DARK MATTER AND DARK ENERGY AT HIGH REDSHIFT. MATTEO VIEL INAF & INFN Trieste
|
|
- Christal Newman
- 5 years ago
- Views:
Transcription
1 DARK MATTER AND DARK ENERGY AT HIGH REDSHIFT MATTEO VIEL INAF & INFN Trieste SISSA IDEALS WORKSHOP th November 2011
2 RATIONALE HIGHLIGHT THE IMPORTANCE OF HIGH REDSHIFT (z>1) OBSERVABLES IN ORDER TO CONSTRAIN: 1) NEUTRINOS 2) COLDNESS OF COLD DARK MATTER 3) EARLY DARK ENERGY 4) BAOs STATUS THE MEASUREMENT OF MATTER POWER AT HIGH-z (COMBINED with the CMB) IS CURRENTLY PROVIDING THE TIGHTEST CONSTRAINTS on 1), 2) and 3) AND WILL PROVIDE THE TIGHTEST CONSTRAINTS on 4).
3 NEUTRINOS High-z BAO WDM z=1100
4 NEUTRINOS
5 N-body + Hydro neutrino simulations I: slices TreeSPH code Gadget-III follows DM, neutrinos, gas and star particles in a cosmological volume Viel, Haehnelt & Springel 2010, JCAP, 06,15
6 EVOLUTION of LSS I : dynamics in the linear regime CMB GALAXIES IGM (WL) Effects in terms of matter clustering, Hubble constant, Energy density (see Lesgourgues & Pastor 2006) Different evolution in terms of dynamics and geometry as compared to massless neutrino universes
7 N-body simulations II: effects in terms of non-linear power Brandbyge et al 08 --
8 Hydro simulations III: redshift/scale dependence of non-linear power Full hydro simulations: gas physics does impact at the <10 % level at scales k < 10 h/mpc Viel, Haehnelt & Springel 2010, JCAP, 06,15
9 Hydro simulations IV: redshift space distortions Marulli, Carbone, MV, Moscardini e Cimatti 2011
10 Hydro simulations V: the distribution of high-z voids Navarro-Villaescusa, Vogelsberger, MV, Loeb 2011
11 N-body simulations VI: very non-linear regime LINEAR SIMULATIONS HALOFIT Bird, MV, Haehnelt 2011
12 Neutrino constraints from SDSS flux power 3 normal 1,2 2 inverted 3 1 2σ limit Seljak, Slosar, McDonald, 2006, JCAP, 0610, 014 DISFAVOURED BY LYMAN-α
13 Non-linear neutrinos VII: EUCLID forecasts Lesgourgues, Bird, MV, Haehnelt 2012
14 DARK MATTER S COLDNESS
15 Warm Dark Matter and structure formation - I k FS ~ 5 Tv/Tx (m x/1kev) Mpc-1 ΛCDM 1 kev MV, Markovic, Baldi & Weller 2011 z=0 z=2 z=5 See Bode, Ostriker, Turok 2001 Abazajian, Fuller, Patel 2001 Avila-Reese et al Boyarsky et al Colin et al Wang & White 2007 Gao & Theuns 2007 Abazajian et al Lovell et al. 2011
16 Warm Dark Matter and non-linear power - II MV, Markovic, Baldi & Weller 2011 Range of wavenumbers important for weak lensing tomography, IGM and small scale clustering of galaxies!
