184 results on '"Planck temperature"'
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2. Temperature of the Surface of Powders in Experiments with Chain Plasma-Chemical Reactions Initiated by the Radiation of a Gyrotron in Pd + Al2O3 Mixtures
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Voronova, E. V., Knyazev, A. V., Letunov, A. A., Logvinenko, V. P., Skvortsova, N. N., and Stepakhin, V. D.
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- 2021
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3. Variation of the speed of light and a minimum speed in the scenario of an inflationary universe with accelerated expansion.
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Cruz, Cláudio Nassif and da Silva, Fernando Antônio
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Abstract In this paper we aim to investigate a deformed relativistic dynamics so-called Symmetrical Special Relativity (SSR) with a universal minimum speed related to a cosmic background field that plays the role of a variable vacuum energy density associated to the temperature of the expanding universe with a cosmic inflation in its early time and an accelerated expansion for its very far future time. In this scenario, we show that both the speed of light and the universal minimum speed present an explicit dependence on the background temperature of the expanding universe. Although finding both the speed of light and the minimum speed in the early universe with very high temperature and also in the very old one with very low temperature being respectively much larger and much smaller than its current value, our approach does not violate the postulates of SSR which claims that both the speed of light and the minimum speed are invariant in a kinematics point of view. Moreover, it is shown that the high value of the speed of light and the quasi zero value of the minimum speed in the early universe was drastically decreased and increased respectively before the beginning of the inflationary period. So we are led to conclude that the theory of Varying Speed of Light (VSL) should be questioned as a possible solution of the horizon problem for the hot universe. Furthermore we will show that both the speed of light and the minimum speed are respectively increased to infinite and decreased to zero in a future horizon given by a ultra-cold universe governed by a rapid accelerated expansion. So we conclude that both universal speeds have the same variations in the early time and the future cosmic time governed by the vacuum energy. [ABSTRACT FROM AUTHOR]
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- 2018
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4. Techniques for Measuring the Parameters of X-Ray Transport in Closed Cavities and Determining the Time of Thermal Breakdown of Foils
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S. I. Petrov, A. N. Muntyan, N. M. Romanova, and S. S. Taran
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Range (particle radiation) ,Materials science ,business.industry ,Thermal breakdown ,X-ray ,Streak ,Planck temperature ,Radiation temperature ,Radiation ,symbols.namesake ,Optics ,symbols ,business ,Instrumentation ,Image resolution - Abstract
Techniques are described that make it possible to measure the X-ray transport velocity in closed cavities, the time of radiation heating of foils, the radiation temperature, and the timing parameters of X-ray pulses in experiments at the ISKRA-5 facility. The methods are based on position-sensitive time-resolving (with a spatial resolution of 150 µm and a time resolution of 50 ps) measurements of X-rays in four narrow spectral regions of 0.2–1.0 keV using X-ray streak cameras, as well as on multiframe recording (with a frame duration of 100 ps, a frame number of 10, and a spatial resolution of 30 µm). In the experiments the peak Planck temperature of the radiation was 110–150 eV in the irradiating target and 50–90 eV in the additional box and behind the foils; the X-ray transport velocity in closed cavities ranged from 0.5 to 13 mm/ns and the time of thermal breakdown of foils was in range of 50–550 ps.
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- 2021
5. An Alternative to Dark Matter? Part 1: The Early Universe (tp to 10-9 s), Energy Creation the Alphaton, Baryogenesis
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Jean Perron
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Physics ,Inflation (cosmology) ,Particle physics ,Planck energy ,Age of the universe ,media_common.quotation_subject ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmological constant ,Universe ,symbols.namesake ,Planck time ,symbols ,Planck ,media_common - Abstract
A cosmological model was developed using the equation of state of photon gas, as well as cosmic time. The primary objective of this model is to see if determining the observed rotation speed of galactic matter is possible, without using dark matter (halo) as a parameter. To do so, a numerical application of the evolution of variables in accordance with cosmic time and a new state equation was developed to determine precise, realistic values for a number of cosmological parameters, such as the energy of the universe U, cosmological constant Λ, the curvature of space k, energy density ρΛe, age of the universe tΩ etc. The development of the state equation highlights the importance of not neglecting any of the differential terms given the very large amounts in play that can counterbalance the infinitesimals. Some assumptions were put forth in order to solve these equations. The current version of the model partially explains several of the observed phenomena that raise questions. Numerical application of the model has yielded the following results, among others: Initially, during the Planck era, at the very beginning of Planck time, tp, the universe contained a single photon at Planck temperature TP, almost Planck energy EP in the Planck volume. During the photon inflation phase (before characteristic time ~10-9 [s]), the number of original photons (alphatons) increased at each unit of Planck time tp and geometrical progression~n3, where n is the quotient of cosmic time over Planck time t/tp. Then, the primordial number of photons reached a maximum of N~1089, where it remained constant. These primordial photons (alphatons) are still present today and represent the essential of the energy contained in the universe via the cosmological constant expressed in the form of energy EΛ. Such geometric growth in the number of photons can bring a solution to the horizon problem through γγ exchange and a photon energy volume that is in phase with that of the volume energy of the universe. The predicted total mass (p, n, e, and ν), based on the Maxwell-Juttner relativistic statistical distribution, is ~7 × 1050 [kg]. The predicted cosmic neutrino mass is ≤8.69 × 10-32 [kg] (≤48.7 [keV·c-2]) if based on observations of SN1987A. The temperature variation of the cosmic microwave background (CMB), as measured by Planck, can be said to be partially due to energy variations in the universe (ΔU/U) during the primordial baryon synthesis (energy jump from the creation of protons and neutrons).
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- 2021
6. The Quantum Corrections on Kerr-Newman Black Hole Thermodynamics by the Generalized Uncertainty Principle
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Cheng-Zhou Liu and Shanping Wu
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Physics ,Uncertainty principle ,Physics and Astronomy (miscellaneous) ,010308 nuclear & particles physics ,Event horizon ,Astrophysics::High Energy Astrophysical Phenomena ,General Mathematics ,Planck temperature ,01 natural sciences ,Black hole ,General Relativity and Quantum Cosmology ,symbols.namesake ,Rotating black hole ,Quantum mechanics ,0103 physical sciences ,symbols ,Quantum gravity ,010306 general physics ,Black hole thermodynamics ,Entropy (arrow of time) - Abstract
By the generalized uncertainty principle, the quantum corrections on Kerr-Newman black hole thermodynamics is studied. Using the modified quantum uncertainty of particles near the event horizon, the relationship between the temperature and the horizon radius for the general stationary black hole is given. Then, to ensure the relational formula having the basic physics meaning, the critical state with Planck temperature for the black hole is obtained. In addition, considering the quantum gravity effects and using the first law of black hole thermodynamics, the entropy of the charged rotating black hole is calculated and the quantum corrections including the logarithmic item to the Bekenstein-Hawking entropy are obtained. Also, in the context of the generalized uncertainty principle, the thermal capacity of Kerr-Newman black hole is obtained. Letting the thermal capacity equal zero, the black hole radiation remnant with Planck temperature is derived. It is found that, for Kerr-Newman black hole, the remnant state is consistent with the critical state. Such, using the generalized uncertainty principle, the temperature divergence at the last stage of evaporation in the traditional Kerr-Newman black hole thermodynamics is removed.
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- 2020
7. A Detailed Description of the CAMSPEC Likelihood Pipeline and a Reanalysis of the Planck High Frequency Maps
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George Efstathiou and Steven Gratton
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High Energy Physics - Theory ,Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmic microwave background ,FOS: Physical sciences ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Statistical fluctuations ,Cosmology ,symbols.namesake ,Amplitude ,High Energy Physics - Theory (hep-th) ,symbols ,Planck ,Neutrino ,Multipole expansion ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
This paper presents a detailed description of the CamSpec likelihood which has been used to analyse Planck temperature and polarization maps of the cosmic microwave background since the first Planck data release. We have created a number of likelihoods using a range of Galactic sky masks and different methods of temperature foreground cleaning. Our most powerful likelihood uses 80 percent of the sky in temperature and polarization. Our results show that the six-parameter LCDM cosmology provides an excellent fit to the Planck data. There is no evidence for statistically significant internal tensions in the Planck TT, TE and EE spectra computed for different frequency combinations. We present evidence that the tendencies for the Planck temperature power spectra to favour a lensing amplitude A_L>1 and positive spatial curvature are caused by statistical fluctuations in the temperature power spectra. Using our statistically most powerful likelihood, we find that the A_L parameter differs from unity at no more than the 2.2 sigma level. We find no evidence for anomalous shifts in cosmological parameters with multipole range. In fact, we show that the combined TTTEEE likelihood over the restricted multipole range 2-800 gives cosmological parameters for the base LCDM cosmology that are very close to those derived from the full multipole range 2-2500. We present revised constraints on a few extensions of the base LCDM cosmology, focussing on the sum of neutrino masses, number of relativistic species and the tensor-scalar ratio. The results presented here show that the Planck data are remarkably consistent between detector-sets, frequencies and sky area. We find no evidence in our analysis that cosmological parameters determined from the CamSpec likelihood are affected to any significant degree by systematic errors in the Planck data (abridged)., accepted for publication in the Open Journal of Astrophysics
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- 2021
8. Invariance of the fine structure constant with temperature of the expanding universe.
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Nassif, Cláudio and de Faria, A.C. Amaro
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FINE-structure constant , *TEMPERATURE , *PLANCK'S energy , *EXPANDING universe , *PARSIMONIOUS models - Abstract
Our goal is to interpret the energy equation from doubly special relativity of Magueijo-Smolin with an invariant Planck energy scale to obtain the speed of light with an explicit dependence on the background temperature of the expanding universe (Nassif and de Faria. Phys. Rev. D, 86, 027703 (2012). ). We also investigate how other universal constants, including the fine structure constant, have varied since the early universe and, thus, how they have evolved over the cosmological time related to the temperature of the expanding universe. For instance, we show that both the Planck constant and the electron charge were also too large in the early universe. However, we finally conclude that the fine structure constant has remained invariant with the age and temperature of the universe, which is in agreement with laboratory tests and some observational data. [ABSTRACT FROM AUTHOR]
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- 2015
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9. Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory
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Yuting Wang, Héctor Gil-Marín, Peter M. Frinchaboy, Rossana Ruggeri, Andreu Font-Ribera, Jean-Paul Kneib, Christophe Balland, Mark A. Klaene, Jiamin Hou, Graziano Rossi, Abhishek Prakash, Adam D. Myers, Richard Neveux, Kathleen Grabowski, Chia-Hsun Chuang, M. C. Cousinou, Andrea Muñoz-Gutiérrez, Matthew M. Pieri, Patrick Petitjean, C. Yeche, Adam S. Bolton, Hui Kong, Pauline Zarrouk, Johan Comparat, Thomas Etourneau, Audrey Oravetz, Ashley J. Ross, Dmitry Bizyaev, Romain Paviot, Mehdi Rezaie, Amélie Tamone, James C. Parker, Gong-Bo Zhao, Faizan G. Mohammad, Santiago Avila, Jeffrey A. Newman, F. Javier Sánchez, Joel R. Brownstein, Kyle S. Dawson, Sylvain de la Torre, Peter Doohyun Choi, Daniel Long, Julian E. Bautista, Sicheng Lin, Alex Smith, José R. Sánchez-Gallego, Andrei Variu, Seshadri Nadathur, Daniel Oravetz, Stephanie Escoffier, Eva Maria Mueller, Jeongin Moon, Etienne Burtin, Mariana Vargas-Magaña, Julianna Stermer, Axel de la Macorra, Matthew A. Bershady, Hee-Jong Seo, Anand Raichoor, Paul Martini, Solène Chabanier, Ignasi Pérez-Ràfols, J. Rich, Anne-Marie Weijmans, Ariel G. Sánchez, Benjamin A. Weaver, Conor Sayres, Violeta Gonzalez-Perez, Kaike Pan, Will J. Percival, Corentin Ravoux, Adam J. Hawken, Jeremy L. Tinker, Zheng Zheng, Anže Slosar, Nathalie Palanque-Delabrouille, Cheng Zhao, Alma X. Gonzalez-Morales, Andrei Cuceu, P. Noterdaeme, V. Ruhlmann-Kleider, Arnaud de Mattia, Julien Guy, James Farr, Jo Bovy, Brad W. Lyke, Marie Aubert, Michael J. Chapman, Jean Marc Le Goff, Hélion du Mas des Bourboux, S. Fromenteau, Jonathan Brinkmann, Shadab Alam, Rita Tojeiro, Arman Shafieloo, Michael R. Blanton, Donald P. Schneider, Karen L. Masters, Victoria de Sainte Agathe, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), eBOSS, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ANR-16-CE31-0021,eBOSS,Sondes cosmologiques de la gravitation et de l'énergie noire(2016), UAM. Departamento de Física Teórica, Alfred P. Sloan Foundation, Department of Energy (US), University of St Andrews. School of Physics and Astronomy, and University of St Andrews. Centre for Contemporary Art
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galaxy redshift survey ,Cosmic microwave background ,Astrophysics ,supernova legacy survey ,Atomic ,01 natural sciences ,7. Clean energy ,Particle and Plasma Physics ,QB Astronomy ,Large-scale structure of the Universe ,angular power spectrum ,QC ,Weak gravitational lensing ,QB ,Physics ,Quantum Physics ,ly-alpha forest ,Cosmic distance ladder ,Astrophysics::Instrumentation and Methods for Astrophysics ,Planck temperature ,acoustic-oscillations ,Nuclear & Particles Physics ,Cosmology ,photometry data release ,symbols ,astro-ph.CO ,hubble-space-telescope ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmological parameters ,Red Shift ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Halo ,symbols.namesake ,0103 physical sciences ,Nuclear ,Planck ,010306 general physics ,dark-energy constraints ,010308 nuclear & particles physics ,Molecular ,Física ,DAS ,Galaxies ,Redshift ,QC Physics ,Dark energy ,digital sky survey ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,growth-rate ,Hubble's law - Abstract
Shadab, Alam et al., We present the cosmological implications from final measurements of clustering using galaxies, quasars, and Lyα forests from the completed Sloan Digital Sky Survey (SDSS) lineage of experiments in large-scale structure. These experiments, composed of data from SDSS, SDSS-II, BOSS, and eBOSS, offer independent measurements of baryon acoustic oscillation (BAO) measurements of angular-diameter distances and Hubble distances relative to the sound horizon, rd, from eight different samples and six measurements of the growth rate parameter, fσ8, from redshift-space distortions (RSD). This composite sample is the most constraining of its kind and allows us to perform a comprehensive assessment of the cosmological model after two decades of dedicated spectroscopic observation. We show that the BAO data alone are able to rule out dark-energy-free models at more than eight standard deviations in an extension to the flat, ΛCDM model that allows for curvature. When combined with Planck Cosmic Microwave Background (CMB) measurements of temperature and polarization, under the same model, the BAO data provide nearly an order of magnitude improvement on curvature constraints relative to primary CMB constraints alone. Independent of distance measurements, the SDSS RSD data complement weak lensing measurements from the Dark Energy Survey (DES) in demonstrating a preference for a flat ΛCDM cosmological model when combined with Planck measurements. The combined BAO and RSD measurements indicate σ8=0.85±0.03, implying a growth rate that is consistent with predictions from Planck temperature and polarization data and with General Relativity. When combining the results of SDSS BAO and RSD, Planck, Pantheon Type Ia supernovae (SNe Ia), and DES weak lensing and clustering measurements, all multiple-parameter extensions remain consistent with a ΛCDM model. Regardless of cosmological model, the precision on each of the three parameters, ωΛ, H0, and σ8, remains at roughly 1%, showing changes of less than 0.6% in the central values between models. In a model that allows for free curvature and a time-evolving equation of state for dark energy, the combined samples produce a constraint ωk=-0.0022±0.0022. The dark energy constraints lead to w0=-0.909±0.081 and wa=-0.49-0.30+0.35, corresponding to an equation of state of wp=-1.018±0.032 at a pivot redshift zp=0.29 and a Dark Energy Task Force Figure of Merit of 94. The inverse distance ladder measurement under this model yields H0=68.18±0.79 km s-1 Mpc-1, remaining in tension with several direct determination methods; the BAO data allow Hubble constant estimates that are robust against the assumption of the cosmological model. In addition, the BAO data allow estimates of H0 that are independent of the CMB data, with similar central values and precision under a ΛCDM model. Our most constraining combination of data gives the upper limit on the sum of neutrino masses at mν, This paper represents an effort by both the SDSS-III and SDSS-IV collaborations. Funding for SDSS-III was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, the Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.
