Understanding the Properties of Dark Energy in the Universe p.1/37
|
|
- Piers West
- 6 years ago
- Views:
Transcription
1 Understanding the Properties of Dark Energy in the Universe Dragan Huterer Case Western Reserve University Understanding the Properties of Dark Energy in the Universe p.1/37
2 The Cosmic Food Pyramid?? Radiation ( ) Luminous Matter ( ) Baryonic Matter ( ) Dark Matter ( ) Dark Energy ( ) Understanding the Properties of Dark Energy in the Universe p.2/37
3 Type Ia Supernovae -20 B Band -19 as measured M B 5 log(h/65) days -20 Calan/Tololo SNe Ia -19 light-curve timescale stretch-factor corrected M B 5 log(h/65) days Kim, et al. (1997) Understanding the Properties of Dark Energy in the Universe p.3/37
4 Discovering SNe Ia Supernova 1998ba Supernova Cosmology Project (Perlmutter, et al., 1998) (as seen from Hubble Space Telescope) 3 Weeks Before Supernova Discovery (as seen from telescopes on Earth) Difference Understanding the Properties of Dark Energy in the Universe p.4/37
5 =0.0 =1.0, &! )( "$% "$#! + * Understanding the Properties of Dark Energy in the Universe p.5/37 Recent Supernova data High-Z SN Search Team Supernova Cosmology Project =0.7 =0.3, m-m (mag) =0.0 =0.3, (m-m) (mag) z
6 ) & & ) & & & & Parameterizing Dark Energy %, & % " % % (flat) ( " % ( " # ( % % # Understanding the Properties of Dark Energy in the Universe p.6/37
7 ) & & ) & & & & Parameterizing Dark Energy %, & % " % % (flat) ( " % ( " # ( % % # may be varying: ( ( * Understanding the Properties of Dark Energy in the Universe p.6/37
8 Current Supernova Constraints Understanding the Properties of Dark Energy in the Universe p.7/37
9 & & Fine-Tuning Problems I: Why Now? DE is important only at, since % # " % " # ( and ) ρ RAD Λ dominates ρ (GeV 4 ) ρ M ρ Λ z Understanding the Properties of Dark Energy in the Universe p.8/37
10 )( )( Fine-Tuning Problems II: Why so small? Refers to the vacuum energy,. (recall ) orders of magnitude discrepancy! Understanding the Properties of Dark Energy in the Universe p.9/37
11 A candidate: Quintessence 1.2 V Equation-of-state ( w Q ) KE dominates Q frozen Q joins tracker sol z ρ (GeV 4 ) φ Peebles & Ratra 1987, Caldwell, Dave & Steinhardt z Understanding the Properties of Dark Energy in the Universe p.10/37
12 Classical Tests r(z) w=-1.0 w=-0.4 dv/dωdz w= dr/dw z z δ(z)/δ(today) 0.1 w= 1/3 w= z Understanding the Properties of Dark Energy in the Universe p.11/37
13 & Wish List, " % Goals: Measure & % equivalently, Measure Measure any clustering of DE Difficulties: DE may cluster at scales Understanding the Properties of Dark Energy in the Universe p.12/37
14 Cosmological Tests of Dark Energy SNAP CURRENT SN 1a Matter density Vacuum density constant Tegmark 2001 Understanding the Properties of Dark Energy in the Universe p.13/37
15 Weak Gravitational Lensing Understanding the Properties of Dark Energy in the Universe p.14/37
16 Current Data and Constraints 1.5 σ Ω M Refregier 2003, Bacon et al Understanding the Properties of Dark Energy in the Universe p.15/37
17 Weak Lensing and DE Ω X =0.70, w= 1.0 Ω X =0.70, w= 0.5 Ω X =0.65, w= 1.0 l(l+1)p l κ/(2π) linear l Hu 1999, Huterer 2002, Refregier et al Understanding the Properties of Dark Energy in the Universe p.16/37
18 Weak Lensing and DE n(z) 0.4 l(l+1)p l κ/(2π) Ω X =0.70, w= 1.0 Ω X =0.70, w= 0.5 Ω X =0.65, w= 1.0 linear z 1 redshift bin 2 bins 10 bins w l 0.8 Hu 1999, Huterer 2002, Refregier et al Ω M Understanding the Properties of Dark Energy in the Universe p.16/37
19 Deeper and Wider σ(w) 0.08 σ(w) σ(ω X ) 0.04 σ(ω X ) depth (R band mag) sky coverage (deg 2 ) Huterer 2002 Understanding the Properties of Dark Energy in the Universe p.17/37
20 Number Counts dn/dz (4000 deg 2 ) w=-0.8 Ω M =1, Ω DE =0 Ω M =0.3, Ω DE =0.7, w= z Understanding the Properties of Dark Energy in the Universe p.18/37
