Why the Universe needs Dark Matter?
|
|
|
- Adela Miller
- 5 years ago
- Views:
Transcription
1 Why the Universe needs Dark Matter? Shant Baghram Physics Department Sharif University of Technology IPM Workshop on Particle Physics Phenomenology (IWPPP 15 February 2017 Almond Blossoms by Vincent van Gogh (1890 Van Gogh Museum - Amsterdam
2 DM and Zwicky, Rubin, Peebles, Ostriker, White, Rees and NFW اربخوهش محل ی Vera Rubin (ورا L107 رونیب 225, J. (Rubin,V.C., Ford, W.K. & Thonnard, N. 1978, Astrophys زویکی 1937
3 This collision site, known officially as Abell 2744, has been dubbed "Pandora's Cluster" X- ray: NASA/CXC/ITA/INAF/J.Merten et al, Lensing: NASA/STScI; NAOJ/Subaru; ESO/VLT, Optical: NASA/STScI/R.Dupke Release date: June 22, 2011
4 Multiwavelength Astronomy / gravitational lensing (Picture Credit: X-ray(pink: NASA/CXC/CfA/M.Markevitch et al.; Optical: NASA/STScI; Magellan/U.Arizona/D.Clowe et al.; Lensing Map (blue: NASA/STScI; ESO WFI; Magellan/U.Arizona/D.Clowe et al Bullet Cluster Z~0.296
5 There is nothing more deceptive than an obvious fact. Sherlock Holmes Quote -The Bascombe Valley Mystery
6 Baryonic Tully Fisher Relation Silk Mamon (2012
7 Cosmic Microwave Background radiation
8 Angular power-spectrum Universe in the eyes of Planck Scale
9 LSS: LARGE SCALE STRUCTURE
10 Cosmic Evolution of structures
11 رامآ اب و تلالاتخ ا اب ناه یک.م ی راد یا هطقن ود ع ب تا هبساح م به جایتحا یرامآ ی س ربر یابر : ن ی ابت مو ه فم :یا هطقن ود همبستگی ع ب تا :ناو ت ف یط ( ( ( r x x r b b x x ( ( ( ( (2 ( ( 3 k k k P k k D g g g g n n R n R ( ( Millennium Simulation Project - Max-Planck-Institut für Astrophysik
12 Matter power spectrum The matter power spectrum of structures: A Triumph of Modern Cosmology Scale
13 BAO: Baryonic Acoustic Oscillation Martin White WMAP team
14 The two point correlation of structures and BAO
15 The musing of Press and Schechter arxiv: Matrix Formalism of Excursion Set Theory: A new approach to statistics of dark matter halo counting Farnik Nikakhtar, SB
16 Press Scheschter c M c collapsed M e P e P ( 2 2 ( ( 2 1 ( c c e f 2 ( 2 2 large R medium R small R fraction of volumes
