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T.n. Varga - One of the best experts on this subject based on the ideXlab platform.
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Synthetic Galaxy Clusters and Observations Based on Dark Energy Survey Year 3 Data
2021Co-Authors: T.n. Varga, D. Gruen, S. Seitz, N. Maccrann, E. Sheldon, W.g. Hartley, A. Amon, A. Choi, A. Palmese, Y. ZhangAbstract: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 $\lambda\in[30;\,45)$, $\lambda\in[45;\,60)$ and three bins in Cluster redshift ($z\in[0.3;\,0.35)$, $z\in[0.45;\,0.5)$ and $z\in[0.6;\,0.65)$. 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 catalogs 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.
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μ⋆ masses: weak-lensing calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using stellar masses
Mon.Not.Roy.Astron.Soc., 2020Co-Authors: M.e.s. Pereira, A. Farahi, T.n. Varga, A. Palmese, T. Mcclintock, M. Soares-santos, J. Burgad, J. Annis, H. Lin, A. ChoiAbstract:We present the weak-lensing mass calibration of the stellar-mass-based μ_⋆ 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 μ_⋆ at high redshifts, z > 0.33. In a blinded analysis, we use ∼6000 Clusters split into 12 subsets spanning the ranges 0.1 ≤ z < 0.65 and μ_⋆ up to |${\sim} 5.5 \times 10^{13} \, \mathrm{M}_{\odot }$|, and infer the average masses of these subsets through modelling of their stacked weak-lensing signal. In our model, we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, Cluster-Member contamination of the source sample, deviations from the Navarro–Frenk–White halo profile, halo triaxiality, and projection effects. We use the inferred masses to estimate the joint mass–μ_⋆–z scaling relation given by |$\langle M_{200c} | \mu _{\star },z \rangle = M_0 (\mu _{\star }/5.16\times 10^{12} \, \mathrm{M_{\odot }})^{F_{\mu _{\star }}} ((1+z)/1.35)^{G_z}$|. We find |$M_0= (1.14 \pm 0.07) \times 10^{14} \, \mathrm{M_{\odot }}$| with |$F_{\mu _{\star }}= 0.76 \pm 0.06$| and = −1.14 ± 0.37. We discuss the use of μ_⋆ as a complementary mass proxy to the well-studied richness λ for: (i) exploring the regimes of low z, λ < 20 and high λ, z ∼ 1; and (ii) testing systematics such as projection effects for applications in Cluster cosmology.
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dark energy survey year 1 results validation of weak lensing Cluster Member contamination estimates from p z decomposition
Monthly Notices of the Royal Astronomical Society, 2019Co-Authors: D. Gruen, T.n. Varga, S. Seitz, J. Derose, T. Mcclintock, E. Rozo, M. Costanzi, B. HoyleAbstract:Deutsche Forschungsgemeinschaft (DFG)German Research Foundation (DFG) [SFB-Transregio 33]; DFG Cluster of excellence 'Origin and Structure of the Universe'German Research Foundation (DFG); U.S. Department of EnergyUnited States Department of Energy (DOE); DOEUnited States Department of Energy (DOE); Sloan FoundationAlfred P. Sloan Foundation [DE-SC0015975]; Cottrell Scholar program of the Research Corporation for Science Advancement [FG-2016-6443]; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA); Stanford UniversityStanford University; Office of Science of the U.S. Department of EnergyUnited States Department of Energy (DOE) [DE-AC02-05CH11231]; U.S. National Science FoundationNational Science Foundation (NSF); Ministry of Science and Education of SpainMinistry of Education and Science, Spain; Science and Technology Facilities Council of the United KingdomScience & Technology Facilities Council (STFC); Higher Education Funding Council for EnglandHigher Education Funding Council for England; Center for Cosmology and Astro-Particle Physics at the Ohio State UniversityOhio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e ProjetosCiencia Tecnologia e Inovacao (FINEP); Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e TecnologicoNational Council for Scientific and Technological Development (CNPq); Deutsche ForschungsgemeinschaftGerman Research Foundation (DFG); University of California at Santa Cruz; University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) ZurichETH Zurich; Ludwig-Maximilians Universitat Munchen; University of Portsmouth; OzDES Membership Consortium; National Science FoundationNational Science Foundation (NSF) [AST-1138766, AST-1536171]; MINECO; ERDFEuropean Union (EU) [AYA201571825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, MDM-2015-0509]; European Union - CERCA program of the Generalitat de Catalunya; European Research Council under the European UnionEuropean Research Council (ERC) [240672, 291329, 306478]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)Australian Research Council; Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq)National Council for Scientific and Technological Development (CNPq) [CE110001020]; U.S. Department of Energy, Office of Science, Office of High Energy PhysicsUnited States Department of Energy (DOE) [465376/2014-2, DE-AC02-07CH11359]
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Dark Energy Survey Year 1 results: Validation of weak lensing Cluster Member contamination estimates from P(z) decomposition
Mon.Not.Roy.Astron.Soc., 2019Co-Authors: T.n. Varga, D. Gruen, S. Seitz, N. Maccrann, J. Derose, T. Mcclintock, E. Rozo, M. Costanzi, B. Hoyle, A.a. PlazasAbstract:Weak lensing source galaxy catalogues used in estimating the masses of galaxy Clusters can be heavily contaminated by Cluster Members, prohibiting accurate mass calibration. In this study, we test the performance of an estimator for the extent of Cluster Member contamination based on decomposing the photometric redshift P(z) of source galaxies into contaminating and background components. We perform a full scale mock analysis on a simulated sky survey approximately mirroring the observational properties of the Dark Energy Survey Year One observations (DES Y1), and find excellent agreement between the true number profile of contaminating Cluster Member galaxies in the simulation and the estimated one. We further apply the method to estimate the Cluster Member contamination for the DES Y1 redMaPPer Cluster mass calibration analysis, and compare the results to an alternative approach based on the angular correlation of weak lensing source galaxies. We find indications that the correlation based estimates are biased by the selection of the weak lensing sources in the Cluster vicinity, which does not strongly impact the P(z) decomposition method. Collectively, these benchmarks demonstrate the strength of the P(z) decomposition method in alleviating Membership contamination and enabling highly accurate Cluster weak lensing studies without broad exclusion of source galaxies, thereby improving the total constraining power of Cluster mass calibration via weak lensing.
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dark energy survey year 1 results weak lensing mass calibration of redmapper galaxy Clusters
Monthly Notices of the Royal Astronomical Society, 2019Co-Authors: T. Mcclintock, D. Gruen, T.n. Varga, E. Rozo, E S Rykoff, T Shin, P MelchiorAbstract: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 4×3 bins of richness λ and redshift z for λ≥20 and 0.2≤z≤0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as ⟨M 200m |λ,z⟩=M 0 (λ/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±0.075(stat)±0.133(sys)]⋅10 14 M ⊙ at λ=40 and z=0.35 . The richness scaling index is constrained to be F=1.356±0.051 (stat)±0.008 (sys) and the redshift scaling index G=−0.30±0.30 (stat)±0.06 (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.
Patrick Côté - One of the best experts on this subject based on the ideXlab platform.