17 Lyman-α and Warm Dark Matter - III MV et al., Phys.Rev.Lett. 100 (2008) SDSS + HIRES data (SDSS still very constraining!) Tightest constraints on mass of WDM particles to date: m WDM > 4 kev (early decoupled thermal relics) m sterile > 28 kev (standard DodelsonWidrow mechanism) SDSS range Completely new small scale regime
18 WDM and non-linear power - IV: weak lensing with EUCLID MV, Markovic, Baldi & Weller 2011
19 Lyman-α and Cold+Warm Dark Matter Boyarsky et al. 09 SDSS+WMAP5 SDSS + VHS
20 HIGH-Z DARK ENERGY
21 Early Dark Energy from the CMB Calabrese et al Reichardt et al. 2011
22 Early Dark Energy in the Dark Ages Xia & Viel 2009
23 Coupled dark energy and the IGM Baldi & MV 10
24 BAOs
25 SDSS from low to high redshift Slosar et al (BOSS collaboration)
26 Future perspectives: BAOs about 20 QSOs per square degree with BOSS McDonald & Eisenstein 2007 BOSS-like simulated flux power
27 Future perspectives-ii: BAOs McDonald & Eisenstein 2007
28 BAOs in the Lyman-α forest: probing the transverse direction Transverse direction: MV et al 2002; White 2003; McDonald & Eisenstein 2007; Slosar et al. 2009, 2010
29 3D Correlations in BOSS 1yr data! Slosar et al Estimates of b and β performed
30 SUMMARY Bridging the gap between z=1100 and z=0 via LSS probes: Lyman-α Weak Lensing Clustering of galaxies is important and is providing and will provide tight constraints on the small scale properties of the matter distribution and the cosmological model Mν < 0.17 ev (0.3 ev) MWDM > 4 kev (2 kev) Ω EDE < 0.02 in the structure formation era Close to BAO detection at z=3 via Lyman-α
31
32
33
34
35 Outline - What data we got The data sets - How we used them Theoretical framework - What we achieved Results
36 The data sets SDSS vs LUQAS McDonald et al Kim, MV et al SDSS 3035 LOW RESOLUTION LOW S/N LUQAS vs 30 HIGH RESOLUTION HIGH S/N
37 The interpretation: full grid of sims - I SDSS power analysed by forward modelling motivated by the huge amount of data with small statistical errors CMB: Spergel et al. (05) Galaxy P(k): Sanchez & Cole (07) + Flux Power: McDonald (05) data points z=4.2 z=2.2 Cosmological parameters + e.g. bias IGM physics + Parameters describing
38 The interpretation: full grid of sims - II McDonald et al. 05 Tens of thousands of models Monte Carlo Markov Chains - Cosmology - Cosmology - Mean flux - T=T0 (1+δ )γ -1 - Reionization - Metals - Noise - Resolution - Damped Systems - Physics - UV background - Small scales
39 The interpretation: flux derivatives - III Independent analysis of SDSS power The flux power spectrum is a smooth function of k and z Both methods have drawbacks and advantages: 1- McDonald et al. 05 better sample the parameter space 2- Viel & Haehnelt 06 rely on hydro simulations, but probably error bars are underestimated Flux power P F (k, z; p) = P F (k, z; p0) + Σ i=1,n Best fit P F (k, z; pi) pi p = p0 (pi - pi0) p: astrophysical and cosmological parameters but even resolution and/or box size effects if you want to save CPU time
40 RESULTS
41 Summary (highlights) of results 1. Competitive constraints in terms of cosmological parameters (in particular shape and curvature of the power spectrum) Lesgourgues, MV, Haehnelt, Massey (2007) JCAP Tightest constraints to date on neutrino masses and running of the spectral index Seljak, Slosar, McDonald JCAP (2006) Tightest constraints to date on the coldness of cold dark matter MV et al., Phys.Rev.Lett. 100 (2008)
42 Results Lyman-α only with full grid: amplitude and slope McDonald et al. 05 Croft et al. 98,02 40% uncertainty Croft et al % uncertainty Viel et al % uncertainty McDonald et al % uncertainty AMPLITUDE χ2 likelihood code distributed with COSMOMC SLOPE Redshift z=3 and k=0.009 s/km corresponding to 7 comoving Mpc/h
