41 results on '"miscellaneous [Cosmology]"'
Search Results
2. Collisional cooling of primordial and interstellar media by H2
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G. Pineau des Forêts, P. Hily-Blant, François Lique, Tomás González-Lezana, D. R. Flower, Alexandre Faure, European Commission, Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Institut Universitaire de France, Agencia Estatal de Investigación (España), Science and Technology Facilities Council (UK), Durham University, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Spanish National Research Council (CSIC), European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programmeEuropean Research Council (ERC) [811363], Programme National Physique et Chimie du Milieu Interstellaire (PCMI) of CNRS/INSU with INC/INP, CNES Centre National D'etudes Spatiales, CEA French Atomic Energy Commission, MINECO/AEI/FEDER, UE [FIS2017-83157-P], STFCUK Research and Innovation (UKRI) Science and Technology Facilities Council (STFC) [ST/L00075X/1], Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Université de Rennes 1 (UR1), and Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)
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Shock wave ,Mean kinetic temperature ,molecular data ,Abundance (chemistry) ,Quantum dynamics ,Linear interpolation ,7. Clean energy ,01 natural sciences ,Molecular processes ,Shock waves ,0103 physical sciences ,atomic data ,Molecule ,miscellaneous [Cosmology] ,010306 general physics ,010303 astronomy & astrophysics ,Collisional excitation ,Atomic data ,Physics ,[PHYS]Physics [physics] ,Molecular data ,Astronomy and Astrophysics ,Function (mathematics) ,shock waves ,molecular processes ,Space and Planetary Science ,Atomic and molecular collisions ,Atomic physics ,cosmology: miscellaneous ,Molecular physics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - Abstract
8 pags., 10 figs., 2 tabs., We have computed the rate of collisional cooling of a gas by H2 molecules under conditions appropriate to the primordial and interstellar media. We incorporated the results of recent calculations of the rate coefficients for collisional excitation of H2 by H and H+, which are essential to a reliable evaluation of the ortho:para H2 ratio and the cooling rate. Comparison is made with the results of previous calculations of the cooling function. The data are made available for grids of values of the kinetic temperature, density, H:H2 ratio, and the fractional abundance of H+, together with a programme to perform linear interpolation of the data sets for any given set of values of these parameters, within the ranges of the grids., This project received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 811363). We acknowledge the Programme National Physique et Chimie du Milieu Interstellaire (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES. FL acknowledges financial support from the Institut Universitaire de France. TG-L acknowledges support from project no. FIS2017-83157-P (MINECO/AEI/FEDER, UE). DRF acknowledges support from STFC (ST/L00075X/1), including provision of local computing resources.
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- 2021
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3. ESPRESSO at VLT. On-sky performance and first results
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G. Avila, Alexandre Cabral, Andrea Mehner, S. Deiries, C. Allende Prieto, Vardan Adibekyan, Roberto Cirami, Manuel Abreu, Luca Pasquini, M. Affolter, Luca Oggioni, Igor Coretti, Nelson J. Nunes, J. Knudstrup, G. Lo Curto, Nuno C. Santos, C. Lovis, Enric Palle, Damien Ségransan, Filippo Maria Zerbi, Yann Alibert, Jose Luis Rasilla, I. Hughes, A. Fragoso, S. Santana Tschudi, T. M. Schmidt, Romain Allart, Florian Kerber, Antonino Bianco, R. Génova Santos, Mahmoudreza Oshagh, Matteo Genoni, A. Segovia, João P. Faria, Rafael Rebolo, Vincent Bourrier, M. Moschetti, Olivier Demangeon, M. A. Monteiro, Marco Landoni, Danuta Sosnowska, Valentina D'Odorico, Willy Benz, P. Figueira, François Bouchy, Baptiste Lavie, Andrea Modigliani, Marco Riva, L. Genolet, Matteo Aliverti, Paolo Santin, B. Delabre, Paolo Molaro, J. L. Lizon, F. Tenegi, M. R. Zapatero Osorio, Antonio Gouveia Oliveira, Francesco Pepe, Paolo Conconi, Stéphane Udry, Guido Cupani, Hugo M. Tabernero, S. G. Sousa, José Manuel Rebordão, Hans Dekker, T. Bandy, Ennio Poretti, S. C. C. Barros, D. Álvarez, A. Suárez Mascareño, Stefano Cristiani, C. Maire, J. I. González Hernández, Giuseppina Micela, Giorgio Calderone, V. Baldini, Xavier Dumusque, Alessandro Sozzetti, Claudio Cumani, João Coelho, M. Amate, Francesco Borsa, Olaf Iwert, Denis Mégevand, Cristina Martins, Antonio Manescau, Alessio Zanutta, Michael T. Murphy, C. Broeg, Mario Damasso, M. Mayor, Jorge Lillo-Box, Pedro Santos, P. Di Marcantonio, P. Spano, Edoardo Maria Alberto Redaelli, Diogo Alves, Giorgio Pariani, Mário J. P. F. G. Monteiro, David Ehrenreich, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Swiss National Science Foundation (SNSF), Fundacao para a Ciencia e a Tecnologia (FCT), European Research Council (ERC), Agencia Estatal de Investigación (AEI), and Australian Research Council
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Accuracy and precision ,FOS: Physical sciences ,Context (language use) ,Astrophysics ,01 natural sciences ,7. Clean energy ,law.invention ,010309 optics ,Telescope ,Espresso ,Observatory ,law ,0103 physical sciences ,miscellaneous [Cosmology] ,spectrographs [Instrumentation] ,010303 astronomy & astrophysics ,Spectrograph ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Very Large Telescope ,radial velocities [Techniques] ,Asteroseismology ,Astronomy ,Astronomy and Astrophysics ,Exoplanet ,detection [Planets and satellites] ,Space and Planetary Science ,atmospheres [Planets and satellites] ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
ESPRESSO is the new high-resolution spectrograph of ESO's Very-Large Telescope (VLT). It was designed for ultra-high radial-velocity precision and extreme spectral fidelity with the aim of performing exoplanet research and fundamental astrophysical experiments with unprecedented precision and accuracy. It is able to observe with any of the four Unit Telescopes (UT) of the VLT at a spectral resolving power of 140,000 or 190,000 over the 378.2 to 788.7 nm wavelength range, or with all UTs together, turning the VLT into a 16-m diameter equivalent telescope in terms of collecting area, while still providing a resolving power of 70,000. We provide a general description of the ESPRESSO instrument, report on the actual on-sky performance, and present our Guaranteed-Time Observation (GTO) program with its first results. ESPRESSO was installed on the Paranal Observatory in fall 2017. Commissioning (on-sky testing) was conducted between December 2017 and September 2018. The instrument saw its official start of operations on October 1st, 2018, but improvements to the instrument and re-commissioning runs were conducted until July 2019. The measured overall optical throughput of ESPRESSO at 550 nm and a seeing of 0.65 arcsec exceeds the 10% mark under nominal astro-climatic conditions. We demonstrate a radial-velocity precision of better than 25 cm/s during one night and 50 cm/s over several months. These values being limited by photon noise and stellar jitter show that the performanceis compatible with an instrumental precision of 10 cm/s. No difference has been measured across the UTs neither in throughput nor RV precision. The combination of the large collecting telescope area with the efficiency and the exquisite spectral fidelity of ESPRESSO opens a new parameter space in RV measurements, the study of planetary atmospheres, fundamental constants, stellar characterisation and many other fields., 26 pages, 28 figures
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- 2021
4. Selection of highly-accreting quasars: Spectral properties of Fe II opt emitters not belonging to extreme Population A
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A. del Olmo, Deborah Dultzin, Mary Loli Martínez-Aldama, Mauro D'Onofrio, N. Bon, C. A. Negrete, Edi Bon, Paola Marziani, Ministry of Education, Science and Technological Development (Serbia), Istituto Nazionale di Astrofisica, Universidad Nacional Autónoma de México, Ministerio de Economía y Competitividad (España), European Commission, Agencia Estatal de Investigación (España), National Science Centre (Poland), and Consejo Nacional de Ciencia y Tecnología (México)
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Active galactic nucleus ,absorption lines [Quasars] ,Astrophysics::High Energy Astrophysical Phenomena ,Cosmology: miscellaneous ,Population ,FOS: Physical sciences ,Quasars: supermassive black holes ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Stellar classification ,01 natural sciences ,Spectral line ,Luminosity ,emission lines [Quasars] ,0103 physical sciences ,miscellaneous [Cosmology] ,Emission spectrum ,Galaxies: stellar content ,Quasars: absorption lines ,Quasars: emission lines ,Quasars: general ,010306 general physics ,education ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,education.field_of_study ,Astronomy and Astrophysics ,Quasar ,general [Quasars] ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,stellar content [Galaxies] ,supermassive black holes [Quasars] - Abstract
Context. The quasar class of extreme Population A (xA) (also known as super-Eddington accreting massive black holes, SEAMBHs) has been hailed as potential distance indicators for cosmology. Aims. The aim of this paper is to define tight criteria for their proper identification, starting from the main selection criterion RFeII > 1, and to identify potential intruders that do not meet the selection criteria, which nonetheless have been selected as xA because of the coarseness of automatic searches. The inclusion of the spurious xA sources may dramatically increase the dispersion in the Hubble diagram of quasars, which were obtained from virial luminosity estimates. Methods. We studied a sample of 32 low-z quasars that were originally selected from the seventh data release of the Sloan Digital Sky Survey as xA or SEAMBHs, which have been proved to be almost certainly misclassified sources. All of them show moderate to strong Fe II emission and the large majority show strong absorption features in their spectra which are typical of fairly evolved stellar populations. We performed a simultaneous fit of a host galaxy spectrum, active galactic nucleus (AGN) continuum, FeII template, and emission lines to spectra, using the fitting technique based on ULySS, the full spectrum fitting package. We derived the main accretion parameters (i.e., luminosity, black hole mass, and Eddington ratio) and investigate the relation between host galaxy properties and AGN. Results. For sources in our sample with spectral types that correspond to a relatively low Eddington ratio, we find an overall consistency between HβNC, [O III]λλ4959,5007 line shifts, and the mean stellar velocity obtained from the host galaxy fit (within|60| km s-1). Only one source in our sample qualifies as a xA source. Conclusions. The correct classification of spectra that were contaminated by heavy absorption requires careful determination of the host galaxy spectrum. Contamination and misclassification are not usual in the identification of the xAs, nor at low z or at high z. We find a high fraction of host galaxy spectrum; in half of the sample this is even higher than 40%. When absorption lines are prominent, and the fraction of the host galaxy is high, host galaxy spectrum mimics FeII, which may result in a mistaken identification of FeII spectral features. We have identified several stellar absorption lines that, along with the continuum shape, may lead to an overestimate of RFeII, and therefore to the misclassification of sources as xA sources. © ESO 2020., This research is part of the projects 176001 "Astrophysical spectroscopy of extragalactic objects" and 176003 "Gravitation and the large scale structure of the Universe", funded by Ministry of Education, Science and Technological Development of the Republic of Serbia. PM and MDO acknowledge funding from the INAF PRIN-SKA 2017 program 1.05.01.88.04. PM also acknowledges the Programa de Estancias de Investigacion (PREI) No. DGAP/DFA/2192/2018 of UNAM. A.d.O. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness through grant AYA2016-76682-C3-1-P and from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). ML. M. A. acknowledges financial support of National Science Centre, Poland, grant No. 2017/26/A/ST9/00756 (Maestro 9). DD acknowledges support from grants PAPIIT, UNAM 113719, Mexico D.F. 04510, Mexico. AN acknowledges support from grant CONACyT research fellow -Instituto de Astronomia, UNAM, Mexico D.F. 04510, Mexico. We thank to Pu Du for his help and constructive comments. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/.The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.
