DOCSLIB.ORG

Constraining Stochastic Gravitational Wave Background from Weak Lensing of CMB B-Modes

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Constraining Stochastic Gravitational Wave Background from Weak Lensing of CMB B-Modes Prepared for submission to JCAP Constraining stochastic gravitational wave background from weak lensing of CMB B-modes Shabbir Shaikh,y Suvodip Mukherjee,y Aditya Rotti,z and Tarun Souradeepy yInter University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune- 411007, India zDepartment of Physics, Florida State University, Tallahassee, FL 32304, USA E-mail: [email protected], [email protected], [email protected], [email protected] Abstract. A stochastic gravitational wave background (SGWB) will affect the CMB anisotropies via weak lensing. Unlike weak lensing due to large scale structure which only deflects pho- ton trajectories, a SGWB has an additional effect of rotating the polarization vector along the trajectory. We study the relative importance of these two effects, deflection & rotation, specifically in the context of E-mode to B-mode power transfer caused by weak lensing due to SGWB. Using weak lensing distortion of the CMB as a probe, we derive constraints on the spectral energy density (ΩGW ) of the SGWB, sourced at different redshifts, without assuming any particular model for its origin. We present these bounds on ΩGW for different power-law models characterizing the SGWB, indicating the threshold above which observable imprints of SGWB must be present in CMB. arXiv:1606.08862v2 [astro-ph.CO] 20 Sep 2016 Contents 1 Introduction1 2 Weak lensing of CMB by gravitational waves2 3 Method 6 4 Results 8 5 Conclusion9 6 Acknowledgements 10 1 Introduction The Cosmic Microwave Background (CMB) is an exquisite tool to study the universe. It is being used to probe the early universe scenarios as well as the physics of processes happening in between the surface of last scattering and the observer. Well studied processes among these include lensing by large scale structure, Sunyaev-Zeldovich effect, integrated Sachs- Wolfe effect etc. These effects give rise to secondary anisotropies in the CMB. The stochastic gravitational wave background (SGWB), if present, will affect the CMB via weak lensing [1,2]. The SGWB can be sourced by inflation, astrophysical phenomena like halo mergers and halo formation [3,4], second order density perturbations [5], early universe phase transitions [6], etc. In the new era, post the first direct detection of gravitational wave by LIGO [7] and studies assessing a SGWB for such populations [8], a reassessment of SGWB probed by weak lensing of CMB considered earlier [9] appears to be timely. Effects of lensing by scalar and tensor perturbations on CMB have been calculated in full detail in literature [2, 10{13]. Padmanabhan et al. ([12]) carried out a comparative study of lensing by scalar and tensor perturbations, concluding that tensor perturbations are more efficient than scalar perturbations at converting E-modes of CMB polarization to B-modes. More recently, Dai [13] noted the effect of the rotation of CMB polarization due to tensor perturbations, arguing that the B-mode power generated by lensing deflection due to tensor perturbations is largely canceled by the rotation of polarization induced by these perturbations. In summary, unlike in the case of weak lensing