43 Results Lyman-α only with flux derivatives: correlations Fitting SDSS data with GADGET-2 this is SDSS Ly-α only!! FLUX DERIVATIVES SDSS data only σ8 = 0.91 ± 0.07 n = 0.97 ± 0.04
44 Lyman-α forest + Weak Lensing + WMAP 3yrs AMPLITUDE VHS-LUQAS: high res Ly-a from (Viel, Haehnelt, Springel 2004) SDSS-d: re-analysis of low res data SDSS (Viel & Haehnelt 2006) WL: COSMOS-3D survey Weak Lensing (Massey et al. 2007) 1.64 sq degree public available weak lensing COSMOMC module VHS+WMAP1 MATTER DENSITY Lesgourgues, MV, Haehnelt, Massey, 2007, JCAP, 8, 11 SPECTRAL INDEX
45 Active neutrinos - I Lesgourgues & Pastor Phys.Rept. 2006, 429, 307 Σ m ν = ev Lyman-α forest Σ m ν = 1.38 ev
46 Active neutrinos - II Seljak, Slosar, McDonald, 2006, JCAP, 0610, ,2 normal 2 inverted 3 1 2σ limit DISFAVOURED BY LYMAN-α Tight constraints because data are marginally compatible mν (ev) < 0.17 (95 %C.L.), < Σ 0.19 ev (Fogli et al. 08) r < 0.22 (95 % C.L.) running = ± Neff = 5.2 (3.2 without Ly α) CMB + SN + SDSS gal+ SDSS Ly-α Goobar et al. 06 get upper limits 2-3 times larger for forecasting see Gratton, Lewis, Efstathiou 2007
47 Lyman-α and Warm Dark Matter - II ΛCDM 10 ev [P (k) WDM/P (k) CDM ]1/2 Light gravitino contributing to a fraction of dark matter 100 ev 1/3 Tx Tν = g (T D) WDM 1/3 m gravitino < 16 ev (2 σ C.L.) (or any particle with g(td)~90-100) From high res. Lyman-a data GRAVITINO If the gravitino is the LSP then the susy breaking scale is limited from above Λ susy < 260 TeV MV, Lesgourgues, Haehnelt, Matarrese, Riotto, PRD, 2005, 71,
48 PRIMORDIAL Non Gaussianities in the IGM
49 N-body simulation in NG scenario: the mass distribution Mathis et al. 04 Kang et al. 07 Grossi et al. 07,09 Hikage et al. 08 Desjacques et al. 08
50 First hydrodynamical simulation in NG scenario f nl = f nl = Viel, Branchini, Dolag, Grossi, Matarrese, Moscardini 2009, MNRAS, 393, 774
51 SYSTEMATICS
52 Fitting the flux probability distribution function Bolton, MV, Kim, Haehnelt, Carswell (08), MV et al. 2009, Puchwein et al T=T0(1+δ ) γ -1 Inverted equation of state γ <1 means voids are hotter than mean density regions Flux probability distribution function
53 Systematics: Thermal state T = T0 ( 1 + δ ) γ -1 Thermal histories Flux power fractional differences Statistical SDSS errors on flux power
54 Systematics: UV fluctuations and Metals UV fluctuations from Lyman Break Galaxies Ratio of Flux power McDonald, Seljak, Cen, Ostriker 2004 Croft 2006 Lidz et al Metal contribution Ratio of Flux power Kim, MV, Haehnelt, Carswell, Cristiani (2004)
55 GALAXY-IGM
56 Future perspectives BOSS (or SUPERBOSS) SDSS III 150,000 (1,000,000) QSO spectra tailored for BAO and P(k) studies X-Shooter (taking data now) spectrograph Medium resolution between SDSS and high res at least 100 QSO spectra needed to improve constraints Independent analysis of thermal state using different statistics and constraints both on astrophysics and cosmological at both HIGH and low redshift E-ELT era: measuring the cosmic expansion
57 BAOs
58 Slosar et al (BOSS collaboration)
59 Future perspectives : BAO Importance of transverse direction: MV et al 2002; White 2003; McDonald & Eisenstein 2007; Slosar et al about 20 QSOs per square degree with BOSS McDonald & Eisenstein 2007 BOSS-like simulated flux power
60 BAOs in the Lyman-a forest: probing the transverse direction Importance of transverse direction: MV et al 2002; White 2003; McDonald & Eisenstein 2007; Slosar et al about 20 QSOs per square degree with BOSS