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- 2020
5. KiDS-1000 methodology: Modelling and inference for joint weak gravitational lensing and spectroscopic galaxy clustering analysis
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J. Zuntz, Fabian Köhlinger, Roman Scoccimarro, Hendrik Hildebrandt, Chieh-An Lin, Angus H. Wright, Martin Crocce, Benjamin Joachimi, Henk Hoekstra, E. Sellentin, Maciej Bilicki, Arun Kannawadi, Konrad Kuijken, Nicola R. Napolitano, J. L. van den Busch, Ariel G. Sánchez, Peter Schneider, Fedor Getman, Catherine Heymans, Marika Asgari, Andrej Dvornik, M. von Wietersheim-Kramsta, Huanyuan Shan, Chris Blake, Benjamin Giblin, Thomas Erben, and Tilman Tröster
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Data Analysis ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Large-Scale Structure of Universe ,Large-scale structure of Universe ,Cosmology: miscellaneous ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Standard deviation ,Gravitational lensing: weak ,Methods: data analysis ,analytical [Methods] ,0103 physical sciences ,Methods ,miscellaneous [Cosmology] ,Weak ,Point estimation ,Methods: analytical ,data analysis [Methods] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Photometric redshift ,Gravitational Lensing ,Physics ,010308 nuclear & particles physics ,Estimator ,Astronomy and Astrophysics ,Analytical ,Statistical ,Covariance ,Methods. statistical ,Galaxy ,Cosmology ,Miscellaneous ,Sampling distribution ,Space and Planetary Science ,astro-ph.CO ,Instrumentation and Methods for Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,weak [Gravitational lensing] ,Cosmology and Nongalactic Astrophysics ,astro-ph.IM ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Joachimi, B., et al., We present the methodology for a joint cosmological analysis of weak gravitational lensing from the fourth data release of the ESO Kilo-Degree Survey (KiDS-1000) and galaxy clustering from the partially overlapping Baryon Oscillation Spectroscopic Survey (BOSS) and the 2-degree Field Lensing Survey (2dFLenS). Cross-correlations between BOSS and 2dFLenS galaxy positions and source galaxy ellipticities have been incorporated into the analysis, necessitating the development of a hybrid model of non-linear scales that blends perturbative and non-perturbative approaches, and an assessment of signal contributions by astrophysical effects. All weak lensing signals were measured consistently via Fourier-space statistics that are insensitive to the survey mask and display low levels of mode mixing. The calibration of photometric redshift distributions and multiplicative gravitational shear bias has been updated, and a more complete tally of residual calibration uncertainties was propagated into the likelihood. A dedicated suite of more than 20 000 mocks was used to assess the performance of covariance models and to quantify the impact of survey geometry and spatial variations of survey depth on signals and their errors. The sampling distributions for the likelihood and the χ2 goodness-of-fit statistic have been validated, with proposed changes for calculating the effective number of degrees of freedom. The prior volume was explicitly mapped, and a more conservative, wide top-hat prior on the key structure growth parameter S8 = σ8 (ωm/0.3)1/2 was introduced. The prevalent custom of reporting S8 weak lensing constraints via point estimates derived from its marginal posterior is highlighted to be easily misinterpreted as yielding systematically low values of S8, and an alternative estimator and associated credible interval are proposed. Known systematic effects pertaining to weak lensing modelling and inference are shown to bias S8 by no more than 0.1 standard deviations, with the caveat that no conclusive validation data exist for models of intrinsic galaxy alignments. Compared to the previous KiDS analyses, S8 constraints are expected to improve by 20% for weak lensing alone and by 29% for the joint analysis.
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- 2021
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6. A Fundamental Test for Galaxy Formation Models: Matching the Lyman-α Absorption Profiles of Galactic Halos Over Three Decades in Distance
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Sorini, D., Oñorbe, J., Hennawi, J., and Lukić, Z.
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absorption lines [quasars] ,astro-ph.GA ,Organic Chemistry ,Molecular ,numerical [methods] ,Astrophysics::Cosmology and Extragalactic Astrophysics ,miscellaneous [cosmology] ,Astronomy & Astrophysics ,Physical Chemistry ,Atomic ,halos [galaxies] ,Particle and Plasma Physics ,astro-ph.CO ,Nuclear ,intergalactic medium ,Astrophysics::Galaxy Astrophysics ,Astronomical and Space Sciences ,Physical Chemistry (incl. Structural) - Abstract
© 2018. The American Astronomical Society. All rights reserved.. Galaxy formation depends critically on the physical state of gas in the circumgalactic medium (CGM) and its interface with the intergalactic medium (IGM), determined by the complex interplay between inflow from the IGM and outflows from supernovae and/or AGN feedback. The average Lyα absorption profile around galactic halos represents a powerful tool to probe their gaseous environments. We compare predictions from Illustris and Nyx hydrodynamical simulations with the observed absorption around foreground quasars, damped Lyα systems, and Lyman-break galaxies. We show how large-scale BOSS and small-scale quasar pair measurements can be combined to precisely constrain the absorption profile over three decades in transverse distance . Far from galaxies, , the simulations converge to the same profile and provide a reasonable match to the observations. This asymptotic agreement arises because the ΛCDM model successfully describes the ambient IGM and represents a critical advantage of studying the mean absorption profile. However, significant differences between the simulations, and between simulations and observations, are present on scales , illustrating the challenges of accurately modeling and resolving galaxy formation physics. It is noteworthy that these differences are observed as far out as , indicating that the "sphere of influence" of galaxies could extend to approximately ∼7 times the halo virial radius. Current observations are very precise on these scales and can thus strongly discriminate between different galaxy formation models. We demonstrate that the Lyα absorption profile is primarily sensitive to the underlying temperature-density relationship of diffuse gas around galaxies, and argue that it thus provides a fundamental test of galaxy formation models.
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- 2018
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7. CosmoSIS: Modular cosmological parameter estimation
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James B. Kowalkowski, Saba Sehrish, Douglas H. Rudd, Marc Paterno, Sarah Bridle, Scott Dodelson, Joe Zuntz, A. Manzotti, and Elise Jennings
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statistical [Methods] ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Theoretical computer science ,Computer science ,business.industry ,Estimation theory ,Suite ,FOS: Physical sciences ,Inference ,Astronomy and Astrophysics ,Modular design ,Parameter space ,Cosmology ,Computer Science Applications ,symbols.namesake ,Installation ,Space and Planetary Science ,symbols ,miscellaneous [Cosmology] ,Planck ,data analysis [Methods] ,Astrophysics - Instrumentation and Methods for Astrophysics ,business ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Cosmological parameter estimation is entering a new era. Large collaborations need to coordinate high-stakes analyses using multiple methods; furthermore such analyses have grown in complexity due to sophisticated models of cosmology and systematic uncertainties. In this paper we argue that modularity is the key to addressing these challenges: calculations should be broken up into interchangeable modular units with inputs and outputs clearly defined. We present a new framework for cosmological parameter estimation, CosmoSIS, designed to connect together, share, and advance development of inference tools across the community. We describe the modules already available in CosmoSIS, including CAMB, Planck, cosmic shear calculations, and a suite of samplers. We illustrate it using demonstration code that you can run out-of-the-box with the installer available at http://bitbucket.org/joezuntz/cosmosis, Comment: Finally got around to updating to refereed version. 31 pages, 8 figures
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- 2015
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8. A spectroscopic look at the gravitationally lensed type Ia SN 2016geu at z=0.409
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Zach Cano, D. A. Kann, Lise Christensen, Jens Hjorth, Christa Gall, Antonio de Ugarte Postigo, Jonatan Selsing, Ministerio de Economía y Competitividad (España), European Commission, and Carlsberg Foundation
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High Energy Astrophysical Phenomena (astro-ph.HE) ,individual: SN 2016geu [Supernovae] ,Physics ,Gravitational lensing: strong ,010308 nuclear & particles physics ,Cosmology: miscellaneous ,Supernovae: general ,general [Supernovae] ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,strong [Gravitational lensing] ,01 natural sciences ,Supernovae: individual: SN 2016geu ,Supernova ,Space and Planetary Science ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,miscellaneous [Cosmology] ,Astrophysics - High Energy Astrophysical Phenomena ,010303 astronomy & astrophysics ,Humanities ,Astrophysics::Galaxy Astrophysics - Abstract
The spectacular success of Type Ia supernovae (SNe Ia) in SN-cosmology is based on the assumption that their photometric and spectroscopic properties are invariant with redshift. However, this fundamental assumption needs to be tested with observations of high-z SNe Ia. To date, the majority of SNe Ia observed at moderate to large redshifts (0.4 ≤ z ≤ 1.0) are faint, and the resultant analyses are based on observations with modest signal-to-noise ratios that impart a degree of ambiguity in their determined properties. In rare cases, however, the Universe offers a helping hand: To date a few SNe Ia have been observed that have had their luminosities magnified by intervening galaxies and galaxy clusters acting as gravitational lenses. In this paper, we present long-slit spectroscopy of the lensed SN Ia 2016geu, which occurred at a redshift of z = 0.409, and was magnified by a factor of ≈55 by a galaxy located at z = 0.216. We compared our spectra, which were obtained a couple of weeks to a couple of months past peak light, with the spectroscopic properties of well-observed, nearby SNe Ia, finding that SN 2016geu's properties are commensurate with those of SNe Ia in the local Universe. Based primarily on the velocity and strength of the Si II λ6355 absorption feature, we find that SN 2016geu can be classified as a high-velocity, high-velocity-gradient and 'corenormal' SN Ia. The strength of various features (measured though their pseudo-equivalent widths) argue against SN 2016geu being a faint, broad-lined, cool or shallow-silicon SN Ia. We conclude that the spectroscopic properties of SN 2016geu imply that it is a normal SN Ia, and when taking previous results by other authors into consideration, there is very little, if any, evolution in the observational properties of SNe Ia up to z ≈ 0.4.© 2018 The Authors., ZC acknowledges support from the Juan de la Cierva Incorporacion fellowship IJCI-2014-21669. AdUP acknowledges support from funding associated with the Ramon y Cajal fellowship RyC-2012-09975. DAK acknowledges support from the Juan de la Cierva Incorporacion fellowship IJCI-2015-26153. ZC, DAK and AdUP acknowledge support from the Spanish research project AYA 2014-58381-P. CG was funded by the Carlsberg Foundation.