21 Number Counts Count clusters using X-ray, SZ, weak lensing... Mass-observable relation Haiman, Mohr & Holder 2001, Majumdar & Mohr 2003 Understanding the Properties of Dark Energy in the Universe p.19/37
22 Cosmic Microwave Background Anisotropies Bennett et al (WMAP collaboration) Understanding the Properties of Dark Energy in the Universe p.20/37
23 CMB Sensitivity to Dark Energy Peak locations are sensitive to dark energy (but not much): w = -1.0 w = -0.5 l(l+1)c l / (2π) (µk 2 ) Same as measurement of with fixed End up constraining: (Planck: to %) l Huterer & Turner 2001, Frieman et al Understanding the Properties of Dark Energy in the Universe p.21/37
24 SNe plus CMB constant σ w SNe SNe + σ ΩM = 0.03 SNe + σ ΩM = 0.01 SNe + Planck SNe + Planck + σ ΩM = 0.01 σ dw/dz SNe SNe + σ ΩM = 0.03 SNe + σ ΩM = 0.01 SNe + Planck SNe + Planck + σ ΩM = z MAX z MAX Frieman, Huterer, Linder & Turner 2003 Understanding the Properties of Dark Energy in the Universe p.22/37
25 CMB-LSS cross-correlation Understanding the Properties of Dark Energy in the Universe p.23/37
26 Understanding the Properties of Dark Energy in the Universe p.23/37 CMB-LSS cross-correlation Ω Λ = 0.0 Ω Λ = 0.5 Ω Λ = Number of Realizations XT /σ X σ T Boughn, Crittenden & Turok 1997
27 CMB-LSS cross-correlation z ~ 0.57 z ~ Number of Realizations Ω Λ = 0.0 Ω Λ = 0.5 Ω Λ = 0.8 w gt (θ) [µk] z ~ z ~ XT /σ X σ T θ (degrees) 1 10 Boughn, Crittenden & Turok 1997, Scranton et al Understanding the Properties of Dark Energy in the Universe p.23/37
28 Strong Gravitational Lensing Understanding the Properties of Dark Energy in the Universe p.24/37
29 Strong Lensing Statistics Required input: Cosmology (, Luminosity function (galaxies) or mass function (all halos), ) τ Density profile of lenses e.g. SIS: or generalized NFW: Magnification bias β Kochanek 1993, 1996, Cooray & Huterer 1999, Chae 2003, Davis, Huterer & Krauss 2003, Kuhlen, Keeton & Madau 2003 Understanding the Properties of Dark Energy in the Universe p.25/37
30 Strong Lensing Statistics Required input: Cosmology (,, ) Luminosity function (galaxies) or mass function (all halos) Density profile of lenses e.g. SIS: or generalized NFW: Magnification bias M c / (h -1 M sun ) % CL 95% CL β Huterer & Ma 2003 Understanding the Properties of Dark Energy in the Universe p.25/37
31 Beyond 1.0 ( 0.5 w w 0 Understanding the Properties of Dark Energy in the Universe p.26/37
32 Beyond 1.0 ( 0.5 w w Principal Components of e i (z) 0 4 Huterer & Starkman z Understanding the Properties of Dark Energy in the Universe p.26/37
33 Reconstruction of ( "$# ( ( ( "$# w(z) z Huterer and Turner 1999; Chiba and Nakamura 1999, Weller & Albrecht 2002 Understanding the Properties of Dark Energy in the Universe p.27/37
34 Requirements SCIENCE Measure Ω and Λ M Measure w and w(z) STATISTICAL REQUIREMENTS Sufficient (~2000) numbers of SNe Ia...distributed in redshift...out to z < 1.7 SYSTEMATICS REQUIREMENTS Identified & proposed systematics: Measurements to eliminate / bound each one to +/-0.02mag DATA SET REQUIREMENTS Discoveries 3.8 mag before max. Spectroscopy with S/N=10 at 15 Å bins. Near-IR spectroscopy to 1.7 µm. SATELLITE / INSTRUMENTATION REQUIREMENTS ~2-meter mirror 1-square degree imager 3-channel spectrograph (0.3 µm to 1.7 µm) Derived requirements: High Earth orbit ~5 Mb/sec bandwidth Understanding the Properties of Dark Energy in the Universe p.28/37
35 SuperNova/Acceleration Probe Understanding the Properties of Dark Energy in the Universe p.29/37
36 Understanding the Properties of Dark Energy in the Universe p.30/37
37 Mirror and Focal Plane Understanding the Properties of Dark Energy in the Universe p.31/37
38 SNAP SuperNova Acceleration Probe ~2500 SNe Ia Understanding the Properties of Dark Energy in the Universe p.32/37