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- 2021
10. The first Hubble diagram and cosmological constraints using superluminous supernovae
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D. L. Burke, Yanxi Zhang, C. B. D'Andrea, E. Swann, K. Honscheid, Geraint F. Lewis, J. Gschwend, B. Flaugher, M. Pursiainen, A. G. Kim, Tamara M. Davis, C. R. Angus, T. Giannantonio, D. Gruen, M. Vicenzi, Flavia Sobreira, David J. James, A. K. Romer, B. E. Tucker, S. R. Hinton, Lluís Galbany, M. Schubnell, Ramon Miquel, N. Kuropatkin, E. Suchyta, V. Scarpine, Robert C. Nichol, Daniel Thomas, Anais Möller, M. Soares-Santos, G. Tarle, P. Wiseman, J. Annis, M. Smith, T. S. Li, P. Martini, J. Garcia-Bellido, Josh Frieman, Karl Glazebrook, Daniel Scolnic, D. W. Gerdes, Elisabeth Krause, A. Roodman, T. M. C. Abbott, M. Lima, D. Brout, D. A. Finley, M. Carrasco Kind, K. Kuehn, P. J. Brown, D. L. Tucker, Claudia P. Gutiérrez, J. L. Marshall, C. Lidman, A. R. Walker, T. F. Eifler, Felipe Menanteau, Vinu Vikram, Mark Sullivan, G. Gutierrez, B. P. Thomas, E. Bertin, E. Macaulay, M. E.C. Swanson, J. Carretero, M. Sako, E. J. Sanchez, H. T. Diehl, S. Serrano, R. Cawthon, Rob Sharp, Cosimo Inserra, R. A. Gruendl, Richard Kessler, D. L. Hollowood, J. Calcino, Jacobo Asorey, S. Avila, D. Carollo, E. Gaztanaga, A. A. Plazas Malagón, I. Sevilla-Noarbe, D. Brooks, P. Fosalba, J. K. Hoormann, Yen-Chen Pan, A. Carnero Rosell, F. J. Castander, C. Frohmaier, M. A. G. Maia, S. Desai, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, Australian Research Council, Instituto Nacional de Ciência e Tecnologia (Brasil), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), and UAM. Departamento de Física Teórica
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transients: supernovae ,Cold dark matter ,Ia Supernovae ,TRANSIENT ,Astrophysics ,01 natural sciences ,Cosmology ,cosmological parameters [Cosmology] ,010303 astronomy & astrophysics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,GAMMA-RAY BURSTS ,Physics ,astro-ph.HE ,Transient ,4. Education ,supernovae [Transients] ,dark matter [Cosmology] ,Planck temperature ,Spectra ,cosmology: dark matter ,Supernova ,symbols ,astro-ph.CO ,IC SUPERNOVAE ,cosmology: cosmological parameters ,Astrophysics - High Energy Astrophysical Phenomena ,PAN-STARRS1 ,Host-Galaxy ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Gamma-Ray Bursts ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,INFRARED-EMISSION ,Pan-Starrs1 ,FOS: Physical sciences ,Infrared-Emission ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Moduli ,symbols.namesake ,0103 physical sciences ,SPECTRA ,IA SUPERNOVAE ,010308 nuclear & particles physics ,Baryon Acoustic-Oscillations ,Light-Curve Sample ,Física ,Astronomy and Astrophysics ,LIGHT-CURVE SAMPLE ,Light curve ,Redshift ,HOST-GALAXY ,Space and Planetary Science ,Dark energy ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,BARYON ACOUSTIC-OSCILLATIONS - Abstract
This paper has gone through internal review by the DES collaboration. It has Fermilab preprint number 19-115-AE and DES publication number 13387. We acknowledge support from EU/FP7- ERC grant 615929. RCN would like to acknowledge support from STFC grant ST/N000688/1 and the Faculty of Technology at the University of Portsmouth. LG was funded by the European Union’s Horizon 2020 Framework Programme under the Marie Skłodowska- Curie grant agreement no. 839090. This work has been partially supported by the Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ ˜ao Carlos Chagas Filho de Amparo `a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient´ıfico e Tecnol´ogico and the Minist´erio da Ciˆencia, Tecnologia e Inovac¸ ˜ao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ´eticas, Medioambientales y Tecnol ´ogicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen¨ossische Technische Hochschule (ETH) Z¨urich, Fermi NationalAccelerator Laboratory, theUniversity of Illinois atUrbana- Champaign, the Institut de Ci`encies de l’Espai (IEEC/CSIC), the Institut de F´ısica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit¨at M¨unchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV- 2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478.We acknowledge support from the Australian Research Council Centre of Excellence for All-skyAstrophysics (CAASTRO), through project number CE110001020, and the Brazilian Instituto Nacional de Ciˆencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This paper has been authored by Fermi Research Alliance, LLC under Contract No.DE-AC02-07CH11359 with theU.S.Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the paper for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this paper, or allow others to do so, for United States Government purposes., We present the first Hubble diagram of superluminous supernovae (SLSNe) out to a redshift of two, together with constraints on the matter density, M, and the dark energy equation-of-state parameter, w(≡p/ρ). We build a sample of 20 cosmologically useful SLSNe I based on light curve and spectroscopy quality cuts. We confirm the robustness of the peak–decline SLSN I standardization relation with a larger data set and improved fitting techniques than previous works. We then solve the SLSN model based on the above standardization via minimization of the χ2 computed from a covariance matrix that includes statistical and systematic uncertainties. For a spatially flat cold dark matter ( CDM) cosmological model, we find M = 0.38+0.24 −0.19, with an rms of 0.27 mag for the residuals of the distance moduli. For a w0waCDM cosmological model, the addition of SLSNe I to a ‘baseline’ measurement consisting of Planck temperature together with Type Ia supernovae, results in a small improvement in the constraints of w0 and wa of 4 per cent.We present simulations of future surveys with 868 and 492 SLSNe I (depending on the configuration used) and show that such a sample can deliver cosmological constraints in a flat CDM model with the same precision (considering only statistical uncertainties) as current surveys that use Type Ia supernovae, while providing a factor of 2–3 improvement in the precision of the constraints on the time variation of dark energy, w0 and wa. This paper represents the proof of concept for superluminous supernova cosmology, and demonstrates they can provide an independent test of cosmology in the high-redshift (z > 1) universe., EU/FP7-ERC grant 615929, STFC grant ST/N000688/1, Faculty of Technology at the University of Portsmouth, European Union’s Horizon 2020 Framework Programme under the Marie Skłodowska- Curie grant agreement no. 839090, Spanish grant PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER), U.S. Department of Energy, U.S. National Science Foundation, Ministry of Science and Education of Spain, Science and Technology Facilities Council of the United Kingdom, Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Kavli Institute of Cosmological Physics at the University of Chicago, Center for Cosmology and Astro-Particle Physics at the Ohio State University, Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacão Carlos Chagas Filho de Amparo `a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciencia, Tecnologia e Inovacão, Deutsche Forschungsgemeinschaft, Collaborating Institutions in the Dark Energy Survey., National Science Foundation under grant numbers AST-1138766 and AST-1536171., T MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV- 2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union., CERCA program of the Generalitat de Catalunya., European Research Council under the European Union Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478., Australian Research Council Centre of Excellence for All-skyAstrophysics (CAASTRO), through project number CE110001020, Brazilian Instituto Nacional de Ciˆencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2), Fermi Research Alliance, LLC under Contract No.DE-AC02-07CH11359 with theU.S.Department of Energy, Office of Science, Office of High Energy Physics
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- 2021
11. An Interesting Mathematical Relation between the Proton Mass, the Proton Radius, the Fine Structure Constant, the Compton Wavelength and the Hagedorn Temperature
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Espen Gaarder Haug
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Physics ,Nuclear physics ,Hagedorn temperature ,Quark ,symbols.namesake ,Proton ,Nuclear Theory ,Hadron ,symbols ,Fine-structure constant ,Planck temperature ,Radius ,Compton wavelength - Abstract
In this short note we present a possible connection between the proton radius and the proton mass using the fine structure constant. The Hagedorn temperature is related to the energy levels assumed to be required to free the quarks from the proton, where hadronic matter is unstable. We also speculate that there could be a connection between the Hagedorn temperature and the Planck temperature through the fine structure constant. Regarding whether or not there is something to this (or if it is purely a coincidence), we will leave to others and future research to explore. However, we think these possible relationships are worth further investigation.
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- 2019
12. A Solution of the Cosmological Constant and DE and Arrow of Time, Using Model of a Nonsingular Universe from Rosen from Volume (56) Ettore Majorana International Science Series, Physics, 1991
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Andrew W. Beckwith
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Physics ,Planck temperature ,Cosmological constant ,Inflaton ,Physics::History of Physics ,symbols.namesake ,Theoretical physics ,Massive gravity ,Arrow of time ,symbols ,Dark energy ,nuclear_high_energy_physics ,Planck ,Planck length - Abstract
We reduplicate the Book “Dark Energy” by M. Li, X-D. Li, and Y. Wang, given zero-point energy calculation with an unexpected “length’ added to the ‘width’ of a graviton wave just prior to specifying the creation of ‘gravitons’, using the Rosen and Israelit model of a nonsingular universe. In doing so we are in addition to obtaining a wavelength 10^30 times greater than Planck’s length so we can calculate DE, may be able to with the help of the Rosen and Israelit model have a first approximation as to the arrow of time, and a universe with massive gravity. We have left the particulars of the nonsingular starting point undefined but state that the Rosen and Israelit model postulates initial temperatures of 10^-180 Kelvin and also a value of about Planck temperature, at 10^-3 centimeters radii value which may satisfy initial conditions asked by t’Hooft for describing an arrow of time. A key assumption is that the DE is formed at 10^-3 cm, after an expansion of 10^30 times in radii, from the Planck length radius nonsingular starting point. The given starting point for DE in this set of assumptions is where there is a change in the cosmic acceleration, to a zero value, according to Rosen and Israel, with time t = 1.31 times 10^-42 seconds. Which may be where we may specify a potential magnitude, V, which has ties into inflaton physics. The particulars of the model from Rosen and Israelit allow a solution to be found, without discussion of where that nonsingular starting point came from, a point the author found in need of drastic remedies and fixes.