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- 2017
9. Primordial black hole evolution in two-fluid cosmology
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Gustavo E. Romero, Florencia Laura Vieyro, and Eduardo Gutiérrez
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmology: miscellaneous ,media_common.quotation_subject ,Ciencias Físicas ,Astrophysics::High Energy Astrophysical Phenomena ,Early universe ,FOS: Physical sciences ,Primordial black hole ,Astrophysics::Cosmology and Extragalactic Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,01 natural sciences ,Cosmology ,General Relativity and Quantum Cosmology ,BLACK HOLE PHYSICS ,Micro black hole ,EARLY UNIVERSE ,0103 physical sciences ,010306 general physics ,Entropy (arrow of time) ,Astrophysics::Galaxy Astrophysics ,media_common ,Physics ,010308 nuclear & particles physics ,Física ,Astronomy ,MISCELLANEOUS [COSMOLOGY] ,Astronomy and Astrophysics ,Black hole physics ,Universe ,Black hole ,Astronomía ,Space and Planetary Science ,Intermediate-mass black hole ,Stellar black hole ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Several processes in the early Universe might lead to the formation of primordial black holes with different masses. These black holes would interact with the cosmic plasma through accretion and emission processes. Such interactions might have affected the dynamics of the Universe and generated a considerable amount of entropy. In this paper, we investigate the effects of the presence of primordial black holes on the evolution of the early Universe. We adopt a two-fluid cosmological model with radiation and a primordial black hole gas. The latter is modelled with different initial mass functions taking into account the available constraints over the initial primordial black hole abundances.We find that certain populations with narrow initial mass functions are capable to produce significant changes in the scalefactor and the entropy., Instituto Argentino de Radioastronomía, Facultad de Ciencias Astronómicas y Geofísicas
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- 2017
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10. The XMM Cluster Survey: evolution of the velocity dispersion–temperature relation over half a Hubble time
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Caroline Caldwell, John P. Stott, A. Kathy Romer, Matt Hilton, P. Rooney, Christopher J. Miller, Robert G. Mann, Martin Sahlén, Chris A. Collins, Luiz N. da Costa, Peter A. Thomas, Ricardo L. C. Ogando, Tesla E. Jeltema, Ben Hoyle, Susan Wilson, Ian G. McCarthy, Scott T. Kay, J. A. Mayers, H. Wilcox, Andrew R. Liddle, Nicola Mehrtens, Rebecca Bernstein, Marcio A. G. Maia, Daniel Gifford, A. Bermeo, Pedro T. P. Viana, Robert C. Nichol, Benjamin E. Stahl, and Devon L. Hollowood
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,miscellaneous [cosmology] ,ST/L000652/1 ,01 natural sciences ,Galaxy groups and clusters ,Galaxy group ,0103 physical sciences ,Cluster (physics) ,clusters: general [galaxies] ,010303 astronomy & astrophysics ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,STFC ,QB ,Physics ,010308 nuclear & particles physics ,Velocity dispersion ,RCUK ,Astronomy and Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Redshift ,Space and Planetary Science ,clusters: intracluster medium [galaxies] ,Astrophysics of Galaxies (astro-ph.GA) ,Elliptical galaxy ,Cluster sampling ,distances and redshifts [galaxies] ,galaxies: clusters [X-rays] ,ST/L000768/1 ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We measure the evolution of the velocity dispersion--temperature ($\sigma_{\rm v}$--$T_{\rm X}$) relation up to $z = 1$ using a sample of 38 galaxy clusters drawn from the \textit{XMM} Cluster Survey. This work improves upon previous studies by the use of a homogeneous cluster sample and in terms of the number of high redshift clusters included. We present here new redshift and velocity dispersion measurements for 12 $z > 0.5$ clusters observed with the GMOS instruments on the Gemini telescopes. Using an orthogonal regression method, we find that the slope of the relation is steeper than that expected if clusters were self-similar, and that the evolution of the normalisation is slightly negative, but not significantly different from zero ($\sigma_{\rm v} \propto T^{0.86 \pm 0.14} E(z)^{-0.37 \pm 0.33}$). We verify our results by applying our methods to cosmological hydrodynamical simulations. The lack of evolution seen in our data is consistent with simulations that include both feedback and radiative cooling., Comment: Accepted to MNRAS (3 August 2016); Paper: 15 pages, 12 figures; Appendix A: 1 table; Appendix B: 34 Tables; Appendix C: 2 Figures
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- 2016
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11. Extragalactic number counts at 100 m, free from cosmic variance
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Bruce Sibthorpe, P. van der Werf, Rob Ivison, Isaac Roseboom, Brenda C. Matthews, Jane Greaves, and Richard Massey
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Physics ,Luminous infrared galaxy ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Large-scale structure of Universe ,Spectrometer ,media_common.quotation_subject ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astronomy ,Sampling (statistics) ,Astronomy and Astrophysics ,Scale (descriptive set theory) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Cosmic variance ,Galaxy ,galaxies. [Infrared] ,Space and Planetary Science ,Sky ,Cosmic infrared background ,miscellaneous [Cosmology] ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,media_common - Abstract
We use data from the Disc Emission via a Bias-free Reconnaissance in the Infrared/Submillimetre (DEBRIS) survey, taken at 100 um with the Photoconductor Array Camera and Spectrometer instrument on board the Herschel Space Observatory, to make a cosmic variance independent measurement of the extragalactic number counts. These data consist of 323 small-area mapping observations performed uniformly across the sky, and thus represent a sparse sampling of the astronomical sky with an effective coverage of ~2.5 deg^2. We find our cosmic variance independent analysis to be consistent with previous count measurements made using relatively small area surveys. Furthermore, we find no statistically significant cosmic variance on any scale within the errors of our data. Finally, we interpret these results to estimate the probability of galaxy source confusion in the study of debris discs., Comment: Accepted for publication by MNRAS Letter
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- 2012
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12. The stochastic background of gravitational waves due to the f-mode instability in neutron stars
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Kostas D. Kokkotas, Marco Surace, and Pantelis Pnigouras
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics::High Energy Astrophysical Phenomena ,oscillations [Stars] ,Population ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Instability ,General Relativity and Quantum Cosmology ,Gravitational waves ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,miscellaneous [Cosmology] ,education ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,education.field_of_study ,Einstein Telescope ,010308 nuclear & particles physics ,Gravitational wave ,Star formation ,neutron [Stars] ,Astronomy and Astrophysics ,LIGO ,Supernova ,Neutron star ,Space and Planetary Science ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
This paper presents an estimate for the spectral properties of the stochastic background of gravitational waves emitted by a population of hot, young, rapidly rotating neutron stars throughout the Universe undergoing $f$-mode instabilities, formed through either core-collapse supernova explosions or the merger of binary neutron star systems. Their formation rate, from which the gravitational wave event rate is obtained, is deduced from observation-based determinations of the cosmic star formation rate. The gravitational wave emission occurs during the spin-down phase of the $f$-mode instability. For low magnetized neutron stars and assuming 10\% of supernova events lead to $f$-mode unstable neutron stars, the background from supernova-derived neutron stars peaks at $\Omega_{\text{gw}} \sim 10^{-9}$ for the $l=m=2$ $f$-mode, which should be detectable by cross-correlating a pair of second generation interferometers (e.g. Advanced LIGO/Virgo) with an upper estimate for the signal-to-noise ratio of $\approx$ 9.8. The background from supramassive neutron stars formed from binary mergers peaks at $\Omega_{\text{gw}} \sim 10^{-10}$ and should not be detectable, even with third generation interferometers (e.g. Einstein Telescope).
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- 2016
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13. Neutral hydrogen in galaxy clusters: impact of AGN feedback and implications for intensity mapping
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Francisco Villaescusa-Navarro, Stefano Borgani, Giuseppe Murante, Elena Rasia, A. M. Beck, Lisa K. Steinborn, Susana Planelles, Klaus Dolag, Veronica Biffi, Cinthia Ragone-Figueroa, Matteo Viel, Villaescusa Navarro, Francisco, Planelles, Susana, Borgani, Stefano, Viel, Matteo, Rasia, Elena, Murante, Giuseppe, Dolag, Klau, Steinborn, Lisa K., Biffi, Veronica, Beck, Alexander M., and Ragone Figueroa, Cinthia
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Active galactic nucleus ,Dark matter ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,miscellaneous [cosmology] ,01 natural sciences ,7. Clean energy ,methods: numerical ,Settore FIS/05 - Astronomia e Astrofisica ,galaxies: clusters: general ,cosmology: miscellaneous ,0103 physical sciences ,clusters: general [galaxies] ,010303 astronomy & astrophysics ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,Star formation ,Astronomy ,numerical [methods] ,Astronomy and Astrophysics ,Cosmology: Miscellaneous ,Galaxies: Clusters: General ,Methods: Numerical ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,Supernova ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Halo ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
By means of zoom-in hydrodynamic simulations we quantify the amount of neutral hydrogen (HI) hosted by groups and clusters of galaxies. Our simulations, which are based on an improved formulation of smoothed particle hydrodynamics (SPH), include radiative cooling, star formation, metal enrichment and supernova feedback, and can be split in two different groups, depending on whether feedback from active galactic nuclei (AGN) is turned on or off. Simulations are analyzed to account for HI self-shielding and the presence of molecular hydrogen. We find that the mass in neutral hydrogen of dark matter halos monotonically increases with the halo mass and can be well described by a power-law of the form $M_{\rm HI}(M,z)\propto M^{3/4}$. Our results point out that AGN feedback reduces both the total halo mass and its HI mass, although it is more efficient in removing HI. We conclude that AGN feedback reduces the neutral hydrogen mass of a given halo by $\sim50\%$, with a weak dependence on halo mass and redshift. The spatial distribution of neutral hydrogen within halos is also affected by AGN feedback, whose effect is to decrease the fraction of HI that resides in the halo inner regions. By extrapolating our results to halos not resolved in our simulations we derive astrophysical implications from the measurements of $\Omega_{\rm HI}(z)$: halos with circular velocities larger than $\sim25~{\rm km/s}$ are needed to host HI in order to reproduce observations. We find that only the model with AGN feedback is capable of reproducing the value of $\Omega_{\rm HI}b_{\rm HI}$ derived from available 21cm intensity mapping observations., Comment: 19 pages, 12 figures. Accepted for publication in MNRAS
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- 2016
14. Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters
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Ricardo L. C. Ogando, Martin Crocce, A. Roodman, David J. Brooks, Robert Armstrong, A. A. Plazas, Joseph J. Mohr, Jochen Weller, Mark Brodwin, Diego Capozzi, W. L. Holzapfel, M. A. G. Maia, J. J. Thaler, E. Bertin, C. Gangkofner, A. Saro, David J. James, T. M. C. Abbott, Ofer Lahav, M. Carrasco Kind, E. Fernandez, R. Covarrubias, Robert Connon Smith, Darren L. DePoy, Alistair R. Walker, Pablo Fosalba, Marcelle Soares-Santos, R. Capasso, V. Strazzullo, E. J. Sanchez, Michael McDonald, B. Stalder, Gary Bernstein, Risa H. Wechsler, V. Upadhyay, Enrique Gaztanaga, Vinu Vikram, Huan Lin, Lindsey Bleem, T. M. Crawford, John E. Carlstrom, Peter Melchior, Tianjun Li, Shantanu Desai, Sebastian Bocquet, Brian Nord, Bhuvnesh Jain, Peter Doel, J. P. Dietrich, A. von der Linden, Bradford Benson, Daniel Thomas, M. E. C. Swanson, I. Sevilla, E. Buckley-Geer, Michael Schubnell, F. B. Abdalla, Scott Dodelson, A. Benoit-Lévy, Carlos E. Cunha, T. de Haan, H. T. Diehl, Jennifer L. Marshall, Christian L. Reichardt, D. L. Burke, Tim Eifler, Antony A. Stark, A. H. Bauer, S. Allam, Robert A. Gruendl, Alfredo Zenteno, Flavia Sobreira, I-Non Chiu, C. Hennig, B. Flaugher, C. B. D'Andrea, M. March, Ramon Miquel, Eduardo Rozo, K. E. Ziegler, A. K. Romer, Paul Martini, W. C. Wester, A. Fausti Neto, K. Honscheid, Christopher J. Miller, Matthew B. Bayliss, Eli S. Rykoff, N. Kuropatkin, L. N. da Costa, M. Banerji, Joshua A. Frieman, A. Carnero Rosell, M. Sako, Douglas L. Tucker, Kyler Kuehn, Gregory Tarle, Nikhel Gupta, E. Suchyta, August E. Evrard, Daniel Gruen, D. W. Gerdes, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, McDonald, Michael A., Saro, A., Bocquet, S., Rozo, E., Benson, B. A., Mohr, J., Rykoff, E. S., Soares-Santos, M., Bleem, L., Dodelson, S., Melchior, P., Sobreira, F., Upadhyay, V., Weller, J., Abbott, T., Abdalla, F. B., Allam, S., Armstrong, R., Banerji, M., Bauer, A. H., Bayliss, M., Benoit-Lévy, A., Bernstein, G. M., Bertin, E., Brodwin, M., Brooks, D., Buckley-Geer, E., Burke, D. L., Carlstrom, J. E., Capasso, R., Capozzi, D., Carnero Rosell, A., Carrasco Kind, M., Chiu, I., Covarrubias, R., Crawford, T. M., Crocce, M., D'Andrea, C. B., da Costa, L. N., Depoy, D. L., Desai, S., de Haan, T., Diehl, H. T., Dietrich, J. P., Doel, P., Cunha, C. E, Eifler, T. F., Evrard, A. E., Fausti Neto, A., Fernandez, E., Flaugher, B., Fosalba, P., Frieman, J., Gangkofner, C., Gaztanaga, E., Gerdes, D., Gruen, D., Gruendl, R. A., Gupta, N., Hennig, C., Holzapfel, W. L., Honscheid, K., Jain, B., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lin, H., Maia, M. A. G., March, M., Marshall, J. L., Martini, Paul, Mcdonald, M., Miller, C. J., Miquel, R., Nord, B., Ogando, R., Plazas, A. A., Reichardt, C. L., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Schubnell, M., Sevilla, I., Smith, R. C., Stalder, B., Stark, A. A., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Tucker, D., Vikram, V., von der Linden, A., Walker, A. R., Wechsler, R. H., Wester, W., Zenteno, A., and Ziegler, K. E.
