinson, Sunayana Bhargava, Risa H. Wechsler, J. Myles, David J. James, Jennifer L. Marshall, Agnès Ferté, Michael Troxel, I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, Alex Drlica-Wagner, K. D. Eckert, T. N. Varga, Dragan Huterer, L. N. da Costa, Bhuvnesh Jain, J. Annis, Douglas L. Tucker, Erin Sheldon, Robert Morgan, G. Tarle, Ian Harrison, A. Roodman, Tommaso Giannantonio, A. Carnero Rosell, Gatti, M., Sheldon, E., Amon, A., Becker, M., Troxel, M., Choi, A., Doux, C., Maccrann, N., Navarro Alsina, A., Harrison, I., Gruen, D., Bernstein, G., Jarvis, M., Secco, L. F., Ferté, A., Shin, T., Mccullough, J., Rollins, R. P., Chen, R., Chang, C., Pandey, S., Tutusaus, I., Prat, J., Elvin-Poole, J., Sanchez, C., Plazas, A. A., Roodman, A., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., da Costa, L. N., Davis, T. M., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huff, E. M., Huterer, D., Jain, B., James, D. J., Jeltema, T., Krause, E., Kron, R., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Miquel, R., Morgan, R., Myles, J., Palmese, A., Paz-Chinchón, F., Rykoff, E. S., Samuroff, S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Wechsler, R. H., Weller, J., Wester, W., Wilkinson, R. D., National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), 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), and DES
Subjects: Effective Area, Point spread function, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Techniques: image processing, FOS: Physical sciences, Astrophysics, Surveys, 01 natural sciences, surveys, weak [gravitational lensing], Gravitational lensing: weak, Methods: data analysis, 0103 physical sciences, data analysis [methods], survey, Spurious relationship, weak [ravitational lensing], 010303 astronomy & astrophysics, catalogues, Weak gravitational lensing, media_common, Physics, Energy Surveys, Number density, image processing [techniques], 010308 nuclear & particles physics, Cosmology: observations, Física, Astronomy and Astrophysics, Catalogues, Dark Energy, observations [cosmology], Galaxy, Weak Lensing, Space and Planetary Science, Sky, data analysi [methods], Dark energy, ravitational lensing: weak, Catalog, methods: data analysis, techniques: image processing, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology Observations, catalogue, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], observation [cosmology]
Abstract: Gatti, M., et al. (DES Collaboration), We present and characterize the galaxy shape catalogue from the first 3 yr of Dark Energy Survey (DES) observations, over an effective area of 4143 deg2 of the southern sky. We describe our data analysis process and our self-calibrating shear measurement pipeline metacalibration, which builds and improves upon the pipeline used in the DES Year 1 analysis in several aspects. The DES Year 3 weak-lensing shape catalogue consists of 100 204 026 galaxies, measured in the riz bands, resulting in a weighted source number density of neff = 5.59 gal arcmin-2 and corresponding shape noise σe = 0.261. We perform a battery of internal null tests on the catalogue, including tests on systematics related to the point spread function (PSF) modelling, spurious catalogue B-mode signals, catalogue contamination, and galaxy properties., Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grants 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 programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).
Published: 2021

3. Dark Energy Survey year 3 results: point spread function modelling

Author: Alex Drlica-Wagner, A. Hernandez, David J. James, Pablo Fosalba, Michael Schubnell, V. Scarpine, M. March, Sarah Bridle, Santiago Avila, Chihway Chang, A. Navarro-Alsina, S. Kent, S. Desai, R. D. Wilkinson, C. Davis, Samuel Hinton, Erin Sheldon, Josh Frieman, M. Costanzi, J. Meyers, G. Gutierrez, Gary Bernstein, Enrique Gaztanaga, B. Flaugher, Ofer Lahav, Ramon Miquel, Eli S. Rykoff, M. A. G. Maia, J. Carretero, G. Tarle, A. R. Walker, Ian Harrison, M. E. C. Swanson, P. F. Léget, S. Everett, S. Pandey, E. Suchyta, I. Sevilla-Noarbe, M. Smith, Peter Melchior, T. M. C. Abbott, Keith Bechtol, Juan Garcia-Bellido, J. De Vicente, N. Kuropatkin, D. L. Hollowood, M. Carrasco Kind, Michael Troxel, Daniel Gruen, M. Gatti, S. Serrano, A. Choi, W. C. Wester, A. Roodman, Matt J. Jarvis, E. J. Sanchez, David J. Brooks, T. N. Varga, K. Honscheid, Peter Doel, A. Carnero Rosell, R. L. C. Ogando, Joe Zuntz, H. T. Diehl, L. N. da Costa, Niall MacCrann, Alexandra Amon, Felipe Menanteau, D. W. Gerdes, A. A. Plazas, S. Vorperian, Kyler Kuehn, L. F. Secco, Sunayana Bhargava, Jennifer L. Marshall, K. Wei, S. Allam, Robert A. Gruendl, R. Chen, Michel Aguena, F. Paz-Chinchón, UAM. Departamento de Física Teórica, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), DES, Jarvis, M., Bernstein, G. M., Amon, A., Davis, C., Léget, P. F., Bechtol, K., Harrison, I., Gatti, M., Roodman, A., Chang, C., Chen, R., Choi, A., Desai, S., Drlica-Wagner, A., Gruen, D., Gruendl, R. A., Hernandez, A., Maccrann, N., Meyers, J., Navarro-Alsina, A., Pandey, S., Plazas, A. A., Secco, L. F., Sheldon, E., Troxel, M. A., Vorperian, S., Wei, K., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bhargava, S., Bridle, S. L., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Diehl, H. T., Doel, P., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kent, S., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Walker, A. R., Wester, W., and Wilkinson, R. D. (DES Collaboration)
Subjects: Point spread function, Systematic error, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Sextractor, FOS: Physical sciences, Image Processing [Techniques], Field of view, Surveys, Cosmology: Observations, 01 natural sciences, data analysi [software], Observations [Cosmology], Techniques: Image Processing, 0103 physical sciences, Range (statistics), survey, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 2mass, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Software: Data Analysis, Weak gravitational lensing, Physics, Gravitational Lensing: Weak, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, Mass, Catalogues, Software package, Galaxy, gravitational lensing: weak, techniques: image processing, catalogues, surveys, software: data analysis, cosmology: observations, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Space and Planetary Science, Weak [Gravitational Lensing], Dark energy, Data Analysis [Software], Catalog, catalogue, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, [PHYS.PHYS.PHYS-DATA-AN]Physics [physics]/Physics [physics]/Data Analysis, Statistics and Probability [physics.data-an], observation [cosmology]
Abstract: We introduce a new software package for modeling the point-spread function (PSF) of astronomical images, called Piff (PSFs In the Full FOV), which we apply to the first three years (known as Y3) of the Dark Energy Survey (DES) data. We describe the relevant details about the algorithms used by Piff to model the PSF, including how the PSF model varies across the field of view (FOV). Diagnostic results show that the systematic errors from the PSF modeling are very small over the range of scales that are important for the DES Y3 weak lensing analysis. In particular, the systematic errors from the PSF modeling are significantly smaller than the corresponding results from the DES year one (Y1) analysis. We also briefly describe some planned improvements to Piff that we expect to further reduce the modeling errors in future analyses., Comment: 19 pages, accepted/published by MNRAS. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release
Published: 2020

4. The XXL survey - XLVI. Forward cosmological analysis of the C1 cluster sample

Author: C. Adami, C. Garrel, Marguerite Pierre, Keiichi Umetsu, Lauro Moscardini, Elias Koulouridis, L. Chiappetti, Dominique Eckert, Sunayana Bhargava, Fabio Gastaldello, Jean-Paul Le Fevre, N. Clerc, Alfonso Veropalumbo, Mauro Sereno, Florian Pacaud, Patrick Valageas, Manolis Plionis, Federico Marulli, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Population, FOS: Physical sciences, Astrophysics, Correlation function (astronomy), 01 natural sciences, Omega, Cosmology, symbols.namesake, surveys, 0103 physical sciences, Planck, cosmological parameters, education, 010303 astronomy & astrophysics, Galaxy cluster, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Space and Planetary Science, X-rays: galaxies: clusters, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the forward cosmological analysis of an $XMM$ selected sample of galaxy clusters out to a redshift of unity. Following our previous 2018 study based on the dn/dz quantity alone, we perform an upgraded cosmological analysis of the same XXL C1 cluster catalogue (178 objects), with a detailed account of the systematic errors. We follow the ASpiX methodology: the distribution of the observed X-ray properties of the cluster population is analysed in a 3D observable space (count rate, hardness ratio, redshift) and modelled as a function of cosmology. Compared to more traditional methods, ASpiX allows the inclusion of clusters down to a few tens of photons. We obtain an improvement by a factor of 2 compared to the previous analysis by letting the normalisation of the M-T relation and the evolution of the L-T relation free. Adding constraints from the XXL cluster 2-point correlation function and the BAO from various surveys decreases the uncertainties by 23 and 53 % respectively, and 62% when adding both. Switching to the scaling relations from the Subaru analysis, and letting free more parameters, our final constraints are $\sigma_8$ = $0.99^{+0.14}_{-0.23}$, $\Omega_m$ = 0.296 $\pm$ 0.034 ($S_8 = 0.98^{+0.11}_{-0.21}$) for the XXL sample alone. Finally, we combine XXL ASpiX, the XXL cluster 2-point correlation function and the BAO, with 11 free parameters, allowing for the cosmological dependence of the scaling relations in the fit. We find $\sigma_8$ = $0.793^{+0.063}_{-0.12}$, $\Omega_m$ = 0.364 $\pm$ 0.015 ($S_8 = 0.872^{+0.068}_{-0.12}$), but still compatible with Planck CMB at 2.2$\sigma$. The results obtained by the ASpiX method are promising; further improvement is expected from the final XXL cosmological analysis involving a cluster sample twice as large. Such a study paves the way for the analysis of the eROSITA and future Athena surveys., Comment: 20 pages, 10 figures, accepted for publication in A&A, A&A version has the unabridged abstract
Published: 2022

5. The Growth of Intracluster Light in XCS-HSC Galaxy Clusters from $0.1 < z < 0.5$

Author: Paul Giles, Phil A. James, Maria Manolopoulou, K. Furnell, R. D. Wilkinson, Pedro T. P. Viana, Chris A. Collins, Carlos Vergara, Lee S. Kelvin, Ivan K. Baldry, A. Bermeo, Sunayana Bhargava, Robert G. Mann, Matt Hilton, John P. Stott, Julian A. Mayers, and A. Kathy Romer
Subjects: Physics, Stellar mass, 010308 nuclear & particles physics, astro-ph.GA, Flux, Order (ring theory), Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, 0103 physical sciences, Cluster (physics), Brightest cluster galaxy, 010303 astronomy & astrophysics, Galaxy cluster, QC, QB
Abstract: We estimate the Intracluster Light (ICL) component within a sample of 18 clusters detected in XMM Cluster Survey (XCS) data using deep ($\sim$ 26.8 mag) Hyper Suprime Cam Subaru Strategic Program DR1 (HSC-SSP DR1) $i$-band data. We apply a rest-frame ${\mu}_{B} = 25 \ \mathrm{mag/arcsec^{2}}$ isophotal threshold to our clusters, below which we define light as the ICL within an aperture of $R_{X,500}$ (X-ray estimate of $R_{500}$) centered on the Brightest Cluster Galaxy (BCG). After applying careful masking and corrections for flux losses from background subtraction, we recover $\sim$20% of the ICL flux, approximately four times our estimate of the typical background at the same isophotal level ($\sim$ 5%). We find that the ICL makes up about $\sim$ 24% of the total cluster stellar mass on average ($\sim$ 41% including the flux contained in the BCG within 50 kpc); this value is well-matched with other observational studies and semi-analytic/numerical simulations, but is significantly smaller than results from recent hydrodynamical simulations (even when measured in an observationally consistent way). We find no evidence for any links between the amount of ICL flux with cluster mass, but find a growth rate of $2-4$ for the ICL between $0.1 < z < 0.5$. We conclude that the ICL is the dominant evolutionary component of stellar mass in clusters from $z \sim 1$. Our work highlights the need for a consistent approach when measuring ICL alongside the need for deeper imaging, in order to unambiguously measure the ICL across as broad a redshift range as possible (e.g. 10-year stacked imaging from the Vera C. Rubin Observatory)., Comment: Accepted by MNRAS (05/01/2021), 20 pages, 17 figures
Published: 2021

6. Dark energy survey year 3 results: Photometric data set for cosmology

Author: Tesla E. Jeltema, Samuel Hinton, I. Ferrero, Matt J. Jarvis, G. Gutierrez, C.Pond, Ramon Miquel, C. Lidman, E. M. Huff, Michel Aguena, Risa H. Wechsler, Eric H. Neilsen, Martin Crocce, R. D. Wilkinson, A. Benoit-Lévy, Daniel Thomas, David J. James, J. De Vicente, Boris Leistedt, D. J. Brout, E. Suchyta, August E. Evrard, Jochen Weller, Douglas L. Tucker, Matthew R. Becker, Eric Morganson, G. Tarle, Sunayana Bhargava, F. J. Castander, Tianjun Li, V. Scarpine, Ian Harrison, Peter Doel, J. Carretero, Tamara M. Davis, Jennifer L. Marshall, Keith Bechtol, T. M. C. Abbott, A. A. Plazas, Ami Choi, Ben Hoyle, K. M. Stringer, C. J. Conselice, Huan Lin, H. T. Diehl, M. Carrasco Kind, Chun-Hao To, E. J. Sanchez, Ofer Lahav, K. Kuehn, M.E.E.Pereira, Robert Morgan, Erin Sheldon, R. Cawthon, Peter Melchior, E. S. Rykoff, Alex Drlica-Wagner, D. L. Burke, I. Sevilla-Noarbe, A. Alarcon, Y.-H. Zhang, David J. Brooks, Dragan Huterer, J. Gschwend, Brian Yanny, Antonella Palmese, N. Kuropatkin, Michael Troxel, W. C. Wester, Gary Bernstein, J. Annis, A. Roodman, M. A. G. Maia, M. Rodriguez-Monroy, S. Allam, Robert A. Gruendl, Tommaso Giannantonio, K. D. Eckert, T. N. Varga, A. K. Romer, Adriano Pieres, L. N. da Costa, P. Martini, Enrique Gaztanaga, R. L. C. Ogando, Sarah Bridle, Santiago Avila, Chihway Chang, S. Everett, S. Desai, J.Allyn-Smith, E. Bertin, D. L. Hollowood, S. Serrano, Richard Kessler, Michael Schubnell, Marcos Lima, Joseph J. Mohr, Alexandra Amon, Felipe Menanteau, Richard G. Kron, A. Carnero Rosell, K. Honscheid, F. Paz-Chinchón, M. Smith, Daniel Gruen, D. W. Gerdes, M. Costanzi, B. Flaugher, M. D. Johnson, P. Fosalba, W. G. Hartley, J. P. Dietrich, Juan Garcia-Bellido, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Instituto Nacional de Ciência e Tecnologia (Brasil), European Commission, Generalitat de Catalunya, Department of Energy (US), Sevilla-Noarbe, I., Bechtol, K., Carrasco Kind, M., Carnero Rosell, A., Becker, M. R., Drlica-Wagner, A., Gruendl, R. A., Rykoff, E. S., Sheldon, E., Yanny, B., Alarcon, A., Allam, S., Amon, A., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Burke, D. L., Carretero, J., Choi, A., Diehl, H. T., Everett, S., Flaugher, B., Gaztanaga, E., Gschwend, J., Harrison, I., Hartley, W. G., Hoyle, B., Jarvis, M., Johnson, M. D., Kessler, R., Kron, R., Kuropatkin, N., Leistedt, B., T. S., Li, Menanteau, F., Morganson, E., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pieres, A., Pond, C., Rodriguez-Monroy, M., Allyn-Smith, J., Stringer, K. M., Troxel, M. A., Tucker, D. L., de Vicente, J., Wester, W., Zhang, Y., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bhargava, S., Bridle, S. L., Brooks, D., Brout, D., Castander, F. J., Cawthon, R., Chang, C., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. E., Davis, T. M., Desai, S., Dietrich, J. P., Doel, P., Eckert, K., Evrard, A. E., Ferrero, I., Fosalba, P., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huff, E. M., Huterer, D., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Mohr, J. J., Morgan, R., Neilsen, E., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Wechsler, R. H., Weller, J., Wilkinson, R. D., 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 UAM. Departamento de Física Teórica
Subjects: Observational cosmology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Surveys, 7. Clean energy, 01 natural sciences, Cosmology, Photometric calibration, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysic, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Survey, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Catalogs, 1671, 205, 1146, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, 010308 nuclear & particles physics, Image (category theory), Física, Astronomy and Astrophysics, Galaxy, Data set, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Catalog, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data release, Quality information
Abstract: Sevilla-Noarbe, I., et al. (DES Collaboration), We describe the Dark Energy Survey (DES) photometric data set assembled from the first three years of science operations to support DES Year 3 cosmologic analyses, and provide usage notes aimed at the broad astrophysics community. Y3 GOLD improves on previous releases from DES, Y1 GOLD, and Data Release 1 (DES DR1), presenting an expanded and curated data set that incorporates algorithmic developments in image detrending and processing, photometric calibration, and object classification. Y3 GOLD comprises nearly 5000 deg of grizY imaging in the south Galactic cap, including nearly 390 million objects, with depth reaching a signal-to-noise ratio ∼10 for extended objects up to i ∼ 23.0, and top-of-the-atmosphere photometric uniformity 98% and purity >99% for galaxies with 19 < i < 22.5. Additionally, it includes per-object quality information, and accompanying maps of the footprint coverage, masked regions, imaging depth, survey conditions, and astrophysical foregrounds that are used to select the cosmologic analysis samples., K.B. acknowledges support from the U. S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Nos. DE-SC0020278 and DE-SC0017647. The DES data management system is supported by the NSF under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union?s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ci?ncia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). A.C.R. acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under grant AYA2017-84061-P, co-financed by FEDER (European Regional Development Funds) and by the Spanish Space Research Program ?Participation in the NISP instrument and preparation for the science of EUCLID? (ESP2017-84272-C2-1-R). 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

7. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations

Author: G. Gutierrez, David J. Brooks, Robert Morgan, Erin Sheldon, J. Prat, Joe Zuntz, S. Samuroff, Jack Elvin-Poole, Matthew R. Becker, M. Carrasco Kind, M. E. C. Swanson, Alex Drlica-Wagner, J. Carretero, Dragan Huterer, V. Scarpine, Ashley J. Ross, Tamara M. Davis, E. Bertin, Xiao Fang, Douglas L. Tucker, Kyler Kuehn, Basilio X. Santiago, T. N. Varga, M. Gatti, J. Annis, A. Carnero Rosell, Youngsoo Park, D. L. Burke, W. C. Wester, Robert A. Gruendl, R. Cawthon, Marcos Lima, I. Ferrero, Matt J. Jarvis, P. Vielzeuf, Yanxi Zhang, Tim Eifler, M. Costanzi, W. G. Hartley, Arya Farahi, Josh Frieman, J. P. Dietrich, Juan Garcia-Bellido, Eduardo Rozo, Oliver Friedrich, I. Sevilla-Noarbe, T. McClintock, J. Muir, N. Kuropatkin, J. DeRose, E. Suchyta, August E. Evrard, Martin Crocce, R. D. Wilkinson, Ben Hoyle, Jochen Weller, L. N. da Costa, Tesla E. Jeltema, G. Tarle, Antonella Palmese, M. A. G. Maia, Michael Troxel, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, J. Myles, David J. James, Enrique Gaztanaga, Jonathan Blazek, Christopher J. Conselice, Markus Rau, Sarah Bridle, Santiago Avila, Chihway Chang, P. Fosalba, Carlos Solans Sanchez, Michel Aguena, Sunayana Bhargava, A. K. Romer, S. Desai, B. Flaugher, Sebastian Bocquet, Daniel Thomas, H. T. Diehl, Ramon Miquel, D. L. Hollowood, Niall MacCrann, S. Serrano, C. Davis, M. Smith, A. A. Plazas, Gary Bernstein, Hao-Yi Wu, Daniel Gruen, A. Porredon, V. Miranda, Maria E. S. Pereira, Elisabeth Krause, S. Everett, F. Paz-Chinchón, Jennifer L. Marshall, Eli S. Rykoff, Risa H. Wechsler, Richard G. Kron, A. Roodman, Tommaso Giannantonio, A. Choi, K. Honscheid, Alexandra Amon, Felipe Menanteau, Samuel Hinton, Department of Energy (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), German Research Foundation, European Commission, To, C., Krause, E., Rozo, E., Wu, H., Gruen, D., Wechsler, R. H., Eifler, T. F., Rykoff, E. S., Costanzi, M., Becker, M. R., Bernstein, G. M., Blazek, J., Bocquet, S., Bridle, S. L., Cawthon, R., Choi, A., Crocce, M., Davis, C., Derose, J., Drlica-Wagner, A., Elvin-Poole, J., Fang, X., Farahi, A., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Hartley, W. G., Hoyle, B., Jarvis, M., Maccrann, N., Mcclintock, T., Miranda, V., Pereira, M. E. S., Park, Y., Porredon, A., Prat, J., Rau, M. M., Ross, A. J., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Troxel, M. A., Varga, T. N., Vielzeuf, P., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Chang, C., Conselice, C., da Costa, L. N., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Huterer, D., James, D. J., Jeltema, T., Kron, R., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Myles, J., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Weller, J., 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), DES, and UAM. Departamento de Física Teórica
Subjects: SDSS, Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, Cosmological parameters, General Physics and Astronomy, Astrophysics, SPT, Astrophysics::Cosmology and Extragalactic Astrophysics, Data_CODINGANDINFORMATIONTHEORY, des, Gravitation and Astrophysics, 01 natural sciences, 7. Clean energy, Cosmology, scale, TRACER, evolution, 0103 physical sciences, Dark energy, Hardware_INTEGRATEDCIRCUITS, Dark matter, 010306 general physics, Cluster analysis, Scaling, Weak gravitational lensing, STFC, Physics, model, COSMIC cancer database, RCUK, Física, spt, Mass Calibration, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Galaxy, Scale, red galaxies, 13. Climate action, Cosmic Shear, mass calibration, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, cosmic shear, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: To, C. et al. (DES Collaboration), We present the first joint analysis of cluster abundances and auto or cross-correlations of three cosmic tracer fields: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis (4×2pt+N) of cluster abundances, three cluster cross-correlations, and the auto correlations of the galaxy density measured from the first year data of the Dark Energy Survey, we obtain ωm=0.305-0.038+0.055 and σ8=0.783-0.054+0.064. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat νΛCDM model. Consequently, we combine cluster abundances and all two-point correlations from across all three cosmic tracer fields (6×2pt+N) and find improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys., This Letter has gone through internal review by the DES Collaboration. This work was supported in part by the U.S. Department of Energy contract to SLAC National Accelerator Laboratory, under Contract No. DE-AC02- 76SF00515 (C. H., D. G., R. W.) including a Panofsky Fellowship awarded to D. G. E. K. is supported by the Department of Energy Grant No. DE-SC0020247. E. R. is supported by DOE Grants No. DE-SC0015975 and No. DE-SC0009913, and by NSF Grant No. 2009401. E. R. also acknowledges funding from the Cottrell Scholar program of the Research Corporation for Science Advancement. H. W. is supported by NSF Grant No. AST-1516997. Some of the computing for this project was performed on the Sherlock cluster at Stanford. We would like to thank KIPAC, Stanford University, and the Stanford Research Computing Center for providing computational resources and support that contributed to these research results. Funding for the DES Projects has been provided by the DOE and NSF(USA), MEC/MICINN/ MINECO(Spain), STFC(UK), HEFCE(UK). NCSA (UIUC), KICP(U. Chicago), CCAPP(Ohio State), MIFPA(Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), DFG(Germany), and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Zürich, Fermilab, University of Illinois, ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU München and the associated Excellence Cluster Universe, University of Michigan, NFS’s NOIRLab, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford University, University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSFs NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES Data Management System is supported by the NSF under Grants No. AST-1138766 and No. 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 MDM2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2021