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- 2021
13. Exploring an early dark energy solution to the Hubble tension with Planck and SPTPol data
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Nikita Nedelko, Anton Chudaykin, and Dmitry Gorbunov
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Physics ,Particle physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Cosmic microwave background ,Cosmic distance ladder ,FOS: Physical sciences ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Parameter space ,Lambda ,01 natural sciences ,High Energy Physics - Phenomenology ,symbols.namesake ,High Energy Physics - Phenomenology (hep-ph) ,0103 physical sciences ,symbols ,Dark energy ,Planck ,010306 general physics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Hubble's law - Abstract
A promising idea to resolve the long standing Hubble tension is to postulate a new subdominant dark-energy-like component in the pre-recombination Universe which is traditionally termed as the Early Dark Energy (EDE). However, as shown in Refs. \cite{Hill:2020osr,Ivanov:2020ril} the cosmic microwave background (CMB) and large-scale structure (LSS) data impose tight constraints on this proposal. Here, we revisit these strong bounds considering the Planck CMB temperature anisotropy data at large angular scales and the SPTPol polarization and lensing measurements. As advocated in Ref. \cite{Chudaykin:2020acu}, this combined data approach predicts the CMB lensing effect consistent with the $\Lambda$CDM expectation and allows one to efficiently probe both large and small angular scales. Combining Planck and SPTPol CMB data with the full-shape BOSS likelihood and information from photometric LSS surveys in the EDE analysis we found for the Hubble constant $H_0=69.79\pm0.99\,{\rm km\,s^{-1}Mpc^{-1}}$ and for the EDE fraction $f_{\rm EDE}, Comment: 14+3 pages, 2+1 figures, 4 tables; v2: Appendix A added, matched version accepted by Phys. Rev. D
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- 2021
14. Informational approach to cosmological parameter estimation
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Michelle Stephens, Sara Vannah, and Marcelo Gleiser
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,FOS: Physical sciences ,Spectral density ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Parameter space ,Lambda ,01 natural sciences ,Combinatorics ,High Energy Physics - Phenomenology ,symbols.namesake ,High Energy Physics - Phenomenology (hep-ph) ,0103 physical sciences ,symbols ,Dark energy ,010306 general physics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Hubble's law - Abstract
We introduce a new approach for cosmological parameter estimation based on the information-theoretical Jensen-Shannon divergence (${\cal D}_{\rm JS}$), calculating it for models in the restricted parameter space $\{H_0, w_0, w_a\}$, where $H_0$ is the value of the Hubble constant today, and $w_0$ and $w_a$ are dark energy parameters, with the other parameters held fixed at their best-fit values from the Planck 2018 data. As an application, we investigate the $H_0$ tension between the Planck temperature power spectrum data (TT) and the local astronomical data by comparing the $\Lambda$CDM model with the $w$CDM and the $w_0w_a$CDM dynamic dark energy models. We find agreement with other works using the standard Bayesian inference for parameter estimation; in addition, we show that while the ${\cal D}_{\rm JS}$ is equally minimized for both values of $H_0$ along the $(w_0,w_a)$ plane, the lines of degeneracy are different for each value of $H_0$. This allows for distinguishing between the two, once the value of either $w_0$ or $w_a$ is known., Comment: 5 pages, 3 figures. Final version accepted for publication in Physical Review D. Includes a new error analysis, a new figure, additional references, and a new author
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- 2020
15. Measuring the integrated Sachs-Wolfe effect from the low-density regions of the universe
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Pengjie Zhang, Jun Zhang, Xiaohu Yang, Fuyu Dong, and Yu Yu
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Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmic microwave background ,Cosmic background radiation ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planck temperature ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Sachs–Wolfe effect ,Galaxy ,Cosmology ,Gravitational potential ,symbols.namesake ,Space and Planetary Science ,Dark energy ,symbols ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The integrated Sachs-Wolfe (ISW) effect is caused by the decay of cosmological gravitational potential, and is therefore a unique probe of dark energy. However, its robust detection is still problematic. Various tensions between different data sets, different large scale structure (LSS) tracers, and between data and the $\Lambda$CDM theory prediction, exist. We propose a novel method of ISW measurement by cross correlating CMB and the LSS traced by "low-density-position" (LDP, \citet{2019ApJ...874....7D}). It isolates the ISW effect generated by low-density regions of the universe, but insensitive to selection effects associated with voids. We apply it to the DR8 galaxy catalogue of the DESI Legacy imaging surveys, and obtain the LDPs at $z\leq 0.6$ over $\sim$ 20000 $deg^2$ sky coverage. We then cross correlate with the Planck temperature map, and detect the ISW effect at $3.2\sigma$. We further compare the measurement with numerical simulations of the concordance $\Lambda$CDM cosmology, and find the ISW amplitude parameter $A_{ISW}=1.14\pm0.38$ when we adopt a LDP definition radius $R_s=3^{'}$, fully consistent with the prediction of the standard $\Lambda$CDM cosmology ($A_{ISW}=1$). This agreement with $\Lambda$CDM cosmology holds for all the galaxy samples and $R_s$ that we have investigated. Furthermore, the S/N is comparable to that of galaxy ISW measurement. These results demonstrate the LDP method as a competitive alternative to existing ISW measurement methods, and provide independent checks to existing tensions., Comment: 16 pages, 14 figures
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- 2020
16. Full-sky Cosmic Microwave Background Foreground Cleaning Using Machine Learning
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Graeme E. Addison, Janet L. Weiland, Matthew Petroff, and Charles L. Bennett
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Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010504 meteorology & atmospheric sciences ,media_common.quotation_subject ,Cosmic microwave background ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Machine learning ,computer.software_genre ,01 natural sciences ,symbols.namesake ,Observational cosmology ,0103 physical sciences ,Planck ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,media_common ,Physics ,business.industry ,HEALPix ,Astrophysics::Instrumentation and Methods for Astrophysics ,Spectral density ,Astronomy and Astrophysics ,Planck temperature ,Space and Planetary Science ,Sky ,symbols ,Millimeter ,Artificial intelligence ,business ,computer ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
In order to extract cosmological information from observations of the millimeter and submillimeter sky, foreground components must first be removed to produce an estimate of the cosmic microwave background (CMB). We developed a machine-learning approach for doing so for full-sky temperature maps of the millimeter and submillimeter sky. We constructed a Bayesian spherical convolutional neural network architecture to produce a model that captures both spectral and morphological aspects of the foregrounds. Additionally, the model outputs a per-pixel error estimate that incorporates both statistical and model uncertainties. The model was then trained using simulations that incorporated knowledge of these foreground components that was available at the time of the launch of the Planck satellite. On simulated maps, the CMB is recovered with a mean absolute difference of $50��$K; the angular power spectrum is also accurately recovered. Once validated with the simulations, this model was applied to Planck temperature observations from its 70GHz through 857GHz channels to produce a foreground-cleaned CMB map at a Healpix map resolution of NSIDE=512. Furthermore, we demonstrate the utility of the technique for evaluating how well different simulations match observations, particularly in regard to the modeling of thermal dust., 10 pages, 6 figures, submitted to ApJ
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- 2020
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17. Variation of the speed of light and a minimum speed in the scenario of an inflationary universe with accelerated expansion
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Cláudio Nassif Cruz and Fernando Antônio da Silva
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Physics ,COSMIC cancer database ,010308 nuclear & particles physics ,Planck mass ,Relativistic dynamics ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planck temperature ,Invariant (physics) ,01 natural sciences ,Metric expansion of space ,symbols.namesake ,Physics - General Physics ,General Physics (physics.gen-ph) ,Vacuum energy ,Space and Planetary Science ,Quantum electrodynamics ,0103 physical sciences ,symbols ,Horizon problem ,010303 astronomy & astrophysics - Abstract
In this paper we aim to investigate a deformed relativistic dynamics well-known as Symmetrical Special Relativity (SSR) related to a cosmic background field that plays the role of a variable vacuum energy density associated to the temperature of the expanding universe with a cosmic inflation in its early time and an accelerated expansion for its very far future time. In this scenario, we show that the speed of light and an invariant minimum speed present an explicit dependence on the background temperature of the expanding universe. Although finding the speed of light in the early universe with very high temperature and also in the very old one with very low temperature, being respectively much larger and much smaller than its current value, our approach does not violate the postulate of Special Relativity (SR), which claims the speed of light is invariant in a kinematics point of view. Moreover, it is shown that the high value of the speed of light in the early universe was drastically decreased and increased respectively before the beginning of the inflationary period. So we are led to conclude that the theory of Varying Speed of Light (VSL) should be questioned as a possible solution of the horizon problem for the hot universe., Comment: 18 pages, 8 figures. arXiv admin note: text overlap with arXiv:1710.11497, arXiv:1205.2298
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- 2020
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18. The evidence for a spatially flat Universe
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Steven Gratton and George Efstathiou
- Subjects
High Energy Physics - Theory ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,media_common.quotation_subject ,Cosmic microwave background ,Cosmic background radiation ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,symbols.namesake ,0103 physical sciences ,Planck ,010303 astronomy & astrophysics ,media_common ,Inflation (cosmology) ,Physics ,010308 nuclear & particles physics ,Shape of the universe ,Astronomy and Astrophysics ,Planck temperature ,Universe ,High Energy Physics - Theory (hep-th) ,Space and Planetary Science ,symbols ,Baryon acoustic oscillations ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We revisit the observational constraints on spatial curvature following recent claims that the Planck data favour a closed Universe. We use a new and statistically powerful Planck likelihood to show that the Planck temperature and polarization spectra are consistent with a spatially flat Universe, though because of a geometrical degeneracy cosmic microwave background spectra on their own do not lead to tight constraints on the curvature density parameter Omega_K. When combined with other astrophysical data, particularly geometrical measurements of baryon acoustic oscillations, the Universe is constrained to be spatially flat to extremely high precision, with Omega_ K = 0.0004 +/-0.0018 in agreement with the 2018 results of the Planck team. In the context of inflationary cosmology, the observations offer strong support for models of inflation with a large number of e-foldings and disfavour models of incomplete inflation., Comment: submitted to MNRAS
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- 2020
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19. Revised planet brightness temperatures using the Planck/LFI 2018 data release
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E. Romelli, Andrea Zacchei, Daniele Tavagnacco, M. Tomasi, M. Frailis, Gianmarco Maggio, Michele Maris, Anna Gregorio, S. Galeotta, M. Sandri, Maris, M., Romelli, E., Tomasi, M., Gregorio, A., Sandri, M., Galeotta, S., Tavagnacco, D., Frailis, M., Maggio, G., and Zacchei, A.
- Subjects
Cosmic background radiation ,Instrumentation: detectors ,Methods: data analysis ,Planets and satellites: general ,FOS: Physical sciences ,Astrophysics ,Jupiter ,symbols.namesake ,Planet ,Neptune ,Saturn ,Planck ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Uranus ,Astronomy and Astrophysics ,Planck temperature ,CMB cold spot ,general [Planets and satellites] ,data analysi [Methods] ,Space and Planetary Science ,symbols ,detector [Instrumentation] ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present new estimates of the brightness temperatures of Jupiter, Saturn, Uranus, and Neptune based on the measurements carried in 2009--2013 by PLANCK/LFI at 30, 44, and 70 GHz and released to the public in 2018. This work extends the results presented in the 2013 and 2015 PLANCK/LFI Calibration Papers, based on the data acquired in 2009--2011. PLANCK observed each planet up to eight times during the nominal mission. We processed time-ordered data from the 22 LFI radiometers to derive planet antenna temperatures for each planet and transit. We accounted for the beam shape, radiometer bandpasses, and several systematic effects. We compared our results with the results from the ninth year of WMAP, PLANCK/HFI observations, and existing data and models for planetary microwave emissivity. For Jupiter, we obtain Tb = 144.9, 159.8, 170.5 K (+/- 0.2 K at 1 sigma, with temperatures expressed using the Rayleigh-Jeans scale) at 30, 44 and 70 GHz, respectively, or equivalently a band averaged Planck temperature TbBA=144.7$, 160.3, 171.2 K in good agreement with WMAP and existing models. A slight excess at 30 GHz with respect to models is interpreted as an effect of synchrotron emission. Our measures for Saturn agree with the results from WMAP for rings Tb = 9.2 +/- 1.4, 12.6 +/- 2.3, 16.2 +/- 0.8 K, while for the disc we obtain Tb = 140.0 +/- 1.4, 147.2 +/- 1.2, 150.2 +/- 0.4 K, or equivalently a TbBA=139.7, 147.8, 151.0 K. Our measures for Uranus (Tb = 152 +/- 6, 145 +/- 3, 132.0 +/- 2 K, or TbBA=152, 145, 133 K and Neptune Tb = 154 +/- 11, 148 +/- 9, 128 +/- 3 K, or TbBA=154 , 149, 128 K) agree closely with WMAP and previous data in literature., Comment: V2: language and formatting corrected according to Astronomy and Astrophysics standards. V1 as accepted from A&A in December 3, 2020; 14 figures; 17 tables; 29 pages
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- 2020
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20. Effects of the K-value solution schemes on radiation heat transfer modelling in oxy-fuel flames using the full-spectrum correlated K-distribution method
- Author
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Guanghai Liu, Jean-Louis Consalvi, Fengshan Liu, Yuying Liu, School of Energy and Power Engineering [Beijing], Beihang University (BUAA), National Research Council of Canada (NRC), Institut universitaire des systèmes thermiques industriels (IUSTI), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), and consalvi, jean-louis
- Subjects
full-spectrum correlated K-distribution ,Length scale ,Materials science ,dry and wet oxy-fuel flames ,Rank (linear algebra) ,[SPI] Engineering Sciences [physics] ,020209 energy ,Energy Engineering and Power Technology ,Planck temperature ,02 engineering and technology ,Industrial and Manufacturing Engineering ,Computational physics ,symbols.namesake ,Oxy-fuel ,[SPI]Engineering Sciences [physics] ,020401 chemical engineering ,rank correlated full-spectrum K-distribution ,correlated-K solution scheme ,Heat transfer ,0202 electrical engineering, electronic engineering, information engineering ,symbols ,Radiative transfer ,0204 chemical engineering ,ComputingMilieux_MISCELLANEOUS ,K-distribution - Abstract
Radiation heat transfer in oxy-fuel flames is more important than in conventional fuel-air flames. The Full-Spectrum Correlated K-distribution methods (FSCK) with the original correlated-K solution scheme (Modest and Zhang, 2002) and a newly proposed one (Cai and Modest, 2014), and the Rank Correlated Full-Spectrum K-distribution method (RC-FSK) are used in radiative calculations of oxy-fuel flames. Twelve one-dimensional flames, including fuel-air, dry and wet oxy-fuel flames with various length scales, as well as a two-dimensional dry oxy-fuel flame are studied. The results show that the reference temperature has a non-negligible impact on the accuracy of original scheme and the emission-weighted temperature leads to a good accuracy. The accuracy of the new scheme is almost unaffected by the reference temperature, except for small-scale dry oxy-fuel flames. The error of the new scheme is mainly in the low-temperature region, and its accuracy depends on the length scale of computational domain. A hybrid correlated-K scheme using either the original or the new scheme according to local temperature is proposed. It combines the advantages of two schemes in different temperature regions, and is independent of the reference temperature. In addition, the RC-FSK demonstrates almost the same accuracy as FSCK with the hybrid scheme when the Planck temperature is set equal to the reference temperature.