- Subjects
statistics [galaxies] ,Large-scale structure of Universe ,Galaxies: abundances ,Astrophysics ,abundance [Galaxies] ,miscellaneous [cosmology] ,Lambda ,Catalogue ,01 natural sciences ,haloe [Galaxies] ,clusters: general [galaxies] ,010303 astronomy & astrophysics ,catalogues ,QB ,Physics ,education.field_of_study ,Sigma ,haloes [galaxies] ,South Pole Telescope ,astro-ph.CO ,large-scale structure of Universe ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics and Astronomy ,Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Galaxies: statistics ,Cosmology: miscellaneous ,Population ,FOS: Physical sciences ,Methods: data analysis ,abundances [galaxies] ,0103 physical sciences ,data analysis [methods] ,Cluster (physics) ,miscellaneou [Cosmology] ,Galaxies: haloes ,education ,STFC ,Galaxy cluster ,Catalogues ,Galaxies: clusters: general ,Astronomy and Astrophysics ,Space and Planetary Science ,statistic [Galaxies] ,010308 nuclear & particles physics ,RCUK ,Astronomy ,Astronomy and Astrophysic ,Redshift ,data analysi [Methods] ,Dark energy - Abstract
We cross-match galaxy cluster candidates selected via their Sunyaev–Zel'dovich effect (SZE) signatures in 129.1 deg[superscript 2] of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey science verification data. We identify 25 clusters between 0.1 ≲ z ≲ 0.8 in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness λ-mass relation with the following function 〈ln λ|M500〉 ∝ Bλln M500 + Cλln E(z) and use SPT-SZ cluster masses and RM richnesses λ to constrain the parameters. We find Bλ=1.14[superscript +0.21][subscript −0.18 and Cλ=0.73[superscript +0.77][subscript −0.75]. The associated scatter in mass at fixed richness is σlnM|λ=0.18[superscript +0.08][subscript −0.05] at a characteristic richness λ = 70. We demonstrate that our model provides an adequate description of the matched sample, showing that the fraction of SPT-SZ-selected clusters with RM counterparts is consistent with expectations and that the fraction of RM-selected clusters with SPT-SZ counterparts is in mild tension with expectation. We model the optical-SZE cluster positional offset distribution with the sum of two Gaussians, showing that it is consistent with a dominant, centrally peaked population and a subdominant population characterized by larger offsets. We also cross-match the RM catalogue with SPT-SZ candidates below the official catalogue threshold significance ξ = 4.5, using the RM catalogue to provide optical confirmation and redshifts for 15 additional clusters with ξ ∈ [4, 4.5]., Kavli Foundation, Gordon and Betty Moore Foundation (Grant GBMF 947)
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- 2015
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15. The variation of the fine structure constant: testing the dipole model with thermonuclear supernovae
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Carolina Negrelli, Susana J. Landau, Lucila Kraiselburd, Enrique García-Berro, Universitat Politècnica de Catalunya. Departament de Física Aplicada, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica
- Subjects
Ciencias Astronómicas ,Thermonuclear fusion ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,absorption lines [Quasars] ,Astrophysics::High Energy Astrophysical Phenomena ,Cosmology: miscellaneous ,Ciencias Físicas ,Supernovae: general ,general [Supernovae] ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmology ,Luminosity ,purl.org/becyt/ford/1 [https] ,white dwarfs [Stars] ,Phenomenological model ,Astrophysics::Solar and Stellar Astrophysics ,SPECTRA ,miscellaneous [Cosmology] ,TIME-VARIATION ,Luminosity distance ,Quasars ,Physics ,LEGACY SURVEY ,Cosmologia ,IA SUPERNOVAE ,Supernoves ,CONSTRAINTS ,Astronomy and Astrophysics ,Fine-structure constant ,Quasars: absorption lines ,purl.org/becyt/ford/1.3 [https] ,HUBBLE-SPACE-TELESCOPE ,Stars: white dwarfs ,Astronomía ,Dipole ,Supernovae ,Space and Planetary Science ,Física::Astronomia i astrofísica [Àrees temàtiques de la UPC] ,COSMOLOGY ,DISTANCE ,White dwarfs starts ,Baryon acoustic oscillations ,FUNDAMENTAL CONSTANTS ,BARYON ACOUSTIC-OSCILLATIONS ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The large-number hypothesis conjectures that fundamental constants may vary. Accordingly, the spacetime variation of fundamental constants has been an active subject of research for decades. Recently, using data obtained with large telescopes a phenomenological model in which the fine structure constant might vary spatially has been proposed. We test whether this hypothetical spatial variation of {\alpha}, which follows a dipole law, is compatible with the data of distant thermonuclear supernovae. Unlike previous works, in our calculations we consider not only the variation of the luminosity distance when a varying {\alpha} is adopted, but we also take into account the variation of the peak luminosity of Type Ia supernovae resulting from a variation of {\alpha}. This is done using an empirical relation for the peak bolometric magnitude of thermonuclear supernovae that correctly reproduces the results of detailed numerical simulations. We find that there is no significant difference between the several phenomenological models studied here and the standard one, in which {\alpha} does not vary spatially. We conclude that the present set of data of Type Ia supernovae is not able to distinguish the standard model from the dipole models, and thus cannot be used to discard nor to confirm the proposed spatial variation of {\alpha}., Comment: 8 pages, 4 figures. Accepted for publication in Ap&SS
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- 2015
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16. Foreground contamination of the WMAP CMB maps from the perspective of the matched circle test
- Author
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H. Then
- Subjects
Physics ,cosmic microwave background ,media_common.quotation_subject ,Astrophysics (astro-ph) ,statistical [methods] ,Perspective (graphical) ,Cosmic microwave background ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,miscellaneous [cosmology] ,Galactic plane ,Residual ,CMB cold spot ,Space and Planetary Science ,Sky ,data analysis [methods] ,large-scale structure of Universe ,Linear combination ,Astrophysics::Galaxy Astrophysics ,Statistic ,media_common - Abstract
Wilkinson Microwave Anisotropy Probe has provided cosmic microwave background (CMB) maps of the full sky. The raw data are subject toforeground contamination, in particular near to the Galactic plane. Foreground-cleaned maps have been derived, e.g. the internal linearcombination map of Bennett et al., and the reduced foreground TOH map ofTegmark et al. Using S statistics, we examine whether residual foreground contamination is left over in the foreground-cleaned maps. Inparticular, we specify which parts of the foreground-cleaned maps are sufficiently accurate for the circle-in-the-sky signature. We generalizethe S statistic, called D statistic, such that the circle test can dealwith CMB maps in which the contaminated regions of the sky are excludedwith masks.
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- 2006
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17. HUNTING DOWN HORIZON-SCALE EFFECTS with MULTI-WAVELENGTH SURVEYS
- Author
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Roy Maartens, Mario G. Santos, José Fonseca, and Stefano Camera
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Cosmology and Gravitation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,media_common.quotation_subject ,gr-qc ,cosmological parameters ,cosmology: miscellaneous ,large-scale structure of universe ,Space and Planetary Science ,Astronomy and Astrophysics ,Dark matter ,Cosmic microwave background ,FOS: Physical sciences ,Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,miscellaneous [cosmology] ,01 natural sciences ,Cosmology ,General Relativity and Quantum Cosmology ,0103 physical sciences ,ST/K0090X/1 ,010303 astronomy & astrophysics ,STFC ,media_common ,Physics ,010308 nuclear & particles physics ,Horizon ,Intensity mapping ,RCUK ,Cosmic variance ,Galaxy ,Sky ,astro-ph.CO ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Next-generation cosmological surveys will probe ever larger volumes of the Universe, including the largest scales, near and beyond the horizon. On these scales, the galaxy power spectrum carries signatures of local primordial non-Gaussianity (PNG) and horizon-scale general relativistic (GR) effects. However, cosmic variance limits the detection of horizon-scale effects. Combining different surveys via the multi-tracer method allows us to reduce the effect down cosmic variance. This method benefits from large bias differences between two tracers of the underlying dark matter distribution, which suggests a multi-wavelength combination of large volume surveys that are planned on a similar timescale. We show that the combination of two contemporaneous surveys, a large neutral hydrogen intensity mapping survey in SKA Phase1 and a Euclid-like photometric survey, will provide unprecedented constraints on PNG as well as detection of the GR effects. We forecast that the error on local PNG will break through the cosmic variance limit on cosmic microwave background surveys and achieve $\sigma(f_{NL})\simeq1.4-0.5$, depending on assumed priors, bias, and sky coverage. GR effects are more robust to changes in the assumed fiducial model, and we forecast that they can be detected with a signal-to-noise of about $14$., Comment: Typos corrected; Accepted for publication by the Astrophysical Journal Letters; 5 pages, 3 figures, 2 tables
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- 2015
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18. A statistical analysis of varying α data
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Kraiselburd, Lucila, Landau, Susana Judith, and Simeone, Claudio Mauricio
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Astronomía ,purl.org/becyt/ford/1 [https] ,Miscellaneous [Cosmology] ,Ciencias Físicas ,Cosmology: miscellaneous ,Absorption lines ,Absorption Lines ,purl.org/becyt/ford/1.3 [https] ,Quasars ,CIENCIAS NATURALES Y EXACTAS - Abstract
We collect different groups of data of the variation of the fine structure constant to compare and verify the consistency between them using the Student test and Confidence Intervals. We separate data sets in smaller intervals based on a proposed criterion. Another statistical analysis is proposed that considers phenomenological models for the variation in α. The results show consistency for a certain amount of reduced intervals, in contrast to those obtained considering the mean values from the entire interval., Facultad de Ciencias Astronómicas y Geofísicas
- Published
- 2014
19. Planck 2013 results. XXIII. Isotropy and statistics of the CMB
- Author
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Ade, PAR, Aghanim, N, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartlett, JG, Bartolo, N, Battaner, E, Battye, R, Benabed, K, Benoît, A, Benoit-Lévy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, JJ, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Bridges, M, Bucher, M, Burigana, C, Butler, RC, Cardoso, J-F, Catalano, A, Challinor, A, Chamballu, A, Chary, R-R, Chiang, HC, Chiang, L-Y, Christensen, PR, Church, S, Clements, DL, Colombi, S, Colombo, LPL, Couchot, F, Coulais, A, Crill, BP, Cruz, M, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Delouis, J-M, Désert, F-X, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Fantaye, Y, Fergusson, J, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Frommert, M, Galeotta, S, Ganga, K, Giard, M, Giardino, G, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, FK, Hansen, M, Hanson, D, Harrison, DL, Helou, G, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, and Hovest, W
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astro-ph.CO ,cosmic background radiation ,miscellaneous [cosmology] ,Astronomy & Astrophysics ,observations [cosmology] ,Astronomical and Space Sciences - Abstract
The two fundamental assumptions of the standard cosmological model-that the initial fluctuations are statistically isotropic and Gaussian-are rigorously tested using maps of the cosmic microwave background (CMB) anisotropy from the Planck satellite. The detailed results are based on studies of four independent estimates of the CMB that are compared to simulations using a fiducial ΛCDM model and incorporating essential aspects of the Planck measurement process. Deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask choice, and frequency dependence. Many of these anomalies were previously observed in the WMAP data, and are now confirmed at similar levels of significance (about 3σ). However, we find little evidence of non-Gaussianity, with the exception of a few statistical signatures that seem to be associated with specific anomalies. In particular, we find that the quadrupole-octopole alignment is also connected to a low observed variance in the CMB signal. A power asymmetry is now found to persist on scales corresponding to about â.," = 600 and can be described in the low-â.," regime by a phenomenological dipole modulation model. However, any primordial power asymmetry is strongly scale-dependent and does not extend to arbitrarily small angular scales. Finally, it is plausible that some of these features may be reflected in the angular power spectrum of the data, which shows a deficit of power on similar scales. Indeed, when the power spectra of two hemispheres defined by a preferred direction are considered separately, one shows evidence of a deficit in power, while its opposite contains oscillations between odd and even modes that may be related to the parity violation and phase correlations also detected in the data. Although these analyses represent a step forward in building an understanding of the anomalies, a satisfactory explanation based on physically motivated models is still lacking.