61 3D Correlations in BOSS 1yr data! Slosar et al Estimates of b and β performed
62 COSMIC EXPANSION
63 Measuring the cosmic expansion? This is a fundamental quantity not related at all to the FRW equations.
64 COsmicDynamicEXperiment CODEX-I Ultra-stable spectrograph Dz/Dt (10-10 yr-1) REDSHIFT
65 COsmicDynamicEXperiment Liske et al. 2008, MNRAS, 386, 1192 CODEX - II
66 BRIEF HISTORICAL OVERVIEW of the Lyman-α forest ISOLATED CLOUDS NETWORK OF FILAMENTS PROBES OF THE JEANS SCALE COSMOLOGICAL PROBES
67 Modelling the IGM Dark matter evolution: linear theory of density perturbation + Jeans length LJ ~ sqrt(t/ρ) + mildly non linear evolution Hydrodynamical processes: mainly gas cooling cooling by adiabatic expansion of the universe heating of gaseous structures (reionization) - photoionization by a uniform Ultraviolet Background - Hydrostatic equilibrium of gas clouds dynamical time = 1/sqrt(G ρ) ~ sound crossing time= size /gas sound speed Size of the cloud: > 100 kpc Temperature: ~ 104 K Mass in the cloud: ~ 109 M sun Neutral hydrogen fraction: 10-5 In practice, since the process is mildly non linear you need numerical simulations To get convergence of the simulated flux at the percent level (observed)
68 Modelling the IGM II M (> ρ) V (> ρ) Bi & Davidsen 1997, ApJ, 479, 523
69 N-body simulations II: neutrino velocities matter Draw velocity from Fermi-Dirac distribution Brandbyge et al 08
70 N-body simulations VII: halo density profile CDM q/t=3 q/t total q/t=4 q/t=1 q/t=5 q/t=2 q/t=6 Brandbyge, Hannestad Haugbolle, Wong 2010
71 N-body simulations IV: mesh method Computing the neutrino gravitational potential on the PM grid and summing up its contribution to the total matter gravitational potential this is much faster! COMPARISON GRID VS PARTICLES M ν =0.6 ev M ν = 1.2 ev Brandbyge et al 08b
72 N-body simulations V: a hybrid approach After neutrino decoupling CBE Expansion of ψ in Legendre series Brandbyge & Hannestad 09
73 N-body simulations VI: comparison PARTICLES: accurate non-linear sampling but prone to shot-noise errors GRID: fast and accurate but no phase mixing (i.e. non-linear regime suppression maybe it is less than it should be) HYBRID: ideal for non-linear objects but memory demanding and prone to convergence issues
74 NEUTRINOS in the IGM IV: impact on neutrino power spectrum Increasing neutrino mass
75 INTRO
76
77 DATA: high resolution spectrum
78 SIMULATING NEUTRINOS at high-redshift II: methods Methods differ Matter z = 3 1) Significant non linear evolution at the smallest scales 2) Percent level discrepancies between particle and grid methods 3) Poissonian contribution affects small scales
79 Hydro simulations VI: matter and halo clustering Marulli, Carbone, MV, Moscardini e Cimatti 2011
80 THEORY: GAS in a LCDM universe 80 % of the baryons at z=3 are in the Lyman-α forest Bi & Davidsen (1997), Rauch (1998) baryons as tracer of the dark matter density field δ IGM ~ δ DM at scales larger than the Jeans length ~ 1 com Mpc
81 Little room for standard warm dark matter scenarios the cosmic web is likely to be quite cold COLD (a bit) WARM sterile 10 kev
82 Hydro simulations IV: halo mass functions Marulli, Carbone, MV, Moscardini e Cimatti 2011
COSMOLOGICAL SPECTROSCOPY OF THE HIGH REDSHIFT UNIVERSE: STATUS & PERSPECTIVES
COSMOLOGICAL SPECTROSCOPY OF THE HIGH REDSHIFT UNIVERSE: STATUS & PERSPECTIVES 60 comoving Mpc/h MATTEO VIEL INAF & INFN Trieste HEIDELBERG JOINT ASTRONOMICAL COLLOQUIUM 14 t/h DECEMBER 2010 OUTLINE 1-
More informationCOSMOLOGICAL SIGNIFICANCE of the IGM
COSMOLOGICAL SIGNIFICANCE of the IGM MATTEO VIEL INAF and INFN Trieste (Italy) Bologna University Oct. 2011 Lecture 2 OUTLINE: LECTURES 1. Physics of Lyman- alpha and its cosmological relevance 2. Lyman-
More informationNEUTRINOS AND LARGE SCALE STRUCTURES
NEUTRINOS AND LARGE SCALE STRUCTURES MATTEO VIEL INAF & INFN Trieste PADOVA 18 th May 2011 Scuola Neutrini in Cosmologia OUTLINE Quan'fying the impact of neutrinos on cosmological observables Simula'ng
More informationNeutrino 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
More informationProbing dark matter and the physical state of the IGM with the Lyα forest
Probing dark matter and the physical state of the IGM with the Lyα forest Martin Haehnelt in collaboration with: George Becker, James Bolton, Jonathan Chardin, Laura Keating, Ewald Puchwein, Debora Sijacki,
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 informationMeasuring Neutrino Masses and Dark Energy
Huitzu Tu UC Irvine June 7, 2007 Dark Side of the Universe, Minnesota, June 5-10 2007 In collaboration with: Steen Hannestad, Yvonne Wong, Julien Lesgourgues, Laurence Perotto, Ariel Goobar, Edvard Mörtsell
More informationNeutrinos in Large-scale structure
Neutrinos in Large-scale structure Marilena LoVerde University of Chicago ( Fall 2015 > Yang Institute for Theoretical Physics, Stony Brook University) Neutrinos in Large-scale structure Marilena LoVerde
More informationWarm dark matter with future cosmic shear data
Workshop CIAS Meudon, Tuesday, June 7, 2011 Warm dark matter with future cosmic shear data Katarina Markovic (University Observatory Munich) markovic@usm.lmu.de in collaboration with Jochen Weller and
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 informationCurrent 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
More informationNeutrinos and cosmology