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- 2020
21. Combined analysis of Planck and SPTPol data favors the early dark energy models
- Author
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Dmitry Gorbunov, Nikita Nedelko, and Anton Chudaykin
- Subjects
Physics ,Particle physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Spectral density ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmology ,Baryon ,symbols.namesake ,High Energy Physics - Phenomenology ,High Energy Physics - Phenomenology (hep-ph) ,symbols ,Dark energy ,Planck ,Weak gravitational lensing ,Hubble's law ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We study the implications of the Planck temperature power spectrum at low multipoles, $\ell, Comment: 28+6 pages, 6 figures, 3+3 tables. SPTPol likelihoods for montepython environment are available at https://github.com/ksardase/SPTPol-montepython. v2: major revision which includes chi2 analysis for each likelihood in LCDM and EDE fits, detailed comparison with previous works and various clarifications. The results are unchanged. v3: minor corrections, accepted in JCAP
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- 2020
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22. Analytical evaluation of the numerical values of the Hubble constant and main spatial-energy characteristics of the observable Universe
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Konstantin Afanasiev, Vladimir Zhukov, Valery Timkov, Serg Timkov, Institute of Telecommunications and Global Geoinformation Space, National Academy of Sciences of Ukraine (NASU), Research and Production Enterprise «TZHK», Ukraine, and Valery, Timkov
- Subjects
Physics ,[PHYS]Physics [physics] ,Planck energy ,Hubble constant ,Planck temperature ,Observable universe ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,[PHYS] Physics [physics] ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,symbols.namesake ,the Hubble sphere ,Planck force ,Universe ,[PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Hubble volume ,fractals ,proportions and constants of Planck ,symbols ,Dark energy ,black hole ,Planck ,[PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Hubble's law - Abstract
International audience; Since the baryonic matter of the observable Universe consists mainly of protons and neutrons, then the numerical value of its mass can be represented and calculated on the basis of an additive-multiplicative golden algebraic fractal, based on golden algebraic fractals of the masse of proton, neutron, and muon. Based on an analytical estimate of the mass of the observable Universe, using the law “Planck’s Universal Proportions”, an analytical estimate of the Hubble constant and the main spatial-energy characteristics of the observed Universe is obtained. An analytical estimate of the Hubble constant is consistent with the experimental data of Planck’s mission, SDSS-III Baryon Oscillation Spectroscopic Survey, DES Collaboration. The objectivity of the experimental estimation of the Hubble constant from the H0LiCOW, Riess et al, Hubble Space Telescope collaborations does not raise any doubts. This means that the Hubble constant describes two similar, but different physical processes and has at least two values. The value of the Hubble constant from the collaborations Planck’s mission, SDSS-III Baryon Oscillation Spectroscopic Survey, DES Collaboration describes the process of rotation of the space of the observed Universe, and the value of the Hubble constant from the collaborations H0LiCOW, Riess et al, Hubble Space Telescope describes the process of rotation of substance in the space of the observed Universe. New estimates of the values of Dirac's large energy numbers are presented. It is confirmed that all coefficients in Planck’s proportions, which are calculated on the basis of Planck’s constants — length, mass, time, are equal to similar coefficients, which are calculated on the basis of the main characteristics of the observed Universe. Estimation of the numerical values of the Schwarzschild and Hubble radii for the observable Universe suggests that the Hubble sphere is inside the Schwarzschild sphere, therefore the observable Universe is a black hole. The presence of a redshift from distant objects of the observable Universe suggests that this is a rotating black hole. It has been shown that the vacuum pressure cannot be a source of dark energy. It is shown that the force of imaginary dark energy is equal in magnitude to the force of gravitational compression of the observed Universe and is equal to the Planck force. It is shown that after the Big Bang, the space of the observable Universe made one incomplete revolution of at 345 degrees, and the substance in it made one complete revolution of approximately 379 degrees. Estimates are given for the energy of dark matter, as the kinetic energy of rotation of the space of the observable Universe, as well as the equivalent mass of dark matter. New estimates are given: of the gravitational constant, of the Planck energy, of the Planck acceleration, of the Planck force, of the gravity factor of the observable Universe, of the Planck temperature, of the angular velocity of rotation of the space of the observable Universe. Estimates of temperature and wavelength of thermal radiation of the observable Universe, as the Hubble sphere, are given.
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- 2019
23. On a quadratic equation of state and a universe mildly bouncing above the Planck temperature
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Johanna Pasquet, Joanna Berteaud, Andre Tilquin, Thomas Schucker, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), CPT - E3 Cosmologie, and Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
Physics ,010308 nuclear & particles physics ,Initial singularity ,media_common.quotation_subject ,Diagram ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planck temperature ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,General Relativity and Quantum Cosmology ,Universe ,Baryon ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Supernova ,symbols.namesake ,Quadratic equation ,0103 physical sciences ,symbols ,Baryon acoustic oscillations ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Mathematical physics ,media_common - Abstract
A 1-parameter class of quadratic equations of state is confronted with the Hubble diagram of supernovae and Baryonic Acoustic Oscillations. The fit is found to be as good as the one using the LambdaCDM model. The corresponding universe has no initial singularity, only a mild bounce at a temperature well above the Planck temperature., Comment: To the memory of Daniel Kastler and Raymond Stora. 21 pages, 7 figures. arXiv admin note: text overlap with arXiv:1508.00809; version 2: 2 references added; version 3: corrected equations (9), (15) and the second of (36), matches published version
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- 2019
24. Symmetric Theory: Planck’s Particle
- Author
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Giuseppe Azzarello
- Subjects
Physics ,symbols.namesake ,Planck energy ,Planck force ,Planck time ,Planck particle ,Quantum mechanics ,symbols ,Planck mass ,Planck temperature ,Planck units ,Planck length - Abstract
The properties of symmetry of the Planck particle will be presented, and its magnetic charge will be extracted. This particle unifies the gravitational force, the electric force and the magnetic force into a single one, referred to as superforce. The phy...
- Published
- 2017
25. Lensing covariance on cut sky and SPT−Planck lensing tensions
- Author
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Wayne Hu and Pavel Motloch
- Subjects
Physics ,010308 nuclear & particles physics ,Cosmic microwave background ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Covariance ,01 natural sciences ,symbols.namesake ,Gravitational lens ,South Pole Telescope ,Amplitude ,0103 physical sciences ,symbols ,010306 general physics ,Scaling ,Smoothing - Abstract
We investigate correlations induced by gravitational lensing on simulated cosmic microwave background data of experiments with an incomplete sky coverage and their effect on inferences from the South Pole Telescope data. These correlations agree well with the theoretical expectations, given by the sum of super-sample and intra-sample lensing terms, with only a typically negligible $\sim$ 5% discrepancy in the amplitude of the super-sample lensing effect. Including these effects we find that lensing constraints are in $3.0\sigma$ or $2.1\sigma$ tension between the SPT polarization measurements and Planck temperature or lensing reconstruction constraints respectively. If the lensing-induced covariance effects are neglected, the significance of these tensions increases to $3.5\sigma$ or $2.5\sigma$. Using the standard scaling parameter $A_L$ substantially underestimates the significance of the tension once other parameters are marginalized over. By parameterizing the super-sample lensing through the mean convergence in the SPT footprint, we find a hint of underdensity in the SPT region. We also constrain extra sharpening of the CMB acoustic peaks due to missing smoothing of the peaks by super-sample lenses at a level that is much smaller than the lens sample variance. Finally, we extend the usual "shift in the means" statistic for evaluating tensions to non-Gaussian posteriors, generalize an approach to extract correlation modes from noisy simulated covariance matrices, and present a treatment of correlation modes not as data covariances but as auxiliary model parameters.
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- 2019
26. Searching for Light Relics with the CMB
- Author
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Benjamin Wallisch
- Subjects
Physics ,Cosmic neutrino background ,Gravitational potential ,symbols.namesake ,Dark radiation ,Physics beyond the Standard Model ,Cosmic microwave background ,symbols ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Neutrino ,Relativistic particle - Abstract
Fluctuations in the cosmic neutrino background are known to produce a phase shift in the acoustic peaks of the cosmic microwave background (CMB). It is through the sensitivity to this effect that the recent CMB data has provided a robust detection of free-streaming neutrinos. In this chapter, we revisit the phase shift of the CMB anisotropy spectrum as a probe of new physics. The phase shift is particularly interesting because its physical origin is strongly constrained by the analytic properties of the Green’s function of the gravitational potential. For adiabatic fluctuations, a phase shift requires modes that propagate faster than the speed of fluctuations in the photon-baryon plasma. This possibility is realized by free-streaming relativistic particles, such as neutrinos or other forms of dark radiation. Alternatively, a phase shift can arise from isocurvature fluctuations. We present simple models to illustrate each of these effects and provide observational constraints from the Planck temperature and polarization data on additional forms of radiation. We also estimate the capabilities of future CMB Stage-4 experiments. Whenever possible, we give analytic interpretations and consider possible implications of our results.
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- 2019
27. Super-CMB fluctuations and the Hubble tension
- Author
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Dragan Huterer and Saroj Adhikari
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High Energy Physics - Theory ,Inflation (cosmology) ,Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Primordial fluctuations ,Cosmic microwave background ,Spectral density ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planck temperature ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Covariance ,01 natural sciences ,symbols.namesake ,High Energy Physics - Theory (hep-th) ,Space and Planetary Science ,0103 physical sciences ,symbols ,Trispectrum ,010303 astronomy & astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Hubble's law - Abstract
We study the covariance in the angular power spectrum estimates of CMB fluctuations when the primordial fluctuations are non-Gaussian. The non-Gaussian covariance comes from a nonzero connected four-point correlation function -- or the trispectrum in Fourier space -- and can be large when long-wavelength (super-CMB) modes are strongly coupled to short-wavelength modes. The effect of such non-Gaussian covariance can be modeled through additional freedom in the theoretical CMB angular power spectrum and can lead to different inferred values of the standard cosmological parameters relative to those in $\Lambda$CDM. Taking the collapsed limit of the primordial trispectrum in the quasi-single field inflation model as an example, we study how the six standard $\Lambda$CDM parameters shift when two additional parameters describing the trispectrum are allowed. The reduced statistical significance of the Hubble tension in the extended model allows us to combine the {\it Planck} temperature data and the type Ia supernovae data from Panstarrs with the distance-ladder measurement of the Hubble constant. This combination of data shows strong evidence for a primordial trispectrum-induced non-Gaussian covariance, with a likelihood improvement of $\Delta \chi^2 \approx -15$ (with two additional parameters) relative to $\Lambda$CDM., Comment: 7 pages, 3 figures; v3: title changed, discussion of SDDR added, and other minor changes made to match published version
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- 2019
- Full Text
- View/download PDF
28. Cosmological discordances III: more on measure properties, Large-Scale-Structure constraints, the Hubble constant and Planck
- Author
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Mustapha Ishak, Cristhian Garcia-Quintero, Weikang Lin, and Logan Fox
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Cosmic microwave background ,Sigma ,FOS: Physical sciences ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,01 natural sciences ,CMB cold spot ,Redshift ,General Relativity and Quantum Cosmology ,symbols.namesake ,Theoretical physics ,0103 physical sciences ,symbols ,Dark energy ,Planck ,010306 general physics ,Hubble's law ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Consistency between cosmological data sets is essential for ongoing and future cosmological analyses. We first investigate the questions of stability and applicability of some moment-based inconsistency measures to multiple data sets. We show that the recently introduced index of inconsistency (IOI) is numerically stable while it can be applied to multiple data sets. We use an illustrative construction of constraints as well as an example with real data sets (i.e. WMAP versus Planck) to show some limitations of the application of the Karhunen-Loeve decomposition to discordance measures. Second, we perform various consistency analyzes using IOI between multiple current data sets while \textit{working with the entire common parameter spaces}. We find current Large-Scale-Structure (LSS) data sets (Planck CMB lensing, DES lensing-clustering and SDSS RSD) all to be consistent with one another. This is found to be not the case for Planck temperature (TT) versus polarization (TE,EE) data, where moderate inconsistencies are present. Noteworthy, we find a strong inconsistency between joint LSS probes and Planck with IOI=5.27, and a moderate tension between DES and Planck with IOI=3.14. Next, using the IOI metric, we compare the Hubble constant from five independent probes. We confirm previous strong tensions between local measurement (SH0ES) and Planck as well as between H0LiCOW and Planck, but also find new strong tensions between SH0ES measurement and the joint LSS probes with IOI=6.73 (i.e. 3.7-$\sigma$ in 1D) as well as between joint LSS and combined probes SH0ES+H0LiCOW with IOI=8.59 (i.e. 4.1-$\sigma$ in 1D). Whether due to systematic effects in the data sets or problems with the underlying model, sources of these old and new tensions need to be identified and dealt with., Comment: 20 pages, 6 figures
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- 2019
- Full Text
- View/download PDF
29. Constraints on Primordial Gravitational Waves Using Planck , WMAP, and New BICEP2/ Keck Observations through the 2015 Season
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Peter A. R. Ade, Lorenzo Moncelsi, N. A. Larsen, Abigail G. Vieregg, S. Kefeli, J. A. Grayson, Justus A. Brevik, Randol W. Aikin, King Tong Lau, Toshiya Namikawa, John M Kovac, Z. K. Staniszewski, Stefan Richter, Kirit Karkare, S. Palladino, K. G. Megerian, C. D. Sheehy, Chao-Lin Kuo, Denis Barkats, A. Wandui, J. J. Bock, Kent D. Irwin, Victor Buza, A. D. Turner, E. Karpel, L. Duband, R. Bowens-Rubin, M. Lueker, J. Cornelison, J. Kang, Cora Dvorkin, K. L. Thompson, Colin A. Bischoff, Howard Hui, Calvin B. Netterfield, J. P. Kaufman, J. E. Tolan, C. Tucker, R. Schwarz, Alessandro Schillaci, Marion Dierickx, T. St. Germaine, D. V. Wiebe, M. Crumrine, A. C. Weber, R. V. Sudiwala, Jake Connors, G. Hall, Brian Keating, J. Willmert, W. L. K. Wu, S. Fliescher, Ahmed Soliman, C. Umilta, Ki Won Yoon, Kate D. Alexander, Gene C. Hilton, Jeffrey P. Filippini, Steven J. Benton, R. W. Ogburn, B. P. Crill, Chao Zhang, C. Pryke, Grant Teply, Hyunsoo Yang, B. Racine, C. L. Wong, Sarah M. Harrison, H. T. Nguyen, E. M. Leitch, I. Buder, Bryan Steinbach, E. Bullock, Roger O'Brient, Mark Halpern, Z. Ahmed, S. A. Kernasovskiy, and S. R. Hildebrandt
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Physics ,010308 nuclear & particles physics ,Gravitational wave ,media_common.quotation_subject ,Cosmic microwave background ,Astrophysics::Instrumentation and Methods for Astrophysics ,General Physics and Astronomy ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Polarization (waves) ,01 natural sciences ,7. Clean energy ,CMB cold spot ,Spectral line ,symbols.namesake ,13. Climate action ,Sky ,0103 physical sciences ,symbols ,Astrophysics::Earth and Planetary Astrophysics ,Planck ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common - Abstract
We present results from an analysis of all data taken by the bicep2/Keck CMB polarization experiments up to and including the 2015 observing season. This includes the first Keck Array observations at 220 GHz and additional observations at 95 and 150 GHz. The Q and U maps reach depths of 5.2, 2.9, and 26 μKCMB arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈400 square degrees. The 220 GHz maps achieve a signal to noise on polarized dust emission approximately equal to that of Planck at 353 GHz. We take auto and cross spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz. We evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and we impose priors on some of these using external information from Planck and WMAP derived from larger regions of sky. The model is shown to be an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r0.05
