Testing gravity on cosmological scales with the observed abundance of massive clusters
|
|
- Jacob Moody
- 6 years ago
- Views:
Transcription
1 Testing gravity on cosmological scales with the observed abundance of massive clusters David Rapetti, KIPAC (Stanford/SLAC) In collaboration with Steve Allen (KIPAC), Adam Mantz (KIPAC), Harald Ebeling (Hawaii)
2 Outline * We have pursued/developed two different and complementary experiments that use X-ray luminous galaxy clusters to constrain cosmology: 1. Gas mass fraction (f gas ): distances to galaxy clusters 2. Abundance of massive galaxy clusters: growth of cosmic structure * We measure properties of: 1. Dark matter, dark energy 2. Cluster astrophysics 3. Gravity on large scales 4. Neutrinos 5. Etc * Current observations are in agreement with the cosmological constant plus cold dark matter (ΛCDM) paradigm (constant w=-1). We perform a number of (complementary) tests on different properties of this paradigm: 1. Evolution of the dark energy equation of state, w(z). 2. The growth rate of General Relativity. 3. Etc
3 The growth of structure experiment e.g. Henry 00, 04, 08; Borgani et al 01, 06; Reiprich & Bohringer 02; Seljak 02; Viana et al 02; Allen et al 03; Pierpaoli et al 03; Schuecker et al 03; Voevodkin &Vikhlinin 04; Kravtsov et al 06; Dahle 06; Mantz et al 08; Vikhlinin et al 08, 09; Mantz et al 09a, 09b
4 Theory: N-body Simulations Linear Cosmology
5 Cluster surveys ( z<0.3 ) Low redshift ( 00 BCS (Ebeling et al 98, F > 4.4 x erg s -1 cm -2 ~33% sky coverage REFLEX (Böhringer et al 04) F > 3.0 x erg s -1 cm -2 ~33% sky coverage ( 0.3<z<0.5 ) Intermediate redshifts ( 09 Bright MACS (Ebeling et al 01, F > 2.0 x erg s -1 cm -2 ~55% sky coverage L > 2.55x10 44 h 70-2 erg s -1 (dashed line). Cuts leave =238 massive clusters All based on RASS detections. Continuous and all 100% redshift complete.
6 Mantz et al 09b Scaling relations data Best fit for all the data (survey+follow-up+other data). Both, power law, self-similar, constant log-normal scatter. * Crucial: self-consistent and simultaneous analysis of survey+follow-up data, accounting for selection biases, degeneracies, covariances, and systematic uncertainties. * Data does not require additional evolution beyond self-similar (see tests in Mantz et al 09b) * Important cluster astrophysics conclusions (see Mantz et al 09b)
7 Dark Energy results: flat wcdm Mantz et al 09a Green: SNIa (Kowalski et al 08, Union) Blue: CMB (WMAP5) Red: cluster f gas (Allen et al 08) Brown: BAO (Percival et al 07) Gold: XLF+f gas +WMAP5+SNIa+BAO XLF(survey+follow-up data): BCS+REFLEX+MACS (z<0.5) 238 clusters (Mantz et al 09a). Including systematics Ω m = σ 8 = w =
8 Beyond LCDM: Evolving dark energy w(z), and test of GR
9 Constraints on w, 0 w marginalizing et over z t Combined constraints (marginalized 68%) Ω m = w 0 = w et = WMAP1+CBI+ACBAR SNIa: Riess et al 04 f gas : Allen et al 04 marginalized over 0.05<z t <1 Rapetti et al. 05 Two parameters: w=w 0 +w 1 (1-a) fix transition at z t =1 between w 0 (present) and w et =w 0 +w 1 (early times). Three parameters: free transition z t between w 0 and w et : Rapetti et al. 05
10 Constraints on w, 0 w marginalizing et over z t Combined constraints (marginalized 68%) Ω m = ± w 0 = w et = WMAP3+CBI+Boomerang+ACBAR SNIa: Davis et al. 07 f gas : Allen et al. 08 marginalized over 0.05<z t <1 Allen et al. 08 Three parameters: Three parameters: free transition z t between w 0 and w et :
11 Current constraints: evolving w Combined constraints (marginalized 68%) Ω m = w 0 = w et = WMAP5 SNIa: Kowalski et al. 08 f gas : Allen et al. 08 BAO: Percival et al. 07 XLF: Mantz et al. 09a marginalized over 0.05<z t <1 Mantz et al. 09a Three parameters: Three parameters: free transition z t between w 0 and w et : Allen et al. 08
12 Testing General Relativity Rapetti et al 09a, 09b
13 Motivation: Theory 1. Cosmic acceleration measurement + cosmological constant problem (from fundamental theory) 2. In the Friedmann equation: we can either include a new component, dark energy, or modify the theory of gravity [e.g. DGP, f(r), etc.]. (There are also other possibilities such as non-frw metrics, etc.) 3. Test General Relativity (GR). 4. Note that GR has been very well tested from small to Solar system scales. Here we test modifications of GR at cosmological scales.