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- 2014
20. Subhaloes gone Notts: subhaloes as tracers of the dark matter halo shape
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Mark C. Neyrinck, H. Lux, Julian Onions, Jiaxin Han, Enrique Gaztanaga, Yago Ascasibar, Kai Hoffmann, Stuart I. Muldrew, Mario Agustín Sgró, Alexander Knebe, Michal Maciejewski, S. Planelles, Frazer R. Pearce, Manuel E. Merchán, Peter Behroozi, Andrés N. Ruiz, and Pascal J. Elahi
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Field (physics) ,Milky Way ,Ciencias Físicas ,Astrophysics::High Energy Astrophysical Phenomena ,Dark matter ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,miscellaneous [cosmology] ,01 natural sciences ,purl.org/becyt/ford/1 [https] ,0103 physical sciences ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,numerical [methods] ,purl.org/becyt/ford/1.3 [https] ,Accretion (astrophysics) ,Dark matter halo ,Astronomía ,Orbit ,methods: numerical, galaxies: haloes, cosmology: miscellaneous ,haloes [galaxies] ,Space and Planetary Science ,Satellite ,Halo ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We study the shapes of subhalo distributions from four dark-matter-only simulations of Milky Way type haloes. Comparing the shapes derived from the subhalo distributions at high resolution to those of the underlying dark matter fields we find the former to be more triaxial if theanalysis is restricted to massive subhaloes. For three of the four analysed haloes the increased triaxiality of the distributions of massive subhaloes can be explained by a systematic effect caused by the low number of objects. Subhaloes of the fourth halo show indications for anisotropic accretion via their strong triaxial distribution and orbit alignment with respect to the dark matter field. These results are independent of the employed subhalo finder. Comparing the shape of the observed Milky Way satellite distribution to those of high-resolution subhalo samples from simulations, we find an agreement for samples of bright satellites, but significant deviations if faint satellites are included in the analysis. These deviations might result from observational incompleteness., 15 pages, 11 figures, 2 tables. 1 figure removed to reduce paper extension, shorter discussion, accepted for publication in MNRAS
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- 2014
21. Cosmic reionization by primordial cosmic rays
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Matias Jorge Tueros, Gustavo E. Romero, and Maria Victoria del Valle
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Ciencias Astronómicas ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Ciencias Físicas ,Astrophysics::High Energy Astrophysical Phenomena ,Cosmology: miscellaneous ,first stars ,FOS: Physical sciences ,Cosmic ray ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,miscellaneous [cosmology] ,purl.org/becyt/ford/1 [https] ,Dark ages, reionization, first stars ,cosmic rays ,dark ages ,Reionization ,Cosmic rays ,Astrophysics::Galaxy Astrophysics ,Intergalactic medium ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,COSMIC cancer database ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy and Astrophysics ,purl.org/becyt/ford/1.3 [https] ,Astronomía ,Space and Planetary Science ,Dark Ages ,reionization ,intergalactic medium ,Astrophysics - High Energy Astrophysical Phenomena ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Context. After the so-called cosmic recombination, the expanding universe entered into a period of darkness since most of the matter was in a neutral state. About a billion years later, however, the intergalactic space was once again ionized. The process, known as the cosmic reionization, required the operation of mechanisms that are not well understood. Among other ionizing sources, Population III stars, mini-quasars, and X-ray emitting microquasars have been invoked. Aims. We propose that primordial cosmic rays, accelerated at the termination points of the jets of the first microquasars, may have contributed to the reionization of the intergalactic space as well. Methods. We quantify the ionization power of cosmic rays (electrons and protons) in the primordial intergalactic medium. This power is calculated using extensive particle cascade simulations. Results. We establish that, depending on the fraction of electrons to protons accelerated in the microquasar jets, cosmic rays should have contributed to the reionization of the primordial intergalactic medium as much as X-rays from microquasar accretion disks. If the primordial magnetic field was of the order of 10-17 G, as some models suggest, cosmic rays had an important role in ionizing the neutral material far beyond the birth places of the first stars., Facultad de Ciencias Astronómicas y Geofísicas
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- 2014
22. Planck 2013 results. XXIII. Isotropy and statistics of the CMB
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Olivier Doré, A. Renzi, Luigi Danese, E. P. S. Shellard, C. Hernández-Monteagudo, T. J. Pearson, O. Perdereau, J. Tuovinen, A. Coulais, L. Mendes, Jose Alberto Rubino-Martin, Sabino Matarrese, L. Toffolatti, G. de Zotti, C. Gauthier, Andrea Zonca, A. Curto, R. Fernandez-Cobos, Federico Nati, S. Colombi, Luca Terenzi, C. Combet, Charles R. Lawrence, Anthony Lasenby, M. Ashdown, Sophie Henrot-Versille, R. A. Sunyaev, Jean-François Cardoso, E. Martínez-González, M. Piat, A. Gregorio, F. Boulanger, H. C. Chiang, Paolo Natoli, A. Benoit-Lévy, M. Giard, E. Keihänen, Aurelien A. Fraisse, K. Ganga, L. Montier, Theodore Kisner, Allan Hornstrup, B. P. Crill, H. K. Eriksen, Laura Bonavera, R. V. Sudiwala, F. Pasian, C. A. Oxborrow, V. Stolyarov, Etienne Pointecouteau, M. Cruz, K. Mikkelsen, A. Frejsel, C. Renault, Jose M. Diego, Andrea Zacchei, Peter G. Martin, Rafael Rebolo, Martin Kunz, Alain Benoit, J.-L. Puget, Alessandro Melchiorri, François R. Bouchet, M. Rossetti, S. R. Hildebrandt, Mathieu Remazeilles, L. P. L. Colombo, D. Molinari, Dmitry Novikov, T. R. Jaffe, Reijo Keskitalo, E. Battaner, Andrei V. Frolov, M. Tristram, G. Polenta, M. Linden-Vørnle, Sarah E. Church, Pavel Naselsky, Jon E. Gudmundsson, L. Pagano, Carlo Burigana, Zhiqi Huang, Julien Lesgourgues, J. Knoche, Simon Prunet, M. Migliaccio, R. J. Davis, Tarun Souradeep, P. Bielewicz, L. A. Wade, James R. Fergusson, Daniela Paoletti, Jörg P. Rachen, F. Piacentini, Y. Giraud-Héraud, J.-P. Bernard, Ben Rusholme, Davide Pietrobon, A. Mangilli, F. Pajot, Gianmarco Maggio, Dipak Munshi, George Efstathiou, Francesca Perrotta, Soumen Basak, I. Ristorcelli, D. Herranz, W. Hovest, Torsten A. Enßlin, Monique Arnaud, Calvin B. Netterfield, X. Dupac, J. J. Bock, Peter A. R. Ade, Benjamin D. Wandelt, Julian Borrill, A. Moneti, M. Reinecke, F. Couchot, R. B. Barreiro, B. Van Tent, L. Popa, Serge Gratton, Jussi-Pekka Väliviita, Tuhin Ghosh, G. Patanchon, A. de Rosa, Hans Ulrik Nørgaard-Nielsen, A. J. Banday, F. Paci, N. Mandolesi, F.-X. Désert, E. Pierpaoli, Yabebal Fantaye, Locke D. Spencer, Andrew H. Jaffe, Philip Lubin, R. Leonardi, M. Sandri, S. Galli, L. Perotto, W. A. Holmes, M. Maris, Davide Maino, A. Chamballu, G. W. Pratt, Gianluca Morgante, D. Yvon, F. Cuttaia, P. B. Lilje, Michael Seiffert, Duncan Hanson, Pavan K. Aluri, Valeria Pettorino, Jacques Delabrouille, J. A. Murphy, R. C. Butler, D. L. Harrison, Fabio Finelli, Anna Bonaldi, Michele Liguori, Erminia Calabrese, E. Franceschi, Adam Moss, P. M. McGehee, Hao Liu, Anne Lähteenmäki, D. Santos, S. Galeotta, Guilaine Lagache, M. López-Caniego, Daniel J. Mortlock, Olivier Forni, I. D. Novikov, M.-A. Miville-Deschênes, P. de Bernardis, M. Tomasi, Marco Bersanelli, C. Rosset, Stéphane Plaszczynski, Michael P. Hobson, G. Prézeau, Yashar Akrami, Anthony Challinor, H. Dole, Subhabrata Mitra, J. A. Tauber, M. Savelainen, J. Aumont, F. K. Hansen, A. Ducout, D. Contreras, Marian Douspis, J. P. Zibin, P. Vielva, G. Hurier, Silvia Masi, B. Casaponsa, Nicola Bartolo, M. Frailis, Carlo Baccigalupi, Kevin M. Huffenberger, François Levrier, E. Hivon, Ingunn Kathrine Wehus, M. Tucci, N. Pant, A.-S. Suur-Uski, J. B. Kim, J.-F. Sygnet, Massimiliano Lattanzi, R. D. Davies, Peter Meinhold, Luca Valenziano, K. Benabed, Fabrizio Villa, J. González-Nuevo, J. R. Bond, E. Gjerløw, Alessandro Gruppuso, J. F. Macías-Pérez, W. C. Jones, Aditya Rotti, M. Bucher, Douglas Scott, Graca Rocha, J.-M. Lamarre, S. Donzelli, Radek Stompor, Giorgio Savini, Mika Juvela, A. Catalano, D. Sutton, Tiziana Trombetti, F. Noviello, Krzysztof M. Gorski, Domenico Marinucci, Hannu Kurki-Suonio, P. R. Christensen, A. Mennella, Nabila Aghanim, David L. Clements, G. Roudier, F. Elsner, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, PLANCK, Ade, P, Aghanim, N, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartlett, J, Bartolo, N, Battaner, E, Battye, R, Benabed, K, Benoit, A, Benoit-Levy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, J, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Bridges, M, Bucher, M, Burigana, C, Butler, R, Cardoso, J, Catalano, A, Challinor, A, Chamballu, A, Chary, R, Chiang, H, Chiang, L, Christensen, P, Church, S, Clements, D, Colombi, S, Colombo, L, Couchot, F, Coulais, A, Crill, B, Cruz, M, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, J, Desert, F, Diego, J, Dole, H, Donzelli, S, Dore, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Ensslin, T, Eriksen, H, Fantaye, Y, Fergusson, J, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Frommert, M, Galeotta, S, Ganga, K, Giard, M, Giardino, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, F, Hansen, M, Hanson, D, Harrison, D, Helou, G, Henrot-Versille, S, Hernandez-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihanen, E, Keskitalo, R, Kim, J, Kisner, T, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Laureijs, R, Lawrence, C, Leahy, J, Leonardi, R, Leroy, C, Lesgourgues, J, Liguori, M, Lilje, P, Linden-Vornle, M, Lopez-Caniego, M, Lubin, P, Macias-Perez, J, Maffei, B, Maino, D, Mandolesi, N, Mangilli, A, Marinucci, D, Maris, M, Marshall, D, Martin, P, Martinez-Gonzalez, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Mcewen, J, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mikkelsen, K, Mitra, S, Miville-Deschenes, M, Molinari, D, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Norgaard-Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Oxborrow, C, Paci, F, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Patanchon, G, Peiris, H, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pogosyan, D, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prezeau, G, Prunet, S, Puget, J, Rachen, J, Racine, B, Rath, C, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Rotti, A, Roudier, G, Rubino-Martin, J, Ruiz-Granados, B, Rusholme, B, Sandri, M, Santos, D, Savini, G, Scott, D, Seiffert, M, Shellard, E, Souradeep, T, Spencer, L, Starck, J, Stolyarov, V, Stompor, R, Sudiwala, R, Sureau, F, Sutter, P, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Turler, M, Valenziano, L, Valiviita, J, Van Tent, B, Varis, J, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, Wehus, I, White, M, Wilkinson, A, Yvon, D, Zacchei, A, Zonca, A, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Universidad de Cantabria, Tauber, Jan, Ade, P. A. R., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., Battye, R., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Challinor, A., Chamballu, A., Chary, R. R., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fantaye, Y., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Frommert, M., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hansen, M., Hanson, D., Harrison, D. L., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kim, J., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leahy, J. P., Leonardi, R., Leroy, C., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mangilli, A., Marinucci, D., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Mcewen, J. D., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mikkelsen, K., Mitra, S., Miville Deschênes, M. A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Peiris, H. V., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pogosyan, D., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Racine, B., Räth, C., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rotti, A., Roudier, G., Rubinõ Martín, J. A., Ruiz Granados, B., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Souradeep, T., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sureau, F., Sutter, P., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wehus, I. K., White, M., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A., Anne Lähteenmäki Group, Department of Electronics and Nanoengineering, Aalto-yliopisto, Aalto University, Department of Physics, Helsinki Institute of Physics, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)