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- 2018
30. Constraints on non-resonant photon-axion conversion from the Planck satellite data
- Author
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Suvodip Mukherjee, Benjamin D. Wandelt, Rishi Khatri, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), and Sorbonne Universités
- Subjects
High Energy Physics - Theory ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Photon ,satellite: Planck ,Scalar (mathematics) ,Cosmic microwave background ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,symbols.namesake ,photon axion ,High Energy Physics - Phenomenology (hep-ph) ,Distortion ,0103 physical sciences ,Planck ,Axion ,Physics ,magnetic field: turbulence ,010308 nuclear & particles physics ,fluctuation ,[PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th] ,pseudoscalar particle ,photon ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy and Astrophysics ,Planck temperature ,Computational physics ,cosmic background radiation: temperature ,Pseudoscalar ,High Energy Physics - Phenomenology ,High Energy Physics - Theory (hep-th) ,angular resolution ,[PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph] ,symbols ,spectral ,axion-like particles ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The non-resonant conversion of Cosmic Microwave Background (CMB) photons into scalar as well as light pseudoscalar particles such as axion-like particles (ALPs) in the presence of turbulent magnetic fields can cause a unique, spatially fluctuating spectral distortion in the CMB. We use the publicly available Planck temperature maps for the frequency channels (70-545 GHz) to obtain the first ALP distortion map using $45\%$ clean part of the sky. The $95^{th}$ percentile upper limit on the RMS fluctuation of ALP distortions from the cleanest part of the CMB sky at $15$ arcmin angular resolution is $18.5 \times 10^{-6}$. The RMS fluctuation in the distortion map is also consistent with different combinations of frequency channels and sky-fractions., 12 pages and 4 figures. Matches the published version
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- 2018
31. Planck 2015 results. VI. LFI mapmaking
- Author
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Planck Collaboration, Ade, P. A. R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P, Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. -F, Catalano, A., Chamballu, A., Chary, R. -R, Christensen, P. R., Colombi, S., Colombo, L. P. L., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., Bernardis, P., Rosa, A., Zotti, G., Delabrouille, J., Dickinson, C., 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., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D. L., Henrot-Versillé, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Juvela, M., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Kunz, M., Kurki-Suonio, H., Lähteenmäki, A., Lamarre, J. -M, Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., 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., Novikov, D., Novikov, I., Paci, F., Pagano, L., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Timothy Pearson, Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L, Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Stompor, R., Sutton, D., Suur-Uski, A. -S, Sygnet, J. -F, Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Yvon, D., Zacchei, A., Zonca, A., Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de l'Accélérateur Linéaire (LAL), 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), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Planck, Ade, P. A. R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. F., Catalano, A., Chamballu, A., Chary, R. R., Christensen, P. R., Colombi, S., Colombo, L. P. L., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dole, H., Donzelli, Simona, Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D. L., Henrot Versillé, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Juvela, M., Keihänen, E, Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Kunz, M., Kurki Suonio, H., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., 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., Novikov, D., Novikov, I., Paci, F., Pagano, L., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Stompor, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Yvon, D., Zacchei, A., Zonca, A., Hélium : du fondamental aux applications (NEEL - HELFA), 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), 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), 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 Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Ade, P, Aghanim, N, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartolo, N, Battaner, E, Benabed, K, Benoît, A, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Bucher, M, Burigana, C, Butler, R, Calabrese, E, Cardoso, J, Catalano, A, Chamballu, A, Chary, R, Christensen, P, Colombi, S, Colombo, L, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, T, Eriksen, H, Fergusson, J, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Giard, M, Giraud Héraud, Y, Gjerløw, E, González Nuevo, J, Górski, K, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, F, Hanson, D, Harrison, D, Henrot Versillé, S, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Hurier, G, Jaffe, A, Jaffe, T, Juvela, M, Keskitalo, R, Kiiveri, K, Kisner, T, Knoche, J, Kunz, M, Kurki Suonio, H, Lähteenmäki, A, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leahy, J, Leonardi, R, Lesgourgues, J, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, Lindholm, V, López Caniego, M, Lubin, P, Macías Pérez, J, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Martin, P, Martínez González, E, Masi, S, Matarrese, S, Mazzotta, P, Mcgehee, P, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Nørgaard Nielsen, H, Novikov, D, Novikov, I, Paci, F, Pagano, L, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Pearson, T, Perdereau, O, Perotto, L, Perrotta, F, Pettorino, V, Pierpaoli, E, Pietrobon, D, Pointecouteau, E, Polenta, G, Pratt, G, Prézeau, G, Prunet, S, Puget, J, Rachen, J, Rebolo, R, Reinecke, M, Remazeilles, M, Renzi, A, Rocha, G, Rosset, C, Rossetti, M, Roudier, G, Rubiño Martín, J, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Scott, D, Seiffert, M, Shellard, E, Spencer, L, Stolyarov, V, Stompor, R, Sutton, D, Suur Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Valenziano, L, Valiviita, J, Van Tent, B, Vassallo, T, Vielva, P, Villa, F, Wade, L, Wandelt, B, Watson, R, Wehus, I, Yvon, D, Zacchei, A, and Zonca, A
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,Astronomy ,Monte Carlo method ,FOS: Physical sciences ,Cosmic background radiation ,01 natural sciences ,NO ,symbols.namesake ,Band-pass filter ,Settore FIS/05 - Astronomia e Astrofisica ,Methods: data analysis ,0103 physical sciences ,Planck ,data analysis [Methods] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries) ,QC ,QB ,Physics ,Astronomy and Astrophysics ,Space and Planetary Science ,Radiometer ,010308 nuclear & particles physics ,Estimation theory ,Astrophysics::Instrumentation and Methods for Astrophysics ,Planck temperature ,methods: data analysis – cosmic microwave background – numerical methods ,Covariance ,Astronomy and Astrophysic ,Polarization (waves) ,data analysi [Methods] ,symbols ,Astrophysics - Instrumentation and Methods for Astrophysics ,Cartography ,Methods: data analysi ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
CSIC, Consejo Superior de Investigaciones Científicas; ERC, European Research Council; MINECO, Ministerio de Economía y Competitividad; MPG, Max-Planck-Gesellschaft; NASA, National Aeronautics and Space Administration; etc., Ade, P.A.R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Bucher, M., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Catalano, A., Chamballu, A., Chary, R.-R., Christensen, P.R., Colombi, S., Colombo, L.P.L., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., 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., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K.M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F.K., Hanson, D., Harrison, D.L., Henrot-Versillé, S., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Juvela, M., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T.S., Knoche, J., Kunz, M., Kurki-Suonio, H., Lähteenmäki, A., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leahy, J.P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lubin, P.M., Macías-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Martin, P.G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., McGehee, P., Meinhold, P.R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., 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., Novikov, D., Novikov, I., Paci, F., Pagano, L., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T.J., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G.W., Prézeau, G., Prunet, S., Puget, J.-L., Rachen, J.P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J.A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M.D., Shellard, E.P.S., Spencer, L.D., Stolyarov, V., Stompor, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Watson, R., Wehus, I.K., Yvon, D., Zacchei, A., Zonca, A.
- Published
- 2016
32. Maximum rate of entropy emission
- Author
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Hamideh Nadi, Zahra Mirzaiyan, and Behrouz Mirza
- Subjects
Physics ,Angular momentum ,010308 nuclear & particles physics ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,General Physics and Astronomy ,Planck temperature ,General Relativity and Quantum Cosmology (gr-qc) ,Surface gravity ,01 natural sciences ,Upper and lower bounds ,Electric charge ,General Relativity and Quantum Cosmology ,Rényi entropy ,symbols.namesake ,Quantum mechanics ,0103 physical sciences ,symbols ,Planck ,010306 general physics ,Entropy (arrow of time) - Abstract
It is shown that adding hair like electric charge or angular momentum to the black hole decreases the amount of entropy emission. This motivates us to study the emission rate of entropy from black holes and conjecture a maximum limit (upper bound) on the rate of local entropy emission ($\dot{S}$) for thermal systems in four dimensional space time and argue that this upper bound is $\dot{S}\simeq k_{B} \sqrt{\frac{c^5}{\hbar G}}$. Also by considering R\`{e}nyi entropy, it is shown that Bekenstein-Hawking entropy leads to a maximum limit for the rate of entropy emission. We also suggest an upper bound on the surface gravity of the black holes which is called Planck surface gravity. Finally we obtain a relation between maximum rate of entropy emission, Planck surface gravity and Planck temperature of black holes., Comment: 18 pages, 1 figure
- Published
- 2020
33. Bayesian evidence against the Harrison-Zel’dovich spectrum in tensions with cosmological data sets
- Author
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Yabebal Fantaye, Alessandro Melchiorri, Alan Heavens, and Eleonora Di Valentino
- Subjects
Physics ,Spectral index ,Particle physics ,010308 nuclear & particles physics ,Physics beyond the Standard Model ,Dark matter ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Lambda ,01 natural sciences ,symbols.namesake ,0103 physical sciences ,symbols ,Neutrino ,Planck ,10. No inequality ,010303 astronomy & astrophysics ,Hubble's law - Abstract
Current cosmological constraints on the scalar spectral index of primordial fluctuations ${n}_{\mathrm{s}}$ in the $\mathrm{\ensuremath{\Lambda}}$Vcold dark matter ($\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$) model have excluded the minimal scale-invariant Harrison-Zel'dovich model (${n}_{\mathrm{s}}=1$; hereafter HZ) at high significance, providing support for inflation. In recent years, however, some tensions have emerged between different cosmological data sets that, if not due to systematics, could indicate the presence of new physics beyond the $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ model. In light of these developments, we evaluate the Bayesian evidence against HZ in different data combinations and model extensions. Considering only the Planck temperature data, we find inconclusive evidence against HZ when including variations in the neutrino number ${N}_{\mathrm{eff}}$ and/or the helium abundance ${Y}_{\text{He}}$. Adding the Planck polarization data, on the other hand, yields strong evidence against HZ in the extensions we considered. Perhaps most interestingly, Planck temperature data combined with local measurements of the Hubble parameter [A. G. Riess et al., Astrophys. J. 826, 56 (2016); A. G. Riess et al. Astrophys. J. 861, 126 (2018)] give as the most probable model a HZ spectrum, with additional neutrinos. However, with the inclusion of polarization, standard $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ is once again preferred, but the HZ model with extra neutrinos is not strongly disfavored. The possibility of fully ruling out the HZ spectrum is therefore ultimately connected with the solution to current tensions between cosmological data sets. If these tensions are confirmed by future data, then new physical mechanisms could be at work and a HZ spectrum could still offer a valid alternative.
- Published
- 2018
34. Constraints on Cosmological Parameters from the Angular Power Spectrum of a Combined 2500 deg2 SPT-SZ and Planck Gravitational Lensing Map
- Author
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Y. Omori, Lindsey Bleem, K. K. Schaffer, Adrian T. Lee, Lloyd Knox, N. W. Halverson, K. Vanderlinde, Matt Dobbs, T. M. Crawford, Gilbert Holder, Jason W. Henning, J. D. Hrubes, Eric J. Baxter, Stephen Padin, Antony A. Stark, Jeff McMahon, Elizabeth George, G. Simard, Joaquin Vieira, Zhen Hou, John E. Carlstrom, R. Williamson, W. B. Everett, K. T. Story, T. de Haan, Christian L. Reichardt, J. E. Ruhl, E. M. Leitch, T. Natoli, W. L. K. Wu, H-M. Cho, A. Manzotti, Z. K. Staniszewski, A. T. Crites, W. L. Holzapfel, J. T. Sayre, L. M. Mocanu, C. Pryke, R. Chown, Erik Shirokoff, Joseph J. Mohr, S. S. Meyer, N. L. Harrington, Daniel M. Luong-Van, Bradford Benson, C. L. Chang, and K. Aylor
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cold dark matter ,Cosmic microwave background ,FOS: Physical sciences ,Astrophysics ,Cosmological constant ,Astrophysics::Cosmology and Extragalactic Astrophysics ,cosmic background radiation ,Astronomy & Astrophysics ,01 natural sciences ,7. Clean energy ,Physical Chemistry ,Atomic ,symbols.namesake ,Particle and Plasma Physics ,weak [gravitational lensing] ,0103 physical sciences ,Nuclear ,Planck ,cosmological parameters ,010303 astronomy & astrophysics ,Physics ,010308 nuclear & particles physics ,Organic Chemistry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Spectral density ,Molecular ,Astronomy and Astrophysics ,Planck temperature ,South Pole Telescope ,Gravitational lens ,13. Climate action ,Space and Planetary Science ,symbols ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Physical Chemistry (incl. Structural) - Abstract
We report constraints on cosmological parameters from the angular power spectrum of a cosmic microwave background (CMB) gravitational lensing potential map created using temperature data from 2500 deg$^2$ of South Pole Telescope (SPT) data supplemented with data from Planck in the same sky region, with the statistical power in the combined map primarily from the SPT data. We fit the corresponding lensing angular power spectrum to a model including cold dark matter and a cosmological constant ($\Lambda$CDM), and to models with single-parameter extensions to $\Lambda$CDM. We find constraints that are comparable to and consistent with constraints found using the full-sky Planck CMB lensing data. Specifically, we find $\sigma_8 \Omega_{\rm m}^{0.25}=0.598 \pm 0.024$ from the lensing data alone with relatively weak priors placed on the other $\Lambda$CDM parameters. In combination with primary CMB data from Planck, we explore single-parameter extensions to the $\Lambda$CDM model. We find $\Omega_k = -0.012^{+0.021}_{-0.023}$ or $M_{\nu}< 0.70$eV both at 95% confidence, all in good agreement with results that include the lensing potential as measured by Planck over the full sky. We include two independent free parameters that scale the effect of lensing on the CMB: $A_{L}$, which scales the lensing power spectrum in both the lens reconstruction power and in the smearing of the acoustic peaks, and $A^{\phi \phi}$, which scales only the amplitude of the CMB lensing reconstruction power spectrum. We find $A^{\phi \phi} \times A_{L} =1.01 \pm 0.08$ for the lensing map made from combined SPT and Planck temperature data, indicating that the amount of lensing is in excellent agreement with what is expected from the observed CMB angular power spectrum when not including the information from smearing of the acoustic peaks., Comment: 12 pages, 7 figures, submitted to ApJ, typo in bandpower table corrected
- Published
- 2018
35. Reducing the H0 and σ8 tensions with dark matter-neutrino interactions
- Author
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François R. Bouchet, Céline Bœhm, Eleonora Di Valentino, and E. Hivon
- Subjects
Physics ,010308 nuclear & particles physics ,Cosmic microwave background ,Dark matter ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,symbols.namesake ,0103 physical sciences ,symbols ,Planck ,Neutrino ,Multipole expansion ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Hubble's law - Abstract
The introduction of dark matter-neutrino interactions modifies the cosmic microwave background (CMB) angular power spectrum at all scales, thus affecting the reconstruction of the cosmological parameters. Such interactions can lead to a slight increase of the value of H 0 and a slight decrease of S 8 ≡ σ 8 √ Ω m / 0.3 , which can help reduce somewhat the tension between the CMB and weak lensing or Cepheids data sets. Here we show that it is impossible to solve both tensions simultaneously. While the 2015 Planck temperature and low multipole polarization data combined with the Cepheids data sets prefer large values of the Hubble rate (up to H 0 = 72.1 + 1.5 − 1.7 km / s / Mpc , when N eff is free to vary), the σ 8 parameter remains too large to reduce the σ 8 tension. Adding high multipole Planck polarization data does not help since this data shows a strong preference for low values of H 0 , thus worsening current tensions, even though they also prefer smaller value of σ 8 .