39 SNAP predicted constraints 3 No Big Bang Dark Energy Unknown Component,Ωu, of Energy Density 2 Supernovae 0.0 Supernova Cosmology Project Perlmutter et al. (1998) vacuum energy density (cosmological constant) Clusters Maxima SNAP Target Statistical Uncertainty CMB Boomerang open expands forever recollapses eventually flat closed equation of state w = p u / ρ u Flat Universe Constant w 99% 95% 90% 68% network of cosmic strings w = 1/3 range of "Quintessence" models cosmological constant w = Ω Μ = 1 Ωu mass density SNAP Satellite Target Statistical Uncertainty Understanding the Properties of Dark Energy in the Universe p.33/37
40 Weak Lensing with SNAP WL (PS) WL (PS+BS) SNe w SNe + WL (PS+BS) SNe WL (PS) WL (PS+BS) dw/dz SNe + WL (PS+BS) Ω M w 0 Understanding the Properties of Dark Energy in the Universe p.34/37
41 Understanding the Properties of Dark Energy in the Universe p.35/37
42 NASA-DOE Joint Dark Energy Mission Paul Hertz / NASA Robin Staffin / DOE Endorsed by Raymond L. Orbach Edward J. Weiler Director of the Office of Science Associate Administrator for Space Science Department of Energy NASA September 24, 2003 September 25, 2003 Understanding the Properties of Dark Energy in the Universe p.36/37 1
43 Conclusions Dark energy makes up of energy density in the universe. It is smooth and has negative pressure. We describe it via and. It affects cosmology by modifying the expansion rate at recent times ( ). SNe Ia, weak lensing and number counts are most promising probes; variety of other methods can help. Bright prospects with future wide-field surveys (SNAP, LSST, SPT,...) But to understand DE, major insights will be needed from theorists. This will be especially hard if! Understanding the Properties of Dark Energy in the Universe p.37/37
THE ROAD TO DARK ENERGY
Modern Physics Letters A Vol. 23, Nos. 17 20 (2008) 1346 1353 c World Scientific Publishing Company THE ROAD TO DARK ENERGY DRAGAN HUTERER Department of Physics, University of Michigan 450 Church St.,
More informationConstraints on dark energy and its models
Constraints on dark energy and its models Dragan Huterer 1, Eric V. Linder 2 and Jochen Weller 3 1 Department of Physics, The University of Chicago, Chicago, IL 60637-1433 2 E. O. Lawrence Berkeley National
More informationDark Energy and the Accelerating Universe
Dark Energy and the Accelerating Universe Dragan Huterer Department of Physics University of Michigan The universe today presents us with a grand puzzle: What is 95% of it made of? Shockingly, we still
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 informationAn Introduction to the Dark Energy Survey
An Introduction to the Dark Energy Survey A study of the dark energy using four independent and complementary techniques Blanco 4m on Cerro Tololo Galaxy cluster surveys Weak lensing Galaxy angular power
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 informationGravitational lensing constraint on the cosmic equation of state
Gravitational lensing constraint on the cosmic equation of state arxiv:astro-ph/0105551v1 31 May 2001 Deepak Jain, Abha Dev, N. Panchapakesan S. Mahajan and V. B. Bhatia Department of Physics and Astrophysics
More informationLambda or Dark Energy or Modified Gravity?
Lambda or Dark Energy or Modified Gravity? Dragan Huterer Department of Physics University of Michigan Evidence for Dark Energy Theory Model Building Which flavor of DE? Experiment Systematics control
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 informationCosmology. Jörn Wilms Department of Physics University of Warwick.
Cosmology Jörn Wilms Department of Physics University of Warwick http://astro.uni-tuebingen.de/~wilms/teach/cosmo Contents 2 Old Cosmology Space and Time Friedmann Equations World Models Modern Cosmology
More informationStructure in the CMB
Cosmic Microwave Background Anisotropies = structure in the CMB Structure in the CMB Boomerang balloon flight. Mapped Cosmic Background Radiation with far higher angular resolution than previously available.
