Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy
|
|
- Jane Walton
- 5 years ago
- Views:
Transcription
1 12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference
2 Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy ΛCDM direct confirmation Doppler peaks structure of the CMB power spectrum hierarchical structure formation via gravitational instability cluster abundances at small redshifts spatial distribution and the number density of galaxies LSS matter power spectrum Lyman-α forest amplitude and spectrum ΛCDM issues on small scale: galaxy rotation curves too much substructure baryon angular momentum problems observed halos have softer cores, lower concentrations, less clumped
3 Probing Fundamental Physics with Planck: add physical properties to the ΛCDM model components Physics behind the dark components of the Universe - DM is the lightest supersymmetric particle? - DE is cosmological constant or quintescence field? - DM & DE are related by an unknown mechanism? - net contribution of the HDM Physics of inflation - nature of the primordial perturbations? - slope of the primordial perturbations depends of the inflation model? - can inflation be realized in string theory? - are cosmic defects produced at the end of inflation? Answer to these questions requires the control of the behavior of systematic effects and the detailed knowledge of the nature and behavior of the foregrounds April 2006, Rome, Italy Francesco Melchiorri Memorial Conference
4 Control of systematic effects in LFI Systematic effects will produce different responses in the in the two instruments provided Planck with a powerful tool for detection and mitigation of systematic which will ensures that the final maps are limited only by instrument sensitivity and unavoidable astrophysical foregrounds sidelobe pickup of the Galaxy and solar system bodies (Burigana et al. 2001, 2004) distorted beam shapes (Burigana et al. 1998, 2001, Mandolesi et al. 2000) non-idealities in the radiometer (Seiffert et al. 2002) 1/f noise and destriping (Maino et al. 1999) effects induced by temperature instability (Mennella et al. 2002) spacecraft pointing errors and nutation (Bersanelli et al. 1996) LFI goal: systematic contribution less than 3μK
5 Planck is designed to extract all information available in temperature anisotropies of the CMB WMAP (1, 4 & 8 yrs) vs. Planck (14 months)
6 EE and TE are noise limited for l >1000 GW BB at l > 150 is swamped by the week lensing EE BB TE April 2006, Rome, Italy Francesco Melchiorri Memorial Conference
7 Planck will achieve a major advance in polarization but will be limited by the knowledge of the polarized foregrounds Typical predicted range for E & B modes compared to the polarized foregrounds contamination
8 Planck can set significant constraints on primordial B-mode if polarized foregrounds are accurately known and subtracted
9
10 4 x 10 8 yrs WMAP 3-Yrs τ es 0.1 z re ~ 12 - affects the subsequent structure formation - direct consequence of the formation of the first structures and luminous souces
11 WMAP 3Yrs PLANCK x e x e 65% 65% 95% 95% 95% z re Spergel et al.2006 WMAP is not sensitive to the details of the ionization history Planck will distinguish among different ionization histories even when they imply the same value of τ es
12 Physical model of reionization J ( υ, z z sc c e τ 4π dt ε ( dz eff ( υ0, 0, ) 0) = υ z 0 z z, z) dz Ionizing UV flux dz dt = H + Ω z) m(1 z) + Ω ( cosmology V Ωb d * Ωm dt M dn ε( υ, z ) Lυ ( z) τlife f ( Mh, z) M dm min h h dm h source dt τ eff ( υ0, z0, z) = c κ( υ, z) dz dz z z 0 IGM properties
13 Reionization history with Planck When: z re, x e How long: Δz Once or twice Ionizing flux and feedback: UV/ X-ray POP III /POPII: z tr SFR IMF UV vs. FIR : role of zodiacal light
14
15 Uncertainty about the ionization history will provide a limit of on how well τ es can be estimated from Planck polarization data
16 Physical model of recombination dx dz e dt = α dz [ ] C ( T ) x 2 n ( z) I ( z) I ( z) B e b s X i recombination rate ionization rate standard sources ionization rate other mechanisms inverse Compton scattering on CMB radiative decay Energy injection delays the recombination at z 10 3 and distorts the temporal evolution of the ionization fraction at high redshifts (z > z re ).
17 υ X υ a + e e γ I X i ( z) = (1 x e ) m E b 0 Ω Ω X b Γ X H ( z)
18 Knowledge of foregrounds and systematics will set the limit on how well we can constrain the Reionization History with CMB anisotropy measurements.