- Published
- 2018
36. Testing the ABS method with the simulated Planck temperature maps
- Author
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Le Zhang, Yuxi Zhao, Jun Zhang, Pengjie Zhang, Jian Yao, and Larissa Santos
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Cosmic microwave background ,Spectral density ,Estimator ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Galactic plane ,01 natural sciences ,Computational physics ,symbols.namesake ,Space and Planetary Science ,0103 physical sciences ,symbols ,Range (statistics) ,Planck ,010303 astronomy & astrophysics ,Microwave ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
In this study, we apply the Analytical method of Blind Separation (ABS) of the cosmic microwave background (CMB) from foregrounds to estimate the CMB temperature power spectrum from multi-frequency microwave maps. We test the robustness of the ABS estimator and assess the accuracy of the power spectrum recovery by using realistic simulations based on the seven-frequency Planck data, including various frequency-dependent and spatially-varying foreground components (synchrotron, free-free, thermal dust and anomalous microwave emission), as well as an uncorrelated Gaussian-distributed instrumental noise. Considering no prior information about the foregrounds, the ABS estimator can analytically recover the CMB power spectrum over almost all scales with less than $0.5\%$ error for maps where the Galactic plane region ($|b, 12 pages, 11 figures, revised version, accepted to APJS
- Published
- 2018
- Full Text
- View/download PDF
37. Foreground Biases on Primordial Non-Gaussianity Measurements from the CMB Temperature Bispectrum: Implications for Planck and Beyond
- Author
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J. Colin Hill
- Subjects
High Energy Physics - Theory ,Physics ,Particle physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Cosmic microwave background ,FOS: Physical sciences ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,High Energy Physics - Phenomenology ,symbols.namesake ,Gravitational lens ,High Energy Physics - Phenomenology (hep-ph) ,High Energy Physics - Theory (hep-th) ,Non-Gaussianity ,Cosmic infrared background ,0103 physical sciences ,symbols ,Trispectrum ,Planck ,010303 astronomy & astrophysics ,Bispectrum ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The cosmic microwave background (CMB) temperature bispectrum is currently the most precise tool for constraining primordial non-Gaussianity (NG). The Planck temperature data tightly constrain the amplitude of local-type NG: $f_{\rm NL}^{\rm loc} = 2.5 \pm 5.7$. Here, we compute previously-neglected foreground biases in temperature-based $f_{\rm NL}^{\rm loc}$ measurements, due to the integrated Sachs-Wolfe (ISW) effect, gravitational lensing, the thermal and kinematic Sunyaev-Zel'dovich effects, and the cosmic infrared background. While standard analyses already subtract a significant bias on $f_{\rm NL}^{\rm loc}$ due to the ISW-lensing bispectrum, many other secondary anisotropy terms are present in the temperature bispectrum. We compute the dominant biases on $f_{\rm NL}^{\rm loc}$ arising from these signals. Most of the biases are non-blackbody, and are thus reduced by multifrequency component separation methods; however, recent analyses have found that extragalactic foregrounds are present at non-negligible levels in the Planck component-separated maps. Moreover, the Planck FFP8 simulations do not include the foreground correlations that generate these biases. We compute the biases for individual frequencies; some are comparable to the statistical error bar on $f_{\rm NL}^{\rm loc}$, even for the main CMB channels (100, 143, and 217 GHz). For future experiments, they greatly exceed the statistical error (considering temperature only). Alternatively, the foreground contributions can be marginalized over, but this leads to a non-negligible increase in the error bar on $f_{\rm NL}^{\rm loc}$. A full assessment will require calculations in tandem with component separation, ideally using simulations. We also compute these biases for equilateral and orthogonal NG, finding large effects for the latter. We conclude that the search for primordial NG using Planck data may not yet be over., Comment: 18 pages, 10 figures, abstract slightly abridged, comments welcome; v2: 26 pages, 22 figures, results unchanged, added new results for equilateral and orthogonal NG; v3: matches published version
- Published
- 2018
- Full Text
- View/download PDF
38. Varying Planck’s Constant
- Author
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Maurice de Gosson
- Subjects
Physics ,symbols.namesake ,Planck energy ,Planck time ,Planck force ,Planck particle ,Quantum electrodynamics ,symbols ,Planck mass ,Planck momentum ,Planck temperature ,Planck length - Published
- 2017
39. Testing physical models for dipolar asymmetry with CMB polarization
- Author
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K. M. Górski, D. Contreras, J. P. Zibin, Douglas Scott, A. J. Banday, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,satellite: Planck ,Primordial fluctuations ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,media_common.quotation_subject ,Cosmic microwave background ,FOS: Physical sciences ,cosmic background radiation: polarization ,Astrophysics ,01 natural sciences ,Asymmetry ,symbols.namesake ,polarization: asymmetry ,0103 physical sciences ,Planck ,010303 astronomy & astrophysics ,media_common ,Physics ,010308 nuclear & particles physics ,fluctuation: primordial ,Planck temperature ,Cosmic variance ,Polarization (waves) ,Computational physics ,modulation ,Amplitude ,symbols ,fluctuation: statistical ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics ,temperature: anisotropy - Abstract
The cosmic microwave background (CMB) temperature anisotropies exhibit a large-scale dipolar power asymmetry. To determine whether this is due to a real, physical modulation or is simply a large statistical fluctuation requires the measurement of new modes. Here we forecast how well CMB polarization data from \Planck\ and future experiments will be able to confirm or constrain physical models for modulation. Fitting several such models to the \Planck\ temperature data allows us to provide predictions for polarization asymmetry. While for some models and parameters \Planck\ polarization will decrease error bars on the modulation amplitude by only a small percentage, we show, importantly, that cosmic-variance-limited (and in some cases even \Planck) polarization data can decrease the errors by considerably better than the expectation of $\sqrt 2$ based on simple $\ell$-space arguments. We project that if the primordial fluctuations are truly modulated (with parameters as indicated by \Planck\ temperature data) then \Planck\ will be able to make a 2$\sigma$ detection of the modulation model with 20--75\% probability, increasing to 45--99\% when cosmic-variance-limited polarization is considered. We stress that these results are quite model dependent. Cosmic variance in temperature is important: combining statistically isotropic polarization with temperature data will spuriously increase the significance of the temperature signal with 30\% probability for \Planck., Comment: 18 pages, 11 figures, 2 tables. Version updated to match PRD version
- Published
- 2017
40. Maximal temperature of the gas in AdS space-time
- Author
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Dejan Stojkovic and De-Chang Dai
- Subjects
High Energy Physics - Theory ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Black hole information paradox ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,01 natural sciences ,General Relativity and Quantum Cosmology ,symbols.namesake ,Micro black hole ,AdS/QCD correspondence ,Quantum mechanics ,0103 physical sciences ,010306 general physics ,Virtual black hole ,Black hole thermodynamics ,Physics ,010308 nuclear & particles physics ,Planck temperature ,Black hole ,High Energy Physics - Theory (hep-th) ,Quantum electrodynamics ,symbols ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Hawking radiation - Abstract
Assuming only statistical mechanics and general relativity, we calculate the maximal temperature of gas of particles placed in AdS space-time. If two particles with a given center of mass energy come close enough, according to classical gravity they will form a black hole. We focus only on the black holes with Hawking temperature lower than the environment, because they do not disappear. The number density of such black holes grows with the temperature in the system. At a certain finite temperature, the thermodynamical system will be dominated by black holes. This critical temperature is lower than the Planck temperature for the values of the AdS vacuum energy density below the Planck density. This result might be interesting from the AdS/CFT correspondence point of view, since it is different from the Hawking-Page phase transition, and it is not immediately clear what effect dynamically limits the maximal temperature of the thermal state on the CFT side of the correspondence., Comment: Published in Phys.Rev. D95 (2017) no.8, 085015
- Published
- 2017
- Full Text
- View/download PDF
41. Cosmological discordances II: Hubble constant, Planck and large-scale-structure data sets
- Author
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Mustapha Ishak and Weikang Lin
- Subjects
Physics ,Planck energy ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Age of the universe ,010308 nuclear & particles physics ,Cosmic microwave background ,FOS: Physical sciences ,Planck temperature ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,General Relativity and Quantum Cosmology (gr-qc) ,01 natural sciences ,General Relativity and Quantum Cosmology ,symbols.namesake ,Hubble volume ,0103 physical sciences ,Outlier ,symbols ,Planck ,010303 astronomy & astrophysics ,Hubble's law ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We examine systematically the (in)consistency between cosmological constraints as obtained from various current data sets of the expansion history, Large Scale Structure (LSS), and Cosmic Microwave Background (CMB) from Planck. We run (dis)concordance tests within each set and across the sets using a recently introduced index of inconsistency (IOI) capable of dissecting inconsistencies between two or more data sets. First, we compare the constraints on $H_0$ from five different methods and find that the IOI drops from 2.85 to 0.88 (on Jeffreys' scales) when the local $H_0$ measurements is removed. This seems to indicate that the local measurement is an outlier, thus favoring a systematics-based explanation. We find a moderate inconsistency (IOI=2.61) between Planck temperature and polarization. We find that current LSS data sets including WiggleZ, SDSS RSD, CFHTLenS, CMB lensing and SZ cluster count, are consistent one with another and when all combined. However, we find a persistent moderate inconsistency between Planck and individual or combined LSS probes. For Planck TT+lowTEB versus individual LSS probes, the IOI spans the range 2.92--3.72 and increases to 3.44--4.20 when the polarization data is added in. The joint LSS versus the combined Planck temperature and polarization has an IOI of 2.83 in the most conservative case. But if Planck lowTEB is added to the joint LSS to constrain $\tau$ and break degeneracies, the inconsistency between Planck and joint LSS data increases to the high-end of the moderate range with IOI=4.81. Whether due to systematic effects in the data or to the underlying model, these inconsistencies need to be resolved. Finally, we perform forecast calculations using LSST and find that the discordance between Planck and future LSS data, if it persists as present, can rise up to a high IOI of 17, thus falling in the strong range of inconsistency. (Abridged)., Comment: 14 pages, 3 figures; matches version published in PRD
- Published
- 2017
- Full Text
- View/download PDF
42. Measurements of the Temperature and E-Mode Polarization of the CMB from 500 Square Degrees of SPTpol Data
- Author
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Elizabeth George, C. Pryke, A. J. Gilbert, Adam Anderson, L. M. Mocanu, W. L. K. Wu, Ryan Keisler, T. Veach, Robert I. Citron, Peter A. R. Ade, K. T. Story, N. Huang, Gensheng Wang, Lindsey Bleem, Johannes Hubmayr, Jason Gallicchio, N. L. Harrington, Volodymyr Yefremenko, T. de Haan, S. S. Meyer, H. C. Chiang, Matt Dobbs, Nathan Whitehorn, Bradford Benson, Dale Li, A. E. Lowitz, Gene C. Hilton, T. M. Crawford, J. T. Sayre, John E. Carlstrom, A. Manzotti, John P. Nibarger, Andrew Nadolski, W. B. Everett, C. Corbett Moran, Jeff McMahon, C. L. Chang, J. D. Hrubes, E. M. Leitch, A. T. Crites, Joshua Montgomery, N. W. Halverson, S. Hoover, Stephen Padin, James A. Beall, J. E. Ruhl, Joaquin Vieira, K. Vanderlinde, Kent D. Irwin, W. L. Holzapfel, V. Novosad, Jason W. Henning, T. Natoli, H-M. Cho, C. Sievers, Christian L. Reichardt, Zhen Hou, Adrian T. Lee, Lloyd Knox, Carole Tucker, Jason E. Austermann, Antony A. Stark, Graeme Smecher, Benjamin Saliwanchik, Gilbert Holder, Amy N. Bender, and K. K. Schaffer
- Subjects
Expansion rate ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmic microwave background ,Cosmic background radiation ,FOS: Physical sciences ,cosmic background radiation ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Atomic ,Physical Chemistry ,01 natural sciences ,Spectral line ,symbols.namesake ,Particle and Plasma Physics ,0103 physical sciences ,Nuclear ,cosmological parameters ,010303 astronomy & astrophysics ,Physics ,polarization ,010308 nuclear & particles physics ,Molecular ,Astronomy and Astrophysics ,Planck temperature ,Polarization (waves) ,observations [cosmology] ,3. Good health ,Space and Planetary Science ,astro-ph.CO ,symbols ,Multipole expansion ,Astronomical and Space Sciences ,Physical Chemistry (incl. Structural) ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present measurements of the $E$-mode polarization angular auto-power spectrum ($EE$) and temperature-$E$-mode cross-power spectrum ($TE$) of the cosmic microwave background (CMB) using 150 GHz data from three seasons of SPTpol observations. We report the power spectra over the spherical harmonic multipole range $50 < \ell \leq 8000$, and detect nine acoustic peaks in the $EE$ spectrum with high signal-to-noise ratio. These measurements are the most sensitive to date of the $EE$ and $TE$ power spectra at $\ell > 1050$ and $\ell > 1475$, respectively. The observations cover 500 deg$^2$, a fivefold increase in area compared to previous SPTpol analyses, which increases our sensitivity to the photon diffusion damping tail of the CMB power spectra enabling tighter constraints on \LCDM model extensions. After masking all sources with unpolarized flux $>50$ mJy we place a 95% confidence upper limit on residual polarized point-source power of $D_\ell = \ell(\ell+1)C_\ell/2\pi 1000$ results in a preference for a higher value of the expansion rate ($H_0 = 71.3 \pm 2.1\,\mbox{km}\,s^{-1}\mbox{Mpc}^{-1}$ ) and a lower value for present-day density fluctuations ($\sigma_8 = 0.77 \pm 0.02$)., Comment: Updated to match version accepted to ApJ. 34 pages, 17 figures, 6 tables
- Published
- 2017
- Full Text
- View/download PDF
43. The Atacama Cosmology Telescope: Two-Season ACTPol Spectra and Parameters
- Author
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Brian J. Koopman, Jeff McMahon, Kavilan Moodley, Joanna Dunkley, Felipe Menanteau, David N. Spergel, Simon Muya Kasanda, Jesse Treu, Graeme E. Addison, J. Richard Bond, Shawn W. Henderson, Sara M. Simon, Simone Aiola, John P. Hughes, Matt Hilton, Joseph W. Britton, Alexander van Engelen, Tobias A. Marriage, Jonathan T. Ward, Robert Thornton, Michael R. Nolta, Christine G. Pappas, Rahul Datta, Peter A. R. Ade, Gene C. Hilton, Jeff Klein, Nicholas Battaglia, Mathew S. Madhavacheril, Matthew Hasselfield, Arthur Kosowsky, Benjamin L. Schmitt, Devin Crichton, Charles Munson, Thibaut Louis, Zhiqi Huang, Erminia Calabrese, Kevin Coughlin, Francesco De Bernardis, Neelima Sehgal, Megan Gralla, Kent D. Irwin, Hsiao-Mei Cho, J. Colin Hill, Edward J. Wollack, Michael D. Niemack, Steve K. Choi, Loïc Maurin, Lyman A. Page, Suzanne T. Staggs, S. P. Patty Ho, Federico Nati, Mandana Amiri, Kevin M. Huffenberger, Emmanuel Schaan, Johannes Hubmayr, Eric R. Switzer, Elio Angile, Mark Halpern, Simone Ferraro, James A. Beall, Kevin T. Crowley, Hy Trac, Mark J. Devlin, Patricio A. Gallardo, R. Allison, Simon Dicker, Sigurd Naess, Leopoldo Infante, Laura Newburgh, Dale Li, Adam D. Hincks, Carole Tucker, Bruce Partridge, Anna E. Fox, Jon Sievers, Renée Hlozek, E. Grace, Felipe Rojas, Rolando Dünner, John P. Nibarger, Marius Lungu, Carolina Núñez, Blake D. Sherwin, 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 ), ACTPol, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Louis, T, Grace, E, Hasselfield, M, Lungu, M, Maurin, L, Addison, G, Ade, P, Aiola, S, Allison, R, Amiri, M, Angile, E, Battaglia, N, Beall, J, De Bernardis, F, Bond, J, Britton, J, Calabrese, E, Cho, H, Choi, S, Coughlin, K, Crichton, D, Crowley, K, Datta, R, Devlin, M, Dicker, S, Dunkley, J, Dünner, R, Ferraro, S, Fox, A, Gallardo, P, Gralla, M, Halpern, M, Henderson, S, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hlozek, R, Patty Ho, S, Huang, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Infante, L, Irwin, K, Kasanda, S, Klein, J, Koopman, B, Kosowsky, A, Li, D, Madhavacheril, M, Marriage, T, Mcmahon, J, Menanteau, F, Moodley, K, Munson, C, Naess, S, Nati, F, Newburgh, L, Nibarger, J, Niemack, M, Nolta, M, Nuñez, C, Page, L, Pappas, C, Partridge, B, Rojas, F, Schaan, E, Schmitt, B, Sehgal, N, Sherwin, B, Sievers, J, Simon, S, Spergel, D, Staggs, S, Switzer, E, Thornton, R, Trac, H, Treu, J, Tucker, C, Engelen, A, Ward, J, and Wollack, E