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 informationSupernovae Observations of the Expanding Universe. Kevin Twedt PHYS798G April 17, 2007
Supernovae Observations of the Expanding Universe Kevin Twedt PHYS798G April 17, 2007 Overview How do we measure expansion? Use of supernovae 1a as a good measuring stick Techniques for observing supernovae
More informationSupernovae Observations of the Accelerating Universe. K Twedt Department of Physics, University of Maryland, College Park, MD, 20740, USA
Supernovae Observations of the Accelerating Universe K Twedt Department of Physics, University of Maryland, College Park, MD, 20740, USA Over the past three decades, supernovae observations have been the
More informationNew techniques to measure the velocity field in Universe.
New techniques to measure the velocity field in Universe. Suman Bhattacharya. Los Alamos National Laboratory Collaborators: Arthur Kosowsky, Andrew Zentner, Jeff Newman (University of Pittsburgh) Constituents
More informationFigures of Merit for Dark Energy Measurements
Figures of Merit for Dark Energy Measurements Dragan Huterer Department of Physics University of Michigan What next for Dark Energy? Theory Model Building Which flavor of DE? Experiment Systematics control
More informationMODERN COSMOLOGY LECTURE FYTN08
1/43 MODERN COSMOLOGY LECTURE Lund University bijnens@thep.lu.se http://www.thep.lu.se/ bijnens Lecture Updated 2015 2/43 3/43 1 2 Some problems with a simple expanding universe 3 4 5 6 7 8 9 Credit many
More informationThe DoE/NASA Joint Dark Energy Mission. November 2005 Kim Griest
The DoE/NASA Joint Dark Energy Mission November 2005 Kim Griest JDEM Science Definition Team (SDT): Cochairs: Chuck Bennett and Kim Griest Members: Albrecht, Baltay, Barish, Bernstein, Blandford, Caldwell,
More informationIntroduction. How did the universe evolve to what it is today?
Cosmology 8 1 Introduction 8 2 Cosmology: science of the universe as a whole How did the universe evolve to what it is today? Based on four basic facts: The universe expands, is isotropic, and is homogeneous.
More informationShear Power of Weak Lensing. Wayne Hu U. Chicago
Shear Power of Weak Lensing 10 3 N-body Shear 300 Sampling errors l(l+1)c l /2π εε 10 4 10 5 Error estimate Shot Noise θ y (arcmin) 200 100 10 6 100 1000 l 100 200 300 θ x (arcmin) Wayne Hu U. Chicago
More informationMapping the Dark Energy Equation of State
**TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Mapping the Dark Energy Equation of State Eric V. Linder Berkeley Lab, 1 Cyclotron Road, M/S 50R5008, Berkeley,
More informationCosmology with the ESA Euclid Mission
Cosmology with the ESA Euclid Mission Andrea Cimatti Università di Bologna Dipartimento di Astronomia On behalf of the Euclid Italy Team ESA Cosmic Vision 2015-2025 M-class Mission Candidate Selected in
More informationCMB anisotropy & Large Scale Structure : Dark energy perspective
CMB anisotropy & Large Scale Structure : Dark energy perspective ICSW-07 IPM, Tehran (Jun 2-9, 2007) Tarun Souradeep I.U.C.A.A, Pune, India India I.U.C.A.A., Pune, India The Realm of Cosmology Basic unit:
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 informationarxiv:astro-ph/ v3 31 Mar 2006
astro-ph/61453 Observational constraints on the acceleration of the Universe Yungui Gong College of Electronic Engineering, Chongqing University of Posts and Telecommunications, Chongqing 465, China and
More informationThe early and late time acceleration of the Universe
The early and late time acceleration of the Universe Tomo Takahashi (Saga University) March 7, 2016 New Generation Quantum Theory -Particle Physics, Cosmology, and Chemistry- @Kyoto University The early
More informationTheoretical Explanations for Cosmic Acceleration
Theoretical Explanations for Cosmic Acceleration Eanna Flanagan, Cornell Physics Colloquium, University of Guelph, 17 October 2006 Outline Recent observations show that the expansion of the Universe is
More informationThe Expanding Universe
Cosmology Expanding Universe History of the Universe Cosmic Background Radiation The Cosmological Principle Cosmology and General Relativity Dark Matter and Dark Energy Primitive Cosmology If the universe
More informationOptimal Supernova Search Strategies
Optimal Supernova Search Strategies Dragan Huterer 1 and Michael S. Turner 1,2,3 1 Department of Physics, University of Chicago, Chicago IL 6637, USA 2 Department of Astronomy and Astrophysics, University
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 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 informationDark energy. P. Binétruy AstroParticule et Cosmologie, Paris. Zakopane, 15 June 2007