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Data Analysis ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Astronomy ,Cosmic microwave background ,Astrophysics ,cosmic background radiation ,CMB ,Cosmic background radiation ,7. Clean energy ,Cosmology: observation ,Gaussian random field ,HEMISPHERICAL POWER ASYMMETRY ,Statistics ,BACKGROUND ANISOTROPY ,observations [Cosmology] ,Physics ,Cosmology: miscellaneou ,Astrophysics::Instrumentation and Methods for Astrophysics ,CMB cold spot ,Computer Science::Computers and Society ,cosmic background radiation, cosmology: observations, cosmology: miscellaneous ,Physics::Space Physics ,Physical Sciences ,ComputingMethodologies_DOCUMENTANDTEXTPROCESSING ,Kurtosis ,symbols ,WMAP DATA ,astro-ph.CO ,DEPENDENT NON-GAUSSIANITIES ,cosmology: miscellaneous ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics and Astronomy ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,education ,MINKOWSKI FUNCTIONALS ,FOS: Physical sciences ,Copernican Principle ,observation [Cosmology] ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Computer Science::Digital Libraries ,PRIMORDIAL NON-GAUSSIANITY ,NO ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,symbols.namesake ,Settore FIS/05 - Astronomia e Astrofisica ,DIRECTIONAL SPHERICAL WAVELETS ,Cosmology: miscellaneous ,Cosmology: observations ,Astronomy and Astrophysics ,Space and Planetary Science ,Non-Gaussianity ,miscellaneou [Cosmology] ,miscellaneous [Cosmology] ,Forschungsgruppe Komplexe Plasmen ,Planck ,Settore MAT/07 - Fisica Matematica ,Science & Technology ,Astronomy and Astrophysic ,115 Astronomy, Space science ,MICROWAVE-ANISOTROPY-PROBE ,POINT CORRELATION-FUNCTIONS ,Settore MAT/06 - Probabilita' e Statistica Matematica ,0201 Astronomical And Space Sciences ,COLD SPOT ,Skewness ,cosmology: observations ,cosmology - Abstract
The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration. We acknowledge the use of resources from the Norewegian national super computing facilities NOTUR. The modal and KSW bispectrum estimator analysis was performed on the COSMOS supercomputer, part of the STFC DiRAC HPC Facility. We further acknowledge the computer resources and technical assistance provided by the Spanish Supercomputing Network nodes at Universidad de Cantabria and Universidad Politecnica de Madrid as well as by the Advanced Computing and e-Science team at IFCA. Some of the results in this paper have been derived using the HEALPix package., The two fundamental assumptions of the standard cosmological model – that the initial fluctuations are statistically isotropic and Gaussian – are rigorously tested using maps of the cosmic microwave background (CMB) anisotropy from the Planck satellite. The detailed results are based on studies of four independent estimates of the CMB that are compared to simulations using a fiducial ΛCDM model and incorporating essential aspects of the Planck measurement process. Deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask choice, and frequency dependence. Many of these anomalies were previously observed in the WMAP data, and are now confirmed at similar levels of significance (about 3σ). However, we find little evidence of non-Gaussianity, with the exception of a few statistical signatures that seem to be associated with specific anomalies. In particular, we find that the quadrupole-octopole alignment is also connected to a low observed variance in the CMB signal. A power asymmetry is now found to persist on scales corresponding to about ‘ = 600 and can be described in the low-‘ regime by a phenomenological dipole modulation model. However, any primordial power asymmetry is strongly scale-dependent and does not extend to arbitrarily small angular scales. Finally, it is plausible that some of these features may be reflected in the angular power spectrum of the data, which shows a deficit of power on similar scales. Indeed, when the power spectra of two hemispheres defined by a preferred direction are considered separately, one shows evidence of a deficit in power, while its opposite contains oscillations between odd and even modes that may be related to the parity violation and phase correlations also detected in the data. Although these analyses represent a step forward in building an understanding of the anomalies, a satisfactory explanation based on physically motivated models is still lacking., European Space Agency, Centre National D'etudes Spatiales, CNRS/INSU-IN2P3-INP (France), Italian Space Agency (ASI), Italian National Research Council, Istituto Nazionale Astrofisica (INAF), National Aeronautics & Space Administration (NASA), United States Department of Energy (DOE), UKSA (UK), Consejo Superior de Investigaciones Cientificas (CSIC), Spanish Government, JA (Spain), RES (Spain), Finnish Funding Agency for Technology & Innovation (TEKES), AoF (Finland), CSC (Finland), Helmholtz Association, German Aerospace Centre (DLR), Max Planck Society, CSA (Canada), DTU Space (Denmark), SER/SSO (Switzerland), RCN (Norway), Science Foundation Ireland, Portuguese Foundation for Science and Technology, European Union (EU), Science & Technology Facilities Council (STFC) ST/G003874/1 ST/H008586/1 ST/K003674/1 ST/L001314/1 ST/M007685/1 ST/I005765/1 ST/K000985/1 ST/K002899/1 ST/K001051/1 ST/J000388/1 ST/I002006/1 ST/J005673/1 ST/H001239/1 ST/J001368/1 ST/K004131/1 ST/K00333X/1 ST/L000768/1 ST/K002805/1 ST/K000977/1 ST/J004812/1
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- 2014
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23. Defining Photometric Peculiar Type Ia Supernovae
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Lluís Galbany, Claudia P. Gutiérrez, F. Forster, Gastón Folatelli, Filomena Bufano, Santiago González-Gaitán, Mario Hamuy, Mark M. Phillips, Giuliano Pignata, T. de Jaeger, Joseph P. Anderson, and Eric Hsiao
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Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,education.field_of_study ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Ciencias Físicas ,Population ,MISCELLANEOUS [COSMOLOGY] ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,01 natural sciences ,Wide field ,GENERAL [SUPERNOVAE] ,Astronomía ,Supernova ,Space and Planetary Science ,0103 physical sciences ,Astrophysics - High Energy Astrophysical Phenomena ,education ,Maxima ,010303 astronomy & astrophysics ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present a new photometric identification technique for SN 1991bg-like type Ia supernovae (SNe Ia), i.e. objects with light-curve characteristics such as later primary maxima and absence of secondary peak in redder filters. This method is capable of selecting out this sub-group from the normal type Ia population. Furthermore, we find that recently identified peculiar sub-types such as SNe Iax and super-Chandrasekhar SNe Ia have similar photometric characteristics as 91bg-like SNe Ia, namely the absence of secondary maxima and shoulders at longer wavelengths, and can also be classified with our technique. The similarity of these different SN Ia sub-groups perhaps suggests common physical conditions. This typing methodology permits the photometric identification of peculiar SNe Ia in large up-coming wide field surveys either to study them further or to obtain a pure sample of normal SNe Ia for cosmological studies., Comment: 28 pages, 12 figures, 4 tables
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- 2014
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24. New cosmological constraints on the variation of fundamental constants: the fine structure constant and the Higgs vacuum expectation value
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Osvaldo Civitarese and M. E. Mosquera
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Physics ,Ciencias Astronómicas ,Ciencias Físicas ,Cosmology: miscellaneous ,Primordial nucleosynthesis ,Null (mathematics) ,Cosmological parameters ,Astronomy and Astrophysics ,Observable ,Fine-structure constant ,purl.org/becyt/ford/1.3 [https] ,Astrophysics ,Otras Ciencias Físicas ,CMB cold spot ,purl.org/becyt/ford/1 [https] ,Big Bang nucleosynthesis ,Space and Planetary Science ,Nucleosynthesis ,Higgs boson ,miscellaneous [Cosmology] ,CIENCIAS NATURALES Y EXACTAS ,Vacuum expectation value - Abstract
Aims. We study the time variation of the fine structure constant, α, and the Higgs vacuum expectation value v, during the Big Bang nucleosynthesis (BBN). Methods. We computed primordial abundances of light nuclei produced during the BBN stage by including resonances in the leading reaction rates which reduce the primordial abundance of beryllium. We performed this calculation considering that α and v may vary during the BBN. Using observable data on deuterium, 4He, and 7Li, we set constraints on the variation of the fundamental constants. Results. Results indicate a null variation of α and v, while the best-fit value for the baryon-to-photon ratio agrees well with the WMAP value. Conclusions. We found that the variation of α is null within 3σ, the variation of v is null within 6σ, and the preferred value of the baryon-to-photon ratio is in good agreement, within 3σ, with the value extracted using the WMAP data. We improve the fits respect to previous works., Facultad de Ciencias Astronómicas y Geofísicas
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- 2013
25. The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths
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F. Dodu, S. Leach, J. P. Bernard, S. Ricciardi, L. Toffolatti, B. M. Schaefer, Soumen Basak, François R. Bouchet, A. Da Silva, M. Ashdown, Simon Prunet, Bruce Partridge, G. de Zotti, A. J. Banday, Klaus Dolag, J. Lesgourgues, Marc-Antoine Miville-Deschênes, Matthieu Roman, Roberta Paladini, M. Le Jeune, Jean-Baptiste Melin, Sabino Matarrese, S. Mottet, J. González-Nuevo, Clive Dickinson, R. Piffaretti, Michele Liguori, Franz Elsner, Carlo Baccigalupi, J. F. Macías-Pérez, G. Castex, G. Giardino, Marc Betoule, David L. Clements, Pasquale Mazzotta, J. Aumont, Gilles Faÿ, Marcella Massardi, G. Prézeau, Jacques Delabrouille, L. A. Montier, L. Fauvet, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Planck, European Research Council, Science and Technology Facilities Council (UK), APC - Gravitation (APC-Gravitation), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Mathématiques Appliquées aux Systèmes - EA 4037 (MAS), Ecole Centrale Paris, Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PLANCK, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)
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Astrophysics and Astronomy ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Point source ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,media_common.quotation_subject ,Astrophysics::High Energy Astrophysical Phenomena ,Cosmic microwave background ,radio continuum: general ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,cosmic background radiation ,general [Submillimeter] ,Cosmic background radiation ,01 natural sciences ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,symbols.namesake ,Settore FIS/05 - Astronomia e Astrofisica ,Cosmic infrared background ,0103 physical sciences ,miscellaneous [Cosmology] ,Planck ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,ISM: general ,Physics ,general [ISM] ,010308 nuclear & particles physics ,Spinning dust ,general [Radio continuum] ,Astrophysics::Instrumentation and Methods for Astrophysics ,Spectral density ,Astronomy and Astrophysics ,submillimeter: general ,general [Galaxies] ,galaxies: general ,Galaxy ,Cosmology ,Miscellaneous ,Cosmology: miscellaneous ,Galaxies: general ,Radio continuum: general ,Submillimeter: general ,Space and Planetary Science ,Sky ,cosmology: miscellaneous, radio continuum: general, submillimeter: general, cosmic background radiation, ISM: general, galaxies: general ,symbols ,cosmology: miscellaneous ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
J. Delabrouille et al., We present the Planck Sky Model (PSM), a parametric model for generating all-sky, few arcminute resolution maps of sky emission at submillimetre to centimetre wavelengths, in both intensity and polarisation. Several options are implemented to model the cosmic microwave background, Galactic diffuse emission (synchrotron, free-free, thermal and spinning dust, CO lines), Galactic H ii regions, extragalactic radio sources, dusty galaxies, and thermal and kinetic Sunyaev-Zeldovich signals from clusters of galaxies. Each component is simulated by means of educated interpolations/extrapolations of data sets available at the time of the launch of the Planck mission, complemented by state-of-the-art models of the emission. Distinctive features of the simulations are spatially varying spectral properties of synchrotron and dust; different spectral parameters for each point source; modelling of the clustering properties of extragalactic sources and of the power spectrum of fluctuations in the cosmic infrared background. The PSM enables the production of random realisations of the sky emission, constrained to match observational data within their uncertainties. It is implemented in a software package that is regularly updated with incoming information from observations. The model is expected to serve as a useful tool for optimising planned microwave and sub-millimetre surveys and testing data processing and analysis pipelines. It is, in particular, used to develop and validate data analysis pipelines within the Planck collaboration. A version of the software that can be used for simulating the observations for a variety of experiments is made available on a dedicated website. © 2013 ESO., SB has been supported by a postdoctoral grant from the “Physique des deux Infinis” (P2I) Consortium. CD acknowledges an STFC Advanced Fellowship and an ERC IRG grant under the FP7.