Really, really, what universe do we live in?
Really, really, what universe do we live in? Fluctuations in cosmic microwave background Origin Amplitude Spectrum Cosmic variance CMB observations and cosmological parameters COBE, balloons WMAP Parameters
More informationCMB studies with Planck
CMB studies with Planck Antony Lewis Institute of Astronomy & Kavli Institute for Cosmology, Cambridge http://cosmologist.info/ Thanks to Anthony Challinor & Anthony Lasenby for a few slides (almost) uniform
More informationThe cosmic background radiation II: The WMAP results. Alexander Schmah
The cosmic background radiation II: The WMAP results Alexander Schmah 27.01.05 General Aspects - WMAP measures temperatue fluctuations of the CMB around 2.726 K - Reason for the temperature fluctuations
More informationA5682: Introduction to Cosmology Course Notes. 11. CMB Anisotropy
Reading: Chapter 9, sections 9.4 and 9.5 11. CMB Anisotropy Gravitational instability and structure formation Today s universe shows structure on scales from individual galaxies to galaxy groups and clusters
More informationPolarization from Rayleigh scattering
Polarization from Rayleigh scattering Blue sky thinking for future CMB observations Previous work: Takahara et al. 91, Yu, et al. astro-ph/0103149 http://en.wikipedia.org/wiki/rayleigh_scattering Antony
More informationWeak gravitational lensing of CMB
Weak gravitational lensing of CMB (Recent progress and future prospects) Toshiya Namikawa (YITP) Lunch meeting @YITP, May 08, 2013 Cosmic Microwave Background (CMB) Precise measurements of CMB fluctuations
More informationThe ultimate measurement of the CMB temperature anisotropy field UNVEILING THE CMB SKY
The ultimate measurement of the CMB temperature anisotropy field UNVEILING THE CMB SKY PARAMETRIC MODEL 16 spectra in total C(θ) = CMB theoretical spectra plus physically motivated templates for the
More informationCosmology & CMB. Set6: Polarisation & Secondary Anisotropies. Davide Maino
Cosmology & CMB Set6: Polarisation & Secondary Anisotropies Davide Maino Polarisation How? Polarisation is generated via Compton/Thomson scattering (angular dependence of the scattering term M) Who? Only
More informationPLANCK lately and beyond
François R. Bouchet, Institut d Astrophysique de Paris PLANCK lately and beyond CORE/M5 TT, EE, BB 2016 status Only keeping points w. sufficiently small error bars, Fig. E Calabrese τ = 0.055±0.009 1 114
More informationA5682: Introduction to Cosmology Course Notes. 11. CMB Anisotropy
Reading: Chapter 8, sections 8.4 and 8.5 11. CMB Anisotropy Gravitational instability and structure formation Today s universe shows structure on scales from individual galaxies to galaxy groups and clusters
More informationRayleigh scattering:
Rayleigh scattering: blue sky thinking for future CMB observations arxiv:1307.8148; previous work: Takahara et al. 91, Yu, et al. astro-ph/0103149 http://en.wikipedia.org/wiki/rayleigh_scattering Antony
More information3 Observational Cosmology Evolution from the Big Bang Lecture 2
3 Observational Cosmology Evolution from the Big Bang Lecture 2 http://www.sr.bham.ac.uk/~smcgee/obscosmo/ Sean McGee smcgee@star.sr.bham.ac.uk http://www.star.sr.bham.ac.uk/~smcgee/obscosmo Nucleosynthesis
More informationVariation in the cosmic baryon fraction and the CMB
Variation in the cosmic baryon fraction and the CMB with D. Hanson, G. Holder, O. Doré, and M. Kamionkowski Daniel Grin (KICP/Chicago) Presentation for CAP workshop 09/24/2013 arxiv: 1107.1716 (DG, OD,
More informationCMB constraints on dark matter annihilation
CMB constraints on dark matter annihilation Tracy Slatyer, Harvard University NEPPSR 12 August 2009 arxiv:0906.1197 with Nikhil Padmanabhan & Douglas Finkbeiner Dark matter!standard cosmological model:
More informationRupert Croft. QuickTime and a decompressor are needed to see this picture.