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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).III. Star formation in the stripped gas of NGC 4254
Astronomy and Astrophysics - A&A, 2018Co-Authors: Alessandro Boselli, Matteo Fossati, Samuel Boissier, Médéric Boquien, Jean-charles Cuillandre, Giulia Consolandi, Veronique Buat, D. Burgarella, L. Cortese, Patrick CôtéAbstract:During pilot observations of the Virgo Environmental Survey Tracing Galaxy Evolution (VESTIGE), a blind narrow-band Halpha+[NII] imaging survey of the Virgo Cluster carried out with MegaCam at the CFHT, we have observed the spiral galaxy NGC 4254 (M99). Deep Halpha+[NII] narrow-band and GALEX UV images revealed the presence of 60 compact (70-500 pc radius) star forming regions up to ~ 20 kpc outside the optical disc of the galaxy. These regions are located along a tail of HI gas stripped from the disc of the galaxy after a rapid gravitational encounter with another Virgo Cluster Member that simulations indicate occurred 280-750 Myr ago. We have combined the VESTIGE data with multifrequency data from the UV to the far-infrared to characterise the stellar populations of these regions and study the star formation process in an extreme environment such as the tails of stripped gas embedded in the hot intraCluster medium. The colour, spectral energy distribution (SED), and linear size consistently indicate that these regions are coeval and have been formed after a single burst of star formation that occurred ~< 100 Myr ago. These regions might become free floating objects within the Cluster potential well, and be the local analogues of compact sources produced after the interaction of gas-rich systems that occurred during the early formation of Clusters.
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A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)
Astronomy and Astrophysics - A&A, 2018Co-Authors: Alessandro Boselli, Matteo Fossati, Samuel Boissier, Médéric Boquien, Giulia Consolandi, Veronique Buat, D. Burgarella, L. Cortese, J.-c. Cuillandre, Patrick CôtéAbstract:During pilot observations of the Virgo Environmental Survey Tracing Galaxy Evolution (VESTIGE), a blind narrow-band Hα + [NII] imaging survey of the Virgo Cluster carried out with MegaCam at the CFHT, we have observed the spiral galaxy NGC 4254 (M99). Deep Hα + [NII] narrow-band and GALEX UV images reveal the presence of 60 compact (70–500 pc radius) star-forming regions up to ≃20 kpc outside the optical disc of the galaxy. These regions are located along a tail of HI gas stripped from the disc of the galaxy after a rapid gravitational encounter with another Virgo Cluster Member that simulations indicate occurred 280–750 Myr ago. We have combined the VESTIGE data with multifrequency data from the UV to the far-infrared to characterise the stellar populations of these regions and study the star formation process in an extreme environment such as the tails of stripped gas embedded in the hot intraCluster medium. The colour, spectral energy distribution (SED), and linear size consistently indicate that these regions are coeval and have been formed after a single burst of star formation that occurred ≲100 Myr ago. These regions might become free floating objects within the Cluster potential well, and be the local analogues of compact sources produced after the interaction of gas-rich systems that occurred during the early formation of Clusters.
D. Gruen - One of the best experts on this subject based on the ideXlab platform.
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Synthetic Galaxy Clusters and Observations Based on Dark Energy Survey Year 3 Data
2021Co-Authors: T.n. Varga, D. Gruen, S. Seitz, N. Maccrann, E. Sheldon, W.g. Hartley, A. Amon, A. Choi, A. Palmese, Y. ZhangAbstract: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 $\lambda\in[30;\,45)$, $\lambda\in[45;\,60)$ and three bins in Cluster redshift ($z\in[0.3;\,0.35)$, $z\in[0.45;\,0.5)$ and $z\in[0.6;\,0.65)$. 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 catalogs 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.