- Subjects
cosmological model ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Astrophysics ,7. Clean energy ,01 natural sciences ,Atomic ,Particle and Plasma Physics ,CMBR experiments ,010303 astronomy & astrophysics ,QC ,media_common ,QB ,helium: primordial ,Physics ,Hubble constant ,Celestial equator ,Astrophysics::Instrumentation and Methods for Astrophysics ,cosmological parameters from CMBR ,Planck temperature ,CMB cold spot ,Nuclear & Particles Physics ,Atacama Cosmology Telescope ,symbols ,astro-ph.CO ,power spectrum: angular dependence ,Astrophysics::Earth and Planetary Astrophysics ,Neutrino ,CMBR experiment ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics ,CMBR polarisation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,satellite: Planck ,media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,symbols.namesake ,0103 physical sciences ,Nuclear ,Planck ,Astrophysics::Galaxy Astrophysics ,beam: polarization ,010308 nuclear & particles physics ,baryon: density ,Molecular ,Astronomy and Astrophysics ,13. Climate action ,Sky ,WMAP ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Hubble's law - Abstract
We present the temperature and polarization angular power spectra measured by the Atacama Cosmology Telescope Polarimeter (ACTPol). We analyze night-time data collected during 2013-14 using two detector arrays at 149 GHz, from 548 deg$^2$ of sky on the celestial equator. We use these spectra, and the spectra measured with the MBAC camera on ACT from 2008-10, in combination with Planck and WMAP data to estimate cosmological parameters from the temperature, polarization, and temperature-polarization cross-correlations. We find the new ACTPol data to be consistent with the LCDM model. The ACTPol temperature-polarization cross-spectrum now provides stronger constraints on multiple parameters than the ACTPol temperature spectrum, including the baryon density, the acoustic peak angular scale, and the derived Hubble constant. Adding the new data to planck temperature data tightens the limits on damping tail parameters, for example reducing the joint uncertainty on the number of neutrino species and the primordial helium fraction by 20%., 23 pages, 25 figures
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- 2017
44. Planck intermediate results. LI. Features in the cosmic microwave background temperature power spectrum and shifts in cosmological parameters
- Author
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Aghanim, N., Akrami, Y., Ashdown, Mark, Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. Belén, Bartolo, Nicola, Basak, S., Benabed, K., Vittorio, N., Wandelt, B. D., Enßlin, T. A., Wehus, I. K., White, Martin, Zacchei, A., Zonca, A., Borrill, J., Bouchet, F. R., Boulanger, F., Kim, J., Bracco, Andrea, Burigana, C., Calabrese, E., Eriksen, H. K., Cardoso, J. F., Challinor, A., Chiang, H. C., Colombo, L.P.L., Combet, C., Crill, B. P., Kisner, T. S., Curto, Andrés, Cuttaia, F., Bernardis, P. de, Rosa, A. de, Fantaye, Y., Zotti, G. de, Delabrouille, J., Valentino, E. di, Dickinson, C., Diego, José María, Mennella, A., Doré, O., Ducout, A., Dupac, X., Dusini, S., Finelli, F., Forastieri, F., Frailis, M., Franceschi, E., Frolov, A., McEwen, J. D., Knox, L., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R., Gerbino, M., González-Nuevo, J., Górski, K. M., Gratton, S., Gruppuso, A., Gudmundsson, J.E., Krachmalnicof, N., Meinhold, P. R., Herranz, D., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kunz, M., Kurki-Suonio, H., Lagache, Guilaine, Lamarre, J.-M., Lasenby, Anthony N., Renzi, A., Lattanzi, M., Lawrence, C. R., Jeune, M. le, Migliaccio, M., Levrier, F., Lewis, A., Liguori, Michele, Lilje, P. B., Lilley, M., Lindholm, V., Rocha, G., López-Caniego, M., Lubin, P. M., Ma, Y.-Z, Macías-Pérez, J. F., Millea, M., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Bonaldi, A., Martin, P. G., Martínez-González, Enrique, Matarrese, S., Mauri, N., Miville-Deschênes, M. A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Bersanelli, M., Rossetti, M., Moss, A., Narimani, A., Natoli, P., Oxborrow, C. A., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Patrizii, L., Pettorino, V., Roudier, G., Bielewicz, P., Piacentini, F., Polastri, L., Polenta, G., Puget, J.-L., Rachen, J. P., Racine, B., Reinecke, M., Remazeilles, Mathieu, Rubiño-Martín, J. A., Ruiz-Granados, Beatriz, Salvati, L., Sandri, M., Savelainen, M., Efstathiou, G., Scott, D., Sirignano, C., Sirri, G., Bonavera, Laura, Stanco, L., Suur-Uski, A.-S., Tauber, J. A., Tavagnacco, D., Tenti, M., Toffolatti, L., Elsner, F., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Bond, J. R., Tent, F. van, Vielva, P., Villa, F., 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut de recherche en astrophysique et planétologie (IRAP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Traitement et Communication de l'Information (LTCI), Télécom ParisTech-Institut Mines-Télécom [Paris] (IMT)-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), 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)-Université Grenoble Alpes (UGA), Université Paris-Sud - Paris 11 (UP11), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sorbonne (UP4), 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), Planck, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Aghanim, N, Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, A, Barreiro, R, Bartolo, N, Basak, S, Benabed, K, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Burigana, C, Calabrese, E, Cardoso, J, Challinor, A, Chiang, H, Colombo, L, Combet, C, Crill, B, Curto, A, Cuttaia, F, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Di Valentino, E, Dickinson, C, Diego, J, Doré, O, Ducout, A, Dupac, X, Dusini, S, Efstathiou, G, Elsner, F, Enßlin, T, Eriksen, H, Fantaye, Y, Finelli, F, Forastieri, F, Frailis, M, Franceschi, E, Frolov, A, Galeotta, S, Galli, S, Ganga, K, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Górski, K, Gratton, S, Gruppuso, A, Gudmundsson, J, Herranz, D, Hivon, E, Huang, Z, Jaffe, A, Jones, W, Keihänen, E, Keskitalo, R, Kiiveri, K, Kim, J, Kisner, T, Knox, L, Krachmalnicoff, N, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Le Jeune, M, Levrier, F, Lewis, A, Liguori, M, Lilje, P, Lilley, M, Lindholm, V, López-Caniego, M, Lubin, P, Ma, Y, Macías-Pérez, J, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martínez-González, E, Matarrese, S, Mauri, N, Mcewen, J, Meinhold, P, Mennella, A, Migliaccio, M, Millea, M, Miville-Deschênes, M, Molinari, D, Moneti, A, Montier, L, Morgante, G, Moss, A, Narimani, A, Natoli, P, Oxborrow, C, Pagano, L, Paoletti, D, Partridge, B, Patanchon, G, Patrizii, L, Pettorino, V, Piacentini, F, Polastri, L, Polenta, G, Puget, J, Rachen, J, Racine, B, Reinecke, M, Remazeilles, M, Renzi, A, Rocha, G, Rossetti, M, Roudier, G, Rubiño-Martín, J, Ruiz-Granados, B, Salvati, L, Sandri, M, Savelainen, M, Scott, D, Sirignano, C, Sirri, G, Stanco, L, Suur-Uski, A, Tauber, J, Tavagnacco, D, Tenti, M, Toffolatti, L, Tomasi, M, Tristram, M, Trombetti, T, Valiviita, J, Van Tent, F, Vielva, P, Villa, F, Vittorio, N, Wandelt, B, Wehus, I, White, M, Zacchei, A, Zonca, A, Aghanim, N., Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Benabed, K., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Burigana, C., Calabrese, E., Cardoso, J.-F., Challinor, A., Chiang, H.C., Colombo, L.P.L., Combet, C., Crill, B.P., Curto, A., Cuttaia, F., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Di Valentino, E., Dickinson, C., Diego, J.M., Doré, O., Ducout, A., Dupac, X., Dusini, S., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Fantaye, Y., Finelli, F., Forastieri, F., Frailis, M., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Génova-Santos, R.T., Gerbino, M., González-Nuevo, J., Górski, K.M., Gratton, S., Gruppuso, A., Gudmundsson, J.E., Herranz, D., Hivon, E., Huang, Z., Jaffe, A.H., Jones, W.C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T.S., Knox, L., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Le Jeune, M., Levrier, F., Lewis, A., Liguori, M., Lilje, P.B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P.M., Ma, Y.-Z., Macías-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P.G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J.D., Meinhold, P.R., Mennella, A., Migliaccio, M., Millea, M., Miville-Deschênes, M.-A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Moss, A., Narimani, A., Natoli, P., Oxborrow, C.A., Pagano, L., Paoletti, D., Partridge, B., Patanchon, G., Patrizii, L., Pettorino, V., Piacentini, F., Polastri, L., Polenta, G., Puget, J.-L., Rachen, J.P., Racine, B., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rossetti, M., Roudier, G., Rubiño-Martín, J.A., Ruiz-Granados, B., Salvati, L., Sandri, M., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Stanco, L., Suur-Uski, A.-S., Tauber, J.A., Tavagnacco, D., Tenti, M., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, F., Vielva, P., Villa, F., Vittorio, N., Wandelt, B.D., Wehus, I.K., White, M., Zacchei, A., Zonca, A., Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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-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), Université de Toulouse (UT), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Science and Technology Facilities Council (STFC), Science and Technology Facilities Council, 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 ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Université Pierre et Marie Curie - Paris 6 ( UPMC ), Laboratoire Traitement et Communication de l'Information ( LTCI ), Télécom ParisTech-Institut Mines-Télécom [Paris]-Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), 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 ) -Université Grenoble Alpes ( UGA ), Université Paris-Sud - Paris 11 ( UP11 ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), Université Paris-Sorbonne ( UP4 ), 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 ), Fundação para a Ciência e a Tecnologia (Portugal), European Research Council, European Commission, Ministerio de Economía, Industria y Competitividad (España), Consejo Superior de Investigaciones Científicas (España), Department of Energy (US), National Aeronautics and Space Administration (US), Consiglio Nazionale delle Ricerche, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), European Space Agency, Science and Technology Facilities Council (UK), Ministério da Ciência, Tecnologia e Ensino Superior (Portugal), Science Foundation Ireland, Swiss Space Office, DTU Space (Denmark), Canadian Space Agency, Federal Ministry of Education and Research (Germany), German Research Foundation, Academy of Finland, Center for Science (Finland), Red Española de Supercomputación, Research Council of Norway, Department of Physics, and Helsinki Institute of Physics
- Subjects
CMB ANISOTROPIES ,Cosmological parameter ,cosmological model ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Astronomy ,Cosmic microwave background ,UNIVERSE ,Astrophysics ,cosmic background radiation ,Cosmic background radiation ,Cosmology: observation ,7. Clean energy ,01 natural sciences ,Omega ,observations, cosmic background radiation, cosmological parameters, cosmology: theory [cosmology] ,power spectrum: temperature ,cosmology: theory ,MAPS ,Optical depth (astrophysics) ,parameter space ,observations [Cosmology] ,GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries) ,010303 astronomy & astrophysics ,matter: density ,QB ,Physics ,Spectral index ,Settore FIS/05 ,statistical analysis: Bayesian ,Cosmological parameters ,Cosmology: observations ,Cosmology: theory ,astro-ph.CO ,Astronomy and Astrophysics ,Space and Planetary Science ,Planck temperature ,CMB cold spot ,Physical Sciences ,symbols ,moment: multipole ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,satellite: Planck ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,114 Physical sciences ,horizon ,cosmology: observations, cosmic background radiation, cosmological parameters, cosmology: theory ,NO ,power spectrum: primordial ,symbols.namesake ,Settore FIS/05 - Astronomia e Astrofisica ,theory [Cosmology] ,0103 physical sciences ,cosmology: observations ,cosmological parameters ,Planck ,Science & Technology ,010308 nuclear & particles physics ,baryon: density ,Spectral density ,Astronomy and Astrophysic ,115 Astronomy, Space science ,cosmic background radiation: temperature ,0201 Astronomical And Space Sciences ,13. Climate action ,WMAP ,PROBE WMAP OBSERVATIONS ,RADIATION ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,APPROXIMATION - Abstract
European Space Agency, Centre National D'etudes Spatiales, CNRS/INSU-IN2P3-INP (France), Agenzia Spaziale Italiana (ASI), Italian National Research Council, Istituto Nazionale Astrofisica (INAF), National Aeronautics & Space Administration (NASA), United States Department of Energy (DOE), Science & Technology Facilities Council (STFC), UKSA (UK), Consejo Superior de Investigaciones Cientificas (CSIC), MINECO (Spain), JA (Spain), RES (Spain), CSC (Finland), Finnish Funding Agency for Technology & Innovation (TEKES), AoF (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, ERC (EU), European Union (EU), Labex ILP
- Published
- 2017
45. Dark energy at early times, the Hubble parameter, and the string axiverse
- Author
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Marc Kamionkowski and Tanvi Karwal
- Subjects
Physics ,010308 nuclear & particles physics ,Cosmic microwave background ,Spectral density ,Planck temperature ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Cosmological constant ,Astrophysics ,01 natural sciences ,Redshift ,symbols.namesake ,0103 physical sciences ,symbols ,Dark energy ,Planck ,010303 astronomy & astrophysics ,Hubble's law - Abstract
Precise measurements of the cosmic microwave background (CMB) power spectrum are in excellent agreement with the predictions of the standard $\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$ cosmological model. However, there is some tension between the value of the Hubble parameter ${H}_{0}$ inferred from the CMB and that inferred from observations of the Universe at lower redshifts, and the unusually small value of the dark-energy density is a puzzling ingredient of the model. In this paper, we explore a scenario with a new exotic energy density that behaves like a cosmological constant at early times and then decays quickly at some critical redshift ${z}_{c}$. An exotic energy density like this is motivated by some string-axiverse-inspired scenarios for dark energy. By increasing the expansion rate at early times, the very precisely determined angular scale of the sound horizon at decoupling can be preserved with a larger Hubble constant. We find, however, that the Planck temperature power spectrum tightly constrains the magnitude of the early dark-energy density and thus any shift in the Hubble constant obtained from the CMB. If the reionization optical depth is required to be smaller than the Planck 2016 $2\ensuremath{\sigma}$ upper bound $\ensuremath{\tau}\ensuremath{\lesssim}0.0774$, then early dark energy allows a Hubble-parameter shift of at most $1.6\text{ }\mathrm{km}\text{ }{\mathrm{s}}^{\ensuremath{-}1}\text{ }{\mathrm{Mpc}}^{\ensuremath{-}1}$ (at ${z}_{c}\ensuremath{\simeq}1585$), too small to fully alleviate the Hubble-parameter tension. Only if $\ensuremath{\tau}$ is increased by more than $5\ensuremath{\sigma}$ can the CMB Hubble parameter be brought into agreement with that from local measurements. In the process, we derive strong constraints to the contribution of early dark energy at the time of recombination---it can never exceed $\ensuremath{\sim}2%$ of the radiation/matter density for $10\ensuremath{\lesssim}{z}_{c}\ensuremath{\lesssim}1{0}^{5}$.