Dark energy P. Binétruy AstroParticule et Cosmologie, Paris Zakopane, 15 June 2007 Context : the twentieth century legacy Two very successful theories : General relativity A single equation, Einstein s
More informationLecture 37 Cosmology [not on exam] January 16b, 2014
1 Lecture 37 Cosmology [not on exam] January 16b, 2014 2 Structure of the Universe Does clustering of galaxies go on forever? Looked at very narrow regions of space to far distances. On large scales the
More informationCosmology. Introduction Geometry and expansion history (Cosmic Background Radiation) Growth Secondary anisotropies Large Scale Structure
Cosmology Introduction Geometry and expansion history (Cosmic Background Radiation) Growth Secondary anisotropies Large Scale Structure Cosmology from Large Scale Structure Sky Surveys Supernovae Ia CMB
More informationDark Energy. Cluster counts, weak lensing & Supernovae Ia all in one survey. Survey (DES)
Dark Energy Cluster counts, weak lensing & Supernovae Ia all in one survey Survey (DES) What is it? The DES Collaboration will build and use a wide field optical imager (DECam) to perform a wide area,
More informationChapter 1 Introduction. Particle Astrophysics & Cosmology SS
Chapter 1 Introduction Particle Astrophysics & Cosmology SS 2008 1 Ptolemäus (85 165 b.c.) Kopernicus (1473 1543) Kepler (1571 1630) Newton (1643 1727) Kant (1724 1630) Herschel (1738 1822) Einstein (1917)
More information2. Lens population. 3. Lens model. 4. Cosmology. z=0.5. z=0
Chuck Keeton Hubble Fellow, University of Chicago ffl Lens statistics probe the volume of the universe to z ο 1 3. ffl Current constraints on Λ. ffl Systematics! ffl Prospects for equation of state (w,
More informationModern Cosmology Final Examination Solutions 60 Pts
Modern Cosmology Final Examination Solutions 6 Pts Name:... Matr. Nr.:... February,. Observable Universe [4 Pts] 6 Pt: Complete the plot of Redshift vs Luminosity distance in the range < z < and plot (i)
More informationCH 14 MODERN COSMOLOGY The Study of Nature, origin and evolution of the universe Does the Universe have a center and an edge? What is the evidence
CH 14 MODERN COSMOLOGY The Study of Nature, origin and evolution of the universe Does the Universe have a center and an edge? What is the evidence that the Universe began with a Big Bang? How has the Universe
More informationDark Matter and Cosmic Structure Formation
Dark Matter and Cosmic Structure Formation Prof. Luke A. Corwin PHYS 792 South Dakota School of Mines & Technology Jan. 23, 2014 (W2-2) L. Corwin, PHYS 792 (SDSM&T) DM & Cosmic Structure Jan. 23, 2014
More informationExamining Dark Energy With Dark Matter Lenses: The Large Synoptic Survey Telescope. Andrew R. Zentner University of Pittsburgh
Examining Dark Energy With Dark Matter Lenses: The Large Synoptic Survey Telescope Andrew R. Zentner University of Pittsburgh 1 Overview The contents of the Universe The accelerating Universe and Dark
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 informationThe large scale structure of the universe
The large scale structure of the universe Part 1: Deciphering the large scale structure (LSS) With statistics and physics Part 2: Tracers of LSS Broadband power spectrum, BAO, redshift distortion, weak
More informationCosmology with the Sloan Digital Sky Survey Supernova Search. David Cinabro
Cosmology with the Sloan Digital Sky Survey Supernova Search David Cinabro Cosmology Background The study of the origin and evolution of the Universe. First real effort by Einstein in 1916 Gravity is all
More informationIf there is an edge to the universe, we should be able to see our way out of the woods. Olber s Paradox. This is called Olber s Paradox
Suppose the Universe were not expanding, but was in some kind of steady state. How should galaxy recession velocities correlate with distance? They should a) be directly proportional to distance. b) reverse
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 informationComplementarity in Dark Energy measurements. Complementarity of optical data in constraining dark energy. Licia Verde. University of Pennsylvania
Complementarity in Dark Energy measurements Complementarity of optical data in constraining dark energy Licia Verde University of Pennsylvania www.physics.upenn.edu/~lverde The situation: SN 1A (Riess
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 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 informationDiving into precision cosmology and the role of cosmic magnification