8. Atacama Cosmology Telescope: A Catalog of >4000 Sunyaev–Zel’dovich Galaxy Clusters

Author: Eli S. Rykoff, Jo Dunkley, E. Bertin, Ofer Lahav, Nick Battaglia, M. Soares-Santos, Hironao Miyatake, Shannon M. Duff, R. D. Wilkinson, Adriaan J. Duivenvoorden, L. N. da Costa, Joel N. Ullom, Robert Morgan, D. L. Burke, Devin Crichton, Kavilan Moodley, Peter Doel, Alexandra Amon, Edward J. Wollack, N. C. Robertson, H. T. Diehl, Joseph E. Golec, Sunayana Bhargava, Samuel Hinton, Emmanuel Schaan, Enrique Gaztanaga, Megan Gralla, David N. Spergel, Johannes Hubmayr, Simon Dicker, David Bacon, S. Allam, Robert A. Gruendl, Simone Ferraro, C. Aros-Bunster, Felipe Menanteau, G. Gutierrez, Kevin M. Huffenberger, Daniel Thomas, Ramon Miquel, Michael D. Niemack, I. Ferrero, Mathew S. Madhavacheril, J. P. Dietrich, Niall MacCrann, Juan Garcia-Bellido, Tesla E. Jeltema, David J. James, Yanxi Zhang, A. K. Romer, Ben Hoyle, Hy Trac, Mark J. Devlin, Patricio A. Gallardo, J. Gschwend, A. A. Plazas, Brian J. Koopman, Rolando Dünner, Zhilei Xu, Simone Aiola, Behzad Ansarinejad, A. Choi, Jeff McMahon, Eduardo Rozo, Gary Bernstein, K. Honscheid, Michel Aguena, Tanay Bhandarkar, Dan Becker, C. Sifon, Neelima Sehgal, Bhuvnesh Jain, Laura Newburgh, Dongwon Han, F. Paz-Chinchón, J. R. Bond, Kyler Kuehn, Peter Melchior, M. Carrasco Kind, Eve M. Vavagiakis, Steve K. Choi, Suzanne T. Staggs, Paul Giles, R. L. C. Ogando, J. C. Hill, Federico Nati, M. E. C. Swanson, E. V. Denison, Kevin T. Crowley, Tony Mroczkowski, W. G. Hartley, Antonella Palmese, Martine Lokken, S. Kent, Alessandro Schillaci, Masamune Oguri, John P. Hughes, M. A. G. Maia, Maria Salatino, S. Amodeo, T. Shin, S. Adhikari, M. Hasselfield, M. Costanzi, S. I. Loubser, J. Van Lanen, B. Partridge, Sigurd Naess, Adam D. Hincks, J. A. Beall, B. Flaugher, S. M. Simon, Jason E. Austermann, S. P. Ho, John Orlowski-Scherer, M. Smith, Daniel Gruen, J. Martin, D. W. Gerdes, J. Annis, Kenda Knowles, David J. Brooks, Erminia Calabrese, Emilie R. Storer, Gene C. Hilton, Leila R. Vale, Salcedo Romero de Ávila, Phumlani Phakathi, Josh Frieman, Yen-Ting Lin, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, J. Carretero, E. Suchyta, Matt Hilton, Christopher J. Conselice, Tobias A. Marriage, Sebastian Grandis, A. Carnero Rosell, Agnès Ferté, Anton T. Jaelani, Marcos Lima, S. Everett, S. Serrano, Lyman A. Page, J. De Vicente, Atsushi J. Nishizawa, G. Tarle, UAM. Departamento de Física Teórica, Hilton, M, Sifon, C, Naess, S, Madhavacheril, M, Oguri, M, Rozo, E, Rykoff, E, Adhikari, S, Aguena, M, Aiola, S, Allam, S, Amodeo, S, Amon, A, Annis, J, Ansarinejad, B, Abbott, T, Aros-Bunster, C, Austermann, J, Avila, S, Bacon, D, Battaglia, N, Beall, J, Becker, D, Bernstein, G, Bertin, E, Bhandarkar, T, Bhargava, S, Bond, J, Brooks, D, Burke, D, Calabrese, E, Carrasco Kind, M, Carretero, J, Choi, S, Choi, A, Conselice, C, Da Costa, L, Costanzi, M, Crichton, D, Crowley, K, Dunner, R, Denison, E, Devlin, M, Dicker, S, Diehl, H, Dietrich, J, Doel, P, Duff, S, Duivenvoorden, A, Dunkley, J, Everett, S, Ferraro, S, Ferte, A, Flaugher, B, Frieman, J, Ferrero, I, Gallardo, P, Garcia-Bellido, J, Gaztanaga, E, Giles, P, Golec, J, Gralla, M, Grandis, S, Gruen, D, Gerdes, D, Gruendl, R, Gschwend, J, Gutierrez, G, Han, D, Hartley, W, Hasselfield, M, Hill, J, Hilton, G, Hincks, A, Hinton, S, Ho, S, Honscheid, K, Hoyle, B, Hubmayr, J, Huffenberger, K, Hughes, J, Jaelani, A, Jain, B, James, D, Jeltema, T, Kent, S, Knowles, K, Koopman, B, Kuehn, K, Lahav, O, Lima, M, Lin, Y, Lokken, M, Loubser, S, Maccrann, N, Maia, M, Marriage, T, Martin, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Moodley, K, Morgan, R, Mroczkowski, T, Nati, F, Newburgh, L, Niemack, M, Nishizawa, A, Miyatake, H, Ogando, R, Orlowski-Scherer, J, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Phakathi, P, Plazas, A, Robertson, N, Romer, A, Carnero Rosell, A, Sanchez, E, Schaan, E, Schillaci, A, Sehgal, N, Serrano, S, Shin, T, Simon, S, Smith, M, Salatino, M, Soares-Santos, M, Spergel, D, Staggs, S, Storer, E, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Trac, H, Ullom, J, Vale, L, Van Lanen, J, Vavagiakis, E, De Vicente, J, Wilkinson, R, Wollack, E, Xu, Z, Zhan, Y, Hilton, M., Sifón, C., Naess, S., Madhavacheril, M., Oguri, M., Rozo, E., Rykoff, E., Abbott, T. M. C., Adhikari, S., Aguena, M., Aiola, S., Allam, S., Amodeo, S., Amon, A., Annis, J., Ansarinejad, B., Aros-Bunster, C., Austermann, J. E., Avila, S., Bacon, D., Battaglia, N., Beall, J. A., Becker, D. T., Bernstein, G. M., Bertin, E., Bhandarkar, T., Bhargava, S., Bond, J. R., Brooks, D., Burke, D. L., Calabrese, E., Carretero, J., Choi, S. K., Choi, A., Conselice, C., da Costa, L. N., Costanzi, M., Crichton, D., Crowley, K. T., Dünner, R., Denison, E. V., Devlin, M. J., Dicker, S. R., Diehl, H. T., Dietrich, J. P., Doel, P., Duff, S. M., Duivenvoorden, A. J., Dunkley, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giles, P., Golec, J. E., Gralla, M. B., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Han, D., Hartley, W. G., Hasselfield, M., Hill, J. C., Hilton, G. C., Hincks, A. D., Hinton, S. R., S-P. P., Ho, Honscheid, K., Hoyle, B., Hubmayr, J., Huffenberger, K. M., Hughes, J. P., Jaelani, A. T., Jain, B., James, D. J., Jeltema, T., Kent, S., Carrasco Kind, M., Knowles, K., Koopman, B. J., Kuehn, K., Lahav, O., Lima, M., Lin, Y-T., Lokken, M., Loubser, S. I., Maccrann, N., Maia, M. A. G., Marriage, T. A., Martin, J., Mcmahon, J., Melchior, P., Menanteau, F., Miquel, R., Miyatake, H., Moodley, K., Morgan, R., Mroczkowski, T., Nati, F., Newburgh, L. B., Niemack, M. D., Nishizawa, A. J., Ogando, R. L. C., Orlowski-Scherer, J., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Phakathi, P., Plazas, A. A., Robertson, N. C., Romer, A. K., Carnero Rosell, A., Salatino, M., Sanchez, E., Schaan, E., Schillaci, A., Sehgal, N., Serrano, S., Shin, T., Simon, S. M., Smith, M., Soares-Santos, M., Spergel, D. N., Staggs, S. T., Storer, E. R., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Trac, H., Ullom, J. N., Vale, L. R., Van Lanen, J., Vavagiakis, E. M., De Vicente, J., Wilkinson, R. D., Wollack, E. J., Xu, Z., and Zhang, Y.
Subjects: Galaxy clusters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology, Large-scale structure of the universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Intracluster medium, 0103 physical sciences, Cluster (physics), Sunyaev-Zeldovich Effect, 010303 astronomy & astrophysics, Cosmology, Galaxy clusters, Galaxy cluster, Astrophysics::Galaxy Astrophysics, AGLOMERADOS (GALÁXIA), Physics, 010308 nuclear & particles physics, Star formation, Física, Astronomy and Astrophysics, XMM-newton Telescope, Galaxies, Galaxy, Redshift, Space and Planetary Science, Atacama Cosmology Telescope
Abstract: Hilton, M., et al., We present a catalog of 4195 optically confirmed Sunyaev–Zel’dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z < 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M > 3.8 × 10 M, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2 4. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566 deg), the Hyper Suprime-Cam Subaru Strategic Program (469 deg), and the Kilo Degree Survey (825 deg). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr., The DES Data Management System is supported by the NSF under Grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Unionʼs 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

9. Dark Energy Survey Year 3 results: Optimizing the lens sample in a combined galaxy clustering and galaxy-galaxy lensing analysis

Author: F. J. Castander, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, Sarah Bridle, Santiago Avila, Alex Drlica-Wagner, G. Tarle, Xiao Fang, Maria E. S. Pereira, A. Roodman, Tommaso Giannantonio, Samuel Hinton, Alexandra Amon, Josh Frieman, Martin Crocce, R. D. Wilkinson, G. Gutierrez, F. Paz-Chinchón, Sunayana Bhargava, V. Scarpine, Ramon Miquel, Jennifer L. Marshall, Shantanu Desai, Felipe Menanteau, N. Weaverdyck, A. Carnero Rosell, B. Flaugher, David J. Brooks, M. Carrasco Kind, M. E. C. Swanson, J. Carretero, M. Smith, Daniel Gruen, David J. James, Robert Morgan, W. G. Hartley, Pablo Fosalba, E. Gaztanaga, D. W. Gerdes, A. Choi, K. Honscheid, Juan Garcia-Bellido, E. Bertin, Elisabeth Krause, I. Ferrero, Matt J. Jarvis, Agnès Ferté, Peter Doel, D. L. Hollowood, S. Serrano, H. T. Diehl, S. Allam, Robert A. Gruendl, E. Suchyta, David Bacon, R. Cawthon, Niall MacCrann, J. Gschwend, A. Porredon, M. Costanzi, Michel Aguena, S. Pandey, I. Sevilla-Noarbe, J. De Vicente, Kyler Kuehn, N. Kuropatkin, K. D. Eckert, T. N. Varga, L. N. da Costa, M. Soares-Santos, S. Samuroff, Ben Hoyle, Antonella Palmese, M. A. G. Maia, M. Rodriguez-Monroy, Jack Elvin-Poole, A. A. Plazas, Jochen Weller, T. F. Eifler, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), 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, Porredon, A., Crocce, M., Fosalba, P., Elvin-Poole, J., Carnero Rosell, A., Cawthon, R., Eifler, T. F., Fang, X., Ferrero, I., Krause, E., Maccrann, N., Weaverdyck, N., Abbott, T. M. C., Aguena, M., Allam, S., Amon, A., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eckert, K., Ferte, A., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jarvis, M., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Pandey, S., Paz-Chinchon, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., Weller, J., and Wilkinson, R. D.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), Dark matter, Cosmological parameters, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, large scale structure, 01 natural sciences, 7. Clean energy, Cosmology, dark matter, Gravitational lenses, 0103 physical sciences, cosmology, Weak, Large-scale structure of the Universe, cosmological parameters, 010306 general physics, dark energy, Sky suverys, STFC, Photometric redshift, AGLOMERADOS (GALÁXIA), Physics, Gravitational Lensing, 010308 nuclear & particles physics, Equation of state (cosmology), Gravitation, Cosmology and Astrophysics, RCUK, Física, Dark enery, Dark Energy, Redshift, Galaxy, observations, 13. Climate action, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Porredon, A., et al. DES Collaboration, We investigate potential gains in cosmological constraints from the combination of galaxy clustering and galaxy-galaxy lensing by optimizing the lens galaxy sample selection using information from Dark Energy Survey (DES) Year 3 data and assuming the DES Year 1 metacalibration sample for the sources. We explore easily reproducible selections based on magnitude cuts in i-band as a function of (photometric) redshift, zphot, and benchmark the potential gains against those using the well-established redMaGiC [E. Rozo et al., Mon. Not. R. Astron. Soc. 461, 1431 (2016)MNRAA40035-871110.1093/mnras/stw1281] sample. We focus on the balance between density and photometric redshift accuracy, while marginalizing over a realistic set of cosmological and systematic parameters. Our optimal selection, the MagLim sample, satisfies i, Funding for the DES Projects was 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 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. 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 under a cooperative agreement with the National Science Foundation. The DES data management system was supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions were partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. was partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grants No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia do e-Universo (CNPq Grant No. 465376/2014-2). This work was 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

10. 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

11. Synthetic Galaxy Clusters and Observations Based on Dark Energy Survey Year 3 Data

Author: Matthew R. Becker, I. Ferrero, Matt J. Jarvis, Yanxi Zhang, B. Flaugher, Scott Dodelson, A. Choi, Enrique Gaztanaga, M. March, M. Carrasco Kind, K. Honscheid, Maria E. S. Pereira, S. Desai, Brian Yanny, David J. Brooks, V. Scarpine, Eli S. Rykoff, Erin Sheldon, Robert Morgan, Joe Zuntz, Antonella Palmese, Sebastian Grandis, M. A. G. Maia, J. Annis, Samuel Hinton, K. Herner, J. Carretero, Alexandra Amon, Sunayana Bhargava, G. Gutierrez, I. Harrison, I. Sevilla-Noarbe, S. Allam, Robert A. Gruendl, R. P. Rollins, E. Suchyta, A. A. Plazas, M. Soares-Santos, G. Tarle, Jochen Weller, J. Myles, N. Kuropatkin, Felipe Menanteau, Kyler Kuehn, K. D. Eckert, T. N. Varga, A. Carnero Rosell, L. N. da Costa, J. McCullough, J. De Vicente, Chun-Hao To, E. J. Sanchez, M. Costanzi, F. Paz-Chinchón, Peter Melchior, Daniel Thomas, S. Everett, M. E. C. Swanson, Stella Seitz, A. K. Romer, Tesla E. Jeltema, W. G. Hartley, S. Serrano, Ramon Miquel, J. P. Dietrich, Juan Garcia-Bellido, Michael Troxel, Michel Aguena, Eduardo Rozo, M. Smith, Daniel Gruen, H. T. Diehl, Niall MacCrann, E. Bertin, J. Gschwend, Gary Bernstein, Michael Schubnell, D. W. Gerdes, Varga, T N, Gruen, D, Seitz, S, Maccrann, N, Sheldon, E, Hartley, W G, Amon, A, Choi, A, Palmese, A, Zhang, Y, Becker, M R, Mccullough, J, Rozo, E, Rykoff, E S, To, C, Grandis, S, Bernstein, G M, Dodelson, S, Eckert, K, Everett, S, Gruendl, R A, Harrison, I, Herner, K, Rollins, R P, Sevilla-Noarbe, I, Troxel, M A, Yanny, B, Zuntz, J, Diehl, H T, Jarvis, M, Aguena, M, Allam, S, Annis, J, Bertin, E, Bhargava, S, Brooks, D, Carnero&nbsp, Rosell, A, Carrasco&nbsp, Kind, M, Carretero, J, Costanzi, M, da&nbsp, Costa, L N, Pereira, M E S, De&nbsp, Vicente, J, Desai, S, Dietrich, J P, Ferrero, I, Flaugher, B, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gschwend, J, Gutierrez, G, Hinton, S R, Honscheid, K, Jeltema, T, Kuehn, K, Kuropatkin, N, Maia, M A G, March, M, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, Myles, J, Paz-Chinchón, F, Plazas, A A, Romer, A K, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Thomas, D, Weller, J, UAM. Departamento de Física Teórica, Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, 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), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology: Observations, Observations [Cosmology], weak [gravitational lensing], 0103 physical sciences, Cluster (physics), clusters: general [galaxies], 010303 astronomy & astrophysics, Galaxy cluster, Weak gravitational lensing, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Gravitational Lensing: Weak, Física, GALÁXIAS, Astronomy and Astrophysics, Redshift, Galaxy, Distribution function, Space and Planetary Science, gravitational lensing: weak, galaxies: clusters: general, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies: Clusters: General, observation [cosmology]
Abstract: T. N. Varga et al., We develop a novel data-driven method for generating synthetic optical observations of galaxy clusters. In cluster weak lensing, the interplay between analysis choices and systematic effects related to source galaxy selection, shape measurement, and photometric redshift estimation can be best characterized in end-to-end tests going from mock observations to recovered cluster masses. To create such test scenarios, we measure and model the photometric properties of galaxy clusters and their sky environments from the Dark Energy Survey Year 3 (DES Y3) data in two bins of cluster richness λ∈[30;45) ⁠, λ∈[45;60) and three bins in cluster redshift (⁠z∈[0.3;0.35) ⁠, z∈[0.45;0.5) and z∈[0.6;0.65) ⁠. Using deep-field imaging data, we extrapolate galaxy populations beyond the limiting magnitude of DES Y3 and calculate the properties of cluster member galaxies via statistical background subtraction. We construct mock galaxy clusters as random draws from a distribution function, and render mock clusters and line-of-sight catalogues into synthetic images in the same format as actual survey observations. Synthetic galaxy clusters are generated from real observational data, and thus are independent from the assumptions inherent to cosmological simulations. The recipe can be straightforwardly modified to incorporate extra information, and correct for survey incompleteness. New realizations of synthetic clusters can be created at minimal cost, which will allow future analyses to generate the large number of images needed to characterize systematic uncertainties in cluster mass measurements., This research was supported by the Excellence Cluster ORIGINS which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strat- egy –EXC-2094-390783311. The calculations have been in part carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP). This w ork w as supported by the Department of Energy, Laboratory Directed Research and Development program at SLAC National Accelerator Laboratory, under contract DE-AC02-76SF00515 and as part of the P anofsk y Fellowship awarded to DG. 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 Supercomput- ing 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 Te xas A&M Univ ersity, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana- Champaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the Institut de Fisica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit ¨at M ¨unchen 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. The DES data management system is supported by the Na- tional 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 programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.
Published: 2021
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12. Cosmological Constraints from DES Y1 Cluster Abundances and SPT Multi-wavelength data