Rupert Croft QuickTime and a decompressor are needed to see this picture. yesterday: Plan for lecture 1: History : -the first quasar spectra -first theoretical models (all wrong) -CDM cosmology meets the
More informationCosmology with Planck: Nucleosynthesis and neutron life-time constraints
Cosmology with Planck: Nucleosynthesis and neutron life-time constraints Luca Pagano Sapienza University of Rome Torino 07-09-2015 Outline Big Bang Nucleosynthesis as cosmological probe Big Bang Nucleosynthesis
More informationOVERVIEW OF NEW CMB RESULTS
OVERVIEW OF NEW CMB RESULTS C. R. Lawrence, JPL for the Planck Collaboration UCLA Dark Matter 2016 2016 February 17 Overview of new CMB results Lawrence 1 UCLA, 2016 February 17 Introduction Planck First
More informationCosmology after Planck
Cosmology after Planck Raphael Flauger Rencontres de Moriond, March 23, 2014 Looking back Until ca. 1997 data was consistent with defects (such as strings) generating the primordial perturbations. (Pen,
More informationPhysical Cosmology 6/6/2016
Physical Cosmology 6/6/2016 Alessandro Melchiorri alessandro.melchiorri@roma1.infn.it slides can be found here: oberon.roma1.infn.it/alessandro/cosmo2016 CMB anisotropies The temperature fluctuation in
More informationGalaxies 626. Lecture 3: From the CMBR to the first star
Galaxies 626 Lecture 3: From the CMBR to the first star Galaxies 626 Firstly, some very brief cosmology for background and notation: Summary: Foundations of Cosmology 1. Universe is homogenous and isotropic
More informationThe Once and Future CMB
The Once and Future CMB DOE, Jan. 2002 Wayne Hu The On(c)e Ring Original Power Spectra of Maps 64º Band Filtered Ringing in the New Cosmology Gravitational Ringing Potential wells = inflationary seeds
More informationWhat can we learn about reionization from the ksz
What can we learn about reionization from the ksz Andrei Mesinger Scuola Normale Superiore, Pisa IGM effect on CMB primary temperature anisotropies ionized IGM damps CMB temperature anisotropies through
More informationImprint of Scalar Dark Energy on CMB polarization
Imprint of Scalar Dark Energy on CMB polarization Kin-Wang Ng ( 吳建宏 ) Institute of Physics & Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan Cosmology and Gravity Pre-workshop NTHU, Apr
More informationPower spectrum exercise
Power spectrum exercise In this exercise, we will consider different power spectra and how they relate to observations. The intention is to give you some intuition so that when you look at a microwave
More informationCross-correlations of CMB lensing as tools for cosmology and astrophysics. Alberto Vallinotto Los Alamos National Laboratory
Cross-correlations of CMB lensing as tools for cosmology and astrophysics Alberto Vallinotto Los Alamos National Laboratory Dark matter, large scales Structure forms through gravitational collapse......
More informationObservational Cosmology
(C. Porciani / K. Basu) Lecture 7 Cosmology with galaxy clusters (Mass function, clusters surveys) Course website: http://www.astro.uni-bonn.de/~kbasu/astro845.html Outline of the two lecture Galaxy clusters
More informationOutline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ =
Cosmology AS7009, 2008 Lecture 10 Outline Structure formation Jeans length, Jeans mass Structure formation with and without dark matter Cold versus hot dark matter Dissipation The matter power spectrum
More informationThe Epoch of Reionization: Observational & Theoretical Topics
The Epoch of Reionization: Observational & Theoretical Topics Lecture 1 Lecture 2 Lecture 3 Lecture 4 Current constraints on Reionization Physics of the 21cm probe EoR radio experiments Expected Scientific
More informationThe AfterMap Wayne Hu EFI, February 2003
The AfterMap Wayne Hu EFI, February 2003 Connections to the Past Outline What does MAP alone add to the cosmology? What role do other anisotropy experiments still have to play? How do you use the MAP analysis
More informationCOSMIC MICROWAVE BACKGROUND ANISOTROPIES
COSMIC MICROWAVE BACKGROUND ANISOTROPIES Anthony Challinor Institute of Astronomy & Department of Applied Mathematics and Theoretical Physics University of Cambridge, U.K. a.d.challinor@ast.cam.ac.uk 26