Diving into precision cosmology and the role of cosmic magnification Jose Luis Bernal Institute of Cosmos Science - Barcelona University ICC Winter Meeting 2017 06/02/2017 Jose Luis Bernal (ICCUB) ICC
More informationConstraining Modified Gravity and Coupled Dark Energy with Future Observations Matteo Martinelli
Coupled Dark University of Rome La Sapienza Roma, October 28th 2011 Outline 1 2 3 4 5 1 2 3 4 5 Accelerated Expansion Cosmological data agree with an accelerated expansion of the Universe d L [Mpc] 16000
More informationWL and BAO Surveys and Photometric Redshifts
WL and BAO Surveys and Photometric Redshifts Lloyd Knox University of California, Davis Yong-Seon Song (U Chicago) Tony Tyson (UC Davis) and Hu Zhan (UC Davis) Also: Chris Fassnacht, Vera Margoniner and
More informationLecture #25: Plan. Cosmology. The early Universe (cont d) The fate of our Universe The Great Unanswered Questions
Lecture #25: Plan Cosmology The early Universe (cont d) The fate of our Universe The Great Unanswered Questions Announcements Course evaluations: CourseEvalUM.umd.edu Review sheet #3 was emailed to you
More informationFURTHER COSMOLOGY Book page T H E M A K E U P O F T H E U N I V E R S E
FURTHER COSMOLOGY Book page 675-683 T H E M A K E U P O F T H E U N I V E R S E COSMOLOGICAL PRINCIPLE Is the Universe isotropic or homogeneous? There is no place in the Universe that would be considered
More informationNonparametric Inference and the Dark Energy Equation of State
Nonparametric Inference and the Dark Energy Equation of State Christopher R. Genovese Peter E. Freeman Larry Wasserman Department of Statistics Carnegie Mellon University http://www.stat.cmu.edu/ ~ genovese/
More informationThe growth rate index of large scale structure as a probe of the cause of cosmic acceleration
The growth rate index of large scale structure as a probe of the cause of cosmic acceleration Prof. Mustapha Ishak Collaborators: J. Dossett, Y. Gong, A. Wang Cosmology and Relativity Group Department
More informationLecture 7:Our Universe
Lecture 7:Our Universe 1. Traditional Cosmological tests Theta-z Galaxy counts Tolman Surface Brightness test 2. Modern tests HST Key Project (H o ) Nucleosynthesis (Ω b ) BBN+Clusters (Ω M ) SN1a (Ω M
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 informationChapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc.
Chapter 23 Lecture The Cosmic Perspective Seventh Edition Dark Matter, Dark Energy, and the Fate of the Universe Curvature of the Universe The Density Parameter of the Universe Ω 0 is defined as the ratio
More informationRecent BAO observations and plans for the future. David Parkinson University of Sussex, UK
Recent BAO observations and plans for the future David Parkinson University of Sussex, UK Baryon Acoustic Oscillations SDSS GALAXIES CMB Comparing BAO with the CMB CREDIT: WMAP & SDSS websites FLAT GEOMETRY
More informationThe Cosmic Microwave Background
The Cosmic Microwave Background Our probe of the birth of the universe Will Handley wh260@cam.ac.uk Astrophysics Department Cavendish Laboratory University of Cambridge 20 th March 2013 Overview Light
More informationCosmology: Building the Universe.
Cosmology: Building the Universe. The term has several different meanings. We are interested in physical cosmology - the study of the origin and development of the physical universe, and all the structure
More informationSupernova cosmology. The quest to measure the equation of state of dark energy. Bruno Leibundgut European Southern Observatory
Supernova cosmology The quest to measure the equation of state of dark energy Bruno Leibundgut European Southern Observatory Outline Cosmological background Supernovae One-stop shopping for the Hubble
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 informationCosmology with Peculiar Velocity Surveys
Cosmology with Peculiar Velocity Surveys Simulations Fest, Sydney 2011 Morag I Scrimgeour Supervisors: Lister Staveley-Smith, Tamara Davis, Peter Quinn Collaborators: Chris Blake, Brian Schmidt What are
More informationAstr 102: Introduction to Astronomy. Lecture 16: Cosmic Microwave Background and other evidence for the Big Bang
Astr 102: Introduction to Astronomy Fall Quarter 2009, University of Washington, Željko Ivezić Lecture 16: Cosmic Microwave Background and other evidence for the Big Bang 1 Outline Observational Cosmology:
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 informationThe Search for the Complete History of the Cosmos. Neil Turok
The Search for the Complete History of the Cosmos Neil Turok * The Big Bang * Dark Matter and Energy * Precision Tests * A Cyclic Universe? * Future Probes BIG Questions * What are the Laws of Nature?