by large scale structure, a SGWB leads to two different effects in CMB: (i) deflection of photon path and (ii) rotation of polarization vector of photon along the direction of propagation. The SGWB results in additional distortions in the CMB sky, over and above those introduced by lensing due to large scale structure. It has been shown that the lensing due to SGWB sourced by inflation is below the cosmic variance and hence not detectable even for cosmic variance limited experiments [2]. However, in light of other conjectured sources of SGWB, weak lensing of CMB by SGWB has been used in previous work [9] to derive upper bounds on ΩGW . Namikawa et al. [14] have studied the detectability of weak lensing of CMB induced by gravitational waves. They do not include the effect of the rotation of CMB polarization in their evaluations. { 1 { In this paper, we carry out a more careful assessment of the efficiency of tensor per- turbations in mediating power transfer between E-mode and B-mode of CMB polarization. Finally, we incorporate rotation effect in the lensing kernels and derive revised constraints on the energy density ΩGW of the SGWB, for different empirical models of SGWB power generated at a number of representative source redshifts. This paper is organized as follows. In section II we carefully assess the relative con- tributions of rotation and deflection associated with weak lensing due to the SGWB. In section III we present the details of the procedure used to derive the revised upper limits on ΩGW . We conclude with the discussion of our results in section IV. We use the best fit Planck+WP+highL+BAO parameters from Planck 2013 [15] to derive all our results. 2 Weak lensing of CMB by gravitational waves Weak lensing of CMB remaps the temperature and polarization anisotropy field on the sky. The lensed temperature anisotropy T~(^n), observed in the directionn ^ corresponds to the temperature anisotropy T (^n + d~), observed in the absence of lensing in the directionn ^ + d~, T~(^n) = T (^n + d~); (2.1) where d~ is the deflection angle and defines a vector field on the sky. CMB photons are linearly polarized because of Thomson scattering. CMB polarization field is expressed using Q and U Stokes parameters, ±X(^n) = Q(^n) ± iU(^n). To consider the complete effect of lensing on polarization anisotropies, we have to consider the rotation of polarization vector of CMB photons about its direction of propagation due to metric perturbations as described by Dai [13]. Including the effect of photon deflection and rotation of polarization, the lensed polarization field is described as: ∓2i (^n) ±X~(^n) = e ±X(^n + d~); (2.2) where is the angle of rotation of polarization. The vector deflection angle is field decomposed into a gradient potential φ(^n) and a curl potential Ω(^n) jk di = riφ(^n) − "i njrkΩ(^n); (2.3) where r~ is the angular gradient on the sphere. For a statistically isotropic lensing field, φφ ΩΩ φ(^n) and Ω(^n) are described by their angular power spectrum Cl and Cl respectively. φφ ΩΩ Methods to reconstruct both Cl and Cl from the observed CMB sky exist in literature, for example, see [16, 17] and references therein. The rotation angle (^n) is related to curl potential Ω(^n) through [13] 1 (^n) = − r2Ω(^n); (2.4) 2 where r2 is angular Laplacian. Eq. (2.4) shows that the source of the curl potential Ω(^n) gives rise to