14 Motivation: Data 1. Abundance of massive clusters (XLF) to measure cosmic growth of matter fluctuations with respect to the mean density. 2. SNIa, fgas, CMB, BAO to measure the cosmic expansion of the background density. We use three expansion histories well fitted by these data sets. E(a) = H(a)/H 0 i) flat ΛCDM w=-1, Ω k =0 ii) flat wcdm w constant, Ω k =0 iii) non-flat ΛCDM w=-1, Ω k constant
15 Modeling linear, time-dependent departures from GR variance of the density fluctuations Linear power spectrum General Relativity Phenomenological parameterization GR γ~0.55 Scale independent in the synchronous gauge Growth rate
16 Consistency test of the growth rate of General Relativity 1. We use a time-dependent parameterization (growth rate as a function of redshift). 2. We assume the same scale-dependence as GR. 3. We test only for linear effects (not for non-linear effects). We use the universal dark matter halo mass function (Tinker et al 08). 4. We match GR at early times and small scales.
17 Integrated Sachs-Wolfe effect Rapetti et al 09a The ISW effect is also sensitive to the growth rate. For CMB data we consistently account for the ISW, but currently the constraints on γ are not competitive with XLF
18 Investigating luminosity-mass evolution Within the 238 flux-selected clusters we used pointed observations for 23 clusters (z<0.2) from ROSAT 71 clusters (z>0.2) from Chandra Mass-luminosity and its intrinsic scatter "l(m)# = $ 0 lm + $ 1 lm m + $ 2 lm log 10 (1+ z) " lm (z) = " lm (1+ # " lm z) # L l = log 500 & # M 10 % (; m = log 500 E(z) & $ E(z)10 44 erg s "1 10 % ( ' $ M solar '
19 flat ΛCDM + growth index γ Rapetti et al 09b XLF: BCS+REFLEX+MACS (z<0.5) 238 survey with 94 X-ray follow-up CMB (WMAP5) SNIa (Kowalski et al 08, UNION) cluster f gas (Allen et al 08) For General Relativity γ~0.55 Gold: Self-similar evolution and constant scatter Blue: Marginalizing over β lm 2 and σ lm Remarkably these constraints are only a factor of ~3 weaker than those forecasted for JDEMtype experiments (e.g. Thomas 08, Linder 09).
20 GR results robust w.r.t evolution in the luminosity-mass relation Rapetti et al 09b "l(m)# = $ 0 lm + $ 1 lm m + $ 2 lm log 10 (1+ z) " lm (z) = " lm (1+ # " lm z) Current data do not require (i.e. acceptable fit) additional evolution beyond selfsimilar and constant scatter nor asymmetric scatter (Mantz et al 09b).
21 flat ΛCDM + growth index γ Rapetti et al 09b XLF: BCS+REFLEX+MACS (z<0.5) 238 survey with 94 X-ray follow-up CMB (WMAP5) SNIa (Kowalski et al 08, UNION) cluster f gas (Allen et al 08) For General Relativity γ~0.55 Gold: Self-similar evolution and constant scatter Blue: Marginalizing over β lm 2 and σ lm $ " # ' 8 & ) % 0.8( 6.8 Tight correlation between σ 8 and γ: " = # = 0.55 *0.10
22 flat wcdm + growth index γ Rapetti et al 09b XLF: BCS+REFLEX+MACS (z<0.5) 238 survey with 94 X-ray follow-up CMB (WMAP5) SNIa (Kowalski et al 08, UNION) cluster f gas (Allen et al 08) For General Relativity γ~0.55 Gold: Self-similar evolution and constant scatter Simultaneous constraints on the expansion and growth histories of the Universe at late times: Consistent with GR+ΛCDM
23 The impacts of the different data sets Rapetti et al 09a Green, dotted-dashed line: XLF alone Red, dashed line: SNIa+fgas+BAO+CMB(ISW) Blue, solid line: XLF+SNIa+fgas+BAO+CMB
24 The impacts of the different data sets Rapetti et al 09b Red: clusters (XLF+fgas) Green: clusters+snia Blue: clusters+snia+bao Gold: clusters+snia+bao+cmb Adding the CMB tightens Ω m, however the correlation with γ is weak.