Neutrinos and cosmology Yvonne Y. Y. Wong RWTH Aachen LAUNCH, Heidelberg, November 9--12, 2009 Relic neutrino background: Temperature: 4 T,0 = 11 Origin of density perturbations? 1 /3 T CMB, 0=1.95 K Number
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 informationConstraining the IGM thermal state and Cosmology
Constraining the IGM thermal state and Cosmology Antonella Garzilli IEU, Ewha Womans University 29th November, 2013 with: Prof. Tom Theuns Dr. James Bolton Dr. Tae-Sun Kim Dr. Samuel Leach Dr. Matteo Viel
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 informationBAO and Lyman-α with BOSS
BAO and Lyman-α with BOSS Nathalie Palanque-Delabrouille (CEA-Saclay) BAO and Ly-α The SDSS-III/BOSS experiment Current results with BOSS - 3D BAO analysis with QSOs - 1D Ly-α power spectra and ν mass
More informationeboss Lyman-α Forest Cosmology
Moriond Cosmology Conference, La Thuile, 18th March 2018 eboss Lyman-α Forest Cosmology Matthew Pieri and BOSS & eboss Lyα Working Groups Quasar Spectra and Lyman α Forest Quasar Intergalactic medium Line-of-sight
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 informationThe 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
More informationThe Large-scale Structure of Warm Dark Matter
The Large-scale Structure of Warm Dark Matter University Observatory, Ludwig Maximillian University Munich E-mail: markovic@usm.lmu.de Warm Dark Matter (WDM) is a generalisation of the standard Cold Dark
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 informationarxiv: v1 [astro-ph.co] 11 Dec 2017
Cosmology with 21cm intensity mapping arxiv:1712.04022v1 [astro-ph.co] 11 Dec 2017 I P Carucci 1,2,3 1 SISSA - International School for Advanced Studies, Via Bonomea 265, 34136 Trieste, Italy 2 INFN sez.
More informationCosmology from Topology of Large Scale Structure of the Universe
RESCEU 2008 Cosmology from Topology of Large Scale Structure of the Universe RESCEU Symposium on Astroparticle Physics and Cosmology 11-14, November 2008 Changbom Park (Korea Institute for Advanced Study)
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 informationProbing the Nature of Dark Matter with the First Galaxies (Reionization, 21-cm signal)
Probing the Nature of Dark Matter with the First Galaxies (Reionization, 21-cm signal) Anastasia Fialkov Ecole Normale Superieure Debates on the Nature of Dark Matter 20 May 2014 Outline The early Universe
More informationMassive neutrinos and cosmology
Massive neutrinos and cosmology Yvonne Y. Y. Wong RWTH Aachen Theory colloquium, Padova, November 18, 2009 Relic neutrino background: Temperature: 4 T,0 = 11 Origin of density perturbations? 1 /3 T CMB,
More informationNeutrinos in the era of precision Cosmology
Neutrinos in the era of precision Cosmology Marta Spinelli Rencontres du Vietnam Quy Nhon - 21 July 2017 The vanilla model: -CDM (Late times) cosmological probes Supernovae Ia standard candles fundamental
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 informationDetecting Dark Matter in the X-ray
Detecting Dark Matter in the X-ray Kev Abazajian University of Maryland Quantum 2 Cosmos 3: Airlie Center, July 8, 2008 The CDM Ansatz Problems in Cold Dark Matter? Halo Substructure: satellite galaxies
More informationPlanck meets the Lyman-α forest
Planck meets the Lyman-α forest Jose Oñorbe Max Planck Institute for Astronomy (onorbe@mpia.de) Collaborators: J. Hennawi (MPIA), Z. Lukić (LBNL), A. Rorai (IoA), G. Kulkarni (IoA) June 15, 2016 Meeting
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 informationSome like it warm. Andrea V. Macciò
Some like it warm Andrea V. Macciò MPIA - Heidelberg D. Aderhalden, A. Schneider, B. Moore (Zurich), F. Fontanot (HITS), A. Dutton, J. Herpich, G. Stinson (MPIA), X. Kang (PMO) CDM problems, hence WDM
More informationDetermining neutrino masses from cosmology
Determining neutrino masses from cosmology Yvonne Y. Y. Wong The University of New South Wales Sydney, Australia NuFact 2013, Beijing, August 19 24, 2013 The cosmic neutrino background... Embedding the
More informationNeutrinos in Cosmology (IV)
Neutrinos in Cosmology (IV) Sergio Pastor (IFIC Valencia) Cinvestav 8-12 June 2015 Outline Prologue: the physics of (massive) neutrinos IntroducBon: neutrinos and the history of the Universe Basics of
More informationResults from the Baryon Oscillation Spectroscopic Survey (BOSS)
Results from the Baryon Oscillation Spectroscopic Survey (BOSS) Beth Reid for SDSS-III/BOSS collaboration Hubble Fellow Lawrence Berkeley National Lab Outline No Ly-α forest here, but very exciting!! (Slosar
More informationGrowth of structure in an expanding universe The Jeans length Dark matter Large scale structure simulations. Large scale structure
Modern cosmology : The Growth of Structure Growth of structure in an expanding universe The Jeans length Dark matter Large scale structure simulations effect of cosmological parameters Large scale structure
More informationPossible 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
More informationLarge-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)
More informationBaryon Acoustic Oscillations (BAO) in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample
Baryon Acoustic Oscillations (BAO) in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample BOMEE LEE 1. Brief Introduction about BAO In our previous class we learned what is the Baryon Acoustic Oscillations(BAO).