Author: E. Suchyta, F. Ruppin, Samuel Hinton, Sunayana Bhargava, M. Carrasco Kind, Felipe Menanteau, Maria E. S. Pereira, V. Scarpine, S. Samuroff, G. Gutierrez, Ramon Miquel, Enrique Gaztanaga, Jennifer L. Marshall, T. N. Varga, K. Kuehn, Elisabeth Krause, P. Fosalba, A. Choi, Josh Frieman, David J. Brooks, K. Honscheid, G. Tarle, Marcelle Soares-Santos, J. Myles, Daniel Gruen, David J. James, J. P. Dietrich, Sebastian Grandis, A. Roodman, Tommaso Giannantonio, Juan Garcia-Bellido, I. Ferrero, Daniel B. Thomas, D. W. Gerdes, Nikhel Gupta, M. E. C. Swanson, J. Annis, M. Costanzi, N. MacCrann, D. Rapetti, I. Sevilla-Noarbe, Sebastian Bocquet, A. Carnero Rosell, N. Kuropatkin, F. Paz-Chinchón, Shantanu Desai, Risa H. Wechsler, S. Everett, Antonella Palmese, E. Buckley-Geer, Agnès Ferté, L. N. da Costa, M. A. G. Maia, B. Flaugher, Joseph J. Mohr, M. N. K. Smith, Z. Zhang, A. Saro, Marcos Lima, Christian L. Reichardt, O. Lahav, A. A. Plazas, Parampreet Singh, R. L. C. Ogando, J. De Vicente, T. M. C. Abbott, Robert Morgan, Santiago Avila, D. L. Hollowood, S. Serrano, T. F. Eifler, Chun-Hao To, L. Salvati, E. J. Sanchez, H. T. Diehl, David Bacon, P. Doel, A. Amara, Douglas L. Tucker, Paul Giles, Tesla E. Jeltema, Bradford Benson, Michel Aguena, D. L. Burke, S. Allam, Robert A. Gruendl, A. A. Stark, W. G. Hartley, J. Carretero, A. K. Romer, UAM. Departamento de Física Teórica, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), National Science Foundation (US), Costanzi, M., Saro, A., Bocquet, S., Abbott, T. M. C., Aguena, M., Allam, S., Amara, A., Annis, J., Avila, S., Bacon, D., Benson, B. A., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Choi, A., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Everett, S., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giles, P., Grandis, S., Gruen, D., Gruendl, R. A., Gupta, N., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maccrann, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Rapetti, D., Reichardt, C. L., Romer, A. K., Roodman, A., Ruppin, F., Salvati, L., Samuroff, S., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Singh, P., Smith, M., Soares-Santos, M., Stark, A. A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Varga, T. N., Wechsler, R. H., and Zhang, Z.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), media_common.quotation_subject, Cosmological parameters, FOS: Physical sciences, Galaxy clusters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, XMM-Newton Telescope, Cosmology, 0103 physical sciences, Cluster (physics), Large-scale structure of the Universe, 010306 general physics, Weak gravitational lensing, STFC, media_common, AGLOMERADOS (GALÁXIA), Physics, 010308 nuclear & particles physics, Gravitation, Cosmology and Astrophysics, RCUK, Física, Galaxies, Cosmos, Redshift, Universe, Data set, South Pole Telescope, 13. Climate action, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Costanzi, M., et al. DES and SPT Collaborations, We perform a joint analysis of the counts of redMaPPer clusters selected from the Dark Energy Survey (DES) year 1 data and multiwavelength follow-up data collected within the 2500 deg2 South Pole Telescope (SPT) Sunyaev-Zel'dovich (SZ) survey. The SPT follow-up data, calibrating the richness-mass relation of the optically selected redMaPPer catalog, enable the cosmological exploitation of the DES cluster abundance data. To explore possible systematics related to the modeling of projection effects, we consider two calibrations of the observational scatter on richness estimates: a simple Gaussian model which account only for the background contamination (BKG), and a model which further includes contamination and incompleteness due to projection effects (PRJ). Assuming either a ΛCDM+mν or wCDM+mν cosmology, and for both scatter models, we derive cosmological constraints consistent with multiple cosmological probes of the low and high redshift Universe, and in particular with the SPT cluster abundance data. This result demonstrates that the DES Y1 and SPT cluster counts provide consistent cosmological constraints, if the same mass calibration data set is adopted. It thus supports the conclusion of the DES Y1 cluster cosmology analysis which interprets the tension observed with other cosmological probes in terms of systematics affecting the stacked weak lensing analysis of optically selected low-richness clusters. Finally, we analyze the first combined optically SZ selected cluster catalog obtained by including the SPT sample above the maximum redshift probed by the DES Y1 redMaPPer sample (z=0.65). Besides providing a mild improvement of the cosmological constraints, this data combination serves as a stricter test of our scatter models: the PRJ model, providing scaling relations consistent between the two abundance and multiwavelength follow-up data, is favored over the BKG model., Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, National Science Fundation’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 Australian (aka “Oz”) Dark Energy Survey Membership Consortium.Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grants Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. This paper has gone through internal review by the DES Collaboration. M. C. and A. S. are supported by the ERC-StG ’ClustersXCosmo’ Grant Agreement No. 716762. A. S. is supported by the FARE-MIUR Grant
Published: 2021

13. Understanding the extreme luminosity of DES14X2fna

Author: I. Sevilla-Noarbe, M. Soares-Santos, N. Kuropatkin, L. N. da Costa, A. A. Plazas, T. N. Varga, Geraint F. Lewis, Claudia P. Gutiérrez, M. Vincenzi, Santiago González-Gaitán, M. Carrasco Kind, C. Frohmaier, M. Costanzi, Lluís Galbany, A. R. Walker, C. Lidman, B. E. Tucker, E. Swann, Kyler Kuehn, Sunayana Bhargava, Peter Doel, H. T. Diehl, J. De Vicente, Jennifer L. Marshall, Niall MacCrann, I. Ferrero, Enrique Gaztanaga, G. Tarle, A. K. Romer, Pablo Fosalba, Daniel Thomas, V. Scarpine, Robert Morgan, A. Carnero Rosell, Paul Martini, Josh Frieman, Anais Möller, E. Bertin, Karl Glazebrook, Juan Garcia-Bellido, Carlos Solans Sanchez, Ramon Miquel, J. Gschwend, Samuel Hinton, G. Gutierrez, Daniela Carollo, Mark Sullivan, S. A. Uddin, R. D. Wilkinson, J. Carretero, P. Wiseman, S. Everett, Marcos Lima, E. Suchyta, David J. Brooks, S. Serrano, Michel Aguena, Ben Hoyle, Antonella Palmese, F. Paz-Chinchón, M. Grayling, M. Smith, Daniel Gruen, T. M. C. Abbott, Robert A. Gruendl, L. Kelsey, Chun-Hao To, E. J. Sanchez, Santiago Avila, S. Desai, 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), 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, Grayling, M., Gutiérrez, C. P., Sullivan, M., Wiseman, P., Vincenzi, M., González-Gaitán, S., Tucker, B. E., Galbany, L., Kelsey, L., Lidman, C., Swann, E., Smith, M., Frohmaier, C., Carollo, D., Glazebrook, K., Lewis, G. F., Möller, A., Hinton, S. R., Uddin, S. A., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hoyle, B., Kuehn, K., Kuropatkin, N., Lima, M., Maccrann, N., Marshall, J. L., Martini, P., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Sánchez, C., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Walker, A. R., and Wilkinson, R. D. (DES Collaboration)
Subjects: general [Supernovae], individual: DES14X2fna [Supernovae], FOS: Physical sciences, Astrophysics, Magnetar, 01 natural sciences, 7. Clean energy, Luminosity, Photometry (optics), supernovae: individual: DES14X2fna, supernovae: general, 0103 physical sciences, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Redshift, Neutron star, Supernova, 13. Climate action, Space and Planetary Science, Dark energy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: This work was supported by the Science and Technology Facilities Council [grant number ST/P006760/1] through the DISCnet Centre for Doctoral Training. MS acknowledges support from EU/FP7-ERC grant 615929. LG was funded by the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-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). Funding for the DES Projects has been provided by the US Department of Energy, the US '0:funding-source 3:href="http://dx.doi.org/10.13039/100000001"' National Science Foundation'/0:funding-source', 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, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico, and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen 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. This paper is based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management 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 Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. This paper is based in part on data acquired at the Anglo-Australian Telescope, under program A/2013B/012. 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. This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting this paper for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this paper, or allow others to do so, for United States Government purposes. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration., We present DES14X2fna, a high-luminosity, fast-declining Type IIb supernova (SN IIb) at redshift z = 0.0453, detected by the Dark Energy Survey (DES). DES14X2fna is an unusual member of its class, with a light curve showing a broad, luminous peak reaching Mr −19.3mag 20 d after explosion. This object does not show a linear decline tail in the light curve until 60 d after explosion, after which it declines very rapidly (4.30 ± 0.10 mag 100 d−1 in the r band). By fitting semi-analytic models to the photometry of DES14X2fna, we find that its light curve cannot be explained by a standard 56Ni decay model as this is unable to fit the peak and fast tail decline observed. Inclusion of either interaction with surrounding circumstellar material or a rapidly-rotating neutron star (magnetar) significantly increases the quality of the model fit. We also investigate the possibility for an object similar to DES14X2fna to act as a contaminant in photometric samples of SNe Ia for cosmology, finding that a similar simulated object is misclassified by a recurrent neural network (RNN)-based photometric classifier as an SN Ia in ∼1.1–2.4 per cent of cases in DES, depending on the probability threshold used for a positive classification., Science and Technology Facilities Council through the DISCnet Centre for Doctoral Training, EU/FP7-ERC grant 615929, European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant 839090, Spanish grant within the European Funds for Regional Development (FEDER) PGC2018-095317-B-C21, United States Department of Energy (DOE), National Science Foundation (NSF), Spanish Government, UK Research & Innovation (UKRI), Science & Technology Facilities Council (STFC), Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Kavli Institute of Cosmological Physics at the University of Chicago, Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University, Financiadora de Inovacao e Pesquisa (Finep), Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ), Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Ministerio da Ciencia, Tecnologia e Inovacao, German Research Foundation (DFG), Collaborating Institutions in the Dark Energy Survey, National Science Foundation (NSF) AST-1138766 AST-1536171, MINECO AYA2015-71825 ESP2015-66861 FPA2015-68048 SEV-2016-0588 SEV-2016-0597 MDM-2015-0509, European Commission, CERCA program of the Generalitat de Catalunya, European Research Council (ERC) FP7/2007-2013, European Research Council (ERC) European Commission 240672 291329 306478, Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant) 465376/2014-2, Fermi Research Alliance, LLC DE-AC02-07CH11359, Anglo-Australian Telescope A/2013B/012, National Aeronautics & Space Administration (NASA)
Published: 2021

14. A machine learning approach to galaxy properties: Joint redshift-stellar mass probability distributions with Random Forest

Author: A. A. Plazas, L. N. Da Costa, W. G. Hartley, Maria E. S. Pereira, Brian Yanny, Marcos Lima, Alex Drlica-Wagner, J. Carretero, Antonella Palmese, E. M. Huff, Juan Garcia-Bellido, Ramon Miquel, M. A. G. Maia, Michel Aguena, V. Scarpine, A. Choi, Martin Crocce, F. J. Castander, G. Tarle, R. D. Wilkinson, Ian Harrison, S. Mucesh, K. Honscheid, Sunayana Bhargava, A. Alarcon, J. De Vicente, David J. James, Huan Lin, Pablo Fosalba, M. Carrasco Kind, Chun-Hao To, Alexandra Amon, E. J. Sanchez, F. Paz-Chinchón, Keith Bechtol, E. Suchyta, August E. Evrard, M. Costanzi, M. Smith, Felipe Menanteau, Josh Frieman, D. L. Hollowood, S. Allam, Robert A. Gruendl, S. Serrano, Ofer Lahav, Daniel Gruen, Samuel Hinton, Peter Melchior, Christopher J. Conselice, Erin Sheldon, B. Flaugher, E. Bertin, G. Gutierrez, David J. Brooks, S. Desai, Enrique Gaztanaga, Robert Morgan, J. Gschwend, S. Everett, D. W. Gerdes, Gary Bernstein, I. Ferrero, H. T. Diehl, David Bacon, I. Sevilla-Noarbe, N. Kuropatkin, K. D. Eckert, T. N. Varga, Asa F. L. Bluck, Kyler Kuehn, Michael Schubnell, Daniel Thomas, L. Whiteway, A. Carnero Rosell, National Science Foundation (US), 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), DES, Mucesh, S., Hartley, W. G., Palmese, A., Lahav, O., Whiteway, L., Amon, A., Bechtol, K., Bernstein, G. M., Carnero Rosell, A., Carrasco Kind, M., Choi, A., Eckert, K., Everett, S., Gruen, D., Gruendl, R. A., Harrison, I., Huff, E. M., Kuropatkin, N., Sevilla-Noarbe, I., Sheldon, E., Yanny, B., Aguena, M., Allam, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Drlica-Wagner, A., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lima, M., Lin, H., Maia, M. A. G., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., and Wilkinson, R. D.
Subjects: FOS: Computer and information sciences, Computer Science - Machine Learning, statistical [Methods], software: data analysis, computer.software_genre, 01 natural sciences, data analysi [software], Copula (probability theory), Machine Learning (cs.LG), Astrophysics - Cosmology and Nongalactic Astrophysic, data analysis [Methods], 010303 astronomy & astrophysics, Physics, fundamental parameter [galaxies], galaxies: fundamental parameters, Random forest, Software: public realese, fundamental parameters [Galaxies], Probability distribution, galaxies: evolution, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, public realese [Software], Cosmology and Nongalactic Astrophysics (astro-ph.CO), methods: data analysis, methods: statistical, software: public release, Astrophysics - Astrophysics of Galaxies, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Machine learning, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, Galaxy formation and evolution, [INFO]Computer Science [cs], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Probability integral transform, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, business.industry, Univariate, Astronomy and Astrophysics, evolution [Galaxies], public release [software], Redshift, Galaxy, Space and Planetary Science, data analysis [Software], Astrophysics of Galaxies (astro-ph.GA), data analysi [methods], Artificial intelligence, Astrophysics - Instrumentation and Methods for Astrophysic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, computer
Abstract: We demonstrate that highly accurate joint redshift-stellar mass probability distribution functions (PDFs) can be obtained using the Random Forest (RF) machine learning (ML) algorithm, even with few photometric bands available. As an example, we use the Dark Energy Survey (DES), combined with the COSMOS2015 catalogue for redshifts and stellar masses. We build two ML models: one containing deep photometry in the $griz$ bands, and the second reflecting the photometric scatter present in the main DES survey, with carefully constructed representative training data in each case. We validate our joint PDFs for $10,699$ test galaxies by utilizing the copula probability integral transform and the Kendall distribution function, and their univariate counterparts to validate the marginals. Benchmarked against a basic set-up of the template-fitting code BAGPIPES, our ML-based method outperforms template fitting on all of our predefined performance metrics. In addition to accuracy, the RF is extremely fast, able to compute joint PDFs for a million galaxies in just under $6$ min with consumer computer hardware. Such speed enables PDFs to be derived in real time within analysis codes, solving potential storage issues. As part of this work we have developed GALPRO, a highly intuitive and efficient Python package to rapidly generate multivariate PDFs on-the-fly. GALPRO is documented and available for researchers to use in their cosmology and galaxy evolution studies., Comment: 18 pages, 8 figures, Accepted by MNRAS
Published: 2021

15. Dark energy survey internal consistency tests of the joint cosmological probes analysis with posterior predictive distributions

Author: R. L. C. Ogando, J. DeRose, E. Suchyta, M. Smith, G. Tarle, Daniel Gruen, Youngsoo Park, D. W. Gerdes, S. Samuroff, T. N. Varga, R. Cawthon, David J. Brooks, J. Gschwend, Sunayana Bhargava, Michael Schubnell, K. Honscheid, Samuel Hinton, W. G. Hartley, Marcos Lima, J. P. Dietrich, G. Gutierrez, Ofer Lahav, Juan Garcia-Bellido, C. Lidman, Alexandra Amon, J. Carretero, Ramon Miquel, Peter Doel, M. Costanzi, Dragan Huterer, M. Carrasco Kind, Robert Morgan, J. Frieman, H. T. Diehl, David Bacon, Felipe Menanteau, E. Baxter, F. Paz-Chinchón, I. Ferrero, Matt J. Jarvis, J. Annis, Marco Raveri, Elisabeth Krause, M. Gatti, David J. James, Niall MacCrann, J. Muir, Tommaso Giannantonio, D. L. Burke, Pablo Fosalba, Ami Choi, Ben Hoyle, E. Bertin, A. A. Plazas, I. Sevilla-Noarbe, Bhuvnesh Jain, S. Allam, Robert A. Gruendl, V. Scarpine, Antonella Palmese, N. Kuropatkin, D. L. Hollowood, M. A. G. Maia, S. Serrano, A. Alarcon, A. Campos, E. M. Huff, L. N. da Costa, P. Lemos, Michel Aguena, R. D. Wilkinson, S. Everett, Maria E. S. Pereira, J. Prat, M. E. C. Swanson, Jochen Weller, T. M. C. Abbott, C. Doux, Chun-Hao To, Markus Rau, E. J. Sanchez, Santiago Avila, Chihway Chang, Michael Troxel, S. Desai, Joe Zuntz, Douglas L. Tucker, Kyler Kuehn, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), Fermilab, Doux, C., Baxter, E., Lemos, P., Chang, C., Alarcon, A., Amon, A., Campos, A., Choi, A., Gatti, M., Gruen, D., Jarvis, M., Maccrann, N., Park, Y., Prat, J., Rau, M. M., Raveri, M., Samuroff, S., Derose, J., Hartley, W. G., Hoyle, B., Troxel, M. A., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huff, E. M., Huterer, D., Jain, B., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Tucker, D. L., Varga, T. N., Weller, J., Wilkinson, R. D., 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), Large-scale structure of Universe, FOS: Physical sciences, Dark energy, Gravitational lensing: weak, Methods: statistical, gravitational lensing: weak, methods: statistical, dark energy, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 01 natural sciences, Data vector, Goodness of fit, Consistency (statistics), Internal consistency, 0103 physical sciences, Statistics, Astrophysics - Cosmology and Nongalactic Astrophysic, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Joint (geology), Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Data set, Posterior predictive distribution, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], weak [Gravitational lensing]
Abstract: Doux, C., et al. DES Collaboration, Beyond ΛCDM, physics or systematic errors may cause subsets of a cosmological data set to appear inconsistent when analysed assuming ΛCDM. We present an application of internal consistency tests to measurements from the Dark Energy Survey Year 1 (DES Y1) joint probes analysis. Our analysis relies on computing the posterior predictive distribution (PPD) for these data under the assumption of ΛCDM. We find that the DES Y1 data have an acceptable goodness of fit to ΛCDM, with a probability of finding a worse fit by random chance of p = 0.046. Using numerical PPD tests, supplemented by graphical checks, we show that most of the data vector appears completely consistent with expectations, although we observe a small tension between large- and small-scale measurements. A small part (roughly 1.5 per cent) of the data vector shows an unusually large departure from expectations; excluding this part of the data has negligible impact on cosmological constraints, but does significantly improve the p-value to 0.10. The methodology developed here will be applied to test the consistency of DES Year 3 joint probes data sets., Based, in part, on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This 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

16. The WaZP galaxy cluster sample of the dark energy survey year 1

Author: G. Tarle, David J. Brooks, Antonella Palmese, David J. James, Josh Frieman, M. A. G. Maia, Pablo Fosalba, F. Paz-Chinchón, Michael Schubnell, M. Smith, Agnès Ferté, Samuel Hinton, Christophe Benoist, E. Suchyta, Basilio X. Santiago, August E. Evrard, G. Gutierrez, I. Ferrero, Sunayana Bhargava, J. Carretero, R. D. Wilkinson, B. Flaugher, H. Sampaio-Santos, Peter Melchior, Santiago Avila, K. Honscheid, R. L. C. Ogando, J. De Vicente, S. Everett, M. Carrasco Kind, S. Desai, Ramon Miquel, I. Sevilla-Noarbe, Juan Garcia-Bellido, Ofer Lahav, M. Soares-Santos, N. Kuropatkin, L. N. da Costa, Robert Morgan, A. Carnero Rosell, M. Costanzi, Marcos Lima, D. L. Hollowood, S. Serrano, Chun-Hao To, E. J. Sanchez, Douglas L. Tucker, Kyler Kuehn, Paul Giles, E. Bertin, J. Gschwend, Peter Doel, H. T. Diehl, David Bacon, S. Allam, Robert A. Gruendl, Tesla E. Jeltema, A. A. Plazas, Michel Aguena, A. K. Romer, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-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, Aguena, M., Benoist, C., da Costa, L. N., Ogando, R. L., Gschwend, J., Sampaio dos Santos, H., Lima, M., Maia, M. A., Allam, S., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Everett, S., Evrard, A., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Giles, P., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D. L., Honscheid, K., James, D., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Melchior, P., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchon, F., Plazas Malagón, A., Romer, K., Sanchez, E., Santiago, B., Schubnell, M., Serrano, S., Sevilla, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Tucker, D., Wilkinson, R., National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, and Instituto Nacional de Ciência e Tecnologia (Brasil)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Lambda, 01 natural sciences, surveys, 0103 physical sciences, distances and redshifts [Galaxies], Cluster (physics), clusters: general [galaxies], survey, distances and redshift [galaxies], data analysis [Methods], 010303 astronomy & astrophysics, Galaxy cluster, Photometric redshift, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, methods: data analysis, Galaxy, Redshift, South Pole Telescope, Space and Planetary Science, galaxies: clusters: general, data analysi [methods], Cluster sampling, galaxies: distances and redshifts, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aguena, M., et al., We present a new (2+1)D galaxy cluster finder based on photometric redshifts called Wavelet Z Photometric (WaZP) applied to DES first year (Y1A1) data. The results are compared to clusters detected by the South Pole Telescope (SPT) survey and the redMaPPer cluster finder, the latter based on the same photometric data. WaZP searches for clusters in wavelet-based density maps of galaxies selected in photometric redshift space without any assumption on the cluster galaxy populations. The comparison to other cluster samples was performed with a matching algorithm based on angular proximity and redshift difference of the clusters. It led to the development of a new approach to match two optical cluster samples, following an iterative approach to minimize incorrect associations. The WaZP cluster finder applied to DES Y1A1 galaxy survey (1511.13 deg2 up to mi = 23 mag) led to the detection of 60 547 galaxy clusters with redshifts 0.05 < z < 0.9 and richness Ngals ≥ 5. Considering the overlapping regions and redshift ranges between the DES Y1A1 and SPT cluster surveys, all sz based SPT clusters are recovered by the WaZP sample. The comparison between WaZP and redMaPPer cluster samples showed an excellent overall agreement for clusters with richness Ngals (λ for redMaPPer) greater than 25 (20), with 95 per cent recovery on both directions. Based on the cluster cross-match, we explore the relative fragmentation of the two cluster samples and investigate the possible signatures of unmatched clusters., 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