the rotation of polarization vector. Angular power spectrum for rotation Cl is ΩΩ related to Cl through [13] 2 ΩΩ Cl = [l(l + 1)=2] Cl ; (2.5) and the deflection-rotation cross power spectrum is Ω ΩΩ Cl = [l(l + 1)=2]Cl : (2.6) { 2 { 2 Ω Ω Note that Cl is ∼ l Cl , which makes Cl much stronger over Cl at small angular scales (high multipoles l). At the linear order in perturbation, lensing by large scale structure (LSS) in the uni- verse, which corresponds to scalar metric perturbations, induce only gradient type deflections. Gravitational waves, which corresponds to tensor metric perturbations, induce both gradient and curl type deflections even at linear order [10, 11, 18]. Hence, to consider the complete effect of curl deflection sourced by scalar and tensor perturbations at linear order, we include the rotation of polarization in our computation. However, we neglect the scalar deflection caused by the tensor perturbations, because it is an order of magnitude less than the ten- sor deflection [2]. There are several models predicting vector perturbations which can also contribute to curl deflections, for example, vector perturbations caused by cosmic strings [19]. Since the relative amplitude and spectrum of vector perturbations would be model dependent, we choose to neglect the lensing by vector perturbations in our analysis. Effect of lensing on CMB angular power spectrum is computed either using real space correlation function [20] or using spherical harmonic space correlation function method [21]. Here we have provided the expressions obtained using latter method, originally computed in [21] for scalar deflection, in [2] and [12] for scalar and tensor deflection and in [13] for scalar and tensor deflection including the effect of rotation. Lensed TT angular power spectrum is: 1 X C~TT = CTT − l(l + 1)RCTT + CTT [(F φ )2Cφ P + + (F Ω )2CΩP − ]; l l l 2l + 1 l2 ll1l2 l1 ll1l2 ll1l2 l1 ll1l2 (2.7) l1l2 where R is the rms deflection power given by X l(l + 1)(2l + 1) R = (Cφφ + CΩΩ): (2.8) 8π l l l R is measure of rms deflection angle, d2 = R. F φ and F Ω are lensing kernels: rms ll1l2 ll1l2 r Ω φ p Πll1l2 l l1 l2 F = F = − l1(l1 + 1)l2(l2 + 1) ; (2.9) ll1l2 ll1l2 4π 0 −1 1 where Π = (2l + 1)(2l + 1)::: and P ± = (1 ± (−1)l+l1+l2 )=2. It is clear from Eq. (2.7) ll1::: 1 ll1l2 that rotation of polarization has no contribution in the lensing of temperature anisotropy. Polarization E mode and B mode angular power spectra are ~EE EE 2 EE EE Cl = Cl − (l + l − 4)RCl − 4SCl 1 X φφ φ 2 EE + BB − ΩΩ Ω 2 EE − BB + + [C (2F ) (C P + C P ) + C (2F ) (C P + C P )] (2l + 1) l1 ll1l2 l2 ll1l2 l2 ll1l2 l1 ll1l2 l2 ll1l2 l2 ll1l2 l1l2 4 X 2 Ω Ω EE − BB + + [C (2F ) − C 2F 2F ](C P + C P ); (2.10) (2l + 1) l1 ll1l2 l1 ll1l2 ll1l2 l2 ll1l2 l2 ll1l2 l1l2 ~BB BB 2 BB BB Cl = Cl − (l + l − 4)RCl − 4SCl 1 X φφ φ 2 EE − BB + ΩΩ Ω 2 EE + BB − + [C (2F ) (C P + C P ) + C (2F ) (C P + C P )] (2l + 1) l1 ll1l2 l2 ll1l2 l2 ll1l2 l1 ll1l2 l2 ll1l2 l2 ll1l2 l1l2 4 X 2 Ω Ω EE + BB − + [C (2F ) − C 2F 2F ](C P + C P ); (2.11) (2l + 1) l1 ll1l2 l1 ll1l2 ll1l2 l2 ll1l2 l2 ll1l2 l1l2 { 3 { S is the rms rotation power given by X 2l + 1 S = C : (2.12) 4π l l F φ and F Ω are lensing kernels: 2 ll1l2 2 ll1l2 r r r φ/Ω l1(l1 + 1)Πll1l2 h (l2 + 2)(l2 − 1) l l1 l2 (l2 − 2)(l2 + 3) l l1 l2 i 2F = ± ; ll1l2 8π 2 2 −1 −1 2 2 1 −3 (2.13) l l1 l2 φ Ω Here denote Wigner-3j symbols.