More informationHow to cheat with maps. perfectly sensible, honest version
How to cheat with maps watch out for weasel maps : logarithmic (favors solar system) conformal (blows up BB singularity into something significant, popular with CMB types) comoving (makes the local universe
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 informationLarge Scale Structure with the Lyman-α Forest
Large Scale Structure with the Lyman-α Forest Your Name and Collaborators Lecture 1 - The Lyman-α Forest Andreu Font-Ribera - University College London Graphic: Anze Slozar 1 Large scale structure The
More informationSEARCHING FOR LOCAL CUBIC- ORDER NON-GAUSSIANITY WITH GALAXY CLUSTERING
SEARCHING FOR LOCAL CUBIC- ORDER NON-GAUSSIANITY WITH GALAXY CLUSTERING Vincent Desjacques ITP Zurich with: Nico Hamaus (Zurich), Uros Seljak (Berkeley/Zurich) Horiba 2010 cosmology conference, Tokyo,
More informationThe galaxy population in cold and warm dark matter cosmologies
The galaxy population in cold and warm dark matter cosmologies Lan Wang National Astronomical Observatories, CAS Collaborators: Violeta Gonzalez-Perez, Lizhi Xie, Andrew Cooper, Carlos Frenk, Liang Gao,
More informationFrom quasars to dark energy Adventures with the clustering of luminous red galaxies
From quasars to dark energy Adventures with the clustering of luminous red galaxies Nikhil Padmanabhan 1 1 Lawrence Berkeley Labs 04-15-2008 / OSU CCAPP seminar N. Padmanabhan (LBL) Cosmology with LRGs
More informationThe Power. of the Galaxy Power Spectrum. Eric Linder 13 February 2012 WFIRST Meeting, Pasadena
The Power of the Galaxy Power Spectrum Eric Linder 13 February 2012 WFIRST Meeting, Pasadena UC Berkeley & Berkeley Lab Institute for the Early Universe, Korea 11 Baryon Acoustic Oscillations In the beginning...