17. Dark Energy Survey Year 3 results: Curved-sky weak lensing mass map reconstruction

Author: Sunayana Bhargava, Jennifer L. Marshall, David J. Brooks, Carlos Solans Sanchez, G. Tarle, Samuel Hinton, G. Gutierrez, Alexandra Amon, Peter Doel, Ami Choi, Ben Hoyle, Marco Raveri, B. Flaugher, F. Andrade-Oliveira, Jochen Weller, R. P. Rollins, H. T. Diehl, D. L. Burke, Felipe Menanteau, Alex Drlica-Wagner, J. DeRose, F. J. Castander, David Bacon, E. Suchyta, Dragan Huterer, Christopher J. Conselice, Brian Yanny, Jack Elvin-Poole, U. Demirbozan, Maria E. S. Pereira, Niall MacCrann, Keith Bechtol, Erin Sheldon, Martin Crocce, V. Scarpine, T. M. C. Abbott, Peter Melchior, D. L. Hollowood, S. Serrano, Agnès Ferté, J. De Vicente, J. Cordero, P. F. Leget, A. Campos, Eli S. Rykoff, C. Doux, Chun-Hao To, E. J. Sanchez, K. Herner, F. Paz-Chinchón, J. Carretero, Antonella Palmese, Marcos Lima, J. Myles, I. Harrison, G. Pollina, A. Roodman, David J. James, Tommaso Giannantonio, D. Zeurcher, M. A. G. Maia, M. Rodriguez-Monroy, Joe Zuntz, A. Alarcon, B. Yin, S. Allam, Robert A. Gruendl, A. Kovács, Matthew R. Becker, Pablo Fosalba, B. Mawdsley, Ashley J. Ross, S. Pandey, J. Muir, Joseph J. Mohr, Michael Troxel, I. Ferrero, Matt J. Jarvis, A. Carnero Rosell, J. McCullough, P. Vielzeuf, Yanxi Zhang, Seshadri Nadathur, M. Carrasco Kind, M. March, S. Everett, M. Smith, M. Costanzi, Jean-Luc Starck, Daniel Gruen, I. Tutusaus, Francois Lanusse, Chihway Chang, Daniel Thomas, J. Prat, L. Whiteway, F. Elsner, S. Desai, I. Sevilla-Noarbe, M. Soares-Santos, G. Giannini, W. G. Hartley, D. W. Gerdes, R. Cawthon, N. Kuropatkin, Ramon Miquel, K. D. Eckert, T. N. Varga, L. N. da Costa, J. P. Dietrich, Juan Garcia-Bellido, E. Bertin, E. M. Huff, R. Chen, Michel Aguena, Enrique Gaztanaga, R. L. C. Ogando, Bhuvnesh Jain, M Gatti, Ofer Lahav, Niall Jeffrey, Robert Morgan, L. F. Secco, Nico Hamaus, A. A. Plazas, A. Navarro-Alsina, T. Shin, T. Kacprzak, C. Davis, J. Gschwend, Gary Bernstein, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), University of Portsmouth, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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, Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Jeffrey, N., Gatti, M., Chang, C., Whiteway, L., Demirbozan, U., Kovacs, A., Pollina, G., Bacon, D., Hamaus, N., Kacprzak, T., Lahav, O., Lanusse, F., Mawdsley, B., Nadathur, S., Starck, J. L., Vielzeuf, P., Zeurcher, D., Alarcon, A., Amon, A., Bechtol, K., Bernstein, G. M., Campos, A., Rosell, A. C., Kind, M. C., Cawthon, R., Chen, R., Choi, A., Cordero, J., Davis, C., Derose, J., Doux, C., Drlica-Wagner, A., Eckert, K., Elsner, F., Elvin-Poole, J., Everett, S., Ferte, A., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Kuropatkin, N., Jarvis, M., Leget, P. F., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Pandey, S., Prat, J., Raveri, M., Rollins, R. P., Ross, A. J., Rykoff, E. S., Sanchez, C., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M. A., Tutusaus, I., Varga, T. N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Becker, M. R., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Castander, F. J., Conselice, C., Costanzi, M., Crocce, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Ferrero, I., Flaugher, B., Fosalba, P., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Hoyle, B., Jain, B., James, D. J., Lima, M., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Weller, J., Université de Paris, University College London, Barcelona Institute of Science and Technology, University of Pennsylvania, University of Chicago, Calle Viá Láctea, Universidad de La Laguna (ULL), Ludwig-Maximilians Universität München, ETH Zurich, Argonne National Laboratory, Stanford University, University of Wisconsin-Madison, CarnegieMellon University, Instituto de Astrofisica de Canarias, Laboratorio Interinstitucional de e-Astronomia-LIneA, Dpto. Astrofisica, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Duke University, Ohio State University, University of Manchester, University of California,Berkeley, Santa Cruz Institute for Particle Physics, Fermi National Accelerator Laboratory, California Institute of Technology, SLAC National Accelerator Laboratory, Denys Wilkinson Building, University of Geneva, University of Michigan, University of Cambridge, Universidade Estadual de Campinas (UNICAMP), Medioambientales y Tecnologicas (CIEMAT), Brookhaven National Laboratory, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC), Max Planck Institute for Extraterrestrial Physics, University of Edinburgh, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de Saõ Paul, Universidade Estadual Paulista (UNESP), Institut d'Astrophysique deParis, Institut d'Astrophysique de Paris, University of Sussex, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, IIT Hyderabad, Ludwig-Maximilians-Universitat, University of Oslo, Universidad Autonoma de Madrid, University of Queensland, Center for Astrophysics | Harvard and Smithsonian, Texas A and M University, Princeton University, Institucio Catalana de Recerca i Estudis Avancats, University of Southampton, Oak Ridge National Laboratory, and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Gravitational lensing: weak, 0103 physical sciences, Prior probability, Maximum a posteriori estimation, 010303 astronomy & astrophysics, STFC, Weak gravitational lensing, Methods: statistical, media_common, Physics, ST/M001334/1, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Celestial sphere, gravitational lensing: Weak, large-scale structure of Universe, methods: Statistical, ST/R000476/1, Galaxy, Space and Planetary Science, Sky, astro-ph.CO, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Jeffrey, N., et al. DES Collaboration, We present reconstructed convergence maps, mass maps, from the Dark Energy Survey (DES) third year (Y3) weak gravitational lensing data set. The mass maps are weighted projections of the density field (primarily dark matter) in the foreground of the observed galaxies. We use four reconstruction methods, each is a maximum a posteriori estimate with a different model for the prior probability of the map: Kaiser–Squires, null B-mode prior, Gaussian prior, and a sparsity prior. All methods are implemented on the celestial sphere to accommodate the large sky coverage of the DES Y3 data. We compare the methods using realistic ΛCDM simulations with mock data that are closely matched to the DES Y3 data. We quantify the performance of the methods at the map level and then apply the reconstruction methods to the DES Y3 data, performing tests for systematic error effects. The maps are compared with optical foreground cosmic-web structures and are used to evaluate the lensing signal from cosmic-void profiles. The recovered dark matter map covers the largest sky fraction of any galaxy weak lensing map to date., The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. NJ has been supported by funding from l’Ecole Normale Supérieure, Paris. OL and NJ acknowledge support from a European Research Council Advanced Grant TESTDE (FP7/291329) and STFC Consolidated Grants ST/M001334/1 and ST/R000476/1. AK has been supported by a Juan de la Cierva fellowship from MINECO with project number IJC2018-037730-I, and funding for this project was also available in part through SEV-2015-0548 and AYA2017-89891-P. Cosmic voids computational work has been performed on the UK SCIAMA High Performance Computing cluster supported by the ICG, SEPNet, and the University of Portsmouth.
Published: 2021

18. The host galaxies of 106 rapidly evolving transients discovered by the Dark Energy Survey

Author: Juan Garcia-Bellido, E. Bertin, C. Frohmaier, P. Wiseman, Josh Frieman, Douglas L. Tucker, Kyler Kuehn, Antonella Palmese, S. Everett, N. E. Sommer, J. Gschwend, M. Pursiainen, Lluís Galbany, M. A. G. Maia, A. R. Walker, G. Tarle, J. Carretero, M. Sako, Tamara M. Davis, Mark Sullivan, A. Carnero Rosell, D. L. Hollowood, S. Serrano, Anais Möller, David J. James, A. K. Romer, Richard Kessler, Daniel Scolnic, Peter Doel, Paul Martini, Pablo Fosalba, Marcos Lima, H. T. Diehl, Karl Glazebrook, K. Honscheid, V. Scarpine, C. Lidman, B. E. Tucker, Daniela Carollo, E. Swann, I. Sevilla-Noarbe, N. Kuropatkin, Sunayana Bhargava, M. E. C. Swanson, T. N. Varga, D. L. Burke, L. N. da Costa, Jennifer L. Marshall, T. M. C. Abbott, Ryan J. Foley, Claudia P. Gutiérrez, Felipe Menanteau, Samuel Hinton, M. Costanzi, David J. Brooks, G. Gutierrez, S. Allam, Robert A. Gruendl, Geraint F. Lewis, E. J. Sanchez, B. P. Thomas, J. Annis, Michel Aguena, F. Paz-Chinchón, Ramon Miquel, M. Smith, Daniel Gruen, Michael Schubnell, M. Childress, L. Kelsey, A. A. Plazas, M. Vincenzi, E. Suchyta, M. Carrasco Kind, Enrique Gaztanaga, 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), 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, European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Ministerio de Economía y Competitividad (España), and Generalitat de Catalunya
Subjects: transients: supernovae, Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, abundances [Galaxies], Data_CODINGANDINFORMATIONTHEORY, Astrophysics, star formation [Galaxies], 01 natural sciences, Luminosity, Photometry (optics), 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, 010303 astronomy & astrophysics, Fast blue, [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, photometry [Galaxies], supernovae [Transients], Astronomy and Astrophysics, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Galaxy, Redshift, galaxies: photometry, Stars, Supernova, Space and Planetary Science, galaxies: star formation, Dark energy, galaxies: abundances
Abstract: DES Collaboration: et al., Rapidly evolving transients (RETs), also termed fast blue optical transients, are a recently discovered group of astrophysical events that display rapid luminosity evolution. RETs typically rise to peak in less than 10 d and fade within 30, a time-scale unlikely to be compatible with the decay of Nickel-56 that drives conventional supernovae (SNe). Their peak luminosity spans a range of −15 < Mg < −22.5, with some events observed at redshifts greater than 1. Their evolution on fast time-scales has hindered high-quality follow-up observations, and thus their origin and explosion/emission mechanism remains unexplained. In this paper, we present the largest sample of RETs to date, comprising 106 objects discovered by the Dark Energy Survey, and perform the most comprehensive analysis of RET host galaxies. Using deep-stacked photometry and emission lines from OzDES spectroscopy, we derive stellar masses and star formation rates (SFRs) for 49 host galaxies, and metallicities ([O/H]) for 37. We find that RETs explode exclusively in star-forming galaxies and are thus likely associated with massive stars. Comparing RET hosts to samples of host galaxies of other explosive transients as well as field galaxies, we find that RETs prefer galaxies with high specific SFRs (〈log (sSFR)〉 ∼ −9.6), indicating a link to young stellar populations, similar to stripped-envelope SNe. RET hosts appear to show a lack of chemical enrichment, their metallicities akin to long-duration gamma-ray bursts and superluminous SN host galaxies (〈12 + log (O/H)〉 ∼ 9.4). There are no clear relationships between mass or SFR of the host galaxies and the peak magnitudes or decline rates of the transients themselves., We acknowledge support from STFC grant ST/R000506/1. MSm, MSu, and CPG acknowledge support from from the European Union’s 7th Framework Programme (EU/FP7) European Research Council (ERC) grant no. 615929. LG was funded by the European Union’s Horizon 2020 research and innovation programme 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). LK was supported by the Science and Technology Facilities Council (grant number ST/P006760/1) through the DISCnet Centre for Doctoral Training. 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, SEV2016-0597, 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 Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2)
Published: 2020

19. The XMM Cluster Survey:new evidence for the 3.5 keV feature in clusters is inconsistent with a dark matter origin

Author: R. D. Wilkinson, Matt Hilton, P. Rooney, Chris A. Collins, Tesla E. Jeltema, C. Vergara, Maria Manolopoulou, Pedro T. P. Viana, John P. Stott, A. Bermeo, Paul Giles, A. K. Romer, E. Swann, S. Rosborough, K. Sabirli, Julian A. Mayers, and Sunayana Bhargava
Subjects: Sterile neutrino, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Cluster (physics), Emission spectrum, 010306 general physics, 010303 astronomy & astrophysics, QC, Galaxy cluster, Astrophysics::Galaxy Astrophysics, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astronomy and Astrophysics, High Energy Physics - Phenomenology, Space and Planetary Science, Halo, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: There have been several reports of a detection of an unexplained excess of X-ray emission at $\simeq$ 3.5 keV in astrophysical systems. One interpretation of this excess is the decay of sterile neutrino dark matter. The most influential study to date analysed 73 clusters observed by the XMM-Newton satellite. We explore evidence for a $\simeq$ 3.5 keV excess in the XMM-PN spectra of 117 redMaPPer galaxy clusters ($0.1 < z < 0.6$). In our analysis of individual spectra, we identify three systems with an excess of flux at $\simeq$ 3.5 keV. In one case (XCS J0003.3+0204) this excess may result from a discrete emission line. None of these systems are the most dark matter dominated in our sample. We group the remaining 114 clusters into four temperature ($T_{\rm X}$) bins to search for an increase in $\simeq$ 3.5 keV flux excess with $T_{\rm X}$ - a reliable tracer of halo mass. However, we do not find evidence of a significant excess in flux at $\simeq$ 3.5 keV in any $T_{\rm X}$ bins. To maximise sensitivity to a potentially weak dark matter decay feature at $\simeq$ 3.5 keV, we jointly fit 114 clusters. Again, no significant excess is found at $\simeq$ 3.5 keV. We estimate the upper limit of an undetected emission line at $\simeq$ 3.5 keV to be $2.41 \times 10^{-6}$ photons cm$^{-2}$ s$^{-1}$, corresponding to a mixing angle of $\sin^2(2��)=4.4 \times 10^{-11}$, lower than previous estimates from cluster studies. We conclude that a flux excess at $\simeq$ 3.5 keV is not a ubiquitous feature in clusters and therefore unlikely to originate from sterile neutrino dark matter decay., 17 pages, 14 figures. Accepted for publication in MNRAS
Published: 2020

20. Weak lensing of Type Ia Supernovae from the Dark Energy Survey

Author: Anais Möller, E. Bertin, A. K. Romer, Samuel Hinton, J. Gschwend, G. Gutierrez, A. Roodman, David J. Brooks, Sunayana Bhargava, T. N. Varga, Peter Doel, M. Smith, H. T. Diehl, Ramon Miquel, David Bacon, Ofer Lahav, Jennifer L. Marshall, Daniel Gruen, Jack Elvin-Poole, David J. James, Marcelle Soares-Santos, Kyler Kuehn, Ryan J. Foley, Geraint F. Lewis, Daniel Scolnic, D. L. Burke, A. Carnero Rosell, A. R. Walker, G. Tarle, M. E. C. Swanson, Juan Garcia-Bellido, Dragan Huterer, V. Scarpine, E. Suchyta, B. Flaugher, Robert A. Gruendl, Karl Glazebrook, Felipe Menanteau, J. Annis, Daniela Carollo, M. Sako, D. W. Gerdes, Peter Melchior, C. Lidman, B. E. Tucker, D. L. Hollowood, J. Carretero, Michael Schubnell, Tamara M. Davis, S. Desai, Michel Aguena, K. Honscheid, S. Serrano, M. Costanzi, I. Sevilla-Noarbe, N. Kuropatkin, L. N. da Costa, Antonella Palmese, M. A. G. Maia, Salcedo Romero de Ávila, Jochen Weller, Marcos Lima, F. J. Castander, T. M. C. Abbott, E. J. Sanchez, Edward Macaulay, A. A. Plazas, N. E. Sommer, D. J. Brout, M. Carrasco Kind, Robert C. Nichol, Enrique Gaztanaga, 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, 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), Macaulay, E., Bacon, D., Nichol, R. C., Davis, T. M., Elvin-Poole, J., Brout, D., Carollo, D., Glazebrook, K., Hinton, S. R., Lewis, G. F., Lidman, C., Möller, A., Sako, M., Scolnic, D., Smith, M., Sommer, N. E., Tucker, B. E., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Doel, P., Flaugher, B., Foley, R. J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Palmese, A., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Walker, A. R., Weller, J., and Des, Collaboration
Subjects: Cosmological parameter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmological parameters, FOS: Physical sciences, Astrophysics, 01 natural sciences, cosmology: observations, Large-scale structure of the universe, Astrophysics - Cosmology and Nongalactic Astrophysics, 0103 physical sciences, cosmological parameters, 010303 astronomy & astrophysics, Weak gravitational lensing, STFC, Angular correlation function, Physics, 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, Redshift, observations [cosmology], Supernova, Amplitude, Space and Planetary Science, Skewness, Dark energy, large-scale structure of the universe, ST/N000668/1, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], observation [cosmology]
Abstract: We consider the effects of weak gravitational lensing on observations of 196 spectroscopically confirmed Type Ia Supernovae (SNe Ia) from years 1 to 3 of the Dark Energy Survey (DES). We simultaneously measure both the angular correlation function and the non-Gaussian skewness caused by weak lensing. This approach has the advantage of being insensitive to the intrinsic dispersion of SNe Ia magnitudes. We model the amplitude of both effects as a function of $\sigma_8$, and find $\sigma_8 = 1.2^{+0.9}_{-0.8}$. We also apply our method to a subsample of 488 SNe from the Joint Light-curve Analysis (JLA) (chosen to match the redshift range we use for this work), and find $\sigma_8 = 0.8^{+1.1}_{-0.7}$. The comparable uncertainty in $\sigma_8$ between DES-SN and the larger number of SNe from JLA highlights the benefits of homogeneity of the DES-SN sample, and improvements in the calibration and data analysis., Comment: 10 pages, 7 figures, MNRAS
Published: 2020

21. The Diffuse Light Envelope of Luminous Red Galaxies

Author: Yanxi Zhang, Eli S. Rykoff, G. Gutierrez, Antonella Palmese, M. A. G. Maia, M. E. C. Swanson, B. Flaugher, J. Carretero, A. Carnero Rosell, Juan Garcia-Bellido, E. Bertin, Kyler Kuehn, M. Costanzi, Brian Yanny, A. K. Romer, K. Herner, J. Annis, A. Roodman, I. Sevilla-Noarbe, David J. James, N. Kuropatkin, T. N. Varga, L. N. da Costa, Sunayana Bhargava, K. Honscheid, Marcos Lima, Michael Schubnell, H. Sampaio-Santos, S. Everett, V. Scarpine, R. L. C. Ogando, V. Strazzullo, S. Serrano, Ramon Miquel, J. Gschwend, A. A. Plazas, Josh Frieman, E. Suchyta, D. L. Burke, Peter Doel, S. Allam, Robert A. Gruendl, H. T. Diehl, David J. Brooks, M. Carrasco Kind, Michel Aguena, T. F. Eifler, Enrique Gaztanaga, E. J. Sanchez, Santiago Avila, Y. Leung, S. Desai, F. Paz-Chinchón, M. Smith, Daniel Gruen, A. G. Kim, 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, Leung, Y., Zhang, Y., Yanny, B., Herner, K., Annis, J., Palmese, A., Sampaio-Santos, H., Strazzullo, V., Aguena, M., Allam, S., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Kim, A. G., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., and Varga, T. N.
Subjects: Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Flux, General Medicine, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Astrophysics of Galaxies (astro-ph.GA), Galaxy evolution, 0103 physical sciences, Galaxy formation and evolution, Diffuse reflection, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Sersic profile, Astrophysics::Galaxy Astrophysics, Envelope (waves)
Abstract: We use a stacking method to study the radial light profiles of luminous red galaxies (LRGs) at redshift ∼0.62 and ∼0.25, out to a radial range of 200 kpc. We do not find noticeable evolution of the profiles at the two redshifts. The LRG profiles appear to be well approximated by a single Sérsic profile, although some excess light can be seen outside 60 kpc. We quantify the excess light by measuring the integrated flux and find that the excess is about 10%—a non-dominant but still nonnegligible component.
Published: 2020

22. Increasing the census of L and T dwarfs in wide binary and multiple systems using Dark Energy Survey DR1 and Gaia DR2 data

Author: M. E. C. Swanson, Josh Frieman, Peter Doel, I. Sevilla-Noarbe, N. Kuropatkin, T. N. Varga, L. N. da Costa, H. T. Diehl, E. Suchyta, G. Tarle, P. Martini, A. R. Walker, David J. James, Pablo Fosalba, J. Carretero, J. Gschwend, Felipe Menanteau, Tenglin Li, G. Gutierrez, Kyler Kuehn, K. Bechtol, L. de Paris, Enrique Gaztanaga, Santiago Avila, M. Smith, M. Aguena, J. De Vicente, B. Flaugher, Daniel Gruen, Brian Yanny, A. Carnero Rosell, David J. Brooks, Antonella Palmese, D. W. Gerdes, Juan Garcia-Bellido, M. Carrasco Kind, E. Bertin, M. March, Basilio X. Santiago, M. A. G. Maia, Tim Eifler, D. L. Hollowood, K. Honscheid, S. R. Hinton, S. Serrano, F. Paz-Chinchón, Sunayana Bhargava, Daniel Thomas, R. Miquel, E. Buckley-Geer, Jennifer L. Marshall, T. M. C. Abbott, S. Everett, E. J. Sanchez, Ben Burningham, M. dal Ponte, S. Allam, Robert A. Gruendl, A. A. Plazas, V. Scarpine, 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), and German Research Foundation
Subjects: Proper motion, Brown dwarf, FOS: Physical sciences, Binary number, Astrophysics, Stellar classification, 7. Clean energy, 01 natural sciences, general [binaries], stars: low-mass, 0103 physical sciences, low-mass [stars], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Stars, Astrophysics - Solar and Stellar Astrophysics, binaries: general, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics, brown dwarfs
Abstract: Full author list: M dal Ponte, B Santiago, A Carnero Rosell, B Burningham, B Yanny, J L Marshall, K Bechtol, P Martini, T S Li, L De Paris, T M C Abbott, M Aguena, S Allam, S Avila, E Bertin, S Bhargava, D Brooks, E Buckley-Geer, M Carrasco Kind, J Carretero, L N da Costa, J De Vicente, H T Diehl, P Doel, T F Eifler, S Everett, B Flaugher, P Fosalba, J Frieman, J García-Bellido, E Gaztanaga, D W Gerdes, D Gruen, R A Gruendl, J Gschwend, G Gutierrez, S R Hinton, D L Hollowood, K Honscheid, D J James, K Kuehn, N Kuropatkin, M A G Maia, M March, F Menanteau, R Miquel, A Palmese, F Paz-Chinchón, A A Plazas, E Sanchez, V Scarpine, S Serrano, I Sevilla-Noarbe, M Smith, E Suchyta, M E C Swanson, G Tarle, D Thomas, T N Varga, A R Walker, DES Collaboration, We present the discovery of 255 binary and 6 multiple system candidates with wide (> 5 arcsec) separation composed by ultracool dwarfs (UCDs) companions to stars, plus nine double ultracool dwarf systems. These systems were selected based on common distance criteria. About 90 per cent of the total sample has proper motions available and 73 per cent of the systems also satisfy a common proper motion criterion. The sample of ultracool candidates was taken from the Dark Energy Survey (DES) and the candidate stellar primaries are from Gaia DR2 and DES data. We compute chance alignment probabilities in order to assess the physical nature of each pair. We find that 174 candidate pairs with Gaia DR2 primaries and 81 pairs with a DES star as a primary have chance alignment probabilities < 5. Only nine candidate systems composed of two UCDs were identified. The sample of candidate multiple systems is made up of five triple systems and one quadruple system. The majority of the UCDs found in binaries and multiples are of early L type and the typical wide binary fraction over the L spectral types is 2-4. Our sample of candidate wide binaries with UCDs as secondaries constitutes a substantial increase over the known number of such systems, which are very useful to constrain the formation and evolution of UCDs., Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the NSF’s National Optical-Infrared Astronomy Research Laboratory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, NSF’s National Optical-Infrared Astronomy Research Laboratory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant 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 Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration. The analysis presented here is based on observations obtained as part of the VHS, ESO Programme, 179.A-2010 (PI: McMahon). This paper has gone through internal review by the DES collaboration. ACR acknowledges financial support provided by the PAPDRJ CAPES/FAPERJ Fellowship and by ‘Unidad de Excelencia María de Maeztu de CIEMAT – Física de Partículas (Proyecto MDM)’
Published: 2020