Load more

Recommended publications
  • The Silk Damping Tail of the CMB
    The Silk Damping Tail of the CMB 100 K) µ ( T ∆ 10 10 100 1000 l Wayne Hu Oxford, December 2002 Outline • Damping tail of temperature power spectrum and its use as a standard ruler • Generation of polarization through damping • Unveiling of gravitational lensing from features in the damping tail Outline • Damping tail of temperature power spectrum and its use as a standard ruler • Generation of polarization through damping • Unveiling of gravitational lensing from features in the damping tail • Collaborators: Matt Hedman Takemi Okamoto Joe Silk Martin White Matias Zaldarriaga Outline • Damping tail of temperature power spectrum and its use as a standard ruler • Generation of polarization through damping • Unveiling of gravitational lensing from features in the damping tail • Collaborators: Matt Hedman Takemi Okamoto Joe Silk Microsoft Martin White Matias Zaldarriaga http://background.uchicago.edu ("Presentations" in PDF) Damping Tail Photon-Baryon Plasma • Before z~1000 when the CMB had T>3000K, hydrogen ionized • Free electrons act as "glue" between photons and baryons by Compton scattering and Coulomb interactions • Nearly perfect fluid Anisotropy Power Spectrum Damping • Perfect fluid: no anisotropic stresses due to scattering isotropization; baryons and photons move as single fluid Damping • Perfect fluid: no anisotropic stresses due to scattering isotropization; baryons and photons move as single fluid • Fluid imperfections are related to the mean free path of the photons in the baryons −1 λC = τ˙ where τ˙ = neσT a istheconformalopacitytoThomsonscattering
    [Show full text]
  • The Reionization of Cosmic Hydrogen by the First Galaxies Abstract 1
    David Goodstein’s Cosmology Book The Reionization of Cosmic Hydrogen by the First Galaxies Abraham Loeb Department of Astronomy, Harvard University, 60 Garden St., Cambridge MA, 02138 Abstract Cosmology is by now a mature experimental science. We are privileged to live at a time when the story of genesis (how the Universe started and developed) can be critically explored by direct observations. Looking deep into the Universe through powerful telescopes, we can see images of the Universe when it was younger because of the finite time it takes light to travel to us from distant sources. Existing data sets include an image of the Universe when it was 0.4 million years old (in the form of the cosmic microwave background), as well as images of individual galaxies when the Universe was older than a billion years. But there is a serious challenge: in between these two epochs was a period when the Universe was dark, stars had not yet formed, and the cosmic microwave background no longer traced the distribution of matter. And this is precisely the most interesting period, when the primordial soup evolved into the rich zoo of objects we now see. The observers are moving ahead along several fronts. The first involves the construction of large infrared telescopes on the ground and in space, that will provide us with new photos of the first galaxies. Current plans include ground-based telescopes which are 24-42 meter in diameter, and NASA’s successor to the Hubble Space Telescope, called the James Webb Space Telescope. In addition, several observational groups around the globe are constructing radio arrays that will be capable of mapping the three-dimensional distribution of cosmic hydrogen in the infant Universe.
    [Show full text]
  • Cosmic Microwave Background
    1 29. Cosmic Microwave Background 29. Cosmic Microwave Background Revised August 2019 by D. Scott (U. of British Columbia) and G.F. Smoot (HKUST; Paris U.; UC Berkeley; LBNL). 29.1 Introduction The energy content in electromagnetic radiation from beyond our Galaxy is dominated by the cosmic microwave background (CMB), discovered in 1965 [1]. The spectrum of the CMB is well described by a blackbody function with T = 2.7255 K. This spectral form is a main supporting pillar of the hot Big Bang model for the Universe. The lack of any observed deviations from a 7 blackbody spectrum constrains physical processes over cosmic history at redshifts z ∼< 10 (see earlier versions of this review). Currently the key CMB observable is the angular variation in temperature (or intensity) corre- lations, and to a growing extent polarization [2–4]. Since the first detection of these anisotropies by the Cosmic Background Explorer (COBE) satellite [5], there has been intense activity to map the sky at increasing levels of sensitivity and angular resolution by ground-based and balloon-borne measurements. These were joined in 2003 by the first results from NASA’s Wilkinson Microwave Anisotropy Probe (WMAP)[6], which were improved upon by analyses of data added every 2 years, culminating in the 9-year results [7]. In 2013 we had the first results [8] from the third generation CMB satellite, ESA’s Planck mission [9,10], which were enhanced by results from the 2015 Planck data release [11, 12], and then the final 2018 Planck data release [13, 14]. Additionally, CMB an- isotropies have been extended to smaller angular scales by ground-based experiments, particularly the Atacama Cosmology Telescope (ACT) [15] and the South Pole Telescope (SPT) [16].