More informationDistinguishing Between Warm and Cold Dark Matter
Distinguishing Between Warm and Cold Dark Matter Center for Cosmology Aspen Workshop Neutrinos in Physics & Astrophysics 2/2/2007 Collaborators: James Bullock, Manoj Kaplinghat astro-ph/0701581.. Motivations
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 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 informationPhysics 463, Spring 07. Formation and Evolution of Structure: Growth of Inhomogenieties & the Linear Power Spectrum
Physics 463, Spring 07 Lecture 3 Formation and Evolution of Structure: Growth of Inhomogenieties & the Linear Power Spectrum last time: how fluctuations are generated and how the smooth Universe grows
More informationTheory of galaxy formation
Theory of galaxy formation Bibliography: Galaxy Formation and Evolution (Mo, van den Bosch, White 2011) Lectures given by Frank van den Bosch in Yale http://www.astro.yale.edu/vdbosch/teaching.html Theory
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 informationDark Radiation from Particle Decay
Dark Radiation from Particle Decay Jörn Kersten University of Hamburg Based on Jasper Hasenkamp, JK, JCAP 08 (2013), 024 [arxiv:1212.4160] Jörn Kersten (Uni Hamburg) Dark Radiation from Particle Decay
More informationEfficient calculation of cosmological neutrino clustering
Efficient calculation of cosmological neutrino clustering MARIA ARCHIDIACONO RWTH AACHEN UNIVERSITY ARXIV:50.02907 MA, STEEN HANNESTAD COSMOLOGY SEMINAR HELSINKI INSTITUTE OF PHYSICS 06.04.206 Cosmic history
More informationStefano Gariazzo. Light sterile neutrinos with pseudoscalar interactions in cosmology. Based on [JCAP 08 (2016) 067] University and INFN, Torino
Stefano Gariazzo University and INFN, Torino gariazzo@to.infn.it http://personalpages.to.infn.it/~gariazzo/ Light sterile neutrinos with pseudoscalar interactions in cosmology Based on [JCAP 08 (2016)
More informationBAO & RSD. Nikhil Padmanabhan Essential Cosmology for the Next Generation VII December 2017
BAO & RSD Nikhil Padmanabhan Essential Cosmology for the Next Generation VII December 2017 Overview Introduction Standard rulers, a spherical collapse picture of BAO, the Kaiser formula, measuring distance
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 informationCosmology with high (z>1) redshift galaxy surveys
Cosmology with high (z>1) redshift galaxy surveys Donghui Jeong Texas Cosmology Center and Astronomy Department University of Texas at Austin Ph. D. thesis defense talk, 17 May 2010 Cosmology with HETDEX
More informationLSS: Achievements & Goals. John Peacock Munich 20 July 2015
LSS: Achievements & Goals John Peacock LSS @ Munich 20 July 2015 Outline (pre-)history and empirical foundations The ΛCDM toolkit Open issues and outlook Fundamentalist Astrophysical A century of galaxy
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 informationBaryon Acoustic Oscillations Part I
Baryon Acoustic Oscillations Part I Yun Wang (on behalf of the Euclid collaboration) ESTEC, November 17, 2009 Outline Introduction: BAO and galaxy clustering BAO as a standard ruler BAO as a robust dark
More informationThe simulated 21 cm signal during the EoR : Ly-α and X-ray fluctuations
The simulated 21 cm signal during the EoR : Ly-α and X-ray fluctuations Sunghye BAEK Collaborators : B. Semelin, P. Di Matteo, F. Combes, Y. Revaz LERMA - Observatoire de Paris 9 Dec 2008 Physics of the
More informationIntroduction to CosmoMC
Introduction to CosmoMC Part I: Motivation & Basic concepts Institut de Ciències del Cosmos - Universitat de Barcelona Dept. de Física Teórica y del Cosmos, Universidad de Granada, 1-3 Marzo 2016 What
More informationPhysics 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
More informationLarge Scale Structure After these lectures, you should be able to: Describe the matter power spectrum Explain how and why the peak position depends on
Observational cosmology: Large scale structure Filipe B. Abdalla Kathleen Lonsdale Building G.22 http://zuserver2.star.ucl.ac.uk/~hiranya/phas3136/phas3136 Large Scale Structure After these lectures, you
More informationPhysical Cosmology 18/5/2017
Physical Cosmology 18/5/2017 Alessandro Melchiorri alessandro.melchiorri@roma1.infn.it slides can be found here: oberon.roma1.infn.it/alessandro/cosmo2017 Summary If we consider perturbations in a pressureless
More informationFormation and growth of galaxies in the young Universe: progress & challenges
Obergurgl. April 2014 Formation and growth of galaxies in the young Universe: progress & challenges Simon White Max Planck Institute for Astrophysics Ly α forest spectra and small-scale initial structure
More informationMapping the z 2 Large-Scale Structure with 3D Lyα Forest Tomography
Mapping the z 2 Large-Scale Structure with 3D Lyα Forest Tomography Intergalactic Matters Meeting, MPIA Heidelberg Max Planck Institut für Astronomie Heidelberg, Germany June 16, 2014 Collaborators: Joe
More informationBARYON ACOUSTIC OSCILLATIONS. Cosmological Parameters and You
BARYON ACOUSTIC OSCILLATIONS Cosmological Parameters and You OUTLINE OF TOPICS Definitions of Terms Big Picture (Cosmology) What is going on (History) An Acoustic Ruler(CMB) Measurements in Time and Space
More informationBaryon Acoustic Oscillations in the Lyman Alpha Forest
Baryon Acoustic Oscillations in the Lyman Alpha Forest Michael L. Norman, Pascal Paschos & Robert Harkness Laboratory for Computational Astrophysics, SERF 0424, University of California San Diego, 9500
More informationBaryon acoustic oscillations A standard ruler method to constrain dark energy
Baryon acoustic oscillations A standard ruler method to constrain dark energy Martin White University of California, Berkeley Lawrence Berkeley National Laboratory... with thanks to Nikhil Padmanabhan
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 informationCosmological 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 =
More informationCosmological simulations of our Universe Debora Sijacki IoA & KICC Cambridge
Cosmological simulations of our Universe Debora Sijacki IoA & KICC Cambridge Cosmo 17 Paris August 30th 2017 Cosmological simulations of galaxy and structure formation 2 Cosmological simulations of galaxy
More informationThe Intergalactic Medium: Overview and Selected Aspects
The Intergalactic Medium: Overview and Selected Aspects Draft Version Tristan Dederichs June 18, 2018 Contents 1 Introduction 2 2 The IGM at high redshifts (z > 5) 2 2.1 Early Universe and Reionization......................................