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dark energy survey year 1 results validation of weak lensing Cluster Member contamination estimates from p z decomposition
Monthly Notices of the Royal Astronomical Society, 2019Co-Authors: D. Gruen, T.n. Varga, S. Seitz, J. Derose, T. Mcclintock, E. Rozo, M. Costanzi, B. HoyleAbstract:Deutsche Forschungsgemeinschaft (DFG)German Research Foundation (DFG) [SFB-Transregio 33]; DFG Cluster of excellence 'Origin and Structure of the Universe'German Research Foundation (DFG); U.S. Department of EnergyUnited States Department of Energy (DOE); DOEUnited States Department of Energy (DOE); Sloan FoundationAlfred P. Sloan Foundation [DE-SC0015975]; Cottrell Scholar program of the Research Corporation for Science Advancement [FG-2016-6443]; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA); Stanford UniversityStanford University; Office of Science of the U.S. Department of EnergyUnited States Department of Energy (DOE) [DE-AC02-05CH11231]; U.S. National Science FoundationNational Science Foundation (NSF); Ministry of Science and Education of SpainMinistry of Education and Science, Spain; Science and Technology Facilities Council of the United KingdomScience & Technology Facilities Council (STFC); Higher Education Funding Council for EnglandHigher Education Funding Council for England; Center for Cosmology and Astro-Particle Physics at the Ohio State UniversityOhio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e ProjetosCiencia Tecnologia e Inovacao (FINEP); Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e TecnologicoNational Council for Scientific and Technological Development (CNPq); Deutsche ForschungsgemeinschaftGerman Research Foundation (DFG); University of California at Santa Cruz; University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) ZurichETH Zurich; Ludwig-Maximilians Universitat Munchen; University of Portsmouth; OzDES Membership Consortium; National Science FoundationNational Science Foundation (NSF) [AST-1138766, AST-1536171]; MINECO; ERDFEuropean Union (EU) [AYA201571825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, MDM-2015-0509]; European Union - CERCA program of the Generalitat de Catalunya; European Research Council under the European UnionEuropean Research Council (ERC) [240672, 291329, 306478]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)Australian Research Council; Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq)National Council for Scientific and Technological Development (CNPq) [CE110001020]; U.S. Department of Energy, Office of Science, Office of High Energy PhysicsUnited States Department of Energy (DOE) [465376/2014-2, DE-AC02-07CH11359]
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Dark Energy Survey Year 1 results: Validation of weak lensing Cluster Member contamination estimates from P(z) decomposition
Mon.Not.Roy.Astron.Soc., 2019Co-Authors: T.n. Varga, D. Gruen, S. Seitz, N. Maccrann, J. Derose, T. Mcclintock, E. Rozo, M. Costanzi, B. Hoyle, A.a. PlazasAbstract:Weak lensing source galaxy catalogues used in estimating the masses of galaxy Clusters can be heavily contaminated by Cluster Members, prohibiting accurate mass calibration. In this study, we test the performance of an estimator for the extent of Cluster Member contamination based on decomposing the photometric redshift P(z) of source galaxies into contaminating and background components. We perform a full scale mock analysis on a simulated sky survey approximately mirroring the observational properties of the Dark Energy Survey Year One observations (DES Y1), and find excellent agreement between the true number profile of contaminating Cluster Member galaxies in the simulation and the estimated one. We further apply the method to estimate the Cluster Member contamination for the DES Y1 redMaPPer Cluster mass calibration analysis, and compare the results to an alternative approach based on the angular correlation of weak lensing source galaxies. We find indications that the correlation based estimates are biased by the selection of the weak lensing sources in the Cluster vicinity, which does not strongly impact the P(z) decomposition method. Collectively, these benchmarks demonstrate the strength of the P(z) decomposition method in alleviating Membership contamination and enabling highly accurate Cluster weak lensing studies without broad exclusion of source galaxies, thereby improving the total constraining power of Cluster mass calibration via weak lensing.
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dark energy survey year 1 results weak lensing mass calibration of redmapper galaxy Clusters
Monthly Notices of the Royal Astronomical Society, 2019Co-Authors: T. Mcclintock, D. Gruen, T.n. Varga, E. Rozo, E S Rykoff, T Shin, P MelchiorAbstract: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 4×3 bins of richness λ and redshift z for λ≥20 and 0.2≤z≤0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as ⟨M 200m |λ,z⟩=M 0 (λ/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±0.075(stat)±0.133(sys)]⋅10 14 M ⊙ at λ=40 and z=0.35 . The richness scaling index is constrained to be F=1.356±0.051 (stat)±0.008 (sys) and the redshift scaling index G=−0.30±0.30 (stat)±0.06 (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.