More informationCosmological Constraints on Dark Energy via Bulk Viscosity from Decaying Dark Matter
Cosmological Constraints on Dark Energy via Bulk Viscosity from Decaying Dark Matter Nguyen Quynh Lan Hanoi National University of Education, Vietnam (University of Notre Dame, USA) Rencontres du Vietnam:
More informationAstr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic
Astr 2320 Thurs. May 7, 2015 Today s Topics Chapter 24: New Cosmology Problems with the Standard Model Cosmic Nucleosynthesis Particle Physics Cosmic Inflation Galaxy Formation 1 Chapter 24: #3 Chapter
More informationCosmology with CMB & LSS:
Cosmology with CMB & LSS: the Early universe VSP08 lecture 4 (May 12-16, 2008) Tarun Souradeep I.U.C.A.A, Pune, India Ω +Ω +Ω +Ω + Ω +... = 1 0 0 0 0... 1 m DE K r r The Cosmic Triangle (Ostriker & Steinhardt)
More informationNeoClassical Probes. of the Dark Energy. Wayne Hu COSMO04 Toronto, September 2004
NeoClassical Probes in of the Dark Energy Wayne Hu COSMO04 Toronto, September 2004 Structural Fidelity Dark matter simulations approaching the accuracy of CMB calculations WMAP Kravtsov et al (2003) Equation
More informationn=0 l (cos θ) (3) C l a lm 2 (4)
Cosmic Concordance What does the power spectrum of the CMB tell us about the universe? For that matter, what is a power spectrum? In this lecture we will examine the current data and show that we now have
More informationCaldwell, MK, Wadley (open) (flat) CMB determination of the geometry (MK, Spergel, and Sugiyama, 1994) Where did large scale structure (e.g., galaxies, clusters, larger-scale explosions clustering)
More informationConcordance Cosmology and Particle Physics. Richard Easther (Yale University)
Concordance Cosmology and Particle Physics Richard Easther (Yale University) Concordance Cosmology The standard model for cosmology Simplest model that fits the data Smallest number of free parameters
More informationReionization constraints post Planck-15
Reionization constraints post Planck-15 Tirthankar Roy Choudhury National Centre for Radio Astrophysics Tata Institute of Fundamental Research Pune CMB Spectral Distortions from Cosmic Baryon Evolution
More informationThe Probes and Sources of Cosmic Reionization Francesco Haardt University of Como INFN, Milano-Bicocca
1 The Probes and Sources of Cosmic Reionization Francesco Haardt University of Insubria@Lake Como INFN, Milano-Bicocca 2 TALK OUTLINE 1. Dark Ages and Reionization 2. Observations: QSO Absorption Lines
More informationCosmic Microwave Background
Cosmic Microwave Background Following recombination, photons that were coupled to the matter have had very little subsequent interaction with matter. Now observed as the cosmic microwave background. Arguably
More informationSome issues in cluster cosmology
Some issues in cluster cosmology Tim McKay University of Michigan Department of Physics 1/30/2002 CFCP Dark Energy Workshop 1 An outline Cluster counting in theory Cluster counting in practice General
More informationReally, what universe do we live in? White dwarfs Supernova type Ia Accelerating universe Cosmic shear Lyman α forest
Really, what universe do we live in? White dwarfs Supernova type Ia Accelerating universe Cosmic shear Lyman α forest White dwarf Core of solar mass star No energy from fusion or gravitational contraction
More informationModern Cosmology / Scott Dodelson Contents
Modern Cosmology / Scott Dodelson Contents The Standard Model and Beyond p. 1 The Expanding Universe p. 1 The Hubble Diagram p. 7 Big Bang Nucleosynthesis p. 9 The Cosmic Microwave Background p. 13 Beyond
More informationPlanck. Report on the status of the mission Carlo Baccigalupi, SISSA
Planck Report on the status of the mission Carlo Baccigalupi, SISSA Outline CMB The Planck satellite Data processing center Expectations from Planck Planck data CMB CMB angular power spectrum Angle 200/l
More informationDark Energy in Light of the CMB. (or why H 0 is the Dark Energy) Wayne Hu. February 2006, NRAO, VA