25 The impacts of the different data sets Rapetti et al 09b Red: clusters (XLF+fgas) Green: clusters+snia Blue: clusters+snia+bao Gold: clusters+snia+bao+cmb Adding the CMB leads to a tight correlation between σ 8 and γ thanks to the constraints on several cosmological parameters: $ " # ' 8 & ) % 0.8( = 0.55 *0.10 Tight correlation between σ 8 and γ: " = #0.87
26 Conclusions For the first time, simultaneous and self-consistent analysis of the X-ray survey and follow-up data accounting for survey biases, systematic uncertainties and parameter degeneracies. We use follow-up Chandra and ROSAT data within a wide redshift range and the gas mass as total mass proxy (f gas low scatter). We obtain the tightest constraints on w for a single experiment from measurements of the growth of cosmic structure in clusters (flat wcdm): w = Combining XLF+f gas +SNIa+CMB+BAO we obtain: w 0 = , w et = We have performed a consistency test of General Relativity (growth rate) using cluster growth data: BCS+REFLEX+Bright MACS, T08 mass function, 94 clusters with X-ray follow-up observations; and cosmological (background) data from f gas +SNIa+CMB+BAO. We obtain a tight correlation γ(σ 8 /0.8) 6.8 = for the flat ΛCDM model. This promises significant improvements on γ by using independent constraints on σ 8. Our results are robust when allowing additional evolution in the luminosity-mass relation and its scatter. Simultaneously fitting γ and w and data is consistent with GR+ΛCDM. Our results highlight the importance of X-ray cluster data to test dark energy and modified gravity models. Future: more MACS and Chandra data, Spectrum-RG/eROSITA and WFXT, Astro-H, IXO, plus SZ and optical surveys (the same techniques developed here can be applied).
Weighing the Giants:
Weighing the Giants: Accurate Weak Lensing Mass Measurements for Cosmological Cluster Surveys Anja von der Linden Tycho Brahe Fellow DARK Copenhagen + KIPAC, Stanford IACHEC, May 14, 2014 1 Hello! Copenhagen
More informationDark matter in galaxy clusters
Dark matter in galaxy clusters Steve Allen, KIPAC In collaboration with: David Rapetti (KIPAC) Adam Mantz (KIPAC) Robert Schmidt (Heidelberg) Harald Ebeling (Hawaii) R. Glenn Morris (KIPAC) Andy Fabian
More informationGalaxy Clusters in Stage 4 and Beyond
Galaxy Clusters in Stage 4 and Beyond (perturbation on a Cosmic Visions West Coast presentation) Adam Mantz (KIPAC) CMB-S4/Future Cosmic Surveys September 21, 2016 Galaxy clusters: what? Galaxy cluster:
More informationCosmological Constraints from the XMM Cluster Survey (XCS) Martin Sahlén, for the XMM Cluster Survey Collaboration The Oskar Klein Centre for
Cosmological Constraints from the XMM Cluster Survey (XCS) Martin Sahlén, for the XMM Cluster Survey Collaboration The Oskar Klein Centre for Cosmoparticle Physics Stockholm University Key Points The XCS
More informationCHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS
The Astrophysical Journal, in press (692, 2009 February 10) Preprint typeset using L A TEX style emulateapj v. 04/20/08 CHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS A. Vikhlinin
More informationNew constraints on dark energy from the observed growth of the most X-ray luminous galaxy clusters
SLAC-PUB-12852 arxiv:0709.4294[astro-ph] October 2007 New constraints on dark energy from the observed growth of the most X-ray luminous galaxy clusters A. Mantz, 1 S. W. Allen, 1 H. Ebeling 2 and D. Rapetti
More informationCHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS
Submitted to the ApJ, 5/12/08 Preprint typeset using L A TEX style emulateapj v. 04/20/08 CHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS A. Vikhlinin 1,2,A.V.Kravtsov 3,R.A.Burenin
More informationCosmology with Galaxy Clusters. V. The Cluster Mass Function
Cosmology with Galaxy Clusters V. The Cluster Mass Function Baryon Fraction Summary Assuming clusters large enough to be representative, mass composition should match Universe observe fb and constrain
More informationX-ray Cluster Cosmology