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Weak-lensing mass calibration of redMaPPer galaxy Clusters in Dark Energy Survey Science Verification data
Mon.Not.Roy.Astron.Soc., 2017Co-Authors: P Melchior, D. Gruen, T.n. Varga, E. Sheldon, T. Mcclintock, B A Benson, E. Rozo, A. Amara, M.r. Becker, A. BermeoAbstract:We use weak-lensing shear measurements to determine the mean mass of optically selected galaxy Clusters in Dark Energy Survey Science Verification data. In a blinded analysis, we split the sample of more than 8000 redMaPPer Clusters into 15 subsets, spanning ranges in the richness parameter 5 ≤ λ ≤ 180 and redshift 0.2 ≤ z ≤ 0.8, and fit the averaged mass density contrast profiles with a model that accounts for seven distinct sources of systematic uncertainty: shear measurement and photometric redshift errors; Cluster-Member contamination; miscentring; deviations from the NFW halo profile; halo triaxiality and line-of-sight projections. We combine the inferred Cluster masses to estimate the joint scaling relation between mass, richness and redshift, $${\cal M}(\lambda ,z) \propto M_0 \lambda ^{F} (1+z)^{G}$$. We find $$M_0 \equiv \langle M_{200\mathrm{m}}\,|\,\lambda =30,z=0.5 \rangle =[ 2.35 \pm 0.22\ \rm {(stat)} \pm 0.12\ \rm {(sys)} ] \times \ 10^{14}\ \mathrm{M}_{{\odot }}$$, with $$F = 1.12\,\pm \,0.20\ \rm {(stat)}\, \pm \, 0.06\ \rm {(sys)}$$ and $$G = 0.18\,\pm \, 0.75\ \rm {(stat)}\, \pm \, 0.24\ \rm {(sys)}$$. The amplitude of the mass–richness relation is in excellent agreement with the weak-lensing calibration of redMaPPer Clusters in SDSS by Simet et al. and with the Saro et al. calibration based on abundance matching of SPT-detected Clusters. Our results extend the redshift range over which the mass–richness relation of redMaPPer Clusters has been calibrated with weak lensing from z ≤ 0.3 to z ≤ 0.8. Calibration uncertainties of shear measurements and photometric redshift estimates dominate our systematic error budget and require substantial improvements for forthcoming studies.
Alexei V. Filippenko - One of the best experts on this subject based on the ideXlab platform.
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Two transitional type Ia supernovae located in the Fornax Cluster Member NGC 1404: SN 2007on and SN 2011iv
Astronomy & Astrophysics, 2018Co-Authors: Christa Gall, Maximilian Stritzinger, Chris Ashall, E. Baron, Christopher R. Burns, Peter Hoeflich, Eric Y. Hsiao, Paolo A. Mazzali, Mark M. Phillips, Alexei V. FilippenkoAbstract:We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax Cluster Member NGC 1404. The B-ban ...
T. Mcclintock - One of the best experts on this subject based on the ideXlab platform.
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μ⋆ masses: weak-lensing calibration of the Dark Energy Survey Year 1 redMaPPer Clusters using stellar masses
Mon.Not.Roy.Astron.Soc., 2020Co-Authors: M.e.s. Pereira, A. Farahi, T.n. Varga, A. Palmese, T. Mcclintock, M. Soares-santos, J. Burgad, J. Annis, H. Lin, A. ChoiAbstract:We present the weak-lensing mass calibration of the stellar-mass-based μ_⋆ 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 μ_⋆ at high redshifts, z > 0.33. In a blinded analysis, we use ∼6000 Clusters split into 12 subsets spanning the ranges 0.1 ≤ z < 0.65 and μ_⋆ up to |${\sim} 5.5 \times 10^{13} \, \mathrm{M}_{\odot }$|, and infer the average masses of these subsets through modelling of their stacked weak-lensing signal. In our model, we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, Cluster-Member contamination of the source sample, deviations from the Navarro–Frenk–White halo profile, halo triaxiality, and projection effects. We use the inferred masses to estimate the joint mass–μ_⋆–z scaling relation given by |$\langle M_{200c} | \mu _{\star },z \rangle = M_0 (\mu _{\star }/5.16\times 10^{12} \, \mathrm{M_{\odot }})^{F_{\mu _{\star }}} ((1+z)/1.35)^{G_z}$|. We find |$M_0= (1.14 \pm 0.07) \times 10^{14} \, \mathrm{M_{\odot }}$| with |$F_{\mu _{\star }}= 0.76 \pm 0.06$| and = −1.14 ± 0.37. We discuss the use of μ_⋆ as a complementary mass proxy to the well-studied richness λ for: (i) exploring the regimes of low z, λ < 20 and high λ, z ∼ 1; and (ii) testing systematics such as projection effects for applications in Cluster cosmology.