23. The Dark Energy Survey and Operations: Year 6 – The Finale

Author: Johnson, Douglas L. Tucker, Dragan Huterer, Alyssa Garcia, K. Bechtol, M.R. Kirby, Marcelle Soares-Santos, David J. James, Eric H. Neilsen, A. Lathrop, Sunayana Bhargava, Tianjun Li, Robert Morgan, Travis Prochaska, A. A. Plazas, A. Troja, Jennifer L. Marshall, Q. Wang, T.A. Hutchinson, S. Everett, L. Markwardt, R. D. Wilkinson, Kevin Reil, B. Yanny, Z. Zhang, R. Sgeir, Bhuvnesh Jain, K. Herner, J. A. Smith, J. DeRose, J. Muir, A. R. Walker, Salcedo Romero de Ávila, E. Wagoner, Yi Chen, A. K. Vivas, P. Martini, K. Honscheid, T. M. C. Abbott, Don Petravick, Alexandra Amon, Alfredo Zenteno, B. Flaugher, Gary Bernstein, Antonella Palmese, R. G. Kron, Steve Kent, A. Chen, S. Allam, Robert A. Gruendl, M. Murphy, N. Weaverdyck, H. T. Diehl, F. Paz-Chinchón, M. S. S. Gill, Daniel Gruen, Y.-H. Zhang, C. E. Martínez-Vázquez, D. J. Turner, N. Kuropatkin, Josh Frieman, L. N. da Costa, D. L. Hollowood, and Antonio Campos
Subjects: Telescope, Supernova, Observatory, law, Dark energy, Environmental science, Astronomy, Baryon acoustic oscillations, Galaxy cluster, Weak gravitational lensing, Metric expansion of space, law.invention
Abstract: The Dark Energy Survey (DES) is an optical and near-infrared imaging survey aimed at understanding the accelerating expansion of the universe using four complementary methods: weak gravitational lensing, galaxy cluster counts, baryon acoustic oscillations, and Type Ia supernovae. To perform the 6-season 5000 sq-degree wide field and the 5-season 30 sq-degree supernova surveys, the DES Collaboration built the Dark Energy Camera (DECam), a 3 square-degree, 570-Megapixel CCD camera that was installed at the prime focus of the Blanco 4-meter telescope at the Cerro Tololo Inter-American Observatory (CTIO). DES started its observations in “Year 1” (Y1) on Aug. 31, 2013 and completed its sixth and final observing season on January 9, 2019. This paper describes DES Y6, the survey strategy, an outline of the survey operations procedures, the efficiency of operations and the causes of lost observing time. It provides details about the quality of the final season's data, and a summary of the Y1-Y6 observing. It contains a brief description of the last night of observations.
Published: 2020

24. Dark Energy Survey Year 3 Results: Covariance Modelling and its Impact on Parameter Estimation and Quality of Fit

Author: R. Buchs, Jochen Weller, Samuel Hinton, G. Tarle, Marco Raveri, G. Gutierrez, Ian Harrison, A. Troja, J. Prat, Alexandra Amon, Y. Omori, H. Camacho, Brian Yanny, V. Scarpine, J. McCullough, Josh Frieman, M. Smith, M. Costanzi, Bhuvnesh Jain, I. Sevilla-Noarbe, Keith Bechtol, Daniel Gruen, David J. Brooks, M. Soares-Santos, Sunayana Bhargava, Ramon Miquel, Rogerio Rosenfeld, D. L. Hollowood, S. Serrano, Felipe Menanteau, Carlos Solans Sanchez, T. N. Varga, N. Weaverdyck, L. N. da Costa, M. Gatti, Ofer Lahav, Xiao Fang, A. Campos, J. DeRose, E. Suchyta, August E. Evrard, I. Ferrero, Matt J. Jarvis, J. Myles, David J. James, D. W. Gerdes, A. Roodman, Tommaso Giannantonio, Elisabeth Krause, Pablo Fosalba, Alex Drlica-Wagner, Tim Eifler, H. T. Diehl, Robert Morgan, Javier Sanchez, Dragan Huterer, Eli S. Rykoff, Marcos Lima, J. Carretero, J. Cordero, Erin Sheldon, C. Doux, Chun-Hao To, V. Terra, E. J. Sanchez, S. Samuroff, David Bacon, F. Paz-Chinchón, Martin Crocce, O. Alves, A. Carnero Rosell, R. D. Wilkinson, Michael Troxel, L. F. Secco, S. Pandey, J. Muir, A. Choi, K. Honscheid, Jack Elvin-Poole, Kyler Kuehn, A. Alarcon, Niall MacCrann, A. A. Plazas, G. Giannini, C. Davis, S. Everett, Scott Dodelson, Santiago Avila, Chihway Chang, S. Desai, J. Gschwend, Antonella Palmese, Gary Bernstein, Maria E. S. Pereira, M. A. G. Maia, M. Rodriguez-Monroy, A. Porredon, E. Baxter, E. Bertin, W. G. Hartley, Juan Garcia-Bellido, Oliver Friedrich, M. Carrasco Kind, F. Andrade-Oliveira, Enrique Gaztanaga, R. Cawthon, Daniel Thomas, F. Elsner, J. De Vicente, Michel Aguena, D. L. Burke, Robert A. Gruendl, 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, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), University of Cambridge, Universidade Estadual Paulista (UNESP), Laboratório Interinstitucional de e-Astronomia - LIneA, University of Michigan, Fermi National Accelerator Laboratory, University of Arizona, California Institute of Technology, University of Chicago, Stanford University, University of Hawaii, Ohio State University, Institut d'Estudis Espacials de Catalunya (IEEC), CSIC, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, Medioambientales y Tecnológicas (CIEMAT), University of Portsmouth, University of Sussex, Princeton University, University of Southampton, Oak Ridge National Laboratory, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, Friedrich, O., Andrade-Oliveira, F., Camacho, H., Alves, O., Rosenfeld, R., Sanchez, J., Fang, X., Eifler, T. F., Krause, E., Chang, C., Omori, Y., Amon, A., Baxter, E., Elvin-Poole, J., Huterer, D., Porredon, A., Prat, J., Terra, V., Troja, A., Alarcon, A., Bechtol, K., Bernstein, G. M., Buchs, R., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Choi, A., Cordero, J., Crocce, M., Davis, C., Derose, J., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Elsner, F., Everett, S., Fosalba, P., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Harrison, I., Hartley, W. G., Jain, B., Jarvis, M., Maccrann, N., Mccullough, J., Muir, J., Myles, J., Pandey, S., Raveri, M., Roodman, A., Rodriguez-Monroy, M., Rykoff, E. S., Samuroff, S., Sánchez, C., Secco, L. F., Sevilla-Noarbe, I., Sheldon, E., Troxel, M. A., Weaverdyck, N., Yanny, B., Aguena, M., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Evrard, A. E., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Soares-Santos, M., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Wilkinson, R. D., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gaussian, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, symbols.namesake, 0103 physical sciences, Applied mathematics, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Equation of state (cosmology), Estimation theory, Covariance matrix, Astronomy and Astrophysics, Covariance, cosmology: observations, large-scale structure of Universe, observations [cosmology], Weighting, Space and Planetary Science, symbols, Dark energy, Trispectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology]
Abstract: Friedrich, O., et al. DES Collaboration, We describe and test the fiducial covariance matrix model for the combined two-point function analysis of the Dark Energy Survey Year 3 (DES-Y3) data set. Using a variety of new ansatzes for covariance modelling and testing, we validate the assumptions and approximations of this model. These include the assumption of Gaussian likelihood, the trispectrum contribution to the covariance, the impact of evaluating the model at a wrong set of parameters, the impact of masking and survey geometry, deviations from Poissonian shot noise, galaxy weighting schemes, and other sub-dominant effects. We find that our covariance model is robust and that its approximations have little impact on goodness of fit and parameter estimation. The largest impact on best-fitting figure-of-merit arises from the so-called fsky approximation for dealing with finite survey area, which on average increases the χ2 between maximum posterior model and measurement by 3.7 per cent (Δχ2 ≈ 18.9). Standard methods to go beyond this approximation fail for DES-Y3, but we derive an approximate scheme to deal with these features. For parameter estimation, our ignorance of the exact parameters at which to evaluate our covariance model causes the dominant effect. We find that it increases the scatter of maximum posterior values for Ωm and σ8 by about 3 per cent and for the dark energy equation-of-state parameter by about 5 per cent⁠., 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). 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
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25. Candidate periodically variable quasars from the Dark Energy Survey and the Sloan Digital Sky Survey

Author: J. Carretero, Tamara M. Davis, Matias Carrasco Kind, Samuel Hinton, M. March, S. Everett, Timothy M. C. Abbott, E. Suchyta, G. Gutierrez, H. Thomas Diehl, Luiz N. da Costa, Juan Garcia-Bellido, Marcos Lima, Yu-Ching Chen, Antonella Palmese, Xin Liu, Aurelio Carnero Rosell, Alistair R. Walker, M. Costanzi, Sunayana Bhargava, Jennifer L. Marshall, Brad E. Tucker, Kaiwen Zhang, David J. James, Michel Aguena, Ramon Miquel, Wei-Ting Liao, A. A. Plazas, A. Miguel Holgado, Felipe Menanteau, C. Lidman, Geraint F. Lewis, B. Flaugher, Gregory Tarle, Nikolay Kuropatkin, Michael Schubnell, Karl Glazebrook, Peter Doel, David J. Brooks, Hengxiao Guo, Enrique Gaztanaga, Emmanuel Bertin, Santiago Avila, Shantanu Desai, Devon L. Hollowood, Marcio A. G. Maia, Mathew Smith, D. L. Burke, Yue Shen, S. Allam, Robert A. Gruendl, E. J. Sanchez, F. Paz-Chinchón, Daniel Gruen, Daniela Carollo, Alex G. Kim, Santiago Serrano, Molly E. C. Swanson, Eric Morganson, Juan de Vicente, I. Sevilla-Noarbe, T. N. Varga, Joshua A. Frieman, Douglas Friedel, 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, National Science Foundation (US), European Commission, European Research Council, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Chen, Yu-Ching, Liu, Xin, Liao, Wei-Ting, Holgado, A Miguel, Guo, Hengxiao, Gruendl, Robert A, Morganson, Eric, Shen, Yue, Zhang, Kaiwen, Abbott, Tim M C, Aguena, Michel, Allam, Sahar, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L, Rosell, Aurelio Carnero, Carollo, Daniela, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, da Costa, Luiz N, Davis, Tamara M, De Vicente, Juan, Desai, Shantanu, Diehl, H Thoma, Doel, Peter, Everett, Spencer, Flaugher, Brenna, Friedel, Dougla, Frieman, Joshua, García-Bellido, Juan, Gaztanaga, Enrique, Glazebrook, Karl, Gruen, Daniel, Gutierrez, Gaston, Hinton, Samuel R, Hollowood, Devon L, James, David J, Kim, Alex G, Kuehn, Kyler, Kuropatkin, Nikolay, Lewis, Geraint F, Lidman, Christopher, Lima, Marco, Maia, Marcio A G, March, Marisa, Marshall, Jennifer L, Menanteau, Felipe, Miquel, Ramon, Palmese, Antonella, Paz-Chinchón, Francisco, Plazas, Andrés A, Sanchez, Eusebio, Schubnell, Michael, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Suchyta, Eric, Swanson, Molly E C, Tarle, Gregory, Tucker, Brad E, Varga, Tamas Norbert, and Walker, Alistair R
Subjects: Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies: active, nuclei [galaxies], FOS: Physical sciences, Astrophysics, Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, quasars: general, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, survey, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, ONDAS GRAVITACIONAIS, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, general [quasars], 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Quasar, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Light curve, black hole physic, Redshift, Supernova, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies], Astronomical and Space Sciences
Abstract: DES Collaboration: et al., Periodically variable quasars have been suggested as close binary supermassive black holes. We present a systematic search for periodic light curves in 625 spectroscopically confirmed quasars with a median redshift of 1.8 in a 4.6 deg2 overlapping region of the Dark Energy Survey Supernova (DES-SN) fields and the Sloan Digital Sky Survey Stripe 82 (SDSS-S82). Our sample has a unique 20-yr long multicolour (griz) light curve enabled by combining DES-SN Y6 observations with archival SDSS-S82 data. The deep imaging allows us to search for periodic light curves in less luminous quasars (down to r ∼23.5 mag) powered by less massive black holes (with masses ≳ 108.5M⊙) at high redshift for the first time. We find five candidates with significant (at >99.74 per cent single-frequency significance in at least two bands with a global p-value of ∼7 × 10−4–3 × 10−3 accounting for the look-elsewhere effect) periodicity with observed periods of ∼3–5 yr (i.e. 1–2 yr in rest frame) having ∼4–6 cycles spanned by the observations. If all five candidates are periodically variable quasars, this translates into a detection rate of ∼0.8+0.5−0.3 per cent or ∼1.1+0.7−0.5 quasar per deg2. Our detection rate is 4–80 times larger than those found by previous searches using shallower surveys over larger areas. This discrepancy is likely caused by differences in the quasar populations probed and the survey data qualities. We discuss implications on the future direct detection of low-frequency gravitational waves. Continued photometric monitoring will further assess the robustness and characteristics of these candidate periodic quasars to determine their physical origins., The DES data management system is supported by the National Science Foundation under grants 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 grants 240672, 291329, and 306478.
Published: 2020

26. 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

27. A statistical standard siren measurement of the Hubble constant from the LIGO/Virgo gravitational wave compact object merger GW190814 and Dark Energy Survey galaxies

Author: R. L. C. Ogando, Alistair R. Walker, Alyssa Garcia, Marcelle Soares-Santos, V. Scarpine, E. Suchyta, Josh Frieman, August E. Evrard, J. deVicente, C. Nicolaou, Enrique Gaztanaga, M. Carrasco Kind, Michael Schubnell, K. Herner, A. Roodman, Antonella Palmese, W. G. Hartley, D. A. Finley, Alex Drlica-Wagner, O. Lahav, Robert Morgan, Juan Garcia-Bellido, K. Honscheid, Dragan Huterer, J. Carretero, E. Buckley-Geer, David J. James, J. Annis, Pablo Fosalba, I. Sevilla-Noarbe, Maria E. S. Pereira, I. Magaña Hernandez, M. A. G. Maia, W. C. Wester, Samuel Hinton, G. Gutierrez, David J. Brooks, G. Tarle, Elisabeth Krause, Peter Melchior, Ramon Miquel, J. Allyn Smith, Martin Crocce, R. D. Wilkinson, Sunayana Bhargava, Felipe Menanteau, Tamara M. Davis, S. Everett, Ryan J. Foley, K. Bechtol, L. N. da Costa, B. Flaugher, Jennifer L. Marshall, M. N. K. Smith, K. Kuehn, M. Sako, F. Paz-Chinchón, D. L. Hollowood, Daniel E. Holz, S. Serrano, Richard Kessler, J. Zuntz, M. Costanzi, Daniel Gruen, Salcedo Romero de Ávila, Juan Estrada, Michael Troxel, M. March, D. W. Gerdes, E. Bertin, Douglas L. Tucker, J. Gschwend, P. Doel, H. T. Diehl, M. S. S. Gill, Chihway Chang, C. J. Conselice, Huan Lin, S. Desai, Steve Kent, F. J. Castander, T. M. C. Abbott, E. J. Sanchez, D. L. Burke, S. Allam, A. A. Plazas, Robert A. Gruendl, Enrique J. Fernández, Michel Aguena, European Research Council, European Commission, Ministerio de Economía y Competitividad (España), 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, Palmese, A., Devicente, J., Pereira, M. E. S., Annis, J., Hartley, W., Herner, K., Soares-Santos, M., Crocce, M., Huterer, D., Magana Hernandez, I., Davis, T. M., Garcia, A., Garcia-Bellido, J., Gschwend, J., Holz, D. E., Kessler, R., Lahav, O., Morgan, R., Nicolaou, C., Conselice, C., Foley, R. J., Gill, M. S. S., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bechtol, K., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carrasco Kind, M., Carretero, J., Castander, F. J., Chang, C., Costanzi, M., da Costa, L. N., Desai, S., Diehl, H. T., Doel, P., Estrada, J., Everett, S., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kent, S., Krause, E., Kuehn, K., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchon, F., Plazas, A. A., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Allyn Smith, J., Smith, M., Suchyta, E., Tarle, G., Troxel, M. A., Tucker, D. L., Walker, A. R., Wester, W., Wilkinson, R. D., and Zuntz, J.
Subjects: Cosmological parameter, star: compact, cosmological model, coalescence, 010504 meteorology & atmospheric sciences, Physics::Instrumentation and Detectors, Astrophysics, Surveys, 7. Clean energy, 01 natural sciences, localization, Cosmology, Cosmological parameters, Gravitational waves, Hubble constant, Redshift surveys, Gravitational wave astronomy, parameter space, LIGO, Survey, dark energy, 010303 astronomy & astrophysics, Photometric redshift, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, density, photon, Mathematics::History and Overview, GALÁXIAS, Redshift survey, Astrophysics - High Energy Astrophysical Phenomena, Gravitational wave, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, statistical analysis, Binary black hole, 0103 physical sciences, distribution function, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, gravitational radiation, Astronomy and Astrophysics, redshift, Galaxy, Redshift, Black hole, VIRGO, electromagnetic, black hole: binary, Space and Planetary Science, Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: DES Collaboration: et al. arXiv:2006.14961v3, We present a measurement of the Hubble constant H0 using the gravitational wave (GW) event GW190814, which resulted from the coalescence of a 23 M⊙ black hole with a 2.6 M⊙ compact object, as a standard siren. No compelling electromagnetic counterpart has been identified for this event; thus our analysis accounts for thousands of potential host galaxies within a statistical framework. The redshift information is obtained from the photometric redshift (photo-z) catalog from the Dark Energy Survey. The luminosity distance is provided by the LIGO/Virgo gravitational wave sky map. Since this GW event has the second-smallest localization volume after GW170817, GW190814 is likely to provide the best constraint on cosmology from a single standard siren without identifying an electromagnetic counterpart. Our analysis uses photo-z probability distribution functions and corrects for photo-z biases. We also reanalyze the binary black hole GW170814 within this updated framework. We explore how our findings impact the H0 constraints from GW170817, the only GW merger associated with a unique host galaxy. From a combination of GW190814, GW170814, and GW170817, our analysis yields ${H}_{0}={72.0}_{-8.2}^{+12}\,\mathrm{km}\,{{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$(68% highest-density interval, HDI) for a prior in H0 uniform between $[20\mathrm{and}140]\,\mathrm{km}\,{{\rm{s}}}^{-1}\,{\mathrm{Mpc}}^{-1}$. The addition of GW190814 and GW170814 to GW170817 improves the 68% HDI from GW170817 alone by ~18%, showing how well-localized mergers without counterparts can provide a significant contribution to standard siren measurements, provided that a complete galaxy catalog is available at the location of the event., Funding for the DES Projects has been provided by the DOE and NSF(USA), MEC/MICINN/MINECO(Spain), STFC(UK), HEFCE(UK). NCSA(UIUC), KICP(U. Chicago), CCAPP(Ohio State), MIFPA(Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), DFG(Germany) and the Collaborating Institutions in the Dark Energy Survey. The DES Data Management System is supported by the NSF under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-88861, FPA2015-68048, and Centro de Excelencia SEV-2016-0588, SEV-2016-0597 and MDM-2015-0509. Research leading to these results has received funding from the ERC under the EU’s 7th Framework Programme including grants ERC 240672, 291329 and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020.
Published: 2020

28. First cosmology results using type Ia supernovae from the Dark Energy Survey: the effect of host galaxy properties on supernova luminosity