X-ray Cluster Cosmology A white paper submitted to the Decadal Survey Committee Authors: A. Vikhlinin 1, S. Murray 1, R. Gilli 2, P. Tozzi 3, M. Paolillo 4, N. Brandt 8, G. Tagliaferri 9, M. Bautz 12,
More informationObservational Cosmology
(C. Porciani / K. Basu) Lecture 7 Cosmology with galaxy clusters (Mass function, clusters surveys) Course website: http://www.astro.uni-bonn.de/~kbasu/astro845.html Outline of the two lecture Galaxy clusters
More informationConstraining Dark Energy and Modified Gravity with the Kinetic SZ effect
Constraining Dark Energy and Modified Gravity with the Kinetic SZ effect Eva-Maria Mueller Work in collaboration with Rachel Bean, Francesco De Bernardis, Michael Niemack (arxiv 1408.XXXX, coming out tonight)
More informationThe PLANCK Cluster Catalog:
The PLANCK Cluster Catalog: SZ/X-ray Expected Properties Antoine Chamballu James G. Bartlett Jean-Baptiste Melin in the framework of the Planck consortium The Planck mission Background Successfully launched
More informationSébastien C. VAUCLAIR, OMP, Toulouse
XMM-Newton Ω-Project Ω matter from cluster evolution Collaborators : Sébastien C. VAUCLAIR, OMP, Toulouse J.G. Bartlett (PI) J.P. Bernard A. Blanchard M. Boer D.J. Burke* C.A. Collins* M. Giard D.H. Lumb
More informationCosmology and astrophysics with galaxy clusters
Talk @ Multiwavelength Cosmology, Mykonos Island, June 18 th 2003 Cosmology and astrophysics with galaxy clusters Stefano Borgani Dept. of Astronomy, Univ. of Trieste http://www.daut.univ.trieste.it/borgani
More informationarxiv: v3 [astro-ph.co] 24 Jun 2010
Mon. Not. R. Astron. Soc. 000, 1 25 (2010) Printed 10 October 2018 (MN LATEX style file v2.2) The Observed Growth of Massive Galaxy Clusters II: X-ray Scaling Relations arxiv:0909.3099v3 [astro-ph.co]
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 informationTESTING GRAVITY WITH COSMOLOGY
21 IV. TESTING GRAVITY WITH COSMOLOGY We now turn to the different ways with which cosmological observations can constrain modified gravity models. We have already seen that Solar System tests provide
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 informationClusters, lensing and CFHT reprocessing
Clusters, lensing and CFHT reprocessing R. Ansari - French LSST meeting December 2015 1 Clusters as cosmological probes Clusters: characteristics and properties Basics of lensing Weighting the Giants Clusters
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 informationBeyond BAO: Redshift-Space Anisotropy in the WFIRST Galaxy Redshift Survey
Beyond BAO: Redshift-Space Anisotropy in the WFIRST Galaxy Redshift Survey David Weinberg, Ohio State University Dept. of Astronomy and CCAPP Based partly on Observational Probes of Cosmic Acceleration
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 informationX-ray and Sunyaev-Zel dovich Effect cluster scaling relations: numerical simulations vs. observations
X-ray and Sunyaev-Zel dovich Effect cluster scaling relations: numerical simulations vs. observations Daisuke Nagai Theoretical Astrophysics, California Institute of Technology, Mail Code 130-33, Pasadena,
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 informationCosmological Constraints from a Combined Analysis of Clustering & Galaxy-Galaxy Lensing in the SDSS. Frank van den Bosch.
Cosmological Constraints from a Combined Analysis of Clustering & Galaxy-Galaxy Lensing in the SDSS In collaboration with: Marcello Cacciato (Leiden), Surhud More (IPMU), Houjun Mo (UMass), Xiaohu Yang
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 informationModified gravity. Kazuya Koyama ICG, University of Portsmouth
Modified gravity Kazuya Koyama ICG, University of Portsmouth Cosmic acceleration Cosmic acceleration Big surprise in cosmology Simplest best fit model LCDM 4D general relativity + cosmological const. H
More informationModified gravity as an alternative to dark energy. Lecture 3. Observational tests of MG models
Modified gravity as an alternative to dark energy Lecture 3. Observational tests of MG models Observational tests Assume that we manage to construct a model How well can we test the model and distinguish
More informationCosmology with galaxy clusters?