17 Dark Matter as a host of Luminous matter Universality function Ravi Sheth n( M dm 2 2 M f ( d ln ( M d ln M dm
18 Almond Blossoms by Vincent van Gogh (1890 Van Gogh Museum - Amsterdam
19 Secondary effects of CMB CMB Lensing ISW Rees Sciama Reionization tsz - ksz Osiker Vishniac
20 CMB Lensing as an evidence DM Farbod Hassani, SB, Hassan Firouzjahi, arxiv: Mohammad Ansari Master Thesis In progress
21 Dark matter from galaxy to clusters
22 The missing satellite + Too big to fail Strigari et al., Nature 454: , 2008
23 Millennium Simulation Garching Dark Matter Cold or Warm Aquires 2010
24 Warm Dark Matter an idea for cosmology
25 Lyman Alpha forest and Catch 22 problem Zaldarriaga & Tegmark 2002
26 From dark matter to baryons Non linearity RSD Bias
27 From dark Matter to Galaxies n n( M, z,... ( L, z,...
28 The bias and number density of structures ( z,... b ( k, z, L, Env,... g n n m b halo ~ ln n( M, / dm l l
29 Matter Power Spectrum in Non linear regime Asantha Cooray, Ravi Sheth Phys.Rept.372:1-129,2002
30 Niayesh Afshordi Sohrab Rahvar, SB, Niayesh Afshordi, arxiv: SB, Niayesh Afshordi, Kathryn M. Zurek, arxiv: فضای افز ماده اتریک چ گا ل ی فضای افز رد زمان واجفتید گ ی چ گا ل ی ف ضای افز کهکشان راه شی ری f ab رتشیب فضای افز خا ل ی است. E L NGC 3923
31 The Complexity of Phase Space and Indirect Detection!
32 Conclusion: Nothing gives a fearful man more courage than another's fear Umberto Eco
An Introduction to Astronomy Presentation III Fall 2018 Physics Department SUT Shant Baghram. Landscape with peacocks by Paul Gauguin (1892)
An Introduction to Astronomy Presentation III Fall 2018 Physics Department SUT Shant Baghram Landscape with peacocks by Paul Gauguin (1892) History of Galactic (& Extragalactic) Astronomy 1610 - Galileo
Dark 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
2. OBSERVATIONAL COSMOLOGY
2. OBSERVATIONAL COSMOLOGY 1. OBSERVATIONAL PARAMETERS i. Introduction History of modern observational Cosmology ii. Cosmological Parameters The search for 2 (or more) numbers Hubble Parameter Deceleration
Dark 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
Modified Dark Matter: Does Dark Matter Know about the Cosmological Constant?
Modified Dark Matter: Does Dark Matter Know about the Cosmological Constant? Douglas Edmonds Emory & Henry College (moving to Penn State, Hazleton) Collaborators Duncan Farrah Chiu Man Ho Djordje Minic
Modified Dark Matter: Does Dark Matter Know about the Cosmological Constant? Douglas Edmonds Emory & Henry College
Modified Dark Matter: Does Dark Matter Know about the Cosmological Constant? Douglas Edmonds Emory & Henry College Collaborators Duncan Farrah Chiu Man Ho Djordje Minic Y. Jack Ng Tatsu Takeuchi Outline
Advanced Topics on Astrophysics: Lectures on dark matter
Advanced Topics on Astrophysics: Lectures on dark matter Jesús Zavala Franco e-mail: jzavalaf@uwaterloo.ca UW, Department of Physics and Astronomy, office: PHY 208C, ext. 38400 Perimeter Institute for
Cosmology. 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
The 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
Hunting for dark matter in the forest (astrophysical constraints on warm dark matter)
Hunting for dark matter in the forest (astrophysical constraints on warm dark matter) ICC, Durham! with the Eagle collaboration: J Schaye (Leiden), R Crain (Liverpool), R Bower, C Frenk, & M Schaller (ICC)
Modified Gravity (MOG) and Dark Matter: Can Dark Matter be Detected in the Present Universe?
Modified Gravity (MOG) and Dark Matter: Can Dark Matter be Detected in the Present Universe? John Moffat Perimeter Institute, Waterloo, Ontario, Canada Talk given at the Miami 2014 topical conference on
The History of the Universe in One Hour. Max Tegmark, MIT
The History of the Universe in One Hour Max Tegmark, MIT QuickTime and a TIFF (Uncompressed) decompressor are needed to see this picture. Other people associated with MIT who worked on COBE: Chuck Bennett,
AST1100 Lecture Notes
AST1100 Lecture Notes 4 Stellar orbits and dark matter 1 Using Kepler s laws for stars orbiting the center of a galaxy We will now use Kepler s laws of gravitation on much larger scales. We will study
Galaxy 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
Dark matter: summary
Dark matter: summary Gravity and detecting Dark Matter Massive objects, even if they emit no light, exert gravitational forces on other massive objects. m 1 r 12 m 2 We study the motions (dynamics) of
Where are the missing baryons?
Interview of BSc dissertation Where are the missing baryons? Brandon Qiang Wang 6 th February 2018 Image from Millennium Simulation Content I. Introduction II. Simulations III. Results IV. Conclusion 2
Shear 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
INTRODUCTION TO DARK MATTER
Universität Heidelberg Carl Zeiss Stiftung INTRODUCTION TO DARK MATTER Susanne Westhoff 2nd Colima Winter School on High Energy hysics! January 8-19, 2018 Colima, Mexico GALAXY VELOCITIES IN CLUSTERS Redshift
Observational Evidence for Dark Matter. Simona Murgia, SLAC-KIPAC
Observational Evidence for Dark Matter Simona Murgia, SLAC-KIPAC XXXIX SLAC Summer Institute 28 July 2011 Outline Evidence for dark matter at very different scales Galaxies Clusters of galaxies Universe???