More informationarxiv: v2 [astro-ph] 26 Jun 2007
Cosmic Acceleration, Dark Energy and Fundamental Physics Michael S. Turner and Dragan Huterer Kavli Institute for Cosmological Physics, Department of Astronomy and Astrophysics, and Department of Physics,
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 informationCosmology. Clusters of galaxies. Redshift. Late 1920 s: Hubble plots distances versus velocities of galaxies. λ λ. redshift =
Cosmology Study of the structure and origin of the universe Observational science The large-scale distribution of galaxies Looking out to extremely large distances The motions of galaxies Clusters of galaxies
More informationReally, 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 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 informationCOSMOLOGY The Universe what is its age and origin?
COSMOLOGY The Universe what is its age and origin? REVIEW (SUMMARY) Oppenheimer Volkhoff limit: upper limit to mass of neutron star remnant more than 1.4 M à neutron degeneracy Supernova à extremely dense
More informationThe Dark Sector ALAN HEAVENS
The Dark Sector ALAN HEAVENS INSTITUTE FOR ASTRONOMY UNIVERSITY OF EDINBURGH AFH@ROE.AC.UK THIRD TRR33 WINTER SCHOOL PASSO DEL TONALE (ITALY) 6-11 DECEMBER 2009 Outline Dark Matter Dark Energy Dark Gravity
More informationWeak Lensing: a Probe of Dark Matter and Dark Energy. Alexandre Refregier (CEA Saclay)
Weak Lensing: a Probe of Dark Matter and Dark Energy Alexandre Refregier (CEA Saclay) SLAC August 2004 Concordance ΛCDM Model Outstanding questions: initial conditions (inflation?) nature of the dark matter
More informationObservational cosmology: the RENOIR team. Master 2 session
Observational cosmology: the RENOIR team Master 2 session 2014-2015 Observational cosmology: the RENOIR team Outline A brief history of cosmology Introduction to cosmological probes and current projects
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 informationAstronomy 162, Week 10 Cosmology Patrick S. Osmer Spring, 2006
Astronomy 162, Week 10 Cosmology Patrick S. Osmer Spring, 2006 Information Makeup quiz Wednesday, May 31, 5-6PM, Planetarium Review Session, Monday, June 5 6PM, Planetarium Cosmology Study of the universe
More informationDark Matter. Jaan Einasto Tartu Observatory and ICRANet 16 December Saturday, December 15, 12
Dark Matter Jaan Einasto Tartu Observatory and ICRANet 16 December 2012 Local Dark Matter: invisible matter in the Galaxy in Solar vicinity Global Dark Matter: invisible matter surrounding galaxies Global
More informationDr Carolyn Devereux - Daphne Jackson Fellow Dr Jim Geach Prof. Martin Hardcastle. Centre for Astrophysics Research University of Hertfordshire, UK
Millennium simulation of the cosmic web MEASUREMENTS OF THE LINEAR BIAS OF RADIO GALAXIES USING CMB LENSING FROM PLANCK Dr Carolyn Devereux - Daphne Jackson Fellow Dr Jim Geach Prof. Martin Hardcastle
More informationTesla Jeltema. Assistant Professor, Department of Physics. Observational Cosmology and Astroparticle Physics
Tesla Jeltema Assistant Professor, Department of Physics Observational Cosmology and Astroparticle Physics Research Program Research theme: using the evolution of large-scale structure to reveal the fundamental
More informationEUCLID Spectroscopy. Andrea Cimatti. & the EUCLID-NIS Team. University of Bologna Department of Astronomy
EUCLID Spectroscopy Andrea Cimatti University of Bologna Department of Astronomy & the EUCLID-NIS Team Observing the Dark Universe with EUCLID, ESA ESTEC, 17 November 2009 DARK Universe (73% Dark Energy
More informationThe Cosmological Principle
Cosmological Models John O Byrne School of Physics University of Sydney Using diagrams and pp slides from Seeds Foundations of Astronomy and the Supernova Cosmology Project http://www-supernova.lbl.gov
More informationmass times that of the Sun - it once the white dwarf reaches a critical material from its binary companion, and
Learning about the composition of our universe has involved multiple astronomical surveys. Below are a collection of the types of observations that have led to astronomers' current understanding of the