Author: Geraint F. Lewis, C. Frohmaier, David J. Brooks, Samuel Hinton, G. Gutierrez, Sunayana Bhargava, Jennifer L. Marshall, Brad E. Tucker, Eli S. Rykoff, Michel Aguena, A. R. Walker, Josh Frieman, Mark Sullivan, B. Flaugher, Elisabeth Krause, A. Carnero Rosell, M. Pursiainen, G. Tarle, R. R. Gupta, Tim Eifler, D. L. Burke, David J. James, Lluís Galbany, M. E. C. Swanson, Michael Schubnell, Pablo Fosalba, E. Macaulay, R. C. Thomas, S. Allam, Robert A. Gruendl, M. Carrasco Kind, I. Sevilla-Noarbe, J. De Vicente, Robert C. Nichol, Ramon Miquel, E. Suchyta, C. B. D'Andrea, K. Honscheid, Karl Glazebrook, Douglas L. Tucker, Antonella Palmese, N. Kuropatkin, Kyler Kuehn, M. A. G. Maia, Marcus Lima, P. Wiseman, T. N. Varga, L. N. da Costa, Tamara M. Davis, Juan Garcia-Bellido, Daniela Carollo, Peter Melchior, Peter Nugent, Claudia P. Gutiérrez, Felipe Menanteau, Daniel Scolnic, M. Costanzi, A. Roodman, M. Vincenzi, Enrique Gaztanaga, Ryan J. Foley, V. Scarpine, S. Everett, M. Sako, D. L. Hollowood, S. Serrano, Richard Kessler, A. A. Plazas, L. Kelsey, D. J. Brout, W. G. Hartley, N. E. Sommer, A. K. Romer, Paul Martini, F. Paz-Chinchón, M. Smith, Daniel Gruen, Anais Möller, E. Bertin, Peter Doel, H. T. Diehl, Niall MacCrann, J. Gschwend, C. Lidman, E. Swann, Daniel Thomas, E. Buckley-Geer, Santiago Avila, S. Desai, T. M. C. Abbott, E. J. Sanchez, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-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, Smith, M., Sullivan, M., Wiseman, P., Kessler, R., Scolnic, D., Brout, D., D'Andrea, C. B., Davis, T. M., Foley, R. J., Frohmaier, C., Galbany, L., Gupta, R. R., Gutiérrez, C. P., Hinton, S. R., Kelsey, L., Lidman, C., Macaulay, E., Möller, A., Nichol, R. C., Nugent, P., Palmese, A., Pursiainen, M., Sako, M., Swann, E., Thomas, R. C., Tucker, B. E., Vincenzi, M., Carollo, D., Lewis, G. F., Sommer, N. E., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Glazebrook, K., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maccrann, N., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Walker, A. R., Des, Collaboration, 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), and 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)
Subjects: transients: supernovae, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, distance scale, 01 natural sciences, Cosmology, Luminosity, surveys, supernovae: general, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, survey, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Equation of state (cosmology), RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Space and Planetary Science, cosmology: observations, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, Dark energy, Astrophysics::Earth and Planetary Astrophysics, supernovae [transients], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [supernovae], observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present improved photometric measurements for the host galaxies of 206 spectroscopically confirmed type Ia supernovae discovered by the Dark Energy Survey Supernova Program (DES-SN) and used in the first DES-SN cosmological analysis. Fitting spectral energy distributions to the $griz$ photometric measurements of the DES-SN host galaxies, we derive stellar masses and star-formation rates. For the DES-SN sample, when considering a 5D ($z$, $x_1$, $c$, $\alpha$, $\beta$) bias correction, we find evidence of a Hubble residual `mass step', where SNe Ia in high mass galaxies ($>10^{10} \textrm{M}_{\odot}$) are intrinsically more luminous (after correction) than their low mass counterparts by $\gamma=0.040\pm0.019$mag. This value is larger by $0.031$mag than the value found in the first DES-SN cosmological analysis. This difference is due to a combination of updated photometric measurements and improved star formation histories and is not from host-galaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with $\gamma=0.066\pm0.020$mag. The 1D-5D $\gamma$ difference for DES-SN is $0.026\pm0.009$mag. We show that this difference is due to a strong correlation between host galaxy stellar mass and the $x_1$ component of the 5D distance-bias correction. To better understand this effect, we include an intrinsic correlation between light-curve width and stellar mass in simulated SN Ia samples. We show that a 5D fit recovers $\gamma$ with $-9$mmag bias compared to a $+2$mmag bias for a 1D fit. This difference can explain part of the discrepancy seen in the data. Improvements in modeling correlations between galaxy properties and SN is necessary to determine the implications for $\gamma$ and ensure unbiased precision estimates of the dark energy equation-of-state as we enter the era of LSST., Comment: 27 pages, 13 figures; Submitted to MNRAS
Published: 2020
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29. A joint SZ-X-ray-optical analysis of the dynamical state of 288 massive galaxy clusters

Author: Matthew B. Bayliss, Eli S. Rykoff, M. Smith, Daniel Gruen, J. Gschwend, A. Roodman, A. Carnero Rosell, D. W. Gerdes, A. Katzenberger, M. E. C. Swanson, V. Scarpine, Sunayana Bhargava, Samuel Hinton, J. Carretero, G. Gutierrez, Matthias Klein, E. Suchyta, Felipe Menanteau, V. Ojeda, August E. Evrard, C. Vergara Cervantes, Marcos Lima, D. L. Burke, Michael Schubnell, Shantanu Desai, Peter Doel, Josh Frieman, A. A. Plazas, M. Carrasco Kind, Alistair R. Walker, Kyler Kuehn, H. T. Diehl, Marcelle Soares-Santos, F. Paz-Chinchón, I. Sevilla-Noarbe, D. Hernandez-Lang, R. Capasso, S. Allam, Robert A. Gruendl, Antonella Palmese, D. L. Hollowood, David J. James, K. Honscheid, R. D. Wilkinson, S. Serrano, Tesla E. Jeltema, M. A. G. Maia, Pablo Fosalba, T. N. Varga, David J. Brooks, W. G. Hartley, L. N. da Costa, R. L. C. Ogando, C. Lidman, J. De Vicente, Michel Aguena, Daniel Thomas, E. Buckley-Geer, Joseph J. Mohr, B. Floyd, Peter Melchior, A. Saro, A. K. Romer, T. F. Eifler, F. J. Castander, V. Strazzullo, Ofer Lahav, E. J. Sanchez, Santiago Avila, Ramon Miquel, M. March, G. Tarle, Alfredo Zenteno, Juan Garcia-Bellido, B. Flaugher, E. Bertin, Mike McDonald, J. R. Gonzalez, M. Costanzi, Zenteno, A., Hernández-Lang, D., Klein, M., Vergara Cervantes, C., Hollowood, D. L., Bhargava, S., Palmese, A., Strazzullo, V., Romer, A. K., Mohr, J. J., Jeltema, T., Saro, A., Lidman, C., Gruen, D., Ojeda, V., Katzenberger, A., Aguena, M., Allam, S., Avila, S., Bayliss, M., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capasso, R., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Floyd, B., Fosalba, P., Frieman, J., García-Bellido, J., Gerdes, D. W., Gonzalez, J. R., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lima, M., Mcdonald, M., Maia, M. A. G., March, M., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Wilkinson, R. D., Des, Collaboration, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: evolution, galaxies: luminosity function, mass function, galaxies: clusters: general, 01 natural sciences, 0103 physical sciences, Cluster (physics), clusters: general [galaxies], Brightest cluster galaxy, education, 010303 astronomy & astrophysics, Galaxy cluster, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: luminosity function, South Pole Telescope, Space and Planetary Science, mass function, Astrophysics of Galaxies (astro-ph.GA), Cluster sampling, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We use imaging from the first three years of the Dark Energy Survey to characterize the dynamical state of 288 galaxy clusters at $0.1 \lesssim z \lesssim 0.9$ detected in the South Pole Telescope (SPT) Sunyaev-Zeldovich (SZ) effect survey (SPT-SZ). We examine spatial offsets between the position of the brightest cluster galaxy (BCG) and the center of the gas distribution as traced by the SPT-SZ centroid and by the X-ray centroid/peak position from Chandra and XMM data. We show that the radial distribution of offsets provides no evidence that SPT SZ-selected cluster samples include a higher fraction of mergers than X-ray-selected cluster samples. We use the offsets to classify the dynamical state of the clusters, selecting the 43 most disturbed clusters, with half of those at $z \gtrsim 0.5$, a region seldom explored previously. We find that Schechter function fits to the galaxy population in disturbed clusters and relaxed clusters differ at $z>0.55$ but not at lower redshifts. Disturbed clusters at $z>0.55$ have steeper faint-end slopes and brighter characteristic magnitudes. Within the same redshift range, we find that the BCGs in relaxed clusters tend to be brighter than the BCGs in disturbed samples, while in agreement in the lower redshift bin. Possible explanations includes a higher merger rate, and a more efficient dynamical friction at high redshift. The red-sequence population is less affected by the cluster dynamical state than the general galaxy population., 21 pages, 12 Figures, 4 Tables. Accepted for publication in MNRAS
Published: 2020

30. Dark energy survey year 1 results: Cosmological constraints from cluster abundances and weak lensing

Author: Alex Drlica-Wagner, Dragan Huterer, J. Annis, I. Sevilla-Noarbe, Daniel Scolnic, N. Kuropatkin, Tesla E. Jeltema, F. Paz-Chinchón, K. D. Eckert, T. N. Varga, Brian Nord, Adam Mantz, L. N. da Costa, M. Costanzi, M. A. G. Maia, Michel Aguena, E. Suchyta, August E. Evrard, Brian Yanny, Shantanu Desai, A. Alarcon, M. W. G. Johnson, A. K. Romer, J. Carretero, Paul Martini, V. Scarpine, I. Ferrero, Matt J. Jarvis, Tamara M. Davis, Yanxi Zhang, Tim Eifler, Arya Farahi, David James, Z. Zhang, D. W. Gerdes, Joshua A. Frieman, D. Gruen, R. Cawthon, Antonella Palmese, Pablo Fosalba, Carlos Solans Sanchez, D. H. Brooks, A. R. Walker, B. Flaugher, Risa H. Wechsler, P. Rooney, Keith Bechtol, M. Sako, C. Lidman, A. von der Linden, Erin Sheldon, D. L. Hollowood, M. E. C. Swanson, Huan Lin, Sebastian Bocquet, Julian A. Mayers, Steve Kent, J. De Vicente, Martin Crocce, R. D. Wilkinson, D. L. Burke, Daniel Thomas, E. Buckley-Geer, M. Carrasco Kind, S. Everett, Robert C. Nichol, S. Allam, Robert A. Gruendl, R. L. C. Ogando, J. P. Dietrich, Juan Garcia-Bellido, E. Bertin, Marcos Lima, Michael Troxel, Eduardo Rozo, Jack Elvin-Poole, Enrique Gaztanaga, Peter Doel, Peter Melchior, Ofer Lahav, M. Smith, H. T. Diehl, Douglas L. Tucker, Kyler Kuehn, J. Allyn Smith, Paul Giles, David Bacon, Niall MacCrann, Ami Choi, Ben Hoyle, A. Roodman, Markus Rau, Tommaso Giannantonio, J. Gschwend, Gary Bernstein, Hao-Yi Wu, Tenglin Li, Scott Dodelson, S. W. Allen, Santiago Avila, Chihway Chang, M. D. Johnson, Ramon Miquel, A. Bermeo, Elisabeth Krause, Sebastian Grandis, J. Mena-Fernández, Joe Zuntz, Jochen Weller, F. J. Castander, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, K. Honscheid, Eli S. Rykoff, Richard G. Kron, A. Carnero Rosell, Felipe Menanteau, S. Samuroff, Gregory Tarle, Santiago Serrano, J. DeRose, D. J. Brout, J. Prat, Samuel Hinton, G. Gutierrez, Xi Chen, A. A. Plazas, Sunayana Bhargava, Joseph J. Mohr, A. Saro, Jennifer L. Marshall, W. G. Hartley, M. Gatti, Juan Estrada, Michael Schubnell, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, European Research Council, 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, Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Allen, S., Annis, J., Avila, S., Bacon, D., Bechtol, K., Bermeo, A., Bernstein, G. M., Bertin, E., Bhargava, S., Bocquet, S., Brooks, D., Brout, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, X., Choi, A., Costanzi, M., Crocce, M., Da Costa, L. N., Davis, T. M., De Vicente, J., Derose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Estrada, J., Everett, S., Evrard, A. E., Farahi, A., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giles, P., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lima, M., Lin, H., Maccrann, N., Maia, M. A. G., Mantz, A., Marshall, J. L., Martini, P., Mayers, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Prat, J., Rau, M. M., Romer, A. K., Roodman, A., Rooney, P., Rozo, E., Rykoff, E. S., Sako, M., Samuroff, S., Sanchez, C., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, J. A., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tucker, D. L., Varga, T. N., Von Der Linden, A., Walker, A. R., Wechsler, R. H., Weller, J., Wilkinson, R. D., Wu, H., Yanny, B., Zhang, Y., Zhang, Z., and Zuntz, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Data_CODINGANDINFORMATIONTHEORY, 01 natural sciences, XMM-Newton Telescope, symbols.namesake, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, Planck, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Physics, 010308 nuclear & particles physics, Física, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Galaxies, Cosmos, Redshift, Galaxy, Cosmology, Dark energy, symbols, Baryon acoustic oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: DES Collaboration: et al., We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for S8=σ8(Ωm/0.3)0.5=0.65±0.04, driven by a low matter density parameter, Ωm=0.179+0.031−0.038, with σ8−Ωm posteriors in 2.4σ tension with the DES Y1 3x2pt results, and in 5.6σ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with x-ray and microwave data, as well as independent constraints on the observable-mass relation from Sunyaev-Zeldovich selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold (λ≥30) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model., The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-66861, No. FPA2015-68048, No. SEV2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through Project No. CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. M. C. and A. S. are supported by the ERC-StG “ClustersXCosmo” Grant agreement No. 716762. A. S. is supported by the FAREMIUR grant “ClustersXEuclid”. E. R. was supported by the DOE Grant No. DE-SC0015975, by the Sloan Foundation, Grant No. FG-2016-6443, and the Cottrell Scholar program of the Research Corporation for Science Advancement. This research used simulations that were performed resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DEAC02-05CH11231.
Published: 2020

31. Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey

Author: Michael Schubnell, Josh Frieman, K. Honscheid, David Brooks, David J. James, Jochen Weller, Santiago González-Gaitán, A. Roodman, Pablo Fosalba, B. E. Tucker, M. E. C. Swanson, Ryan J. Foley, T. M. C. Abbott, J. Carretero, Tamara M. Davis, Karl Glazebrook, Daniel Thomas, E. J. Sanchez, V. Scarpine, Sunayana Bhargava, A. A. Plazas, M. Costanzi, Claudia P. Gutiérrez, Felipe Menanteau, Marcos Lima, Shantanu Desai, Mario Hamuy, Daniela Carollo, Marcelle Soares-Santos, Gregory Tarle, Edward Macaulay, Juan Estrada, Anais Möller, A. R. Walker, M. A. G. Maia, Mathew Smith, Tenglin Li, D. L. Burke, F. Forster, Daniel Scolnic, W. G. Hartley, B. Flaugher, Enrique Gaztanaga, Santiago Avila, Peter J. Brown, Samuel Hinton, Antonella Palmese, G. Gutierrez, T. de Jaeger, Michel Aguena, Daniel Gruen, J. De Vicente, Geraint F. Lewis, Ramon Miquel, P. Doel, H. T. Diehl, Alexei V. Filippenko, N. E. Sommer, Alex Drlica-Wagner, A. Carnero Rosell, M. Carrasco Kind, J. Annis, J. Gschwend, S. Allam, Robert A. Gruendl, F. Paz-Chinchón, D. J. Brout, T. F. Eifler, I. Sevilla-Noarbe, S. Everett, Douglas L. Tucker, Kyler Kuehn, B. Nichol, N. Kuropatkin, E. Suchyta, T. N. Varga, L. N. da Costa, M. Sako, Cosimo Inserra, D. L. Hollowood, S. Serrano, Richard Kessler, Juan Garcia-Bellido, E. Bertin, Lluís Galbany, Martin Crocce, R. D. Wilkinson, A. K. Romer, 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, 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), de Jaeger, T., Galbany, L., González-Gaitán, S., Kessler, R., Filippenko, A. V., Förster, F., Hamuy, M., Brown, P. J., Davis, T. M., Gutiérrez, C. P., Inserra, C., Lewis, G. F., Möller, A., Scolnic, D., Smith, M., Brout, D., Carollo, D., Foley, R. J., Glazebrook, K., Hinton, S. R., Macaulay, E., Nichol, B., Sako, M., Sommer, N. E., Tucker, B. E., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Crocce, M., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Eifler, T. F., Estrada, J., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., T. S., Li, Lima, M., Maia, M. A. G., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Varga, T. N., Walker, A. R., Weller, J., Wilkinson, R., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), ) distance scale [(Cosmology], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Computer Science::Computational Geometry, 7. Clean energy, 01 natural sciences, symbols.namesake, 0103 physical sciences, Range (statistics), distances and redshifts [Galaxies], Astrophysics::Solar and Stellar Astrophysics, distances and redshift [galaxies], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, 4. Education, Cosmic distance ladder, (stars:) supernovae: general, Astronomy and Astrophysics, Redshift, Term (time), (cosmology:) distance scale, Supernova, 13. Climate action, Space and Planetary Science, ) supernovae: general [(Stars], AGLOMERADOS DE GALÁXIAS, Dark energy, symbols, galaxies: distances and redshifts, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Despite vast improvements in the measurement of the cosmological parameters, the nature of dark energy and an accurate value of the Hubble constant (H0) in the Hubble–Lemaˆıtre law remain unknown. To break the current impasse, it is necessary to develop as many independent techniques as possible, such as the use of Type II supernovae (SNe II). The goal of this paper is to demonstrate the utility of SNe II for deriving accurate extragalactic distances, which will be an asset for the next generation of telescopes where more-distant SNe II will be discovered. More specifically, we present a sample from the Dark Energy Survey Supernova Program (DES-SN) consisting of 15 SNe II with photometric and spectroscopic information spanning a redshift range up to 0.35. Combining our DES SNe with publicly available samples, and using the standard candle method (SCM), we construct the largest available Hubble diagram with SNe II in the Hubble flow (70 SNe II) and find an observed dispersion of 0.27 mag. We demonstrate that adding a colour term to the SN II standardization does not reduce the scatter in the Hubble diagram. Although SNe II are viable as distance indicators, this work points out important issues for improving their utility as independent extragalactic beacons: find new correlations, define a more standard subclass of SNe II, construct new SN II templates, and dedicate more observing time to high-redshift SNe II. Finally, for the first time, we perform simulations to estimate the redshift-dependent distance-modulus bias due to selection effects., National Science Foundation (NSF) AST-1211916, TABASGO Foundation, Gary and Cynthia Bengier, Christopher R. Redlich Fund, Sylvia and Jim Katzman Foundation, Miller Institute for Basic Research in Science (UC Berkeley) - European Union 839090, Spanish grant PGC2018-095317-B-C21, European Union (EU), EU/FP7-ERC grant 615929, National Science Foundation (NSF), Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan, Princeton University, Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), University of Tokyo, High Energy Accelerator Research Organization (KEK), FIRST programme from the Japanese Cabinet Office, Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT), Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science, Japan Science & Technology Agency (JST), Toray Industries, Inc., Institute for Astronomy (the University of Hawaii), Max Planck Society Foundation CELLEX, National Central University of Taiwan, Space Telescope Science Institute, National Aeronautics & Space Administration (NASA) NNX08AR22G, National Science Foundation (NSF) AST-1238877, University of Maryland, Eotvos Lorand University (ELTE), National Aeronautics & Space Administration (NASA), W.M. Keck Foundation, National Research Council of Canada, Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council (STFC), National Research Council, Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT), Australian Research Council, National Council for Scientific and Technological Development (CNPq), Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) GN-2005A-Q11 GN-2005B-Q-7 GN-2006A-Q-7 GS-2005A-Q-11 GS-2005BQ-6 GS-2008B-Q-56, United States Department of Energy (DOE), Spanish Government, Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Ohio State University, Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University, Ciencia Tecnologia e Inovacao (FINEP), Fundacao Carlos Chagas Filho de Amparo, Conselho Nacional de Desenvolvimento Cient'tronomy at Texas AM University, German Research Foundation (DFG), University of Portsmouth, OzDES Membership Consortium, National Science Foundation (NSF) AST-1138766 AST-1536171 AYA2015-71825 ESP2015-66861 FPA2015-68048 SEV2016-0588 SEV-2016-0597, European Union - CERCA programme of the Generalitat de Catalunya, European Research Council (ERC), European Research Council (ERC) 240672 291329 306478, National Council for Scientific and Technological Development (CNPq) 465376/2014-2, United States Department of Energy (DOE) DE-AC02-05CH11231
Published: 2020

32. μ* masses: Weak-lensing calibration of the dark energy survey year 1 redMaPPer clusters using stellar masses

Author: Antonella Palmese, Michael Schubnell, D. L. Burke, M. A. G. Maia, V. Scarpine, Sarah Bridle, A. Choi, Santiago Avila, G. Tarle, K. Honscheid, M. March, E. Bertin, J. Gschwend, Robert A. Gruendl, Peter Doel, A. K. Romer, H. T. Diehl, Niall MacCrann, Tesla E. Jeltema, Josh Frieman, Enrique Gaztanaga, Arya Farahi, Joe Zuntz, Carlos Solans Sanchez, I. Sevilla-Noarbe, Peter Melchior, David J. James, Felipe Menanteau, B. Flaugher, T. McClintock, Michel Aguena, N. Kuropatkin, W. G. Hartley, J. Annis, J. Esteves, Pablo Fosalba, Jochen Weller, J. Carretero, L. N. da Costa, M. Gatti, T. M. C. Abbott, J. Burgad, M. Carrasco Kind, Kyler Kuehn, Samuel Hinton, T. N. Varga, M. Costanzi, E. J. Sanchez, Huan Lin, Ben Hoyle, T. Shin, A. von der Linden, G. Gutierrez, Sunayana Bhargava, Shantanu Desai, Maria E. S. Pereira, A. A. Plazas, M. E. C. Swanson, Juan Estrada, Jennifer L. Marshall, Marcelle Soares-Santos, J. P. Dietrich, Juan Garcia-Bellido, Ofer Lahav, R. L. C. Ogando, Ramon Miquel, M. Smith, Daniel Gruen, Y.-H. Zhang, David J. Brooks, D. W. Gerdes, J. DeRose, E. Suchyta, Risa H. Wechsler, F. Paz-Chinchón, A. Roodman, A. Carnero Rosell, Marcos Lima, S. Everett, D. L. Hollowood, S. Serrano, National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Pereira, M E S, Palmese, A, Varga, T N, Mcclintock, T, Soares-Santos, M, Burgad, J, Annis, J, Farahi, A, Lin, H, Choi, A, Derose, J, Esteves, J, Gatti, M, Gruen, D, Hartley, W G, Hoyle, B, Jeltema, T, Maccrann, N, Roodman, A, Sánchez, C, Shin, T, von der Linden, A, Zuntz, J, Abbott, T M C, Aguena, M, Avila, S, Bertin, E, Bhargava, S, Bridle, S L, Brooks, D, Burke, D L, Rosell, A Carnero, Kind, M Carrasco, Carretero, J, Costanzi, M, da Costa, L N, Desai, S, Diehl, H T, Dietrich, J P, Doel, P, Estrada, J, Everett, S, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, D W, Gruendl, R A, Gschwend, J, Gutierrez, G, Hinton, S R, Hollowood, D L, Honscheid, K, James, D J, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M A G, March, M, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Ogando, R L C, Paz-Chinchón, F, Plazas, A A, Romer, A K, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smith, M, Suchyta, E, Swanson, M E C, Tarle, G, Wechsler, R H, Weller, J, and Zhang, Y
Subjects: Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, FOTOMETRIA, Cosmology, gravitational lensing: weak, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, observations [Cosmology], 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Photometric redshift, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, 13. Climate action, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Dark energy, Halo, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], weak [Gravitational lensing], observation [cosmology]
Abstract: We present the weak lensing mass calibration of the stellar mass based $\mu_{\star}$ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time we are able to perform a calibration of $\mu_{\star}$ at high redshifts, $z>0.33$. In a blinded analysis, we use $\sim 6,000$ clusters split into 12 subsets spanning the ranges $0.1 \leqslant z, Comment: 20 pages, 10 figures, submitted to MNRAS
Published: 2020