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dark energy survey year 1 results validation of weak lensing Cluster Member contamination estimates from p z decomposition
Monthly Notices of the Royal Astronomical Society, 2019Co-Authors: D. Gruen, T.n. Varga, S. Seitz, J. Derose, T. Mcclintock, E. Rozo, M. Costanzi, B. HoyleAbstract:Deutsche Forschungsgemeinschaft (DFG)German Research Foundation (DFG) [SFB-Transregio 33]; DFG Cluster of excellence 'Origin and Structure of the Universe'German Research Foundation (DFG); U.S. Department of EnergyUnited States Department of Energy (DOE); DOEUnited States Department of Energy (DOE); Sloan FoundationAlfred P. Sloan Foundation [DE-SC0015975]; Cottrell Scholar program of the Research Corporation for Science Advancement [FG-2016-6443]; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA); Stanford UniversityStanford University; Office of Science of the U.S. Department of EnergyUnited States Department of Energy (DOE) [DE-AC02-05CH11231]; U.S. National Science FoundationNational Science Foundation (NSF); Ministry of Science and Education of SpainMinistry of Education and Science, Spain; Science and Technology Facilities Council of the United KingdomScience & Technology Facilities Council (STFC); Higher Education Funding Council for EnglandHigher Education Funding Council for England; Center for Cosmology and Astro-Particle Physics at the Ohio State UniversityOhio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e ProjetosCiencia Tecnologia e Inovacao (FINEP); Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e TecnologicoNational Council for Scientific and Technological Development (CNPq); Deutsche ForschungsgemeinschaftGerman Research Foundation (DFG); University of California at Santa Cruz; University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) ZurichETH Zurich; Ludwig-Maximilians Universitat Munchen; University of Portsmouth; OzDES Membership Consortium; National Science FoundationNational Science Foundation (NSF) [AST-1138766, AST-1536171]; MINECO; ERDFEuropean Union (EU) [AYA201571825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, MDM-2015-0509]; European Union - CERCA program of the Generalitat de Catalunya; European Research Council under the European UnionEuropean Research Council (ERC) [240672, 291329, 306478]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)Australian Research Council; Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq)National Council for Scientific and Technological Development (CNPq) [CE110001020]; U.S. Department of Energy, Office of Science, Office of High Energy PhysicsUnited States Department of Energy (DOE) [465376/2014-2, DE-AC02-07CH11359]
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Dark Energy Survey Year 1 results: Validation of weak lensing Cluster Member contamination estimates from P(z) decomposition
Mon.Not.Roy.Astron.Soc., 2019Co-Authors: T.n. Varga, D. Gruen, S. Seitz, N. Maccrann, J. Derose, T. Mcclintock, E. Rozo, M. Costanzi, B. Hoyle, A.a. PlazasAbstract:Weak lensing source galaxy catalogues used in estimating the masses of galaxy Clusters can be heavily contaminated by Cluster Members, prohibiting accurate mass calibration. In this study, we test the performance of an estimator for the extent of Cluster Member contamination based on decomposing the photometric redshift P(z) of source galaxies into contaminating and background components. We perform a full scale mock analysis on a simulated sky survey approximately mirroring the observational properties of the Dark Energy Survey Year One observations (DES Y1), and find excellent agreement between the true number profile of contaminating Cluster Member galaxies in the simulation and the estimated one. We further apply the method to estimate the Cluster Member contamination for the DES Y1 redMaPPer Cluster mass calibration analysis, and compare the results to an alternative approach based on the angular correlation of weak lensing source galaxies. We find indications that the correlation based estimates are biased by the selection of the weak lensing sources in the Cluster vicinity, which does not strongly impact the P(z) decomposition method. Collectively, these benchmarks demonstrate the strength of the P(z) decomposition method in alleviating Membership contamination and enabling highly accurate Cluster weak lensing studies without broad exclusion of source galaxies, thereby improving the total constraining power of Cluster mass calibration via weak lensing.