More informationDark Matter and Dark Energy components chapter 7
Dark Matter and Dark Energy components chapter 7 Lecture 4 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,
More informationThe Tools of Cosmology. Andrew Zentner The University of Pittsburgh
The Tools of Cosmology Andrew Zentner The University of Pittsburgh 1 Part Two: The Contemporary Universe 2 Contents Review of Part One The Pillars of Modern Cosmology Primordial Synthesis of Light Nuclei
More informationCosmology of Photometrically- Classified Type Ia Supernovae
Cosmology of Photometrically- Classified Type Ia Supernovae Campbell et al. 2013 arxiv:1211.4480 Heather Campbell Collaborators: Bob Nichol, Chris D'Andrea, Mat Smith, Masao Sako and all the SDSS-II SN
More informationExploring dark energy in the universe through baryon acoustic oscillation
Exploring dark energy in the universe through baryon acoustic oscillation WMAP CMB power spectrum SDSS galaxy correlation Yasushi Suto Department of Physics, University of Tokyo KEK Annual Theory Meeting
More informationCosmology with the Sloan Digital Sky Survey Supernova Search. David Cinabro
Cosmology with the Sloan Digital Sky Survey Supernova Search David Cinabro Cosmology Background The study of the origin and evolution of the Universe. First real effort by Einstein in 1916 Gravity is all
More informationChapter 23 Lecture. The Cosmic Perspective Seventh Edition. Dark Matter, Dark Energy, and the Fate of the Universe Pearson Education, Inc.
Chapter 23 Lecture The Cosmic Perspective Seventh Edition Dark Matter, Dark Energy, and the Fate of the Universe Curvature of the Universe The Density Parameter of the Universe Ω 0 is defined as the ratio
More informationDark Energy vs. Dark Matter: Towards a unifying scalar field?
Dark Energy vs. Dark Matter: Towards a unifying scalar field? Alexandre ARBEY Centre de Recherche Astrophysique de Lyon Institut de Physique Nucléaire de Lyon, March 2nd, 2007. Introduction The Dark Stuff
More informationDark Matter and Dark Energy
Dark Matter and Dark Energy Sean Carroll, University of Chicago Our universe, as inventoried over the last ten years: 5% Ordinary Matter 25% D ark M atter 70% Dark Energy Dark Energy Dark Matter Ordinary
More informationAstronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 7 Oct. 30, 2015 Today Relativistic Cosmology Dark Side of the Universe I: Dark Matter Assignments This week: read Hawley and
More informationThe structure and evolution of stars. Learning Outcomes
The structure and evolution of stars Lecture14: Type Ia Supernovae The Extravagant Universe By R. Kirshner 1 Learning Outcomes In these final two lectures the student will learn about the following issues:
More informationShort introduction to the accelerating Universe
SEMINAR Short introduction to the accelerating Universe Gašper Kukec Mezek Our expanding Universe Albert Einstein general relativity (1917): Our expanding Universe Curvature = Energy Our expanding Universe
More informationHow many dark energy parameters?
PHYSICAL REVIEW D 72, 043509 (2005) How many dark energy parameters? Eric V. Linder 1 and Dragan Huterer 2 1 Physics Division, Lawrence Berkeley Laboratory, Berkeley, California 94720, USA 2 Kavli Institute
More informationSpacetime Diagrams. Relativity and Astrophysics Lecture 21 Terry Herter
Spacetime Diagrams Relativity and Astrophysics Lecture 21 Terry Herter Outline Fate of the Universe Forever expansion Dark Energy Time is Private Spacetime diagrams Prelim Wednesday, Oct. 21 Closed book
More informationThe Hunt for Dark Energy
The Hunt for Dark Energy Peter Garnavich University of Notre Dame as imagination bodies forth astronomer s The forms of things unknown, the poet's pen Turns them to shapes and gives to airy nothing A local
More informationIntroducing DENET, HSC, & WFMOS
RESCEU & JSPS core-tocore program DENET Summer School Dark energy in the universe September 1-4, 2007 Introducing DENET, HSC, & WFMOS Yasushi Suto Department of Physics, The University of Tokyo 1 International
More information