33. STRIDES: Spectroscopic and photometric characterization of the environment and effects of mass along the line of sight to the gravitational lenses DES J0408-5354 and WGD 2038-4008

Author: F. J. Castander, B. Flaugher, Peter Doel, H. T. Diehl, Josh Frieman, Samuel Hinton, E. J. Sanchez, G. Gutierrez, I. Sevilla-Noarbe, N. Kuropatkin, T. N. Varga, L. N. da Costa, Peter Melchior, Douglas L. Tucker, Kyler Kuehn, Sunayana Bhargava, Huan Lin, M. E. C. Swanson, K. Honscheid, J. Carretero, F. Paz-Chinchón, V. Scarpine, Jennifer L. Marshall, M. Costanzi, Tim Eifler, Santiago Avila, Michael Schubnell, Lise Christensen, Antonella Palmese, G. Tarle, E. Buckley-Geer, G. Meylan, M. Smith, David J. James, Daniel Gruen, M. A. G. Maia, Marcelle Soares-Santos, S. Desai, Cristian Rusu, Felipe Menanteau, E. Bertin, S. Serrano, David J. Brooks, Pablo Fosalba, Tommaso Treu, J. Poh, Anowar J. Shajib, Michel Aguena, J. Gschwend, A. Carnero Rosell, S. Allam, Robert A. Gruendl, A. A. Plazas, E. Suchyta, Simon Birrer, A. Agnello, S. Everett, Ramon Miquel, Thomas E. Collett, R. L. C. Ogando, Christopher D. Fassnacht, Juan Garcia-Bellido, Kenneth C. Wong, M. Carrasco Kind, Sampath Mukherjee, Enrique Gaztanaga, Timo Anguita, J. De Vicente, Buckley-Geer, E J, Lin, H, Rusu, C E, Poh, J, Palmese, A, Agnello, A, Christensen, L, Frieman, J, Shajib, A J, Treu, T, Collett, T, Birrer, S, Anguita, T, Fassnacht, C D, Meylan, G, Mukherjee, S, Wong, K C, Aguena, M, Allam, S, Avila, S, Bertin, E, Bhargava, S, Brooks, D, Carnero&nbsp, Rosell, A, Carrasco&nbsp, Kind, M, Carretero, J, Castander, F J, Costanzi, M, da&nbsp, Costa, L N, De&nbsp, Vicente, J, Desai, S, Diehl, H T, Doel, P, Eifler, T F, Everett, S, Flaugher, B, Fosalba, P, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R A, Gschwend, J, Gutierrez, G, Hinton, S R, Honscheid, K, James, D J, Kuehn, K, Kuropatkin, N, Maia, M A G, Marshall, J L, Melchior, P, Menanteau, F, Miquel, R, Ogando, R L C, Paz-Chinchón, F, Plazas, A A, Sanchez, E, Scarpine, V, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, M E C, Tarle, G, Tucker, D L, Varga, T N, 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, European Space Agency, National Aeronautics and Space Administration (US), European Research Council, European Commission, and Ministerio de Economía y Competitividad (España)
Subjects: Software_OPERATINGSYSTEMS, redshifts, ANGULAR MASKS, h-0, quasars: individual: des j0408-5354, wgd 2038-4008, Astrophysics, I, 7. Clean energy, 01 natural sciences, Spectral line, Gravitation, individual: DES J0408-5354, WGD 2038-4008 [quasars], galaxies: groups: general, clusters, 010303 astronomy & astrophysics, Physics, galaxy-group identification, Line-of-sight, individual: DES J0408-5354 [quasars], gravitational lensing: strong, Velocity dispersion, ComputerSystemsOrganization_PROCESSORARCHITECTURES, i, WGD 2038–4008, STELLAR POPULATION SYNTHESIS, strong [gravitational lensing], quasars: individual: DES J0408–5354, stellar population synthesis, quasars: individual: DES J0408-5354, WGD 2038-4008, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), QUASARES, ComputingMethodologies_SIMULATIONANDMODELING, FOS: Physical sciences, Probability density function, Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, REDSHIFTS, Astrophysics - Astrophysics of Galaxie, evolution, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, GALAXY-GROUP IDENTIFICATION, STFC, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, groups: general [galaxies], H-0, RCUK, resolution, Astronomy and Astrophysics, Quasar, angular masks, Redshift, Galaxy, EVOLUTION, RESOLUTION, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CLUSTERS
Abstract: The DES Collaboration: et al., In time-delay cosmography, three of the key ingredients are (1) determining the velocity dispersion of the lensing galaxy, (2) identifying galaxies and groups along the line of sight with sufficient proximity and mass to be included in the mass model, and (3) estimating the external convergence κext from less massive structures that are not included in the mass model. We present results on all three of these ingredients for two time-delay lensed quad quasar systems, DES J0408–5354 and WGD 2038–4008 . We use the Gemini, Magellan, and VLT telescopes to obtain spectra to both measure the stellar velocity dispersions of the main lensing galaxies and to identify the line-of-sight galaxies in these systems. Next, we identify 10 groups in DES J0408–5354 and two groups in WGD 2038–4008 using a group-finding algorithm. We then identify the most significant galaxy and galaxy-group perturbers using the ‘flexion shift’ criterion. We determine the probability distribution function of the external convergence κext for both of these systems based on our spectroscopy and on the DES-only multiband wide-field observations. Using weighted galaxy counts, calibrated based on the Millennium Simulation, we find that DES J0408–5354 is located in a significantly underdense environment, leading to a tight (width ∼3 per cent⁠), negative-value κext distribution. On the other hand, WGD 2038–4008 is located in an environment of close to unit density, and its low source redshift results in a much tighter κext of ∼1 per cent⁠, as long as no external shear constraints are imposed., JP would like to thank Gourav Khullar for his help and insightful discussions that helped improve the analysis in this paper. This work made use of computing resources and support provided by the Research Computing Center at the University of Chicago. JP is supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. AJS was supported by the National Aeronautics and Space Administration (NASA) through the Space Telescope Science Institute (STScI) grant HST-GO-15320. AJS was also supported by the Dissertation Year Fellowship from the University of California, Los Angeles (UCLA) graduate division. TA acknowledges support from Proyecto FONDECYT N: 1190335. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. CDF acknowledges support for this work from the National Science Foundation under Grant No. AST-1715611. SM acknowledges the funding from the European Research Council (ERC) under the EUs Horizon 2020 research and innovation program (COSMICLENS; grant agreement No. 787886). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management 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, ESP2015-88861, 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 number CE110001020. 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. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.
Published: 2020
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34. Dark Energy Surveyed Year 1 results: calibration of cluster mis-centring in the redMaPPer catalogues

Author: W. G. Hartley, C. Stern, Devon L. Hollowood, John P. Stott, Ramon Miquel, A. Bermeo, B. Flaugher, Martin Sahlén, Chris A. Collins, Eli S. Rykoff, Elisabeth Krause, Tesla E. Jeltema, Yanxi Zhang, Shantanu Desai, C. J. Miller, Arya Farahi, A. A. Plazas, J. Gschwend, Marcelle Soares-Santos, M. E. C. Swanson, M. Costanzi, Xi Chen, Vinu Vikram, J. P. Dietrich, R. H. Schindler, Juan Garcia-Bellido, W. C. Wester, E. Bertin, David J. Brooks, M. Klein, A. Carnero Rosell, J. Carretero, Peter Melchior, Sunayana Bhargava, M. Smith, Eduardo Rozo, Jennifer L. Marshall, Daniel Gruen, G. Gutierrez, S. W. Allen, D. L. Burke, Peter Doel, R. D. Wilkinson, Maria Manolopoulou, S. Allam, Robert A. Gruendl, Pablo Fosalba, K. Honscheid, H. T. Diehl, V. Scarpine, S. Everett, G. Tarle, August E. Evrard, Ricardo L. C. Ogando, Julian A. Mayers, J. De Vicente, Ben Hoyle, Daniel Thomas, Felipe Menanteau, Robert G. Mann, M. A. G. Maia, A. von der Linden, G. Morris, Risa H. Wechsler, E. Suchyta, Matt Hilton, S. Serrano, M. Carrasco Kind, C. Vergara Cervantes, Marcos Lima, I. Sevilla-Noarbe, Enrique Gaztanaga, N. Kuropatkin, M. Splettstoesser, Adam Mantz, L. N. da Costa, Joshua A. Frieman, Douglas L. Tucker, Kyler Kuehn, Paul Giles, A. K. Romer, Santiago Avila, Keith Bechtol, F. J. Castander, Pedro T. P. Viana, 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, Zhang, Y., Jeltema, T., Hollowood, D. L., Everett, S., Rozo, E., Farahi, A., Bermeo, A., Bhargava, S., Giles, P., Romer, A. K., Wilkinson, R., Rykoff, E. S., Mantz, A., Diehl, H. T., Evrard, A. E., Stern, C., Gruen, D., von der Linden, A., Splettstoesser, M., Chen, X., Costanzi, M., Allen, S., Collins, C., Hilton, M., Klein, M., Mann, R. G., Manolopoulou, M., Morris, G., Mayers, J., Sahlen, M., Stott, J., Vergara Cervantes, C., Viana, P. T. P., Wechsler, R. H., Allam, S., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Honscheid, K., Hoyle, B., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miller, C. J., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schindler, R., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Wester, W., and Des, Collaboration
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: general, dark energy, X-rays: galaxies: clusters, FOS: Physical sciences, Library science, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, media_common.cataloged_instance, clusters: general [galaxies], European union, Astronomy observatory, 010303 astronomy & astrophysics, media_common, QB, Physics, 010308 nuclear & particles physics, European research, GALÁXIAS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Research council, Astrophysics of Galaxies (astro-ph.GA), Fundamental physics, Christian ministry, galaxies: clusters [X-rays], National laboratory, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The center determination of a galaxy cluster from an optical cluster finding algorithm can be offset from theoretical prescriptions or $N$-body definitions of its host halo center. These offsets impact the recovered cluster statistics, affecting both richness measurements and the weak lensing shear profile around the clusters. This paper models the centering performance of the \RM~cluster finding algorithm using archival X-ray observations of \RM-selected clusters. Assuming the X-ray emission peaks as the fiducial halo centers, and through analyzing their offsets to the \RM~centers, we find that $\sim 75\pm 8 \%$ of the \RM~clusters are well centered and the mis-centered offset follows a Gamma distribution in normalized, projected distance. These mis-centering offsets cause a systematic underestimation of cluster richness relative to the well-centered clusters, for which we propose a descriptive model. Our results enable the DES Y1 cluster cosmology analysis by characterizing the necessary corrections to both the weak lensing and richness abundance functions of the DES Y1 redMaPPer cluster catalog., Code used in this analysis is available from https://github.com/yyzhang/center_modeling_y1
Published: 2019

35. 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

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

Author: Peter Doel, Elisabeth Krause, David J. James, Alistair R. Walker, Pablo Fosalba, H. T. Diehl, Douglas L. Tucker, J. Carretero, Jochen Weller, Pedro T. P. Viana, Kyler Kuehn, E. J. Sanchez, Paul Giles, I. Sevilla-Noarbe, Eli S. Rykoff, David Brooks, M. E. C. Swanson, N. Kuropatkin, Shantanu Desai, J. P. Dietrich, Ramon Miquel, Adam Mantz, L. N. da Costa, Mathew Smith, M. Carrasco Kind, A. Bermeo, C. Vergara Cervantes, Daniel Thomas, Marcos Lima, E. Buckley-Geer, Xi Chen, V. Scarpine, R. L. C. Ogando, Tesla E. Jeltema, Sunayana Bhargava, Michael Schubnell, Joshua A. Frieman, G. Gutierrez, Robert G. Mann, Jennifer L. Marshall, J. Gschwend, K. Honscheid, Enrique Gaztanaga, M. Costanzi, Yanxi Zhang, Julian A. Mayers, A. K. Romer, August E. Evrard, Arya Farahi, Flavia Sobreira, S. Serrano, Felipe Menanteau, B. Flaugher, John P. Stott, Gregory Tarle, R. D. Wilkinson, A. Carnero Rosell, S. Everett, P. Rooney, D. L. Burke, Juan Garcia-Bellido, Martin Sahlén, Chris A. Collins, Eduardo Rozo, J. Annis, Robert A. Gruendl, Vinu Vikram, J. De Vicente, E. Suchyta, Matt Hilton, Santiago Avila, Devon L. Hollowood, Andrew R. Liddle, Francisco J. Castander, A. A. Plazas, Daniel Gruen, D. W. Gerdes, M. A. G. Maia, Peter Melchior, Farahi, A., Chen, X., Evrard, A. E., Hollowood, D. L., Wilkinson, R., Bhargava, S., Giles, P., Romer, A. K., Jeltema, T., Hilton, M., Bermeo, A., Mayers, J., Vergara Cervantes, C., Rozo, E., Rykoff, E. S., Collins, C., Costanzi, M., Everett, S., Liddle, A. R., Mann, R. G., Mantz, A., Rooney, P., Sahlen, M., Stott, J., Viana, P. T. P., Zhang, Y., Annis, J., Avila, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., da Costa, L. N., de Vicente, J., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D. J., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Ogando, R. L. C., Plazas, A. A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, 0103 physical sciences, 010306 general physics, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, Scaling, STFC, ComputingMilieux_MISCELLANEOUS, QC, Galaxy cluster, QB, Confidence region, Physics, clusters: general - X-rays: galaxies: clusters [Galaxies], RCUK, Astronomy and Astrophysics, Covariance, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Log-normal distribution, astro-ph.CO, Galaxies: clusters: general - X-rays: galaxies: clusters, galaxies: clusters [X-rays], Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using archival X-ray observations and a log-normal population model, we estimate constraints on the intrinsic scatter in halo mass at fixed optical richness for a galaxy cluster sample identified in Dark Energy Survey Year-One (DES-Y1) data with the redMaPPer algorithm. We examine the scaling behavior of X-ray temperatures, $T_X$, with optical richness, $\lambda_{RM}$, for clusters in the redshift range $0.2 50\%$ complete for clusters with $\lambda_{RM} > 130$. Regression analysis on the two samples produces consistent posterior scaling parameters, from which we derive a combined constraint on the residual scatter, $\sigma_{\ln Tx | \lambda} = 0.275 \pm 0.019$. Joined with constraints for $T_X$ scaling with halo mass from the Weighing the Giants program and richness--temperature covariance estimates from the LoCuSS sample, we derive the richness-conditioned scatter in mass, $\sigma_{\ln M | \lambda} = 0.30 \pm 0.04\, _{({\rm stat})} \pm 0.09\, _{({\rm sys})}$, at an optical richness of approximately 70. Uncertainties in external parameters, particularly the slope and variance of the $T_X$--mass relation and the covariance of $T_X$ and $\lambda_{RM}$ at fixed mass, dominate the systematic error. The $95\%$ confidence region from joint sample analysis is relatively broad, $\sigma_{\ln M | \lambda} \in [0.14, \, 0.55]$, or a factor ten in variance., Comment: 14 pages. Main results are Figure 3, 5, and 6, Table 2, and Equation 9. Submitted to MNRAS. Comments welcome
Published: 2019

37. Constraints on the Physical Properties of GW190814 through Simulations Based on DECam Follow-up Observations by the Dark Energy Survey

Author: G. Tarle, Alyssa Garcia, V. Scarpine, Samuel Hinton, Marcelle Soares-Santos, David J. Brooks, Z. Doctor, C. Lidman, Douglas L. Tucker, G. Gutierrez, N. Meza, B. Flaugher, Kyler Kuehn, A. Carnero Rosell, Alex Drlica-Wagner, D. L. Burke, Eric H. Neilsen, J. Carretero, U. Malik, Huanqing Chen, A. K. Vivas, C. Nicolaou, Tamara M. Davis, Jhon Yana Galarza, Enrique Gaztanaga, Michael Schubnell, M. Sako, David J. James, K. Honscheid, J. Gschwend, Antonella Palmese, D. L. Hollowood, S. Allam, Robert A. Gruendl, S. Serrano, Alfredo Zenteno, F. Paz-Chinchón, Richard Kessler, Sunayana Bhargava, Ryan J. Foley, Daniel Scolnic, Ken Herner, Marcos Lima, Andre Luiz Figueiredo, S. Desai, M. Smith, S. Avila, Jennifer L. Marshall, Peter Doel, T. F. Eifler, Edward R. Cook, Daniel Gruen, Daniel E. Holz, E. Suchyta, M. A. G. Maia, James Annis, Clecio R. Bom, H. T. Diehl, T. M. C. Abbott, Michel Aguena, R. E. Butler, M. Costanzi, Melissa Butner, J. P. Marriner, Josh Frieman, M. S. S. Gill, Mackenna L. Wood, M. Carrasco Kind, S. Everett, D. J. Brout, I. Sevilla-Noarbe, R. Cartier, E. J. Sanchez, D. W. Gerdes, C. J. Conselice, Huan Lin, Ben Farr, Ramon Miquel, N. Kuropatkin, C. E. Martínez-Vázquez, W. G. Hartley, L. N. da Costa, Brian Yanny, D. A. Finley, Nora Sherman, Sean D. Points, A. A. Plazas, J. De Vicente, Flavia Sobreira, M. March, M. Wiesner, Tristan Bachmann, R. L. C. Ogando, Juan Garcia-Bellido, E. Bertin, Andrew W. Mann, Ofer Lahav, Robert Morgan, A. Roodman, O. Rodriguez, Keith Bechtol, J. Quirola-Vásquez, 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), National Aeronautics and Space Administration (US), Kavli Institute for Particle Astrophysics and Cosmology, Department of Energy (US), Higher Education Funding Council for England, Ministerio de Ciencia y Tecnología (España), University of Illinois, University of Chicago, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), German Research Foundation, Ministerio de Economía y Competitividad (España), European Commission, University of California, University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (España), University of Edinburgh, University of Michigan, National Optical Astronomy Observatory (US), University of Nottingham, The Ohio State University, University of Pennsylvania, University of Sussex, Texas A&M University, Morgan, R., Soares-Santos, M., Annis, J., Herner, K., Garcia, A., Palmese, A., Drlica-Wagner, A., Kessler, R., Garcia-Bellido, J., Bachmann, T. G., Sherman, N., Allam, S., Bechtol, K., Bom, C. R., Brout, D., Butler, R. E., Butner, M., Cartier, R., Chen, H., Conselice, C., Cook, E., Davis, T. M., Doctor, Z., Farr, B., Figueiredo, A. L., Finley, D. A., Foley, R. J., Galarza, J. Y., Gill, M. S. S., Gruendl, R. A., Holz, D. E., Kuropatkin, N., Lidman, C., Lin, H., Malik, U., Mann, A. W., Marriner, J., Marshall, J. L., Martinez-Vazquez, C. E., Meza, N., Neilsen, E., Nicolaou, C., Olivares, F. E., Paz-Chinchon, F., Points, S., Quirola-Vasquez, J., Rodriguez, O., Sako, M., Scolnic, D., Smith, M., Sobreira, F., Tucker, D. L., Vivas, A. K., Wiesner, M., Wood, M. L., Yanny, B., Zenteno, A., Abbott, T. M. C., Aguena, M., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Costa, L. N. D., Costanzi, M., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., March, M., Miquel, R., Ogando, R. L. C., Plazas, A. A., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., and Tarle, G.
Subjects: Gravitational wave sources, Optical observation, Light curve classification, Astronomical simulations, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kilonova, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gravitational wave, Astronomy and Astrophysics, Light curve, Redshift, Galaxy, LIGO, Neutron star, 13. Climate action, Space and Planetary Science, Gravitational wave source, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Full author list: R. Morgan, M. Soares-Santos, J. Annis, K. Herner, A. Garcia, A. Palmese, A. Drlica-Wagner, R. Kessler, J. García-Bellido, T. G. Bachmann, N. Sherman, S. Allam, K. Bechtol, C. R. Bom, D. Brout, R. E. Butler, M. Butner, R. Cartier, H. Chen, C. Conselice, E. Cook, T. M. Davis, Z. Doctor, B. Farr, A. L. Figueiredo, D. A. Finley, R. J. Foley, J. Y. Galarza, M. S. S. Gill, R. A. Gruendl, D. E. Holz, N. Kuropatkin, C. Lidman, H. Lin, U. Malik, A. W. Mann, J. Marriner, J. L. Marshall, C. E. Martínez-Vázquez N. Meza, E. Neilsen, C. Nicolaou, F. Olivares E., F. Paz-Chinchón, S. Points, J. Quirola-Vásquez, O. Rodriguez, M. Sako, D. Scolnic, M. Smith, F. Sobreira, D. L. Tucker, A. K. Vivas, M. Wiesner, M. L. Wood, B. Yanny, A. Zenteno, T. M. C. Abbott, M. Aguena, S. Avila, E. Bertin, S. Bhargava, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, L. N. da Costa, M. Costanzi, J. De Vicente, S. Desai, H. T. Diehl, P. Doel, T. F. Eifler, S. Everett, B. Flaugher, J. Frieman, E. Gaztanaga, D. W. Gerdes, D. Gruen, J. Gschwend, G. Gutierrez, W. G. Hartley, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, M. Lima, M. A. G. Maia, M. March, R. Miquel, R. L. C. Ogando, A. A. Plazas, A. Roodman, E. Sanchez, V. Scarpine, M. Schubnell, S. Serrano, I. Sevilla-Noarbe, E. Suchyta, and G. Tarle, On 2019 August 14, the LIGO and Virgo Collaborations detected gravitational waves from a black hole and a 2.6 solar mass compact object, possibly the first neutron star-black hole merger. In search of an optical counterpart, the Dark Energy Survey (DES) obtained deep imaging of the entire 90% confidence level localization area with Blanco/DECam 0, 1, 2, 3, 6, and 16 nights after the merger. Objects with varying brightness were detected by the DES Pipeline, and we systematically reduced the candidate counterparts through catalog matching, light-curve properties, host-galaxy photometric redshifts, Southern Astrophysical Research spectroscopic follow-up observations, and machine-learning-based photometric classification. All candidates were rejected as counterparts to the merger. To quantify the sensitivity of our search, we applied our selection criteria to full light-curve simulations of supernovae and kilonovae as they would appear in the DECam observations. Because the source class of the merger was uncertain, we utilized an agnostic, three-component kilonova model based on tidally disrupted neutron star (NS) ejecta properties to quantify our detection efficiency of a counterpart if the merger included an NS. We find that, if a kilonova occurred during this merger, configurations where the ejected matter is greater than 0.07 solar masses, has lanthanide abundance less than 10-8.56, and has a velocity between 0.18c and 0.21c are disfavored at the 2σ level. Furthermore, we estimate that our background reduction methods are capable of associating gravitational wave signals with a detected electromagnetic counterpart at the 4σ level in 95% of future follow-up observations., R. Morgan thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant #1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. F. O.E. acknowledges support from the FONDECYT grant No. 1201223. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. 1744555. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. 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 AstroParticle 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. The UCSC team is supported in part by NASA grant NNG17PX03C, NSF grant AST-1815935, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, and by fellowships from the David and Lucile Packard Foundation to R.J.F. Based in part on observations at Cerro Tololo InterAmerican Observatory at NSFʼs 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. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, Inovação e Comunicações (MCTIC) da República Federativa do Brasil, the U.S. NSF’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007- 2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This paper has gone through internal review by the DES collaboration. This manuscript has been authored by the Fermi Research Alliance, LLC under Contract No. DE-AC02- 07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.
Published: 2020