Dark Energy in Light of the CMB (or why H 0 is the Dark Energy) Wayne Hu February 2006, NRAO, VA If its not dark, it doesn't matter! Cosmic matter-energy budget: Dark Energy Dark Matter Dark Baryons Visible
More informationBrief Introduction to Cosmology
Brief Introduction to Cosmology Matias Zaldarriaga Harvard University August 2006 Basic Questions in Cosmology: How does the Universe evolve? What is the universe made off? How is matter distributed? How
More informationCosmological observables and the nature of dark matter
Cosmological observables and the nature of dark matter Shiv Sethi Raman Research Institute March 18, 2018 SDSS results: power... SDSS results: BAO at... Planck results:... Planck-SDSS comparison Summary
More informationProbing the Dark Ages with 21 cm Absorption
May 13, 2008 Probing the Dark Ages with 21 cm Absorption Emil Polisensky (UMD/NRL) ABSTRACT A brief overview of detecting neutral hydrogen gas during the cosmic Dark Ages in absorption against the background
More informationCosmology II: The thermal history of the Universe
.. Cosmology II: The thermal history of the Universe Ruth Durrer Département de Physique Théorique et CAP Université de Genève Suisse August 6, 2014 Ruth Durrer (Université de Genève) Cosmology II August
More informationLyman-alpha intensity mapping during the Epoch of Reionization
Lyman-alpha intensity mapping during the Epoch of Reionization Mário G. Santos CENTRA IST (Austin, May 15, 2012) Marta Silva, Mario G. Santos, Yan Gong, Asantha Cooray (2012), arxiv:1205.1493 Intensity
More informationCosmology The Road Map
Cosmology The Road Map Peter Schneider Institut für Astrophysik, Bonn University on behalf of the Astronomy Working Group Cosmology s Themes Fundamental Cosmology Probing inflation Investigating Dark Energy
More informationPICO - Probe of Inflation and Cosmic Origins
PICO - Probe of Inflation and Cosmic Origins Shaul Hanany University of Minnesota Executive Committee Bock, Borrill, Crill, Devlin, Flauger, Hanany, Jones, Knox, Kogut, Lawrence, McMahon, Pryke, Trangsrud
More informationPhysics of CMB Polarization and Its Measurement
Physics of CMB Polarization and Its Measurement HEP seminar at Kyoto University April 13 th, 2007 Akito KUSAKA University of Tokyo Outline Physics of CMB and its Polarization What does WMAP shed light
More informationCosmic Rays in Galaxy Clusters: Simulations and Perspectives
Cosmic Rays in Galaxy Clusters: Simulations and Perspectives 1 in collaboration with Volker Springel 2, Torsten Enßlin 2 1 Canadian Institute for Theoretical Astrophysics, Canada 2 Max-Planck Institute
More informationObservational evidence for Dark energy
Observational evidence for Dark energy ICSW-07 (Jun 2-9, 2007) Tarun Souradeep I.U.C.A.A, Pune, India Email: tarun@iucaa.ernet.in Observational evidence for DE poses a major challenge for theoretical cosmology.
More informationObservational Cosmology
The Cosmic Microwave Background Part I: CMB Theory Kaustuv Basu Course website: http://www.astro.uni-bonn.de/~kbasu/obscosmo CMB parameter cheat sheet 2 Make your own CMB experiment! Design experiment
More informationThe Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004
The Early Universe John Peacock ESA Cosmic Vision Paris, Sept 2004 The history of modern cosmology 1917 Static via cosmological constant? (Einstein) 1917 Expansion (Slipher) 1952 Big Bang criticism (Hoyle)
More informationCMB polarization anisotropies from cosmological reionization: extension to B-modes
Prepared for submission to JCAP CMB polarization anisotropies from cosmological reionization: extension to B-modes arxiv:1205.0463v1 [astro-ph.co] 2 May 2012 T. Trombetti, a,b C. Burigana a,c a INAF-IASF
More informationGalaxy Formation Seminar 2: Cosmological Structure Formation as Initial Conditions for Galaxy Formation. Prof. Eric Gawiser
Galaxy Formation Seminar 2: Cosmological Structure Formation as Initial Conditions for Galaxy Formation Prof. Eric Gawiser Cosmic Microwave Background anisotropy and Large-scale structure Cosmic Microwave
More informationAnalyzing the CMB Brightness Fluctuations. Position of first peak measures curvature universe is flat