    [Show full text]
  • Secondary Cosmic Microwave Background Anisotropies in A
    THE ASTROPHYSICAL JOURNAL, 508:435È439, 1998 December 1 ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES IN A UNIVERSE REIONIZED IN PATCHES ANDREIGRUZINOV AND WAYNE HU1 Institute for Advanced Study, School of Natural Sciences, Princeton, NJ 08540 Received 1998 March 17; accepted 1998 July 2 ABSTRACT In a universe reionized in patches, the Doppler e†ect from Thomson scattering o† free electrons gener- ates secondary cosmic microwave background (CMB) anisotropies. For a simple model with small patches and late reionization, we analytically calculate the anisotropy power spectrum. Patchy reioniza- tion can, in principle, be the main source of anisotropies on arcminute scales. On larger angular scales, its contribution to the CMB power spectrum is a small fraction of the primary signal and is only barely detectable in the power spectrum with even an ideal, i.e., cosmic variance limited, experiment and an extreme model of reionization. Consequently, patchy reionization is unlikely to a†ect cosmological parameter estimation from the acoustic peaks in the CMB. Its detection on small angles would help determine the ionization history of the universe, in particular, the typical size of the ionized region and the duration of the reionization process. Subject headings: cosmic microwave background È cosmology: theory È intergalactic medium È large-scale structure of universe 1. INTRODUCTION tion below the degree scale. Such e†ects rely on modulating the Doppler e†ect with spatial variations in the optical It is widely believed that the cosmic microwave back- depth. Incarnations of this general mechanism include the ground (CMB) will become the premier laboratory for the Vishniac e†ect from linear density variations (Vishniac study of the early universe and classical cosmology.
    [Show full text]
  • Observational Prospects I Have Cut This Lecture Back to Be Mostly About BAO Because I Still Have Holdover Topics from Previous Lectures to Cover
    Precision Cosmology with Large Scale Structure David Weinberg Precision Cosmology With Large Scale Structure David Weinberg, Ohio State University ICTP Cosmology Summer School 2015 Lecture 3: Observational Prospects I have cut this lecture back to be mostly about BAO because I still have holdover topics from previous lectures to cover. Where are we now? CMB Planck: All sky (40,000 deg2), near cosmic-variance limited for temperature anisotropy, noise lim- ited for polarization. ACT and SPT: Higher resolution experiments over smaller areas (hundreds or thousands of deg2), frequency coverage for Sunyaev-Zeldovich as well as primary anisotropy, polarization. Smaller area high-sensitivity experiments for B-mode polarization (e.g., BICEP). Type Ia Supernovae Data sets are compilations of surveys of different redshift ranges, local to z 1.2. ≈ “Compilation” requires enormous effort to bring different data sets to common calibration and analysis. Union 2.1, broad compilation. JLA – local samples, SDSS-II from z = 0.1 0.4, SNLS (Canada-France-Hawaii Telescope) from z = 0.4 1, HST at z > 1. − − Approaching 1000 SNe (740 for JLA). Optical imaging/weak lensing SDSS – 104 deg2, 5 bands (ugriz), depth r 22, weak lensing source density approximately − 1 arcmin 2; SDSS “Stripe 82” went 2 magnitudes≈ deeper over 200 deg2 Pan-STARRS – 3 104 deg2, depth comparable to SDSS × CFHTLens – 150 deg2, Dark Energy Survey (DES) is ongoing, discussed at the end. Redshift surveys SDSS-I/II: 106 galaxies, broadly selected, median z = 0.1 ; 105 luminous red galaxies (LRGs) sparsely sampling structure to z = 0.45 SDSS-III BOSS: 1.5 106 luminous galaxies, z = 0.2 0.7, 7 effective volume of SDSS-I/II LRGs; spectra of 160,000 quasars× at z = 2 4 for Lyα forest− analysis× − Clusters Variety of cluster catalogs selected by different methods.