Dark 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
Solving small scale structure puzzles with. dissipative dark matter
Solving small scale structure puzzles with. dissipative dark matter Robert Foot, COEPP, University of Melbourne Okinawa, March 2016 Dark matter: why we think it exists Dark matter issues on small scales
Cosmology 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
Physical 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
۲۷۹۶ 0 "' ی " #! ۴۳ و م د ; < : ی"98! ی"#"!
*+, " ان ی" ت/ ر ل. د& ر/ ی/ ر 3 ی" ی" ق: یb نi ی: ی: ی: ره 0 ی/? ی 3 ۲۷۹۶ +* - د' #"! 6 آ (۱)4, 3 2 ا. -, & + ک& ) & ( % $ # ی ا 6 آ 4, / ) $ 2 & ) ر د آ ر د $ 2 ر د : 9-8 د > E < D 2 ا C د: B? > = A
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
WOLFGANG KLASSEN DARK MATTER
1 WOLFGANG KLASSEN DARK MATTER "Hubble Maps the Cosmic Web of "Clumpy" Dark Matter in 3-D" (Press release). NASA. 7 January 2007. DARK MATTER 2 CONTENTS 1.Relating Mass and Light Tulley-Fisher relation
Shant Baghram. Séminaires de l'iap. IPM-Tehran 13 September 2013
Structure Formation: à la recherche de paramètre perdu Séminaires de l'iap Shant Baghram IPM-Tehran 13 September 013 Collaborators: Hassan Firoujahi IPM, Shahram Khosravi Kharami University-IPM, Mohammad
Brief 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
Modelling the galaxy population
Modelling the galaxy population Simon White Max Planck Institut für Astrophysik IAU 277 Ouagadougou 1 The standard model reproduces -- the linear initial conditions -- IGM structure during galaxy formation
ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014
ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools
A unified multi-wavelength model of galaxy formation. Carlton Baugh Institute for Computational Cosmology
A unified multi-wavelength model of galaxy formation Carlton Baugh Institute for Computational Cosmology M81 Angel Lopez Sanchez A unified multi-wavelength model of galaxy formation Lacey et al. 2015 arxiv:1509.08473
Galaxy formation in cold dark matter
Galaxy formation in cold dark matter Cheng Zhao Tsinghua Center for Astrophysics Oct 27, 2017 Main references: Press & Schechter, 1974 White & Rees, 1978 Galaxy formation mechanism Cosmological initial
The Galaxy Dark Matter Connection
The Galaxy Dark Matter Connection constraining cosmology & galaxy formation Frank C. van den Bosch (MPIA) Collaborators: Houjun Mo (UMass), Xiaohu Yang (SHAO) Marcello Cacciato, Surhud More (MPIA) Kunming,
Analyzing 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
Physics of the Large Scale Structure. Pengjie Zhang. Department of Astronomy Shanghai Jiao Tong University
1 Physics of the Large Scale Structure Pengjie Zhang Department of Astronomy Shanghai Jiao Tong University The observed galaxy distribution of the nearby universe Observer 0.7 billion lys The observed
Understanding the Properties of Dark Energy in the Universe p.1/37
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 The Cosmic Food Pyramid?? Radiation
Where are the missing baryons?
Where are the missing baryons? Qiang Wang (Brandon) B.Sc. Supervisor: Dr Scott Kay School of Physics and Astronomy, University of Manchester 27/29 June 2018 Image from Millennium Simulation 1 Content I.