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- 2013
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26. Environment dependence of dark matter halos in symmetron modified gravity
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Hans A. Winther, Baojiu Li, and David F. Mota
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High Energy Physics - Theory ,Gravity (chemistry) ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,General relativity ,media_common.quotation_subject ,Dark matter ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Cosmology ,General Relativity and Quantum Cosmology ,Gravitation ,High Energy Physics - Phenomenology (hep-ph) ,Large-scale structure of Universe ,theory [Cosmology] ,0103 physical sciences ,miscellaneous [Cosmology] ,010303 astronomy & astrophysics ,media_common ,Physics ,010308 nuclear & particles physics ,Fifth force ,Astronomy and Astrophysics ,Universe ,Dark matter halo ,High Energy Physics - Phenomenology ,High Energy Physics - Theory (hep-th) ,Space and Planetary Science ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We investigate the environment dependence of dark matter halos in the symmetron modified gravity scenario. The symmetron is one of three known mechanisms for screening a fifth-force and thereby recovering General Relativity in dense environments. The effectiveness of the screening depends on both the mass of the object and the environment it lies in. Using high-resolution N-body simulations we find a significant difference, which depends on the halos mass and environment, between the lensing and dynamical masses of dark matter halos similar to the f(R) modified gravity. The symmetron can however yield stronger signatures due to a freedom in the strength of the coupling to matter., 10 pages, 5 figures
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- 2012
27. AzTEC half square degree survey of the SHADES fields - II. Identifications, redshifts, and evidence for large-scale structure
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Michalowski, Michal J., Dunlop, J. S., Ivison, R. J., Cirasuolo, M., Caputi, K. I., Aretxaga, I., Arumugam, V., Austermann, J. E., Chapin, E. L., Chapman, S. C., Coppin, K. E. K., Egami, E., Hughes, D. H., Ibar, E., Mortier, A. M. J., Schael, A. M., Scott, K. S., Smail, I., Targett, T. A., Wagg, J., Wilson, G. W., Xu, L., Yun, M., and Astronomy
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ACTIVE GALACTIC NUCLEI ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,PARKES SELECTED REGIONS ,FOS: Physical sciences ,HUBBLE-DEEP-FIELD ,SPECTRAL ENERGY-DISTRIBUTIONS ,miscellaneous [cosmology] ,galaxies: high-redshift ,SUBMILLIMETER-SELECTED GALAXIES ,galaxies [submillimetre] ,STAR-FORMING GALAXIES ,evolution [galaxies] ,SPITZER-SPACE-TELESCOPE ,DEGREE EXTRAGALACTIC SURVEY ,Astronomy and Astrophysics ,1200-MU-M MAMBO SURVEY ,stellar content [galaxies] ,Space and Planetary Science ,galaxies: stellar content ,GOODS-N FIELD ,distances and redshifts [galaxies] ,galaxies: distances and redshifts ,cosmology: miscellaneous ,galaxies: evolution ,submillimetre: galaxies ,high-redshift [galaxies] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The AzTEC 1.1 mm survey of the SCUBA HAlf Degree Extragalactic Survey (SHADES) fields is the largest (0.7 deg2) blank-field millimetre-wavelength survey undertaken to date at a resolution of ~18" and a depth of ~1 mJy. We have used the deep optical-to-radio multi-wavelength data in the SHADES Lockman Hole East and SXDF/UDS fields to obtain galaxy identifications for ~64% (~80% with tentative identifications) of the 148 AzTEC-SHADES 1.1 mm sources, exploiting deep radio and 24 um data complemented by methods based on 8 um flux-density and red optical-infrared (i-K) colour. This unusually high identification rate can be attributed to the relatively bright millimetre-wavelength flux-density threshold, combined with the relatively deep supporting multi-frequency data. We have further exploited the optical-mid-infrared-radio data to derive a ~60% (~75% with tentative identifications) complete redshift distribution for the AzTEC-SHADES sources, yielding a median redshift of z~2.2, with a high-redshift tail extending to at least z~4. Despite the larger area probed by the AzTEC survey relative to the original SCUBA SHADES imaging, the redshift distribution of the AzTEC sources is consistent with that displayed by the SCUBA sources, and reinforces tentative evidence that the redshift distribution of mm/sub-mm sources in the Lockman Hole field is significantly different from that found in the SXDF/UDS field. Comparison with simulated surveys of similar scale extracted from semi-analytic models based on the Millennium simulation indicates that this is as expected if the mm/sub-mm sources are massive (M>10^11 Mo) star-forming galaxies tracing large-scale structures over scales of 10-20 Mpc. This confirms the importance of surveys covering several square degrees (as now underway with SCUBA2) to obtain representative samples of bright (sub)mm-selected galaxies., Accepted to MNRAS. 15 pages (+38 as appendix), 10 figures, 7 tables. Machine-readable versions of tables B1-B4 are available as 'Ancillary files' and from the source file. V2: added the ID success rate separately for each method; added a discussion on the distribution of the ID separation; added the category flag and the 'best ID' flag in the machine readable files; some minor changes
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- 2012
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28. Large-scale gas dynamics in the adhesion model: Implications for the two-phase massive galaxy formation scenario
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Dom��nguez-Tenreiro, R., O��orbe, J., Mart��nez-Serrano, F., Serna, A., and UAM. Departamento de Física Teórica
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Galaxies: star formation ,Cosmology: miscellaneous ,Galaxies: high-redshift ,FOS: Physical sciences ,Física ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Galaxies: formation ,formation [Galaxies] ,star formation [Galaxies] ,high-redshift [Galaxies] ,theory [Cosmology] ,Hydrodynamics ,miscellaneous [Cosmology] ,Cosmology: theory ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2011 RAS © 2011 The AuthorsPublished by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved, We have studied the mass assembly and star formation histories of massive galaxies identified at low redshift in different cosmological hydrodynamical simulations. To this end, we have carried out a detailed follow-up backwards in time of their constituent mass elements (sampled by particles) of different types. After that, the configurations they depict at progressively higher zs were carefully analysed. The analyses show that these histories share common generic patterns, irrespective of particular circumstances. In any case, however, the results we have found are different depending on the particle type. The most outstanding differences follow. We have found that by z∼ 3.5-6, mass elements identified as stellar particles at z= 0 exhibit a gaseous cosmic-web-like morphology with scales of ∼1 physical Mpc, where the densest mass elements have already turned into stars by z∼ 6. These settings are in fact the densest pieces of the cosmic web, where no hot particles show up, and dynamically organized as a hierarchy of flow convergence regions (FCRs), that is, attraction basins for mass flows. At high z FCRs undergo fast contractive deformations with very low angular momentum, shrinking them violently. Indeed, by z∼ 1 most of the gaseous or stellar mass they contain shows up as bound to a massive elliptical-like object at their centres, with typical half-mass radii of rmass star∼ 2-3kpc. After this, a second phase comes about where the mass assembly rate is much slower and characterized by mergers involving angular momentum. On the other hand, mass elements identified at the diffuse hot coronae surrounding massive galaxies at z= 0 do not display a clear web-like morphology at any z. Diffuse gas is heated when FCRs go through contractive deformations. Most of this gas remains hot and with low density throughout the evolution. To shed light on the physical foundations of the behaviour revealed by our analyses (i.e. a two-phase formation process with different implications for diffuse or shocked mass elements), as well as on their possible observational implications, these patterns have been confronted with some generic properties of singular flows as described by the adhesion model (i.e. potential character of the velocity field, singular versus regular points, dressing, locality when a spectrum of perturbations is implemented). We have found that the common patterns the simulations show can be interpreted as a natural consequence of flow properties that, moreover, could explain different generic observational results from massive galaxies or their samples. We briefly discuss some of them, This work was partially supported by the DGES (Spain) through the grants AYA2009-12792-C03-02 and AYA2009-12792- C03-03 from the PNAyA, as well as by the regional Madrid V PRICIT programme through the ASTROMADRID network (CAM S2009/ESP-1496)
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- 2011
29. Structure Formation in the Symmetron Model
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Anne-Christine Davis, Hans A. Winther, David F. Mota, and Baojiu Li
- Subjects
Structure formation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Scalar (mathematics) ,FOS: Physical sciences ,Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,01 natural sciences ,General Relativity and Quantum Cosmology ,High Energy Physics - Phenomenology (hep-ph) ,Large-scale structure of Universe ,theory [Cosmology] ,0103 physical sciences ,miscellaneous [Cosmology] ,Symmetry breaking ,010303 astronomy & astrophysics ,Physics ,010308 nuclear & particles physics ,Matter power spectrum ,Halo mass function ,Fifth force ,Astronomy and Astrophysics ,Observable ,Nonlinear system ,High Energy Physics - Phenomenology ,Classical mechanics ,Space and Planetary Science ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Scalar fields, strongly coupled to matter, can be present in nature and still be invisible to local experiments if they are subject to a screening mechanism. The symmetron is one such mechanism which relies on restoration of a spontaneously broken symmetry in regions of high density to shield the scalar fifth force. We have investigated structure formation in the symmetron model by using N-body simulations and find strong observable signatures in both the linear and nonlinear matter power spectrum and on the halo mass function. The mechanism for suppressing the scalar fifth force in high density regions is also found to work very well., Comment: 18 pages, 15 figures
- Published
- 2011
- Full Text
- View/download PDF
30. Haloes gone MAD: The Halo-Finder Comparison Project
- Author
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Knebe, Alexander, Knollmann, Steffen R., Muldrew, Stuart I., Pearce, Frazer R., Aragon-Calvo, Miguel Angel, Ascasibar, Yago, Behroozi, Peter S., Ceverino, Daniel, Colombi, Stephane, Diemand, Juerg, Dolag, Klaus, Falck, Bridget L., Fasel, Patricia, Gardner, Jeff, Gottlöber, Stefan, Hsu, Chung Hsing, Iannuzzi, Francesca, Klypin, Anatoly, Lukić, Zarija, Maciejewski, Michal, Mcbride, Cameron, Neyrinck, Mark, Planelles, Susana, Potter, Doug, Quilis, Vicent, Rasera, Yann, Read, Justin I., Ricker, Paul M., Roy, Fabrice, Springel, Volker, Stadel, Joachim, Stinson, Greg, Sutter, Philip, Turchaninov, Victor, Tweed, Dylan, Yepes, Gustavo, Zemp, Marcel, Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), UAM. Departamento de Física Teórica, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
- Subjects
numerical [Methods] ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Methods: numerical ,haloes [Galaxies] ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Cosmology: miscellaneous ,Galaxies: evolution ,Física ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,evolution [Galaxies] ,theory [Cosmology] ,Dark matter ,miscellaneous [Cosmology] ,Cosmology: theory ,Galaxies: haloes ,ComputingMilieux_MISCELLANEOUS ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2011 RAS © 2011 The authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved, We present a detailed comparison of fundamental dark matter halo properties retrieved by a substantial number of different halo finders. These codes span a wide range of techniques including friends-of-friends, spherical-overdensity and phase-space-based algorithms. We further introduce a robust (and publicly available) suite of test scenarios that allow halo finder developers to compare the performance of their codes against those presented here. This set includes mock haloes containing various levels and distributions of substructure at a range of resolutions as well as a cosmological simulation of the large-scale structure of the universe. All the halo-finding codes tested could successfully recover the spatial location of our mock haloes. They further returned lists of particles (potentially) belonging to the object that led to coinciding values for the maximum of the circular velocity profile and the radius where it is reached. All the finders based in configuration space struggled to recover substructure that was located close to the centre of the host halo, and the radial dependence of the mass recovered varies from finder to finder. Those finders based in phase space could resolve central substructure although they found difficulties in accurately recovering its properties. Through a resolution study we found that most of the finders could not reliably recover substructure containing fewer than 30-40 particles. However, also here the phase-space finders excelled by resolving substructure down to 10-20 particles. By comparing the halo finders using a high-resolution cosmological volume, we found that they agree remarkably well on fundamental properties of astrophysical significance (e.g. mass, position, velocity and peak of the rotation curve). We further suggest to utilize the peak of the rotation curve, vmax, as a proxy for mass, given the arbitrariness in defining a proper halo edge, We are greatly indebted to the ASTROSIM network of the European Science Foundation (Science Meeting 2910) for financially supporting the workshop ‘Haloes going MAD’ held in Miraflores de la Sierra near Madrid in 2010 May where all of this work was initiated.AK is supported by the Spanish Ministerio de Ciencia e Innovación (MICINN) in Spain through the Ramón y Cajal programme as well as the grants AYA 2009-13875-C03-02, AYA2009- 12792-C03-03, CSD2009-00064 and CAM S2009/ESP-1496. SRK acknowledges the support by the MICINN under the Consolider-Ingenio, SyeC project CSD-2007-00050. SP and VQ have also been supported by the MICINN (grants AYA2010-21322-C03-01 and CONSOLIDER2007-00050) and the Generalitat Valenciana (grant PROMETEO-2009-103). MZ is supported by NSF grant AST-0708087. GY acknowledges financial support from MICINN (Spain) under project AYA 2009-13875-C03-02 and the ASTROMADRID project S2009/ESP-1496 financed by Comunidad de Madrid
- Published
- 2011
- Full Text
- View/download PDF
31. Varying alpha from N-body Simulations
- Author
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Baojiu Li, John D. Barrow, and David F. Mota
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Dark matter ,FOS: Physical sciences ,Large-scale structure of universe ,Perturbation (astronomy) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Cosmology ,High Energy Physics - Phenomenology (hep-ph) ,0103 physical sciences ,miscellaneous [Cosmology] ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Physics ,010308 nuclear & particles physics ,Numerical analysis ,Astronomy and Astrophysics ,Fine-structure constant ,Computational physics ,High Energy Physics - Phenomenology ,Space and Planetary Science ,numerical. [Methods] ,Halo ,Constant (mathematics) ,Scalar field ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We have studied the Bekenstein-Sandvik-Barrow-Magueijo (BSBM) model for the spatial and temporal variations of the fine structure constant, alpha, with the aid of full N-body simulations which explicitly and self-consistently solve for the scalar field driving the alpha-evolution. We focus on the scalar field (or equivalently alpha) inside the dark matter halos and find that the profile of the scalar field is essentially independent of the BSBM model parameter. This means that given the density profile of an isolated halo and the background value of the scalar field, we can accurately determine the scalar field perturbation in that halo. We also derive an analytic expression for the scalar-field perturbation using the Navarro-Frenk-White halo profile, and show that it agrees well with numerical results, at least for isolated halos; for non-isolated halos this prediction differs from numerical result by a (nearly) constant offset which depends on the environment of the halo., 11 pages, 6 figures
- Published
- 2010
32. AzTEC Half Square Degree Survey of the SHADES Fields -- I. Maps, Catalogues, and Source Counts
- Author
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Ian Smail, Steve Rawlings, Stephen Serjeant, John A. Peacock, Eiichi Egami, D. Ferrusca, Dave Clements, Michele Cirasuolo, E. van Kampen, M. S. Yun, Omar Almaini, James D. Lowenthal, Jamie Stevens, Edward L. Chapin, Jeff Wagg, Isaac Roseboom, A. M. Swinbank, Duncan Farrah, Rob Ivison, Philip Daniel Mauskopf, Ross J. McLure, Simon Dye, Loretta Dunne, Sungeun Kim, Itziar Aretxaga, James Dunlop, M. Rowan-Robinson, Seb Oliver, Kimberly S. Scott, Mark Halpern, Mattia Negrello, David H. Hughes, D. Haig, Stephen Anthony Eales, Edo Ibar, A. Pope, Kristen Coppin, Scott Chapman, George H. Rieke, Grant W. Wilson, Cedric G. Lacey, A. M. J. Mortier, Douglas Scott, Jason E. Austermann, Thushara Perera, Young Woon Kang, M. Velázquez, and S. Flynn
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Hubble Deep Field ,Continuum (design consultancy) ,FOS: Physical sciences ,Astrophysics ,Surveys ,01 natural sciences ,0103 physical sciences ,Galaxy formation and evolution ,miscellaneous [Cosmology] ,Submillimetre ,Source counts ,010303 astronomy & astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,James Clerk Maxwell Telescope ,QB ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Cosmic variance ,evolution [Galaxies] ,Galaxy ,Square degree ,Space and Planetary Science ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present the first results from the largest deep extragalactic millimetre-wavelength survey undertaken to date. These results are derived from maps covering over 0.7 deg^2, made at 1.1mm, using the AzTEC continuum camera mounted on the James Clerk Maxwell Telescope. The maps were made in the two fields originally targeted at 0.85mm with SCUBA in the SHADES project, namely the Lockman Hole East (mapped to a depth of 0.9-1.3 mJy rms) and the Subaru XMM Deep Field (1.0-1.7 mJy rms). The wealth of existing and forthcoming deep multi-frequency data in these two fields will allow the bright mm source population revealed by these images to be explored in detail in subsequent papers. Here we present the maps themselves, a catalogue of 114 high-significance sub-millimetre galaxy detections, and a thorough statistical analysis leading to the most robust determination to date of the 1.1mm source number counts. Through careful comparison, we find that both the COSMOS and GOODS North fields, also imaged with AzTEC, contain an excess of mm sources over the new 1.1mm source-count baseline established here. In particular, our new AzTEC/SHADES results indicate that very luminous high-redshift dust enshrouded starbursts (S_{1.1} > 3 mJy) are 25-50% less common than would have been inferred from these smaller surveys, thus highlighting the potential roles of cosmic variance and clustering in such measurements. We compare number count predictions from recent models of the evolving mm/sub-mm source population to these SMG surveys, which provide important constraints for the ongoing refinement of semi-analytic and hydrodynamical models of galaxy formation, and find that all recent models over-predict the number of bright sub-millimetre galaxies found in this survey., 19 pages, 10 figures, 7 tables - Very minor revisions; accepted for publication in MNRAS
- Published
- 2009
33. A Short Answer to Critics of Our Article 'Eppur si Espande'
- Author
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Abramowicz, M. A., Bajtlik, S., Jean-Pierre Lasota, Moudens, A., Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Department of Applied Physics [Gothenburg], Chalmers University of Technology [Göteborg], Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astrochimie expérimentale, Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS)-Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), and Destouches, Dorothée
- Subjects
theory [cosmology] ,[PHYS.ASTR.SR] Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] ,[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] ,Cosmology: miscellaneous ,[SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmology: theory ,miscellaneous [cosmology] ,[PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR] - Abstract
International audience; Recently we presented a formal mathematical proof that, contrary to a widespread misconception, cosmological expansion cannot be understood as the motion of galaxies in non-expanding space. We showed that the cosmological redshift must be physically interpreted as the expansion of space. Although our proof was generally accepted, a few authors disagreed. We rebut their criticism in this Note.