Analyzing the CMB Brightness Fluctuations (predicted) 1 st rarefaction Power = Average ( / ) 2 of clouds of given size scale 1 st compression 2 nd compression (deg) Fourier analyze WMAP image: Measures
More informationThe cosmic microwave background radiation
The cosmic microwave background radiation László Dobos Dept. of Physics of Complex Systems dobos@complex.elte.hu É 5.60 May 18, 2018. Origin of the cosmic microwave radiation Photons in the plasma are
More informationAstro-2: History of the Universe
Astro-2: History of the Universe Lecture 13; May 30 2013 Previously on astro-2 Energy and mass are equivalent through Einstein s equation and can be converted into each other (pair production and annihilations)
More informationLecture 09. The Cosmic Microwave Background. Part II Features of the Angular Power Spectrum
The Cosmic Microwave Background Part II Features of the Angular Power Spectrum Angular Power Spectrum Recall the angular power spectrum Peak at l=200 corresponds to 1o structure Exactly the horizon distance
More informationMapping Hot Gas in the Universe using the Sunyaev-Zeldovich Effect
Mapping Hot Gas in the Universe using the Sunyaev-Zeldovich Effect Eiichiro Komatsu (Max-Planck-Institut für Astrophysik) Probing Fundamental Physics with CMB Spectral Distortions, CERN March 12, 2018
More informationSynergistic cosmology across the spectrum
Synergistic cosmology across the spectrum Stefano Camera Dipartimento di Fisica, Università degli Studi di Torino, Italy Fundamental Cosmology Lion Panther She-wolf Fundamental Cosmology Dark matter Dark
More informationThe First Cosmic Billion Years. Andrea Ferrara Scuola Normale Superiore, Pisa, Italy
The First Cosmic Billion Years Andrea Ferrara Scuola Normale Superiore, Pisa, Italy DAVID The Dark Ages VIrtual Department http://www.arcetri.astro.it/twiki/bin/view/david/webhome S. Bianchi INAF/Arcetri
More informationSimulating HI 21-cm Signal from EoR and Cosmic Dawn. Kanan K. Datta Presidency University, Kolkata
Simulating HI 21-cm Signal from EoR and Cosmic Dawn Kanan K. Datta Presidency University, Kolkata Plan of the talk Why simulations?! Dynamic ranges of simulations! Basic flowchart for simulation! Various
More informationPrimordial gravitational waves detected? Atsushi Taruya
21 May 2014 Lunch seminar @YITP Primordial gravitational waves detected? Atsushi Taruya Contents Searching for primordial gravitational waves from cosmic microwave background polarizations Gravitational-wave
More informationThe Formation and Evolution of Galaxy Clusters
IAU Joint Discussion # 10 Sydney, July, 2003 The Formation and Evolution of Galaxy Clusters Simon D.M. White Max Planck Institute for Astrophysics The WMAP of the whole CMB sky Bennett et al 2003 > 105
More informationCMB Polarization and Cosmology
CMB Polarization and Cosmology Wayne Hu KIPAC, May 2004 Outline Reionization and its Applications Dark Energy The Quadrupole Gravitational Waves Acoustic Polarization and Initial Power Gravitational Lensing
More informationDark Matter Halos in Warm Dark Matter Models
Dark Matter Halos in Warm Dark Matter Models 5. June @ Workshop CIAS Meudon 2013 Ayuki Kamada (Kavli IPMU, Univ. of Tokyo) in collaboration with Naoki Yoshida (Kavli IPMU, Univ. of Tokyo) Kazunori Kohri
More informationMicrowave Background Polarization: Theoretical Perspectives
Microwave Background Polarization: Theoretical Perspectives Department of Physics and Astronomy University of Pittsburgh CMBpol Technology Workshop Outline Tensor Perturbations and Microwave Polarization
More informationGravitational Lensing of the CMB
Gravitational Lensing of the CMB SNAP Planck 1 Ω DE 1 w a.5-2 -1.5 w -1 -.5 Wayne Hu Leiden, August 26-1 Outline Gravitational Lensing of Temperature and Polarization Fields Cosmological Observables from
More informationWhat I heard about Planck Eiichiro Komatsu (MPA) December 9, 2014 December 22, 2014
What I heard about Planck 2014 Eiichiro Komatsu (MPA) [v1@ipmu] December 9, 2014 [v2@utap] December 22, 2014 Disclaimer I am not involved in Planck I did not attend the conference in Ferrara, Italy, for
More informationWhat do we really know about Dark Energy?