The 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)
Tesla 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
Dark 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
Large-scale structure as a probe of dark energy. David Parkinson University of Sussex, UK
Large-scale structure as a probe of dark energy David Parkinson University of Sussex, UK Question Who was the greatest actor to portray James Bond in the 007 movies? a) Sean Connery b) George Lasenby c)
John Moffat Perimeter Institute Waterloo, Ontario, Canada
New Results in Modified Gravity Without Dark Matter John Moffat Perimeter Institute Waterloo, Ontario, Canada The research was supported by the John Templeton Foundation Talk given at the topical conference
Dark Matter: Observational Constraints
Dark Matter: Observational Constraints Does Dark Matter Exist? Leo Blitz UC Berkeley Stanford July 30, 2007 Questions I ll be addressing Does dark matter exist? Where do we know it does not exist? How
Challenges in Cosmology and why (may be) Modified Gravity
Challenges in Cosmology and why (may be) Modified Gravity David F. Mota Institute for Research in Fundamental Sciences IPM-Teheran 2016 Two Pillars in Cosmology Understanding the Universe and its laws
WALLABY. Jeremy Mould WALLABY Science Meeting December 2, 2010
WALLABY Jeremy Mould WALLABY Science Meeting December 2, 2010 Jeremy Mould Seminar: Monash University School of Physics October 7, 2010 Dark Matter Detected in regions where M/L > 100 Outer parts of spiral
Cosmological 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
Lecture 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
Current status of the ΛCDM structure formation model. Simon White Max Planck Institut für Astrophysik
Current status of the ΛCDM structure formation model Simon White Max Planck Institut für Astrophysik The idea that DM might be a neutral, weakly interacting particle took off around 1980, following a measurement
Absolute 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
CMB 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
The Dark Matter Problem
The Dark Matter Problem matter : anything with equation of state w=0 more obvious contribution to matter: baryons (stars, planets, us!) and both Big Bang Nucleosynthesis and WMAP tell us that Ω baryons
MODERN 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
CMB 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:
The first one second of the early universe and physics beyond the Standard Model
The first one second of the early universe and physics beyond the Standard Model Koichi Hamaguchi (University of Tokyo) @ Colloquium at Yonsei University, November 9th, 2016. Credit: X-ray: NASA/CXC/CfA/M.Markevitch
Physics 661. Particle Physics Phenomenology. October 2, Physics 661, lecture 2
Physics 661 Particle Physics Phenomenology October 2, 2003 Evidence for theory: Hot Big Bang Model Present expansion of the Universe Existence of cosmic microwave background radiation Relative abundance
Where are the missing baryons? Craig Hogan SLAC Summer Institute 2007
Where are the missing baryons? Craig Hogan SLAC Summer Institute 2007 Reasons to care Concordance of many measures of baryon number (BBN, CMB,.) Evolution of our personal baryons (galaxies, stars, planets,
Cosmic 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
Cosmology 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
Modern 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
Cracking the Mysteries of the Universe. Dr Janie K. Hoormann University of Queensland
Cracking the Mysteries of the Universe Dr Janie K. Hoormann University of Queensland Timeline of Cosmological Discoveries 16c BCE: flat earth 5-11c CE: Sun at the centre 1837: Bessel et al. measure distance
Background Picture: Millennium Simulation (MPA); Spectrum-Roentgen-Gamma satellite (P. Predehl 2011)
By Collaborators Alex Kolodzig (MPA) Marat Gilfanov (MPA,IKI), Gert Hütsi (MPA), Rashid Sunyaev (MPA,IKI) Publications Kolodzig et al. 2013b, A&A, 558, 90 (ArXiv : 1305.0819) Hüsti et al. 2014, submitted
n=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
DARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
Detection of hot gas in multi-wavelength datasets. Loïc Verdier DDAYS 2015
