Institution
Institute of Cosmology and Gravitation, University of Portsmouth
About: Institute of Cosmology and Gravitation, University of Portsmouth is a based out in . It is known for research contribution in the topics: Galaxy & Redshift. The organization has 297 authors who have published 1207 publications receiving 76919 citations.
Topics: Galaxy, Redshift, Dark energy, Dark matter, Cosmic microwave background
Papers published on a yearly basis
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Stanford University1, University of Arizona2, Ohio State University3, INAF4, Argonne National Laboratory5, University of Pennsylvania6, Ludwig Maximilian University of Munich7, University of Manchester8, University of Wisconsin-Madison9, University of California, Berkeley10, University of Chicago11, University of Michigan12, University of Cambridge13, IFAE14, University of Geneva15, Carnegie Mellon University16, Brookhaven National Laboratory17, Duke University18, Max Planck Society19, Fermilab20, University of Edinburgh21, University of São Paulo22, Autonomous University of Madrid23, Institut d'Astrophysique de Paris24, University of Sussex25, University College London26, Spanish National Research Council27, University of Illinois at Urbana–Champaign28, University of Queensland29, Indian Institute of Technology, Hyderabad30, Santa Cruz Institute for Particle Physics31, University of Oslo32, Smithsonian Institution33, Macquarie University34, Texas A&M University35, Princeton University36, University of Southampton37, Oak Ridge National Laboratory38, National Center for Supercomputing Applications39, Institute of Cosmology and Gravitation, University of Portsmouth40
TL;DR: This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys and finds improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation.
Abstract: 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.
45 citations
Universidade Federal do Rio Grande do Sul1, Fermilab2, Space Telescope Science Institute3, University of Arizona4, Max Planck Society5, University of Strasbourg6, University of Cambridge7, Spanish National Research Council8, University of La Laguna9, Heidelberg University10, Texas A&M University11, University of Surrey12, University of Virginia13, University of Hertfordshire14, ETH Zurich15, Mount Stromlo Observatory16, University of Colorado Boulder17, University College London18, Rhodes University19, Institut d'Astrophysique de Paris20, National Center for Supercomputing Applications21, University of Illinois at Urbana–Champaign22, Institut de Ciències de l'Espai23, Autonomous University of Madrid24, Stanford University25, University of Southampton26, Institute of Cosmology and Gravitation, University of Portsmouth27, Indian Institute of Technology, Hyderabad28, SLAC National Accelerator Laboratory29, Ohio State University30, University of Washington31, Australian Astronomical Observatory32, IFAE33, Catalan Institution for Research and Advanced Studies34, California Institute of Technology35, University of Sussex36, University of Pennsylvania37, Complutense University of Madrid38, University of Michigan39, Universidade Federal do ABC40, Oak Ridge National Laboratory41
TL;DR: The Milky Way System of the German Research Foundation (DFB) as discussed by the authors is a project of the European Research Council (ERC-StG-335936) and the Sonderforschungsbereich (SDSB) of the Deutsche Forschungsgemeinschaft.
Abstract: European Research Council [ERC-StG-335936]; Sonderforschungsbereich 'The Milky Way System' of the German Research Foundation (DFB) [(SFB) 881]; US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Collaborating Institutions in the DES
45 citations
TL;DR: In this article, the B-polarisation induced in the Cosmic Microwave Background by the non-linear evolution of density perturbations is estimated using the second-order Boltzmann code SONG.
Abstract: We estimate the B-polarisation induced in the Cosmic Microwave Background by the non-linear evolution of density perturbations. Using the second-order Boltzmann code SONG, our analysis incorporates, for the first time, all physical effects at recombination. We also include novel contributions from the redshift part of the Boltzmann equation and from the bolometric definition of the temperature in the presence of polarisation. The remaining line-of-sight terms (lensing and time-delay) have previously been studied and must be calculated non-perturbatively. The intrinsic B-mode polarisation is present independent of the initial conditions and might contaminate the signal from primordial gravitational waves. We find this contamination to be comparable to a primordial tensor-to-scalar ratio of r≃10−7 at the angular scale l≃100, where the primordial signal peaks, and r≃5⋅10−5 at l≃700, where the intrinsic signal peaks. Therefore, we conclude that the intrinsic B-polarisation from second-order effects is not likely to contaminate future searches of primordial gravitational waves.
45 citations
Max Planck Society1, University of Portsmouth2, Institute of Cosmology and Gravitation, University of Portsmouth3, University of Wisconsin-Madison4, Nanjing University5, University of Utah6, Institute for the Physics and Mathematics of the Universe7, Pennsylvania State University8, University of California, San Diego9, Open University10, New Mexico State University11
TL;DR: In this paper, the authors study the evolution of the galaxy parameters effective radius, stellar velocity dispersion, and the dynamical to stellar mass ratio with redshift, and show that this evolution continues beyond z ∼ 0.7u p to z> 2a s M� (d).