Cosmology with galaxy clusters? Cosmology with the cluster mass fct. Piero Rosati (ESO, Garching) Paolo Tozzi (INAF-OAT, Trieste) Colin Norman (JHU, Baltimora) Elena Pierpaoli (Princeton Univ.) Douglas
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 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 informationClusters physics and evolution from new X- ray/sz samples
Clusters physics and evolution from new X- ray/sz samples Monique ARNAUD (CEA Saclay) with Iacopo BARTALUCCI, Jessica DEMOCLES Etienne POINTECOUTEAU, Gabriel PRATT & Planck collaboration thanks to C. JONES
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 informationarxiv:astro-ph/ v1 1 Nov 2006
Modeling Chandra X-ray observations of Galaxy Clusters using Cosmological Simulations arxiv:astro-ph/0611013v1 1 Nov 2006 Daisuke Nagai 1, Andrey V. Kravtsov 2, and Alexey Vikhlinin 3,4 1 Theoretical Astrophysics,
More informationDetecting Dark Energy Perturbations
H. K. Jassal IISER Mohali Ftag 2013, IIT Gandhinagar Outline 1 Overview Present day Observations Constraints on cosmological parameters 2 Theoretical Issues Clustering dark energy Integrated Sachs Wolfe
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 informationMulti-wavelength scaling relations (scaling relations 101)
Multi-wavelength scaling relations (scaling relations 101) Gabriel W. Pratt (DSM - IRFU - SAp, CEA Saclay, France) Argument Astrophysics put constraints on formation physics effect of non-gravitational
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 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 informationCosmology and Astrophysics with Galaxy Clusters Recent Advances and Future Challenges
Cosmology and Astrophysics with Galaxy Clusters Recent Advances and Future Challenges Daisuke Nagai Yale University IPMU, July 15 th, 2010 Large-scale structure in the Universe SDSS (optical) Today δρ/ρ>>1
More informationProbing gravity theory and cosmic acceleration using (in)consistency tests between cosmological data sets
Probing gravity theory and cosmic acceleration using (in)consistency tests between cosmological data sets Prof. Mustapha Ishak Cosmology and Astrophysics Group The University of Texas at Dallas work done
More informationGalileon Cosmology ASTR448 final project. Yin Li December 2012
Galileon Cosmology ASTR448 final project Yin Li December 2012 Outline Theory Why modified gravity? Ostrogradski, Horndeski and scalar-tensor gravity; Galileon gravity as generalized DGP; Galileon in Minkowski
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 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 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 informationDark Energy and Dark Matter Interaction. f (R) A Worked Example. Wayne Hu Florence, February 2009
Dark Energy and Dark Matter Interaction f (R) A Worked Example Wayne Hu Florence, February 2009 Why Study f(r)? Cosmic acceleration, like the cosmological constant, can either be viewed as arising from
More informationEffective Field Theory approach for Dark Energy/ Modified Gravity. Bin HU BNU
Effective Field Theory approach for Dark Energy/ Modified Gravity Bin HU BNU NAOC Nov. 2016 Outline 1. Evidence of late-time cosmic acceleration 2. Effective Field Theory approach for DE/MG 3. The structure
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 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 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 informationPrecision Cosmology with X-ray and SZE Galaxy Cluster Surveys?
Precision Cosmology with X-ray and SZE Galaxy Cluster Surveys? Joe Mohr University of Illinois Outline SZE and X-ray Observations of Clusters Cluster survey yields and cosmology Precision cosmology and
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 informationWhat do we really know about Dark Energy?
What do we really know about Dark Energy? Ruth Durrer Département de Physique Théorique & Center of Astroparticle Physics (CAP) ESTEC, February 3, 2012 Ruth Durrer (Université de Genève ) Dark Energy ESTEC
More informationarxiv: v1 [astro-ph.co] 3 Apr 2019
Forecasting Cosmological Bias due to Local Gravitational Redshift Haoting Xu, Zhiqi Huang, Na Zhang, and Yundong Jiang School of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Tangjia, Zhuhai,
More informationA FIGURE OF MERIT ANALYSIS OF CURRENT CONSTRAINTS ON TESTING GENERAL RELATIVITY USING THE LATEST COSMOLOGICAL DATA SETS.