Detection of hot gas in multi-wavelength datasets Loïc Verdier SPP DDAYS 2015 Loïc Verdier (SPP) Detection of hot gas in multi-wavelength datasets DDAYS 2015 1 / 21 Cluster Abell 520; Credit: X-ray: NASA/CXC/UVic./A.Mahdavi
tsz cluster counts and power spectrum combined with CMB
53rd Constraints on cosmological parameters from galaxy clusters: tsz cluster counts and power spectrum combined with CMB Laura Salvati in collaboration with Nabila Aghanim and Marian Douspis ByoPiC The
Possible sources of very energetic neutrinos. Active Galactic Nuclei
Possible sources of very energetic neutrinos Active Galactic Nuclei 1 What might we learn from astrophysical neutrinos? Neutrinos not attenuated/absorbed Information about central engines of astrophysical
The Dark Matter Puzzle: On the Home Stretch
The Dark Matter Puzzle: On the Home Stretch 10 August 2007 Michael S. Turner Kavli Institute for Cosmological Physics The University of Chicago Quarks & Cosmos Dark Matter is the Central Front of Quarks
TeV Colliders and Cosmology. 1: The Density of Dark Matter
TeV Colliders and Cosmology 1: The Density of Dark Matter M. E. Peskin SSI - July 2006 There are many points of connection between particle physics and cosmology: The elementary particles present at high
Isotropy and Homogeneity
Cosmic inventory Isotropy and Homogeneity On large scales the Universe is isotropic (looks the same in all directions) and homogeneity (the same average density at all locations. This is determined from
Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher accuracy
12-14 April 2006, Rome, Italy Francesco Melchiorri Memorial Conference Planck was conceived to confirm the robustness of the ΛCDM concordance model when the relevant quantities are measured with much higher
Figure 1: The universe in a pie chart [1]
![Figure 1: The universe in a pie chart [1]](/thumbs/76/73578502.jpg "Figure 1: The universe in a pie chart [1]")
Dark matter Marlene Götz (Jena) Dark matter is a hypothetical form of matter. It has to be postulated to describe phenomenons, which could not be explained by known forms of matter. It has to be assumed
Power 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
Can 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
Observational 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.
DARK MATTER IN UNIVERSE. edited by. John Bahcall Institute for Advanced Study, Princeton, USA. Tsvi Piran The Hebrew University, Israel
DARK MATTER IN UNIVERSE n d edited by John Bahcall Institute for Advanced Study, Princeton, USA Tsvi Piran The Hebrew University, Israel Steven Weinberg University of Texas, Austin, USA TECHNiSCHE INFORMATIONSBIBLIOTHEK
The State of Tension Between the CMB and LSS
The State of Tension Between the CMB and LSS Tom Charnock 1 in collaboration with Adam Moss 1 and Richard Battye 2 Phys.Rev. D91 (2015) 10, 103508 1 Particle Theory Group University of Nottingham 2 Jodrell
Dark Baryons and their Hidden Places. Physics 554: Nuclear Astrophysics Towfiq Ahmed December 7, 2007
Dark Baryons and their Hidden Places Physics 554: Nuclear Astrophysics Towfiq Ahmed December 7, 2007 Contents History Inconsistent Matter Inventory Dark Baryon vs. Dark Matter Possible Hidden Places Search
The imprint of the initial conditions on large-scale structure
Stars, Planets and Galaxies 2018 Harnack House, Berlin The imprint of the initial conditions on large-scale structure Simon White Max Planck Institute for Astrophysics The Planck map of TCMB the initial
Disk Galaxy Rotation Curves and Dark Matter Halos
Disk Galaxy Rotation Curves and Dark Matter Halos Thorben H. Mense 1 Galactic Astronomy SS 2018 1 Universität Bielefeld Outline Early Observations of Galaxy Rotation Curves Rotation of the Andromeda Nebula
The Current Status of Too Big To Fail problem! based on Warm Dark Matter cosmology
The Current Status of Too Big To Fail problem! based on Warm Dark Matter cosmology 172th Astronomical Seminar Dec.3 2013 Chiba Lab.M2 Yusuke Komuro Key Word s Too Big To Fail TBTF Cold Dark Matter CDM
Primordial Black Holes in Cosmology. Lectures 1 & 2 : What are PBHs? Do they exist? Massimo Ricotti (University of Maryland, USA)
Primordial Black Holes in Cosmology Lectures 1 & 2 : What are PBHs? Do they exist? Massimo Ricotti (University of Maryland, USA) Institute of Cosmos Sciences, University of Barcelona 23/10/2017 What are
Cosmological neutrinos