    [Show full text]
  • Cosmology with Matter Diffusion
    Prepared for submission to JCAP Cosmology with matter diffusion Simone Calogeroa and Hermano Veltenb aMathematical Sciences, Chalmers University of Technology, Gothenburg University, S-412 96 Gothenburg, Sweden bUniversidade Federal do Esp´ırito Santo, Av. Fernando Ferrari, Goiabeiras, Vit´oria, Brasil E-mail: [email protected], [email protected] Abstract. We construct a viable cosmological model based on velocity diffusion of matter particles. In order to ensure the conservation of the total energy-momentum tensor in the presence of diffusion, we include a cosmological scalar field φ which we identify with the dark energy component of the universe. The model is characterized by only one new degree of freedom, the diffusion parameter σ. The standard ΛCDM model can be recovered by setting σ = 0. If diffusion takes place (σ > 0) the dynamics of the matter and of the dark energy fields are coupled. We argue that the existence of a diffusion mechanism in the universe may serve as a theoretical motivation for interacting models. We constrain the background dynamics of the diffusion model with Supernovae, H(z) and BAO data. We also perform a perturbative analysis of this model in order to understand structure formation in the universe. We calculate the impact of diffusion both on the CMB spectrum, with particular attention to the integrated Sachs-Wolfe signal, and on the matter power spectrum P (k). The latter analysis places strong constraints on the magnitude of the diffusion mechanism but does not rule out the model. Keywords: Cosmology, diffusion,
    [Show full text]
  • Nonparametric Inference for the Cosmic Microwave Background Christopher R
    Nonparametric Inference for the Cosmic Microwave Background Christopher R. Genovese,1 Christopher J. Miller,2 Robert C. Nichol,3 Mihir Arjunwadkar,4 and Larry Wasserman5 Carnegie Mellon University The Cosmic Microwave Background (CMB), which permeates the entire Universe, is the radiation left over from just 390,000 years after the Big Bang. On very large scales, the CMB radiation ¯eld is smooth and isotropic, but the existence of structure in the Universe { stars, galaxies, clusters of galaxies, ::: { suggests that the ¯eld should fluctuate on smaller scales. Recent observations, from the Cosmic Microwave Background Explorer to the Wilkin- son Microwave Anisotropy Project, have strikingly con¯rmed this prediction. CMB fluctuations provide clues to the Universe's structure and composition shortly after the Big Bang that are critical for testing cosmological models. For example, CMB data can be used to determine what portion of the Universe is composed of ordinary matter versus the mysterious dark matter and dark energy. To this end, cosmologists usually summarize the fluctuations by the power spectrum, which gives the variance as a function of angular frequency. The spectrum's shape, and in particular the location and height of its peaks, relates directly to the parameters in the cosmological models. Thus, a critical statistical question is how accurately can these peaks be estimated. We use recently developed techniques to construct a nonpara- metric con¯dence set for the unknown CMB spectrum. Our esti- mated spectrum, based on minimal assumptions, closely matches 1Research supported by NSF Grants SES 9866147 and NSF-ACI-0121671. 2Research supported by NSF-ACI-0121671.