What do we really know about Dark Energy? Ruth Durrer Département de Physique Théorique & Center of Astroparticle Physics (CAP) ESTEC, February 3, 2012 Ruth Durrer (Université de Genève ) Dark Energy ESTEC
More informationThe Interplay Between Galaxies and Black Holes A Theoretical Overview. Massimo Ricotti (U of Maryland)
The Interplay Between Galaxies and Black Holes A Theoretical Overview Massimo Ricotti (U of Maryland) ..a tale of many sleepless nights Maya and Noemi Ricotti Cosmological Context Outline Formation of
More informationNEUTRINO COSMOLOGY. n m. n e. n t STEEN HANNESTAD UNIVERSITY OF AARHUS PLANCK 06, 31 MAY 2006
NEUTRINO COSMOLOGY n e n m n t STEEN HANNESTAD UNIVERSITY OF AARHUS PLANCK 06, 31 MAY 2006 LIMITS ON THE PROPERTIES OF LIGHT NEUTRINOS FROM COSMOLOGICAL DATA THE MASS OF THE ACTIVE SPECIES BOUNDS ON OTHER
More informationDark Matter -- Astrophysical Evidences and Terrestrial Searches
SFB 443 Bosen workshop 2010 Dark Matter -- Astrophysical Evidences and Terrestrial Searches Klaus Eitel, Karlsruhe Institute of Technology, KCETA, IK KIT University of the State of Baden-Württemberg and
More informationPlanck constraints on neutrinos. Massimiliano Lattanzi Università di Ferrara on behalf of the Planck Collaboration
Planck constraints on neutrinos Massimiliano Lattanzi Università di Ferrara on behalf of the Planck Collaboration The Cosmic Neutrino Background (CnB) The presence of a background of relic neutrinos is
More informationMichael Shull (University of Colorado)
Early Galaxies, Stars, Metals, and the Epoch of Reionization Michael Shull (University of Colorado) Far-IR Workshop (Pasadena, CA) May 29, 2008 Submillimeter Galaxies: only the brightest? How long? [dust
More informationDark matter from cosmological probes
PLANCK 2014 Ferrara Dark matter from cosmological probes Simon White Max Planck Institute for Astrophysics Dark matter was discovered in the Coma Cluster by Zwicky (1933) Fritz Zwicky Abell 2218 Corbelli
More informationNEUTRINO COSMOLOGY. ν e ν µ. ν τ STEEN HANNESTAD UNIVERSITY OF AARHUS PARIS, 27 OCTOBER 2006
NEUTRINO COSMOLOGY ν e ν µ ν τ STEEN HANNESTAD UNIVERSITY OF AARHUS PARIS, 27 OCTOBER 2006 OUTLINE A BRIEF REVIEW OF PRESENT COSMOLOGICAL DATA BOUNDS ON THE NEUTRINO MASS STERILE NEUTRINOS WHAT IS TO COME
More informationContents. 1 Introduction... 1 Mauro D Onofrio and Carlo Burigana
Contents 1 Introduction... 1 Mauro D Onofrio and Carlo Burigana 2 Fundamental Cosmological Observations and Data Interpretation... 7 Contributions by Matthias Bartelmann, Charles L. Bennett, Carlo Burigana,
More informationTHE PLANCK MISSION The most accurate measurement of the oldest electromagnetic radiation in the Universe
THE PLANCK MISSION The most accurate measurement of the oldest electromagnetic radiation in the Universe Rodrigo Leonardi Planck Science Office ESTEC/ESA OVERVIEW Planck observational objective & science.