- Published
- 2016
46. Averaged universe confronted with cosmological observations: A fully covariant approach
- Author
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Mustapha Ishak, Weikang Lin, and Tharake Wijenayake
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Cosmic microwave background ,FOS: Physical sciences ,Spectral density ,Planck temperature ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Omega ,General Relativity and Quantum Cosmology ,Cosmology ,symbols.namesake ,Theoretical physics ,Friedmann–Lemaître–Robertson–Walker metric ,0103 physical sciences ,symbols ,Covariant transformation ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
One of the outstanding problems in general relativistic cosmology is that of the averaging. That is, how the lumpy universe that we observe at small scales averages out to a smooth Friedmann-Lemaitre-Robertson-Walker (FLRW) model. The root of the problem is that averaging does not commute with the Einstein equations that govern the dynamics of the model. This leads to the well-know question of backreaction in cosmology. In this work, we approach the problem using the covariant framework of Macroscopic Gravity (MG). We use its cosmological solution with a flat FLRW macroscopic background where the result of averaging cosmic inhomogeneities has been encapsulated into a backreaction density parameter denoted $\Omega_\mathcal{A}$. We constrain this averaged universe using available cosmological data sets of expansion and growth including, for the first time, a full CMB analysis from Planck temperature anisotropy and polarization data, the supernovae data from Union 2.1, the galaxy power spectrum from WiggleZ, the weak lensing tomography shear-shear cross correlations from the CFHTLenS survey and the baryonic acoustic oscillation data from 6Df, SDSS DR7 and BOSS DR9. We find that $-0.0155 \le \Omega_\mathcal{A} \le 0$ (at the 68\% CL) thus providing a tight upper-bound on the backreaction term. We also find that the term is strongly correlated with cosmological parameters such $\Omega_\Lambda$, $\sigma_8$ and $H_0$. While small, a backreaction density parameter of a few percent should be kept in consideration along with other systematics for precision cosmology., Comment: 6 pages, 1 figure; matches version published in PRD
- Published
- 2016
47. Parameter discordance in Planck CMB and low-redshift measurements: projection in the primordial power spectrum
- Author
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Arman Shafieloo, Dhiraj Kumar Hazra, and Tarun Souradeep
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,010308 nuclear & particles physics ,Cosmic microwave background ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planck temperature ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,General Relativity and Quantum Cosmology ,Cosmology ,Redshift ,High Energy Physics - Phenomenology ,symbols.namesake ,High Energy Physics - Phenomenology (hep-ph) ,0103 physical sciences ,Dark energy ,symbols ,Planck ,Weak gravitational lensing ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Hubble's law - Abstract
We discuss the discordance between the estimated values of the cosmological parameters from Planck assuming the concordance $\Lambda$CDM model and low-redshift measurements. In particular, we consider the Hubble constant mismatch between Planck temperature constraint for the $\Lambda$CDM model and the Riess et. al. local measurements as well as the discordance between the estimated value of $S_8$ from Planck and some weak lensing surveys such as Kilo Degree Survey (KiDS-450) and Dark Energy Survey (DES) observations. The discordance can come from a wide range of non-standard cosmological or astrophysical processes as well as from some particular systematics of the observations. In this paper, without considering any particular astrophysical process or extension to the standard model at the background level, we seek solely to project the effect of these differences in the values of the key cosmological parameters on to the shape of the primordial power spectrum (PPS). In order to realise this goal, we uncover the shape of the PPS by implementing the Modified Richardson-Lucy algorithm (MRL) that fits the Planck temperature data as acceptably as the case of the standard model of cosmology, but with a Hubble constant consistent with local measurements as well as improving the consistency between the derived $S_8$ and $\sigma_8$ parameters with estimations of the weak lensing surveys., Comment: 6 pages, 4 figures
- Published
- 2019
48. Cosmology of the Symmetrical Relativity versus Spontaneous Creation of the Universe Ex Nihilo.
- Author
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Nassif Cruz, Cláudio and da Silva, Fernando Antônio
- Abstract
The cosmology of "Spontaneous Creation of the Universe Ex Nihilo" (Lincoln and Wasser, 2013) and the cosmology of the Symmetrical Relativity (Nassif and Silva, 2018) offer proposals to explain the creation and evolution of the universe. In essence they are still very distinct. However, we will argue that there was an antecedent to the big bang. Thus, we will penetrate a trans-Planckian regime, where we find an effective Planck length L P ′ → 0. This will lead to more fundamental physical reflections about nothing in the cosmology of spontaneous creation (Lincoln and Wasser, 2013). From the point of view of spontaneous creation, the step backwards went back to another principle, based on the information , which led to the big bang. While the spontaneous creation refers to the virtual pre-existence of information , which would have emerged randomly from nothing (Lincoln and Wasser, 2013), the cosmology of the Symmetrical Relativity (Nassif and Silva, 2018) does not stop there: we go back to one's own origin by projecting it before the creation of one's own time. From the present perspective, nothing is a primordial vacuum, whose information has made the universe by condensing and igniting. It was not randomly created, since the entropy had to vary from infinite (chaos) to zero (big bang) by violating the 2nd.law of thermodynamics in a trans-Planckian regime. Nothing or chaos with infinite entropy precedes the big bang (null entropy) within a trans-Planckian scenario and it determines the whole plot until the total extinction of the universe. We will show that information , besides not being born of the universe, also does not develop from it like the computational idea of Artificial Intelligence (AI). Thus, the universe is not simply self-taught as defended by the spontaneous creation. This could shed light on the problem of Penrose's Weyl curvature hypothesis, which considers a null Weyl curvature due to a null entropy in the big bang. [ABSTRACT FROM AUTHOR]
- Published
- 2020
- Full Text
- View/download PDF
49. Maps of the Southern Millimeter-wave Sky from Combined 2500 deg 2 SPT-SZ and Planck Temperature Data
- Author
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John E. Carlstrom, Jeff McMahon, Jason W. Henning, G. Simard, J. T. Sayre, R. Chown, W. L. Holzapfel, C. Pryke, Christian L. Reichardt, T. de Haan, K. K. Schaffer, K. Aylor, D. Luong-Van, T. Natoli, K. Vanderlinde, S. S. Meyer, Z. K. Staniszewski, Elizabeth George, W. B. Everett, J. D. Hrubes, H-M. Cho, Erik Shirokoff, Bradford Benson, R. Williamson, K. T. Story, Y. Omori, Antony A. Stark, J. E. Ruhl, Lindsey Bleem, N. W. Halverson, Marius Millea, Stephen Padin, Joseph J. Mohr, Chihway Chang, A. T. Crites, Joaquin Vieira, Matt Dobbs, T. M. Crawford, N. L. Harrington, Gilbert Holder, Adrian T. Lee, Lloyd Knox, L. M. Mocanu, Daniel P. Marrone, Z. Hou, and W. L. K. Wu
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,media_common.quotation_subject ,Cosmic background radiation ,FOS: Physical sciences ,cosmic background radiation ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astronomy & Astrophysics ,Physical Chemistry ,Atomic ,7. Clean energy ,01 natural sciences ,symbols.namesake ,Particle and Plasma Physics ,0103 physical sciences ,Nuclear ,Planck ,Linear combination ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,Physics ,010308 nuclear & particles physics ,Organic Chemistry ,Astrophysics::Instrumentation and Methods for Astrophysics ,Molecular ,Spherical harmonics ,Astronomy and Astrophysics ,Planck temperature ,observations [cosmology] ,South Pole Telescope ,Space and Planetary Science ,Sky ,symbols ,Astronomical and Space Sciences ,Noise (radio) ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Physical Chemistry (incl. Structural) - Abstract
We present three maps of the millimeter-wave sky created by combining data from the South Pole Telescope (SPT) and the Planck satellite. We use data from the SPT-SZ survey, a survey of 2540 deg$^2$ of the the sky with arcminute resolution in three bands centered at 95, 150, and 220 GHz, and the full-mission Planck temperature data in the 100, 143, and 217 GHz bands. A linear combination of the SPT-SZ and Planck data is computed in spherical harmonic space, with weights derived from the noise of both instruments. This weighting scheme results in Planck data providing most of the large-angular-scale information in the combined maps, with the smaller-scale information coming from SPT-SZ data. A number of tests have been done on the maps. We find their angular power spectra to agree very well with theoretically predicted spectra and previously published results., Comment: 21 pages, 12 figures
- Published
- 2018
50. The lensing and temperature imprints of voids on the Cosmic Microwave Background
- Author
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Andreas A. Berlind, John A. Peacock, Qingqing Mao, Yan-Chuan Cai, István Szapudi, Mark C. Neyrinck, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
- Subjects
Void (astronomy) ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cold dark matter ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Strong gravitational lensing ,Cosmic microwave background ,Cosmic background radiation ,FOS: Physical sciences ,Astrophysics ,cosmic background radiation ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,symbols.namesake ,gravitational lensing: weak ,0103 physical sciences ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Physics ,010308 nuclear & particles physics ,Astronomy ,Astronomy and Astrophysics ,Planck temperature ,Galaxy ,Space and Planetary Science ,symbols ,large-scale structure of Universe ,methods: observational ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We have searched for the signature of cosmic voids in the CMB, in both the Planck temperature and lensing-convergence maps; voids should give decrements in both. We use zobov voids from the DR12 SDSS CMASS galaxy sample. We base our analysis on N-body simulations, to avoid a posteriori bias. For the first time, we detect the signature of voids in CMB lensing: the significance is $3.2\sigma$, close to $\Lambda$CDM in both amplitude and projected density-profile shape. A temperature dip is also seen, at modest significance ($2.3\sigma$), with amplitude about 6 times the prediction. This temperature signal is induced mostly by voids with radius between 100 and 150 Mpc/h, while the lensing signal is mostly contributed by smaller voids -- as expected; lensing relates directly to density, while ISW depends on gravitational potential. The void abundance in observations and simulations agree, as well. We also repeated the analysis excluding lower-significance voids: no lensing signal is detected, with an upper limit of about twice the $\Lambda$CDM prediction. But the mean temperature decrement now becomes non-zero at the $3.7\sigma$ level (similar to that found by Granett et al.), with amplitude about 20 times the prediction. However, the observed dependence of temperature on void size is in poor agreement with simulations, whereas the lensing results are consistent with $\Lambda$CDM theory. Thus, the overall tension between theory and observations does not favour non-standard theories of gravity, despite the hints of an enhanced amplitude for the ISW effect from voids., Comment: 12 pages, 6 figures, accepted for publication in MNRAS
- Published
- 2016
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