More informationThe 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
More informationPlanck 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
More informationFundamental cosmology from the galaxy distribution. John Peacock Hiroshima 1 Dec 2016
Fundamental cosmology from the galaxy distribution John Peacock Subaru @ Hiroshima 1 Dec 2016 What we learn from LSS Fundamental: Astrophysical: Matter content (CDM, baryons, neutrino mass) Properties
More informationHunting 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)
More informationNeutrino properties from cosmology
Neutrino properties from cosmology Yvonne Y. Y. Wong The University of New South Wales Sydney, Australia Rencontres de Moriond EW 2014, La Thuile, March 15 22, 2014 The concordance flat ΛCDM model... The
More informationJorge Cervantes-Cota, ININ. on behalf of the DESI Collaboration
Jorge Cervantes-Cota, ININ on behalf of the DESI Collaboration PPC 2014 DESI Overview DESI is the Dark Energy Spectroscopic Instrument Pioneering Stage-IV Experiment recommended by Community DE report
More informationThe 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,
More informationBaryon Acoustic Oscillations and Beyond: Galaxy Clustering as Dark Energy Probe
Baryon Acoustic Oscillations and Beyond: Galaxy Clustering as Dark Energy Probe Yun Wang Univ. of Oklahoma II Jayme Tiomno School of Cosmology August 6-10, 2012 Plan of the Lectures Lecture I: Overview
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 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 informationLecture 27 The Intergalactic Medium
Lecture 27 The Intergalactic Medium 1. Cosmological Scenario 2. The Ly Forest 3. Ionization of the Forest 4. The Gunn-Peterson Effect 5. Comment on HeII Reionization References J Miralda-Escude, Science
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 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 informationNeutrino Mass Limits from Cosmology
Neutrino Physics and Beyond 2012 Shenzhen, September 24th, 2012 This review contains limits obtained in collaboration with: Emilio Ciuffoli, Hong Li and Xinmin Zhang Goal of the talk Cosmology provides
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 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 informationProbing Cosmic Origins with CO and [CII] Emission Lines
Probing Cosmic Origins with CO and [CII] Emission Lines Azadeh Moradinezhad Dizgah A. Moradinezhad Dizgah, G. Keating, A. Fialkov arxiv:1801.10178 A. Moradinezhad Dizgah, G. Keating, A. Fialkov (in prep)
More informationarxiv: v1 [astro-ph.co] 20 Jan 2015
Astronomy & Astrophysics manuscript no. Boehringer 15 c ESO 201 September 23, 201 Letter to the Editor The extended ROSAT-ESO Flux-Limited X-ray Galaxy Cluster Survey (REFLEX II) VI. Effect of massive
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 informationNEUTRINO PROPERTIES FROM COSMOLOGY
NEUTRINO PROPERTIES FROM COSMOLOGY Cosmology 2018 in Dubrovnik 26 October 2018 OKC, Stockholm University Neutrino cosmology BOOKS: Lesgourgues, Mangano, Miele, Pastor, Neutrino Cosmology, Cambridge U.Press,
More informationThe 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
More informationSignatures of MG on. linear scales. non- Fabian Schmidt MPA Garching. Lorentz Center Workshop, 7/15/14
Signatures of MG on non- linear scales Fabian Schmidt MPA Garching Lorentz Center Workshop, 7/15/14 Tests of gravity Smooth Dark Energy (DE): unique prediction for growth factor given w(a) Use evolution
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 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 informationThe impact of relativistic effects on cosmological parameter estimation
The impact of relativistic effects on cosmological parameter estimation arxiv:1710.02477 (PRD) with David Alonso and Pedro Ferreira Christiane S. Lorenz University of Oxford Rencontres de Moriond, La Thuile,
More information