Cosmological neutrinos Yvonne Y. Y. Wong CERN & RWTH Aachen APCTP Focus Program, June 15-25, 2009 2. Neutrinos and structure formation: the linear regime Relic neutrino background: Temperature: 4 T,0 =
The Growth of Structure Read [CO 30.2] The Simplest Picture of Galaxy Formation and Why It Fails (chapter title from Longair, Galaxy Formation )
![The Growth of Structure Read [CO 30.2] The Simplest Picture of Galaxy Formation and Why It Fails (chapter title from Longair, Galaxy Formation )](/thumbs/82/85251520.jpg "The Growth of Structure Read [CO 30.2] The Simplest Picture of Galaxy Formation and Why It Fails (chapter title from Longair, Galaxy Formation )")
WMAP Density fluctuations at t = 79,000 yr he Growth of Structure Read [CO 0.2] 1.0000 1.0001 0.0001 10 4 Early U. contained condensations of many different sizes. Current large-scale structure t = t 0
Weighing the universe : baryons, dark matter, and dark energy
Weighing the universe : baryons, dark matter, and dark energy Department of Physics The University of Tokyo Yasushi Suto The 21 st century COE program of Tohoku University International symposium Exploring
What Is Dark Matter? By NASA 2012
Name: Class: What Is Dark Matter? By NASA 2012 In this informational text, the author describes what scientists know about dark matter today and the mysteries that continue to surround it. As you read,
KINETIC SUNYAEV-ZELDOVICH EFFECT FROM HALO ROTATION Asantha Cooray 1,2 and Xuelei Chen 3
The Astrophysical Journal, 573:43 50, 2002 July 1 # 2002. The American Astronomical Society. All rights reserved. Printed in U.S.A. KINETIC SUNYAEV-ZELDOVICH EFFECT FROM HALO ROTATION Asantha Cooray 1,2
Weak 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
Feb-2015 Hervé Dole, IAS - M2NPAC Advanced Cosmology - Dole/Joyce/Langer 1. problem?
Hervé Dole introduction to the structured universe why is the night sky dark? 1. why galaxy formation is a problem? 2. how to adress these problems? 3. overview of observation facts 4. overview of structure
1.1 Large-scale properties of the Universe
1 Our understanding of both the large-scale properties of our Universe and the processes through which galaxies form and evolve has greatly improved over the last few decades, thanks in part to new observational
Insights into galaxy formation from dwarf galaxies
Potsdam, August 2014 Insights into galaxy formation from dwarf galaxies Simon White Max Planck Institute for Astrophysics Planck CMB map: the IC's for structure formation Planck CMB map: the IC's for structure
CMB 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
Dwarf Galaxies as Cosmological Probes
Dwarf Galaxies as Cosmological Probes Julio F. Navarro The Ursa Minor dwarf spheroidal First Light First Light The Planck Satellite The Cosmological Paradigm The Clustering of Dark Matter The Millennium
Dark 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
Galaxy 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
Announcements. Homework. Set 8now open. due late at night Friday, Dec 10 (3AM Saturday Nov. 11) Set 7 answers on course web site.
Homework. Set 8now. due late at night Friday, Dec 10 (3AM Saturday Nov. 11) Set 7 answers on course web site. Review for Final. In class on Thursday. Course Evaluation. https://rateyourclass.msu.edu /
Quasar 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
A look into the Dark Universe
Zentrum für Astronomie, Institut für Theoretische Astrophysik Universität Heidelberg Dark Energy dark energy: assumed to drive accelerated cosmic expansion scalar field having negative pressure? early
Review of Lecture 15 3/17/10. Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath
Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath A2020 Disk Component: stars of all ages, many gas clouds Review of Lecture 15 Spheroidal Component: bulge & halo, old
Neutrino Mass & the Lyman-α Forest. Kevork Abazajian University of Maryland
Neutrino Mass & the Lyman-α Forest Kevork Abazajian University of Maryland INT Workshop: The Future of Neutrino Mass Measurements February 9, 2010 Dynamics: the cosmological density perturbation spectrum
Made of? What is the Universe. What is the Universe made of? Made of? We are stardust!!! Element Abundances
Made of? Dr Risa H Wechsler Hubble Fellow" Enrico Fermi Fellow University of Chicago Lecture Plan Lecture Two" April #& The Story of Galaxy Formation in Our Universe: Kavli Inst for Cosmological Physics"