Abstract: We study the redshift evolution of the dynamical properties of ∼180,000 massive galaxies from SDSS-III/BOSS combined with a local early-type galaxy sample from SDSS-II in the redshift range 0.1 z 0.6. The typical stellar mass of this sample is M� ∼ 2 × 10 11 M� . We analyze the evolution of the galaxy parameters effective radius, stellar velocity dispersion, and the dynamical to stellar mass ratio with redshift. As the effective radii of BOSS galaxies at these redshifts are not well resolved in the Sloan Digital Sky Survey (SDSS) imaging we calibrate the SDSS size measurements with Hubble Space Telescope/COSMOS photometry for a sub-sample of galaxies. We further apply a correction for progenitor bias to build a sample which consists of a coeval, passively evolving population. Systematic errors due to size correction and the calculation of dynamical mass are assessed through Monte Carlo simulations. At fixed stellar or dynamical mass, we find moderate evolution in galaxy size and stellar velocity dispersion, in agreement with previous studies. We show that this results in a decrease of the dynamical to stellar mass ratio with redshift at >2σ significance. By combining our sample with high-redshift literature data, we find that this evolution of the dynamical to stellar mass ratio continues beyond z ∼ 0. 7u p to z> 2a s M� (d)
45 citations
Max Planck Society1, Ludwig Maximilian University of Munich2, Fermilab3, Institute of Cosmology and Gravitation, University of Portsmouth4, Institut d'Astrophysique de Paris5, University College London6, National Center for Supercomputing Applications7, University of Illinois at Urbana–Champaign8, IFAE9, Spanish National Research Council10, Stanford University11, University of Pennsylvania12, Indian Institute of Technology, Hyderabad13, University of Michigan14, University of Chicago15, Autonomous University of Madrid16, University of Sussex17, SLAC National Accelerator Laboratory18, ETH Zurich19, Santa Cruz Institute for Particle Physics20, Ohio State University21, Harvard University22, Macquarie University23, University of São Paulo24, Texas A&M University25, Catalan Institution for Research and Advanced Studies26, California Institute of Technology27, University of Southampton28, Brandeis University29, State University of Campinas30, Oak Ridge National Laboratory31, Argonne National Laboratory32
TL;DR: The MARD-Y3 X-ray luminosity function was used in this paper to compare the expected luminosity and richness of galaxy clusters with a fiducial cosmology and externally calibrated luminosity-and richness-relations.
Abstract: We present the MARD-Y3 catalogue of between 1086 and 2171 galaxy clusters (52 per cent
and 65 per cent new) produced using multicomponent matched filter (MCMF) follow-up
in 5000 deg2 of DES-Y3 optical data of the ∼20 000 overlapping ROSAT All-Sky Survey
source catalogue (2RXS) X-ray sources. Optical counterparts are identified as peaks in galaxy
richness as a function of redshift along the line of sight towards each 2RXS source within a
search region informed by an X-ray prior. All peaks are assigned a probability fcont of being
a random superposition. The clusters lie at 0.02 0.5. Residual contamination is 2.6 per cent and 9.6 per cent for the cuts adopted here. For
each cluster we present the optical centre, redshift, rest frame X-ray luminosity, M500 mass,
coincidence with NWAY infrared sources, and estimators of dynamical state. About 2 per cent
of MARD-Y3 clusters have multiple possible counterparts, the photo-z’s are high quality
with σ z/(1 + z) = 0.0046, and ∼1 per cent of clusters exhibit evidence of X-ray luminosity
boosting from emission by cluster active galactic nuclei. Comparison with other catalogues
(MCXC, RM, SPT-SZ, Planck) is performed to test consistency of richness, luminosity, and
mass estimates. We measure the MARD-Y3 X-ray luminosity function and compare it to the
expectation from a fiducial cosmology and externally calibrated luminosity- and richness–mass
relations. Agreement is good, providing evidence that MARD-Y3 has low contamination and
can be understood as a simple two step selection – X-ray and then optical – of an underlying
cluster population described by the halo mass function.
45 citations
Authors
Showing all 297 results
| Name | H-index | Papers | Citations |
|---|---|---|---|
| Robert C. Nichol | 187 | 851 | 162994 |
| Daniel Thomas | 134 | 846 | 84224 |
| Will J. Percival | 129 | 473 | 87752 |
| Tommaso Treu | 126 | 715 | 49090 |
| Claudia Maraston | 103 | 362 | 59178 |
| Marco Cavaglia | 93 | 372 | 60157 |
| Ashley J. Ross | 90 | 248 | 46395 |
| David A. Wake | 89 | 214 | 46124 |
| László Á. Gergely | 89 | 426 | 60674 |
| L. K. Nuttall | 89 | 253 | 54834 |
| Rita Tojeiro | 87 | 229 | 43140 |
| Roy Maartens | 86 | 432 | 23747 |
| David Keitel | 85 | 253 | 56849 |
| Davide Pietrobon | 83 | 152 | 62010 |
| Gong-Bo Zhao | 81 | 287 | 35540 |