More informationQuasar Absorption Lines
Tracing the Cosmic Web with Diffuse Gas DARK MATTER GAS STARS NEUTRAL HYDROGEN Quasar Absorption Lines use quasars as bright beacons for probing intervening gaseous material can study both galaxies and
More informationCosmic Microwave Background Introduction
Cosmic Microwave Background Introduction Matt Chasse chasse@hawaii.edu Department of Physics University of Hawaii at Manoa Honolulu, HI 96816 Matt Chasse, CMB Intro, May 3, 2005 p. 1/2 Outline CMB, what
More informationHighlights from Planck 2013 cosmological results Paolo Natoli Università di Ferrara and ASI/ASDC DSU2013, Sissa, 17 October 2013
Highlights from Planck 2013 cosmological results Paolo Natoli Università di Ferrara and ASI/ASDC DSU2013, Sissa, 17 October 2013 On behalf of the Planck collaboration Fluctuation and GW generator Fluctuation
More informationGalaxy Formation and Evolution
Galaxy Formation and Evolution Houjun Mo Department of Astronomy, University of Massachusetts 710 North Pleasant Str., Amherst, MA 01003-9305, USA Frank van den Bosch Department of Physics & Astronomy,
More informationCMB Anisotropies and Fundamental Physics. Lecture II. Alessandro Melchiorri University of Rome «La Sapienza»
CMB Anisotropies and Fundamental Physics Lecture II Alessandro Melchiorri University of Rome «La Sapienza» Lecture II CMB & PARAMETERS (Mostly Dark Energy) Things we learned from lecture I Theory of CMB
More informationCan kinetic Sunyaev-Zel dovich effect be used to detect the interaction between DE and DM? Bin Wang Shanghai Jiao Tong University
Can kinetic Sunyaev-Zel dovich effect be used to detect the interaction between DE and DM? Bin Wang Shanghai Jiao Tong University Outline: The interaction model between DE&DM The ISW effect as a probe
More informationPlanck 2015 parameter constraints
Planck 2015 parameter constraints Antony Lewis On behalf of the Planck Collaboration http://cosmologist.info/ CMB temperature End of inflation Last scattering surface gravity+ pressure+ diffusion Observed
More informationGalaxy Formation Now and Then
Galaxy Formation Now and Then Matthias Steinmetz Astrophysikalisches Institut Potsdam 1 Overview The state of galaxy formation now The state of galaxy formation 10 years ago Extragalactic astronomy in
More informationGalaxy population simulations
Aspen, February 2014 Galaxy population simulations Simon White Max Planck Institute for Astrophysics semi-analytic simulations provide a tool... To explore the statistics and interactions of the many processes
More informationMicrocosmo e Macrocosmo
Microcosmo e Macrocosmo Paolo de Bernardis Dipartimento di Fisica Sapienza Università di Roma Lezioni della Cattedra Fermi 23 Gennaio 2014 Dipartimento di Fisica Sapienza Università di Roma Friedman s
More informationForthcoming CMB experiments and expectations for dark energy. Carlo Baccigalupi
Forthcoming CMB experiments and expectations for dark energy Carlo Baccigalupi Outline Classic dark energy effects on CMB Modern CMB relevance for dark energy: the promise of lensing Lensing (B modes)
More informationLecture 03. The Cosmic Microwave Background
The Cosmic Microwave Background 1 Photons and Charge Remember the lectures on particle physics Photons are the bosons that transmit EM force Charged particles interact by exchanging photons But since they
More informationTomography with CMB polarization A line-of-sight approach in real space
Tomography with CMB polarization A line-of-sight approach in real space University of Pennsylvania - feb/2009 L. Raul Abramo Instituto de Física University of Sao Paulo L. Raul Abramo & H. Xavier, Phys.
More informationAbsolute Neutrino Mass from Cosmology. Manoj Kaplinghat UC Davis
Absolute Neutrino Mass from Cosmology Manoj Kaplinghat UC Davis Kinematic Constraints on Neutrino Mass Tritium decay (Mainz Collaboration, Bloom et al, Nucl. Phys. B91, 273, 2001) p and t decay Future
More informationConstraining Dark Energy and Modified Gravity with the Kinetic SZ effect
Constraining Dark Energy and Modified Gravity with the Kinetic SZ effect Eva-Maria Mueller Work in collaboration with Rachel Bean, Francesco De Bernardis, Michael Niemack (arxiv 1408.XXXX, coming out tonight)
More informationDirect Search for Dark Matter
Direct Search for Dark Matter Herbstschule für Hochenergiephysik Maria Laach 2013, September 2013 Institut für Kernphysik, Westfälische Wilhelms-Universität Münster weinheimer@uni-muenster.de - Astrophysical
More information