    [Show full text]
  • Astro2020 Science White Paper Probing the Origin of Our Universe Through Cosmic Microwave Background Constraints on Gravitational Waves
    Astro2020 Science White Paper Probing the origin of our Universe through cosmic microwave background constraints on gravitational waves Thematic Areas: Planetary Systems Star and Planet Formation Formation and Evolution of Compact Objects X Cosmology and Fundamental Physics Stars and Stellar Evolution Resolved Stellar Populations and their Environments Galaxy Evolution Multi-Messenger Astronomy and Astrophysics Principal Author: Name: Sarah Shandera Institution: The Pennsylvania State University Email: [email protected] Phone: (814)863-9595 Co-authors: Peter Adshead (U. Illinois), Mustafa Amin (Rice University), Emanuela Dimastrogiovanni (University of New South Wales), Cora Dvorkin (Harvard University), Richard Easther (University of Auckland), Matteo Fasiello (Institute of Cosmology and Gravitation, University of Portsmouth), Raphael Flauger (University of California, San Diego), John T. Giblin, Jr (Kenyon College), Shaul Hanany (University of Minnesota), Lloyd Knox (Univerisity of California, Davis), Eugene Lim (King’s College London), Liam McAllister (Cornell University), Joel Meyers (Southern Methodist University), Marco Peloso (University of Padova, and INFN, Sezione di Padova), Graca Rocha (Jet Propulsion Laboratory), Maresuke Shiraishi (National Institute of Technology, Kagawa College), Lorenzo Sorbo (University of Massachusetts, Amherst), Scott Watson (Syracuse University) Endorsers: Zeeshan Ahmed1, David Alonso2, Robert Armstrong3, Mario Ballardini4, Darcy Barron5, Nicholas Battaglia6, Daniel Baumann7;8, Charles Bennett9,
    [Show full text]
  • Primordial Gravitational Waves from Cosmic Inflation
    Mathematical Tripos Part III Essay #75 (colour in electronic version) Submied 5th May 2017, updated 26th August 2017 Primordial Gravitational Waves from Cosmic Inflation Mike S. Wang DAMTP, University of Cambridge Abstract. Cosmic inflation generates primordial gravitational waves (PGWs) through the same physical process that seeds all structure formation in the observable universe. We will demonstrate this mechanism in detail and relate it to the distinctive signatures PGWs could leave in the observable temperature anisotropies and polarisation of the cosmic microwave background (CMB). The detection of primordial gravitational waves is of great significance to validating and understanding inflationary physics, and we shall see why CMB polarisation oers a promising path. In the end, we will remark on the unique observational challenges and prospects of probing primordial gravitational waves in future experiments. Keywords. Inflation, primordial gravitational waves (theory), gravitational waves and CMBR polarisation, power spectrum, gravitational waves / experiments. Contents I A Brief Overview 1 II The Inflation Paradigm and Generation of Gravitational Waves 1 II.1 Dynamics of single-field slow-roll inflation ...............................1 II.2 antum fluctuations and the primordial power spectrum ......................2 II.3 Scalar, vector and tensor perturbations in the FLRW background ...................3 III CMB Signatures from Primordial Gravitational Waves 5 III.1 Temperature anisotropies from PGWs ..................................5 III.2 Polarisation from PGWs ..........................................9 IV B-Mode Polarisation: A Promising Route for Detecting PGWs? 12 IV.1 Cosmological sources of B-mode polarisation .............................. 12 IV.2 Statistical aspects of B-mode polarisation ................................ 13 V A “Smoking Gun”: Physical Significance of PGW Discovery 14 V.1 Alternatives to inflation .........................................
    [Show full text]
  • The Cosmic Microwave Background Radiation Provided by CERN Document Server
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE The Cosmic Microwave Background Radiation provided by CERN Document Server Eric Gawiser 1 Department of Physics, University of California, Berkeley, CA 94720 and Joseph Silk Department of Physics, Astrophysics, 1 Keble Road, University of Oxford, OX1 3NP, UK and Departments of Physics and Astronomy and Center for Particle Astrophysics, University of California, Berkeley, CA 94720 Abstract We summarize the theoretical and observational status of the study of the Cosmic Microwave Background radiation. Its thermodynamic spectrum is a robust prediction of the Hot Big Bang cosmology and has been confirmed observationally. There are now 76 observations of Cosmic Microwave Back- ground anisotropy, which we present in a table with references. We discuss the theoretical origins of these anisotropies and explain the standard jargon associated with their observation. 1 Origin of the Cosmic Background Radiation Our present understanding of the beginning of the universe is based upon the remarkably successful theory of the Hot Big Bang. We believe that our uni- verse began about 15 billion years ago as a hot, dense, nearly uniform sea of radiation a minute fraction of its present size (formally an infinitesimal sin- gularity). If inflation occurred in the first fraction of a second, the universe became matter dominated while expanding exponentially and then returned to radiation domination by the reheating caused by the decay of the inflaton. Baryonic matter formed within the first second, and the nucleosynthesis of the lightest elements took only a few minutes as the universe expanded and cooled.