- Published
- 2009
34. The time variation of the fine structure constant: A statistical analysis of astronomical data
- Author
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Landau, S.J. and Simeone, C.
- Subjects
absorption lines [Quasars] ,Mean values ,Statistical analysis ,Astronomical data ,Confidence intervals ,Testing ,Financial data processing ,miscellaneous [Cosmology] ,Time variations ,Data sets ,Ketones ,observations [Cosmology] ,Fine structure constants - Abstract
Aims. We analyze different data of the variation of the fine structure constant obtained with different methods to check their consistency.Methods. We test consistency using the modified student test and confidence intervals. We split the data sets into smaller intervals. A criterion for this selection is proposed.Results. Results show consistency for reduced intervals for each pair of data sets considered.Conclusions. Results are at variance with the ones obtained considering mean values over the whole interval. © 2008 ESO. Fil:Landau, S.J. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Simeone, C. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
- Published
- 2008
35. The $\Lambda$ CDM model in the lead : a Bayesian cosmological model comparison
- Author
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Marek Szydłowski and Aleksandra Kurek
- Subjects
Physics ,media_common.quotation_subject ,Cosmic microwave background ,Bayesian probability ,statistical [methods] ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,miscellaneous [cosmology] ,Bayesian inference ,Universe ,Lead (geology) ,Space and Planetary Science ,Statistical analysis ,Statistical physics ,cosmological parameters ,Accelerating universe ,media_common - Abstract
Recent astronomical observations indicate that our Universe is undergoing a period of an accelerated expansion. While there are many cosmological models, which explain this phenomenon, the main question remains which is the best one in the light of available data. We consider ten cosmological models of the accelerating Universe and select the best one using the Bayesian model comparison method. We demonstrate that the LambdaCDM model is most favored by the Bayesian statistical analysis of the SNIa, CMB, BAO and H(z) data.
- Published
- 2008
36. Spatial energy spectrum of primordial magnetic fields
- Author
-
Grazyna Siemieniec-Ozieblo
- Subjects
Physics ,theory [cosmology] ,Structure formation ,media_common.quotation_subject ,Astrophysics (astro-ph) ,Spectrum (functional analysis) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,miscellaneous [cosmology] ,Universe ,Magnetic field ,Gravitation ,Space and Planetary Science ,Energy spectrum ,Radiative transfer ,Excitation ,media_common - Abstract
Here, we analyze the primordial magnetic field transition between a radiative and a matter-dominated universe. The gravitational structure formation affects its evolution and energy spectrum. The structure excitation can trigger magnetic field amplification and the steepening of its energy density spectrum., 8 pages, 2 figures, accepted for A&A
- Published
- 2004
37. Magnetized cosmic walls
- Author
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G. Siemieniec-Ozieblo and A. Woszczyna
- Subjects
Physics ,COSMIC cancer database ,theory [cosmology] ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Champ magnetique ,Astrophysics ,miscellaneous [cosmology] ,Cosmology ,Magnetic field ,Nonlinear system ,Space and Planetary Science ,Quantum electrodynamics ,Newtonian fluid ,Vector field - Abstract
Nonlinear growth of one-dimensional density structures with a frozen-in magnetic field is investigated in Newtonian cosmology. A mechanism of magnetic field amplification is discussed. We discuss the relation between the initial conditions for the velocity field and the basic time-scales determining the growth of the magnetized structure., Comment: 7 pages, 3 figures included; A&A accepted
- Published
- 2004
38. Magnetic amplification in cylindrical cosmological structure
- Author
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G. Siemieniec-Ozieblo and Z. A. Golda
- Subjects
Physics ,theory [cosmology] ,Astrophysics (astro-ph) ,Structure (category theory) ,Phase (waves) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,miscellaneous [cosmology] ,Magnetic field ,Gravitation ,Nonlinear system ,Space and Planetary Science ,Quantum electrodynamics ,Magnetohydrodynamic drive - Abstract
We derive the amplification of the cosmological magnetic field associated with forming gravitational structure. The self-similar solutions of magnetohydrodynamic equations are computed both in linear and nonlinear regimes. We find that the relatively fast magnetic field enhancement becomes substantial in the nonlinear phase., Comment: 10 pages, 4 figures included; accepted to A&A
- Published
- 2004
39. NONPARAMETRIC STUDY OF THE EVOLUTION OF THE COSMOLOGICAL EQUATION OF STATE WITH SNeIa, BAO, AND HIGH-REDSHIFT GRBs
- Author
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Salvatore Capozziello, Maria Giovanna Dainotti, Sergey Postnikov, Xavier Hernandez, S., Postnikov, M. G., Dainotti, X., Hernandez, and Capozziello, Salvatore
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics::High Energy Astrophysical Phenomena ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmological constant ,Astrophysics ,miscellaneous [cosmology] ,01 natural sciences ,Omega ,dark matter ,symbols.namesake ,Friedmann–Lemaître–Robertson–Walker metric ,0103 physical sciences ,cosmological parameters ,dark energy ,010303 astronomy & astrophysics ,media_common ,Physics ,theory [cosmology] ,010308 nuclear & particles physics ,Equation of state (cosmology) ,Astronomy and Astrophysics ,observations [cosmology] ,Redshift ,Universe ,Space and Planetary Science ,Dark energy ,symbols ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Hubble's law - Abstract
We study the dark energy equation of state as a function of redshift in a non-parametric way, without imposing any {\it a priori} $w(z)$ (ratio of pressure over energy density) functional form. As a check of the method, we test our scheme through the use of synthetic data sets produced from different input cosmological models which have the same relative errors and redshift distribution as the real data. Using the luminosity-time $L_{X}-T_{a}$ correlation for GRB X-ray afterglows (the Dainotti et al. correlation), we are able to utilize GRB sample from the {\it Swift} satellite as probes of the expansion history of the Universe out to $z \approx 10$. Within the assumption of a flat FLRW universe and combining SNeIa data with BAO constraints, the resulting maximum likelihood solutions are close to a constant $w=-1$. If one imposes the restriction of a constant $w$, we obtain $w=-0.99 \pm 0.06$ (consistent with a cosmological constant) with the present day Hubble constant as $H_{0}=70.0 \pm 0.6$ ${\rm km} \, {\rm s}^{-1} {\rm Mpc}^{-1}$ and density parameter as $\Omega_{\Lambda 0}=0.723 \pm 0.025$, while non-parametric $w(z)$ solutions give us a probability map which is centred at $H_{0}=70.04 \pm 1$ ${\rm km} \, {\rm s}^{-1} {\rm Mpc}^{-1}$ and $\Omega_{\Lambda 0}=0.724 \pm 0.03$. Our chosen GRB data sample with full correlation matrix allows us to estimate the amount, as well as quality (errors) of data, needed to constrain $w(z)$ in the redshift range extending an order of magnitude in beyond the farthest SNeIa measured., Comment: 17 pages, 13 figures, accepted for publication in the ApJ
- Published
- 2014
- Full Text
- View/download PDF
40. Acoustic instabilities at the transition from the radiation-dominated to the matter-dominated universe
- Author
-
Andrzej Woszczyna and Grazyna Siemieniec-Ozieblo
- Subjects
Physics ,Propagation equation ,Stochastic field ,theory [cosmology] ,Gravitational wave ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Decoupling (cosmology) ,Astrophysics ,Radiation ,miscellaneous [cosmology] ,Space and Planetary Science ,Quantum electrodynamics ,Sound wave ,large-scale structure of the universe [cosmology] - Abstract
The transition from acoustic noise in the radiation-dominated universe to the density structures in the matter dominated epoch is considered. The initial state is a stochastic field of sound waves moving in different directions. The construction of the initial state is compatible with the hyperbolic type of propagation equation for density perturbations, and parallel to the theory of stochastic background of gravitational waves. Instantaneous transition between the cosmological epochs is assumed, and Darmois-Israel joining conditions are applied to match solutions for sound waves with growing or decaying modes at the decoupling. As a result a substantial amplification of the low scale structures is obtained., Comment: 11 pages, 6 figures, accepted to A&A
- Published
- 2001
- Full Text
- View/download PDF
41. News (νs) on the Galactic evolution of lithium
- Author
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MATTEUCCI, MARIA FRANCESCA, D'Antona, F., Timmes, F. X., Matteucci, MARIA FRANCESCA, D'Antona, F., and Timmes, F. X.
- Subjects
NUCLEOSYNTHESIS ,GALAXY: ABUNDANCES ,EVOLUTION ,COSMOLOGY: MISCELLANEOUS ,ABUNDANCES [GALAXY] ,MISCELLANEOUS [COSMOLOGY] - Abstract
Galactic chemical evolution models are presented that take into account several recent developments: (1) models of classical novae nucleosynthesis question the total amount of ^7^Li produced by these systems; (2) observations and models for lithium production in asymptotic giant branch stars and the mass of the planetary nebula that they eject; (3) ^7^Li production from ν-process nucleosynthesis in Type II supernova explosions. The best fitting models for the upper envelope of the observed N(Li) as a function of [Fe/H] suggest that Type II supernovae and intermediate-low mass stars each produce about 1/2 of the solar lithium abundance, although fractions between 1/4 to 3/4 for each source are not conclusively ruled out. The variance of these fractions primarily reflect the uncertainties in the input nucleosynthesis.
- Published
- 1995
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