38. The XMM Cluster Survey: joint modelling of the Lx − T scaling relation for clusters and groups of galaxies

Author: Viana, Pedro T P, Manolopoulou, Maria, Vergara-Cervantes, Carlos, A Kathy Romer, Sunayana Bhargava, Giles, Paul, Bermeo-Hernandez, Alberto, Collins, Chris A, Hilton, Matt, Hoyle, Ben, Liddle, Andrew R, Mann, Robert G, Mayers, Julian A, Miller, Christopher J, Nichol, Robert C, Rooney, Philip J, Sahlén, Martin, and Stott, John P
Published: 2018
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39. Dark Energy Survey Year 1 Results: Photometric Data Set for Cosmology

Author: F. J. Castander, Eric H. Neilsen, K. Eckert, R. D. Wilkinson, Michael Troxel, Ramon Miquel, Joseph J. Mohr, R. Kron, S. Everett, F. Paz-Chinchón, M. Rodriguez-Monroy, J. Carretero, Alex Drlica-Wagner, E. Bertin, J. Annis, Brian Yanny, Shantanu Desai, A. Palmese, V. Scarpine, G. Gutierrez, Daniel B. Thomas, M. Jarvis, Enrique Gaztanaga, Mathew Smith, I. Harrison, A. K. Romer, Peter Doel, R. Cawthon, Marcio A. G. Maia, C. Lidman, T. N. Varga, I. Sevilla-Noarbe, Boris Leistedt, Erin Sheldon, David Brooks, Michael Schubnell, Paul Martini, Peter Melchior, H. T. Diehl, N. Kuropatkin, Sunayana Bhargava, M. Costanzi, I. Ferrero, K. Honscheid, Huan Lin, L. N. da Costa, Jennifer L. Marshall, David J. James, D. Huterer, C. Pond, Yanxi Zhang, Pablo Fosalba, M. Carrasco Kind, S. Avila, Risa H. Wechsler, A. Amon, Ricardo L. C. Ogando, K. M. Stringer, Tenglin Li, S. L. Bridle, D. Brout, B. Flaugher, M. Crocce, Chihway Chang, G. Tarle, Ami Choi, Ben Hoyle, A. Alarcon, E. Morganson, A. A. Plazas, D. L. Hollowood, W. C. Wester, D. L. Burke, J. Allyn Smith, J. Gschwend, C. Conselice, Gary Bernstein, E. Suchyta, August E. Evrard, J. P. Dietrich, Felipe Menanteau, Keith Bechtol, Juan Garcia-Bellido, Jochen Weller, Douglas L. Tucker, Marcos Lima, Kyler Kuehn, W. G. Hartley, Maria E. S. Pereira, Eli S. Rykoff, S. Allam, Robert A. Gruendl, T. M. C. Abbott, Tesla E. Jeltema, T. M. Davis, Chun-Hao To, E. J. Sanchez, S. R. Hinton, E. M. Huff, A. Carnero Rosell, A. Pieres, M. D. Johnson, Ofer Lahav, M. Aguena, Daniel Gruen, Robert Morgan, A. Roodman, Tommaso Giannantonio, D. W. Gerdes, A. Benoit-Lévy, S. Serrano, Richard Kessler, Matthew R. Becker, J. De Vicente, 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 ), Banerji, Manda [0000-0002-0639-5141], Giannantonio, Tommaso [0000-0002-9865-0436], McMahon, Richard [0000-0001-8447-8869], and Apollo - University of Cambridge Repository
Subjects: Photometric [techniques], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, techniques: image processing, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Cosmology, Footprint, techniques: photometric, surveys, Observational cosmology, 0201 Astronomical and Space Sciences, 0103 physical sciences, Observations [cosmology], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, QB, 0306 Physical Chemistry (incl. Structural), Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, RCUK, Astronomy, Astronomy and Astrophysics, Galaxy, Data set, Space and Planetary Science, cosmology: observations, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, astro-ph.CO, Dark energy, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Quality information, Data release, Image processing [techniques], catalogs, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract: We describe the creation, content, and validation of the Dark Energy Survey (DES) internal year-one cosmology data set, Y1A1 GOLD, in support of upcoming cosmological analyses. The Y1A1 GOLD data set is assembled from multiple epochs of DES imaging and consists of calibrated photometric zero-points, object catalogs, and ancillary data products—e.g., maps of survey depth and observing conditions, star–galaxy classification, and photometric redshift estimates—that are necessary for accurate cosmological analyses. The Y1A1 GOLD wide-area object catalog consists of $\sim 137$ million objects detected in co-added images covering $\sim 1800\,{\deg }^{2}$ in the DES grizY filters. The 10σ limiting magnitude for galaxies is $g=23.4$, $r=23.2$, $i=22.5$, $z=21.8$, and $Y=20.1$. Photometric calibration of Y1A1 GOLD was performed by combining nightly zero-point solutions with stellar locus regression, and the absolute calibration accuracy is better than 2% over the survey area. DES Y1A1 GOLD is the largest photometric data set at the achieved depth to date, enabling precise measurements of cosmic acceleration at z lesssim 1., Multiple funders including STFC listed on paper.
Published: 2018

40. Dark Energy Survey Year 1 Results: Weak Lensing Mass Calibration of redMaPPer Galaxy Clusters

Author: Eli S. Rykoff, Thomas McClintock, I. Sevilla-Noarbe, David J. James, Stella Seitz, Michael Troxel, A. Carnero Rosell, E. Suchyta, August E. Evrard, Pablo Fosalba, T. N. Varga, Joe Zuntz, Risa H. Wechsler, Adam Mantz, L. N. da Costa, Tesla E. Jeltema, A. Roodman, Tommaso Giannantonio, J. Carretero, Melanie Simet, Alex Drlica-Wagner, A. A. Plazas, C. B. D'Andrea, Scarpine, Markus Rau, P Li, Felipe Menanteau, Elisabeth Krause, Antonella Palmese, J. Annis, Steven W. Allen, G. Pollina, David J. Brooks, Juan Garcia-Bellido, J. P. Dietrich, Vikram, A. von der Linden, Matthew R. Becker, Flavia Sobreira, Eduardo Rozo, R. C. Smith, Filipe B. Abdalla, Tenglin Li, Sarah Bridle, D. L. Hollowood, Santiago Avila, Ramon Miquel, Joshua A. Frieman, G. Gutierrez, J. DeRose, Carlos E. Cunha, A. Bermeo, Mathew Smith, Nico Hamaus, K. Honscheid, Sunayana Bhargava, Douglas L. Tucker, Kyler Kuehn, Martin Crocce, Donnacha Kirk, Alistair R. Walker, Jochen Weller, F. J. Castander, W. G. Hartley, D. L. Burke, Joseph J. Mohr, Marcelle Soares-Santos, Jennifer L. Marshall, Peter Melchior, T. M. C. Abbott, A. K. Romer, Rafe Schindler, M. March, M. E. C. Swanson, T. Shin, Ofer Lahav, Daniel Gruen, E. J. Sanchez, S. Everett, S. Allam, Robert A. Gruendl, Ricardo L. C. Ogando, C. Vergara Cervantes, Marcos Lima, Ben Hoyle, D. W. Gerdes, G Morris, J. De Vicente, Brian Nord, C. Davis, Peter Doel, Yanxi Zhang, H. T. Diehl, Arya Farahi, Niall MacCrann, Erin Sheldon, G. Tarle, M. Costanzi, H. Israel, M. Carrasco Kind, Enrique Gaztanaga, B. Flaugher, Mcclintock, T., Varga, T. N., Gruen, D., Rozo, E., Rykoff, E. S., Shin, T., Melchior, P., Derose, J., Seitz, S., Dietrich, J. P., Sheldon, E., Zhang, Y., von der Linden, A., Jeltema, T., Mantz, A. B., Romer, A. K., Allen, S., Becker, M. R., Bermeo, A., Bhargava, S., Costanzi, M., Everett, S., Farahi, A., Hamaus, N., Hartley, W. G., Hollowood, D. L., Hoyle, B., Israel, H., Li, P., Maccrann, N., Morris, G., Palmese, A., Plazas, A. A., Pollina, G., Rau, M. M., Simet, M., Soares-Santos, M., Troxel, M. A., Vergara Cervantes, C., Wechsler, R. H., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Avila, S., Bridle, S. L., Brooks, D., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., De Vicente, J., Diehl, H. T., Doel, P., Drlica-Wagner, A., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gutierrez, G., Honscheid, K., James, D. J., Kirk, D., Krause, E., Kuehn, K., Lahav, O., T. S., Li, Lima, M., March, M., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Nord, B., Ogando, R. L. C., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Vikram, V., Walker, A. R., and Weller, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), ST/N504452/1, FOS: Physical sciences, observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, Cosmology, Gravitational lensing: weak, ST/P000252/1, 0103 physical sciences, observations [Cosmology], 010303 astronomy & astrophysics, Scaling, Weak gravitational lensing, Galaxy cluster, Astrophysics::Galaxy Astrophysics, STFC, QC, Photometric redshift, Physics, 010308 nuclear & particles physics, Cosmology: observations, RCUK, Astronomy and Astrophysics, Galaxy, Redshift, Space and Planetary Science, Dark energy, astro-ph.CO, Galaxies: clusters: general, weak [Gravitational lensing], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We constrain the mass--richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing. We split clusters into $4\times3$ bins of richness $\lambda$ and redshift $z$ for $\lambda\geq20$ and $0.2 \leq z \leq 0.65$ and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as $\langle M_{\rm 200m}|\lambda,z\rangle = M_0 (\lambda/40)^F ((1+z)/1.35)^G$, we constrain the normalization of the scaling relation at the 5.0 per cent level as $M_0 = [3.081 \pm 0.075 ({\rm stat}) \pm 0.133 ({\rm sys})] \cdot 10^{14}\ {\rm M}_\odot$ at $\lambda=40$ and $z=0.35$. The richness scaling index is constrained to be $F=1.356 \pm 0.051\ ({\rm stat})\pm 0.008\ ({\rm sys})$ and the redshift scaling index $G=-0.30\pm 0.30\ ({\rm stat})\pm 0.06\ ({\rm sys})$. These are the tightest measurements of the normalization and richness scaling index made to date. We use a semi-analytic covariance matrix to characterize the statistical errors in the recovered weak lensing profiles. Our analysis accounts for the following sources of systematic error: shear and photometric redshift errors, cluster miscentering, cluster member dilution of the source sample, systematic uncertainties in the modeling of the halo--mass correlation function, halo triaxiality, and projection effects. We discuss prospects for reducing this systematic error budget, which dominates the uncertainty on $M_0$. Our result is in excellent agreement with, but has significantly smaller uncertainties than, previous measurements in the literature, and augurs well for the power of the DES cluster survey as a tool for precision cosmology and upcoming galaxy surveys such as LSST, Euclid and WFIRST., Comment: 28 pages, 15 figures; matches MNRAS referee response version

41. Stellar mass as a galaxy cluster mass proxy: application to the Dark Energy Survey redMaPPer clusters

Author: Julian A. Mayers, J. De Vicente, Flavia Sobreira, John P. Stott, W. G. Hartley, J. Carretero, N. Kuropatkin, R. D. Wilkinson, M. Carrasco Kind, Joshua A. Frieman, J. P. Dietrich, S. Desai, David J. Brooks, B. Welch, J. Burgad, A. K. Romer, Marcelle Soares-Santos, Robert G. Mann, J. DeRose, David J. James, Pablo Fosalba, V. Scarpine, Andrew R. Liddle, G. Gutierrez, Salcedo Romero de Ávila, F. J. Castander, Pedro T. P. Viana, E. Suchyta, A. A. Plazas, C. Vergara Cervantes, I. Sevilla-Noarbe, Marcos Lima, August E. Evrard, Antonella Palmese, T. McClintock, T. N. Varga, P. Rooney, M. A. G. Maia, L. N. da Costa, Matt Hilton, E. J. Sanchez, B. Flaugher, Daniel Thomas, E. Buckley-Geer, Douglas L. Tucker, Kyler Kuehn, Paul Giles, Martin Sahlén, Chris A. Collins, Daniel Gruen, Michael Schubnell, Vinu Vikram, M. da Silva Pereira, Tesla E. Jeltema, D. L. Hollowood, S. Serrano, Juan Garcia-Bellido, D. W. Gerdes, Eduardo Rozo, Ramon Miquel, Han Lin, A. Bermeo, Peter Doel, D. L. Burke, H. T. Diehl, R. L. C. Ogando, Robert A. Gruendl, J. Gschwend, Elisabeth Krause, Ofer Lahav, Yanxi Zhang, Arya Farahi, A. Roodman, M. E. C. Swanson, J. Annis, Felipe Menanteau, Boris Leistedt, Sunayana Bhargava, Gregory Tarle, Jennifer L. Marshall, K. Honscheid, Risa H. Wechsler, Eli S. Rykoff, A. Carnero Rosell, A. R. Walker, 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), Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, haloesSurveys [Galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: general [Galaxies], 01 natural sciences, surveys, Astronomi, astrofysik och kosmologi, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics and Cosmology, Galaxies: haloesSurveys, observations [Cosmology], 010303 astronomy & astrophysics, Scaling, Astrophysics::Galaxy Astrophysics, Galaxy cluster, QC, QB, Physics, 010308 nuclear & particles physics, Cosmology: observations, Galaxies: evolution, Astronomy and Astrophysics, Observable, evolution [Galaxies], Redshift, haloes [galaxies], Space and Planetary Science, Dark energy, Galaxies: clusters: general, Astrophysics::Earth and Planetary Astrophysics, Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We introduce a galaxy cluster mass observable, μ*, based on the stellar masses of cluster members, and we present results for the Dark Energy Survey (DES) Year 1 (Y1) observations. Stellar masses are computed using a Bayesian model averaging method, and are validated for DES data using simulations and COSMOS data. We show that μ* works as a promising mass proxy by comparing our predictions to X-ray measurements. We measure the X-ray temperature–μ* relation for a total of 129 clusters matched between the wide-field DES Y1 redMaPPer catalogue and Chandra and XMM archival observations, spanning the redshift range 0.1 < z < 0.7. For a scaling relation that is linear in logarithmic space, we find a slope of α = 0.488 ± 0.043 and a scatter in the X-ray temperature at fixed μ* of σ|μ* = 0.266 for the joint sample. By using the halo mass scaling relations of the X-ray temperature from the Weighing the Giants program, we further derive the μ*-conditioned scatter in mass, finding σM|μ* = 0.26. These results are competitive with well-established cluster mass proxies used for cosmological analyses, showing that μ* can be used as a reliable and physically motivated mass proxy to derive cosmological constraints., AP acknowledges the UCL PhD studentship and the URA Visiting scholar award. AF is supported by a McWilliams Postdoctoral Fellowship. OL acknowledges support from a European Research Council Advanced Grant FP7/291329. SB acknowledges support from the UK Science and Technology Facilities Council via Research Training Grant ST/N504452/1. TOPCAT (Taylor 2005) has been extensively used in this work. 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 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. 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.

42. The Dark Energy Survey Data Release 2

Author: Antonella Palmese, Jack Elvin-Poole, M. Rodriguez-Monroy, David Herrera, Peter Melchior, M. Fitzpatrick, Ricardo L. C. Ogando, Alexandra Amon, J. DeRose, E. Suchyta, August E. Evrard, Pier-Emmanuel Tremblay, Jochen Weller, Don Petravick, M. Smith, H. T. Diehl, David Bacon, M. E. C. Swanson, A. R. Walker, Daniel Gruen, Alex Drlica-Wagner, Douglas L. Tucker, Kyler Kuehn, Josh Frieman, K. A. G. Olsen, Felipe Menanteau, Dragan Huterer, F. J. Castander, J. Allyn Smith, M. D. Johnson, Christopher J. Conselice, S. Everett, M. S. S. Gill, Niall MacCrann, C. Lidman, Keith Bechtol, J. Annis, W. C. Wester, J. Myles, Sunayana Bhargava, C. Adean, W. G. Hartley, D. W. Gerdes, Ramon Miquel, V. Scarpine, David L. Nidever, B. Flaugher, M. Banerji, Huan Lin, Samuel Hinton, David J. James, Jennifer L. Marshall, T. M. C. Abbott, G. Gutierrez, Enrique Gaztanaga, T. A. Manning, J. P. Dietrich, Juan Garcia-Bellido, G. Tarle, A. Choi, Pablo Fosalba, Daniel Thomas, Eric H. Neilsen, J. Carretero, Tamara M. Davis, J. De Vicente, A. Roodman, Tommaso Giannantonio, F. N. Freitas, Chun-Hao To, S. Juneau, G. Vila-Verde, K. Honscheid, Martin Crocce, E. Bertin, R. D. Wilkinson, C. Singulani, A. A. Plazas, D. L. Burke, E. J. Sanchez, Matthew R. Becker, David J. Brooks, M. A. G. Maia, C. Pond, J. Gschwend, A. K. Romer, T. N. Varga, Eli S. Rykoff, Gary Bernstein, D. J. Turner, Richard G. Kron, A. Jacques, Michael Troxel, Paul Martini, Douglas N. Friedel, M. de Freitas, B. A. Weaver, L. Huang, M. Sako, Adriano Pieres, I. Sevilla-Noarbe, Brian Yanny, A. Carnero Rosell, M. Soares-Santos, N. Kuropatkin, D. L. Hollowood, S. Serrano, S. Allam, Robert A. Gruendl, M. Carrasco Kind, K. D. Eckert, V. Correia, F. Paz-Chinchón, Tesla E. Jeltema, L. N. da Costa, M. March, Basilio X. Santiago, R. Nikutta, S. Kent, Michel Aguena, I. Ferrero, R. Cawthon, Yanxi Zhang, M. Costanzi, A. Scott, J. D. Maloney, Ofer Lahav, Monika Adamów, Risa H. Wechsler, Agnès Ferté, Tenglin Li, Sarah Bridle, Santiago Avila, L. Gelman, Robert Morgan, Chihway Chang, S. Desai, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), 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), Linea Science Server, and DES
Subjects: Astronomical Objects, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Aperture, Near infrared astronomy, FOS: Physical sciences, Astrophysics, Surveys, 7. Clean energy, 01 natural sciences, Standard deviation, Optical astronomy, law.invention, Telescope, Extragalactic astronomy, law, Observatory, Dark energy, 0103 physical sciences, ComputingMilieux_COMPUTERSANDEDUCATION, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Redshift surveys, Physics, 05 social sciences, 050301 education, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Cosmology, Data set, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Instrumentation and Methods for Astrophysics, 0503 education, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Abbott, T. M. C., et al. (Linea Science Server), We present the second public data release of the Dark Energy Survey, DES DR2, based on optical/near-infrared imaging by the Dark Energy Camera mounted on the 4 m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. DES DR2 consists of reduced single-epoch and coadded images, a source catalog derived from coadded images, and associated data products assembled from 6 yr of DES science operations. This release includes data from the DES wide-area survey covering ∼5000 deg2 of the southern Galactic cap in five broad photometric bands, grizY. DES DR2 has a median delivered point-spread function FWHM of g = 1.11″, r = 0.95″, i = 0.88″, z = 0.83″, and Y = 0.″90, photometric uniformity with a standard deviation of < 3 mmag with respect to Gaia DR2 G band, a photometric accuracy of ∼11 mmag, and a median internal astrometric precision of ∼27 mas. The median coadded catalog depth for a 1.″95 diameter aperture at signal-to-noise ratio = 10 is g = 24.7, r = 24.4, i = 23.8, z = 23.1, and Y = 21.7 mag. DES DR2 includes ∼691 million distinct astronomical objects detected in 10,169 coadded image tiles of size 0.534 deg2 produced from 76,217 single-epoch images. After a basic quality selection, benchmark galaxy and stellar samples contain 543 million and 145 million objects, respectively. These data are accessible through several interfaces, including interactive image visualization tools, web-based query clients, image cutout servers, and Jupyter notebooks. DES DR2 constitutes the largest photometric data set to date at the achieved depth and photometric precision., 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) do e-Universo (CNPq grant 465376/2014-2).
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