    [Show full text]
  • Large-Scale Structure and Integrated Sachs–Wolfe Effect in Decaying Vacuum Cosmology
    MNRAS 452, 2220–2224 (2015) doi:10.1093/mnras/stv1443 Large-scale structure and integrated Sachs–Wolfe effect in decaying vacuum cosmology H. Velten,1,2‹ H. A. Borges,3,4 S. Carneiro,3‹ R. Fazolo1 and S. Gomes1 1Departamento de F´ısica, Universidade Federal do Esp´ırito Santo, 29075-910 Vitoria,´ ES, Brazil 2CPT, Aix Marseille Universite,´ UMR 7332, F-13288 Marseille, France 3Instituto de F´ısica, Universidade Federal da Bahia, 40210-340 Salvador, BA, Brazil 4Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK Accepted 2015 June 26. Received 2015 June 12; in original form 2015 April 17 ABSTRACT The concordance particle creation model – a class of (t) Cold Dark Matter (CDM) cosmolo- gies – is studied using large-scale structure (LSS) formation, with particular attention to the integrated Sachs–Wolfe effect. The evolution of the gravitational potential and the amplitude of the cross-correlation of the cosmic microwave background (CMB) signal with LSS sur- veys are calculated in detail. We properly include in our analysis the peculiarities involving the baryonic dynamics of the (t)CDM model which were not included in previous works. Although both the (t)CDM and the standard cosmology are in agreement with available data for the CMB–LSS correlation, the former presents a slightly higher signal which can be identified with future data. Key words: dark energy – dark matter. ˙ =− 1 INTRODUCTION from which it is not difficult to show that ρm. The back- ground expansion is given by Although the great success of the standard CDM cosmological = − + −3/2 model in describing most observations, we are still distant from H H0 1 m0 m0a , (2) the full understanding of the cosmic dynamics.
    [Show full text]
  • The Inflationary Gravity Waves in Light of Recent Cosmic Microwave
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE The Inflationary Gravity Waves in light of recent Cosmic Microwave Backgroundprovided by CERN Document Server Anisotropies data. Alessandro Melchiorri[ and Carolina J. Odman¨ ] [ Astrophysics, Denys Wilkinson Building, University of Oxford, Keble road, OX1 3RH, Oxford, UK ] Astrophysics Group, Cavendish Laboratory, Cambridge University, Cambridge, U.K. One of the major predictions of inflation is the existence of a stochastic background of cosmo- logical gravitational waves (GW). These gravitational waves can induce significant temperature anisotropies in the Cosmic Microwave Background (CMB) on the angular scales recently probed by the ARCHEOPS experiment. Here, we perform a combined analysis of ARCHEOPS to- gether with information from other CMB experiments and/or cosmological datasets, in order to constrain the amplitude of the GW background. We find that, for a scale-invariant GW back- ground, the ratio of tensor/scalar perturbations at the CMB quadrupole is now constrained to be r 0:43 at 95% c.l., while the bound on the spectral index of primordial density fluctua- ≤ +0:10 tions is nS =0:97 0:12 . We discuss the implications for future GW detections through CMB polarization measurements.− I. INTRODUCTION bination, however, unlike the anisotropies generated by scalar fluctuations, those generated by GW damp The last years have seen spectacular advances in our like fluctuations in a fluid of massless bosons (see e.g. ability to confront the inflationary scenario of struc- [11]). Since the theoretical spectrum, normalized to ture formation to observational data. The “multi- COBE, is a linear sum of the scalar and tensor compo- ple peaks” observed in the Cosmic Microwave Back- nents, if there is a relevant contribution from GW this ground (CMB) angular power spectrum ( [27], [17], would lower the predicted amplitude of the acoustic [22], [31], [34]) are indeed providing strong sup- peaks on sub-degree angular scales.
    [Show full text]