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dark energy survey year 1 results weak lensing mass calibration of redmapper galaxy Clusters
Monthly Notices of the Royal Astronomical Society, 2019Co-Authors: T. Mcclintock, D. Gruen, T.n. Varga, E. Rozo, E S Rykoff, T Shin, P MelchiorAbstract: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 4×3 bins of richness λ and redshift z for λ≥20 and 0.2≤z≤0.65 and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as ⟨M 200m |λ,z⟩=M 0 (λ/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±0.075(stat)±0.133(sys)]⋅10 14 M ⊙ at λ=40 and z=0.35 . The richness scaling index is constrained to be F=1.356±0.051 (stat)±0.008 (sys) and the redshift scaling index G=−0.30±0.30 (stat)±0.06 (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.
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Weak-lensing mass calibration of redMaPPer galaxy Clusters in Dark Energy Survey Science Verification data
Mon.Not.Roy.Astron.Soc., 2017Co-Authors: P Melchior, D. Gruen, T.n. Varga, E. Sheldon, T. Mcclintock, B A Benson, E. Rozo, A. Amara, M.r. Becker, A. BermeoAbstract:We use weak-lensing shear measurements to determine the mean mass of optically selected galaxy Clusters in Dark Energy Survey Science Verification data. In a blinded analysis, we split the sample of more than 8000 redMaPPer Clusters into 15 subsets, spanning ranges in the richness parameter 5 ≤ λ ≤ 180 and redshift 0.2 ≤ z ≤ 0.8, and fit the averaged mass density contrast profiles with a model that accounts for seven distinct sources of systematic uncertainty: shear measurement and photometric redshift errors; Cluster-Member contamination; miscentring; deviations from the NFW halo profile; halo triaxiality and line-of-sight projections. We combine the inferred Cluster masses to estimate the joint scaling relation between mass, richness and redshift, $${\cal M}(\lambda ,z) \propto M_0 \lambda ^{F} (1+z)^{G}$$. We find $$M_0 \equiv \langle M_{200\mathrm{m}}\,|\,\lambda =30,z=0.5 \rangle =[ 2.35 \pm 0.22\ \rm {(stat)} \pm 0.12\ \rm {(sys)} ] \times \ 10^{14}\ \mathrm{M}_{{\odot }}$$, with $$F = 1.12\,\pm \,0.20\ \rm {(stat)}\, \pm \, 0.06\ \rm {(sys)}$$ and $$G = 0.18\,\pm \, 0.75\ \rm {(stat)}\, \pm \, 0.24\ \rm {(sys)}$$. The amplitude of the mass–richness relation is in excellent agreement with the weak-lensing calibration of redMaPPer Clusters in SDSS by Simet et al. and with the Saro et al. calibration based on abundance matching of SPT-detected Clusters. Our results extend the redshift range over which the mass–richness relation of redMaPPer Clusters has been calibrated with weak lensing from z ≤ 0.3 to z ≤ 0.8. Calibration uncertainties of shear measurements and photometric redshift estimates dominate our systematic error budget and require substantial improvements for forthcoming studies.