A FIGURE OF MERIT ANALYSIS OF CURRENT CONSTRAINTS ON TESTING GENERAL RELATIVITY USING THE LATEST COSMOLOGICAL DATA SETS. Jason Dossett OUTLINE Motivations Ways to Test Gravity Growth Equations Modified
More informationOVERVIEW OF NEW CMB RESULTS
OVERVIEW OF NEW CMB RESULTS C. R. Lawrence, JPL for the Planck Collaboration UCLA Dark Matter 2016 2016 February 17 Overview of new CMB results Lawrence 1 UCLA, 2016 February 17 Introduction Planck First
More 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 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 informationExtending Robust Weak Lensing Masses to z~1. Douglas Applegate, Tim Schrabback & the SPT-Lensing Team
Extending Robust Weak Lensing Masses to z~1 Douglas Applegate, Tim Schrabback & the SPT-Lensing Team 1 SPT Lensing Team Bonn Tim Schrabback Douglas Applegate Fatimah Raihan Chicago Brad Benson Lindsay
More informationPhysics 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
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 informationWhere 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,
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 informationThe Nature of Dark Energy and its Implications for Particle Physics and Cosmology
The Nature of Dark Energy and its Implications for Particle Physics and Cosmology May 3, 27@ University of Tokyo Tomo Takahashi Department of Physics, Saga University 1. Introduction Current cosmological
More informationCosmological Constraints from Redshift Dependence of Galaxy Clustering Anisotropy
Cosmological Constraints from Redshift Dependence of Galaxy Clustering Anisotropy Changbom Park (Korea Institute for Advanced Study) with Xiao-Dong Li, Juhan Kim (KIAS), Sungwook Hong, Cris Sabiu, Hyunbae
More informationCOSMOLOGICAL CONSTRAINTS FROM THE SDSS MAXBCG CLUSTER CATALOG
Draft version February 21, 2009 Preprint typeset using L A TEX style emulateapj v. 11/27/05 SLAC-PUB-13719 July 2009 COSMOLOGICAL CONSTRAINTS FROM THE SDSS MAXBCG CLUSTER CATALOG Eduardo Rozo 1, Risa H.
More informationMario Santos (on behalf of the Cosmology SWG) Stockholm, August 24, 2015
Mario Santos (on behalf of the Cosmology SWG) Stockholm, August 24, 2015 Why is the expansion of the Universe accelerating? Dark energy? Modified gravity? What is the nature of the primordial Universe?
More informationCosmology on small scales: Emulating galaxy clustering and galaxy-galaxy lensing into the deeply nonlinear regime
Cosmology on small scales: Emulating galaxy clustering and galaxy-galaxy lensing into the deeply nonlinear regime Ben Wibking Department of Astronomy Ohio State University with Andres Salcedo, David Weinberg,
More informationThe ultimate measurement of the CMB temperature anisotropy field UNVEILING THE CMB SKY
The ultimate measurement of the CMB temperature anisotropy field UNVEILING THE CMB SKY PARAMETRIC MODEL 16 spectra in total C(θ) = CMB theoretical spectra plus physically motivated templates for the
More informationHigh redshift clusters and their evolution. M.Arnaud (CEA-Sap Saclay France)
High redshift clusters and their evolution M.Arnaud (CEA-Sap Saclay France) Clusters and structure formation Z= 5 Z= 0 Simulations AMR: Teyssier (2002) Galaxy cluster Primordial fluctuations (DM) that
More informationBaryon Census in Hydrodynamical Simulations of Galaxy Clusters
Baryon Census in Hydrodynamical Simulations of Galaxy Clusters Susana Planelles (Univ.Trieste-INAF) Collaborators: S.Borgani (Univ. Trieste-INAF), G.Murante (INAF Torino), L.Tornatore (Univ. Trieste),
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 informationpseudo- evolution of halo mass and observable-mass relations Andrey Kravtsov The University of Chicago
pseudo- evolution of halo mass and observable-mass relations Andrey Kravtsov The University of Chicago Baseline model for cluster scaling relations Kaiser 1986, 1991 If mass is defined within a spherical
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 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 informationUnderstanding 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
More informationKinetic Sunyaev-Zel dovich effect: Dark Energy, Modified gravity, Massive Neutrinos
Kinetic Sunyaev-Zel dovich effect: Dark Energy, Modified gravity, Massive Neutrinos Eva-Maria Mueller Work in collaboration with Francesco De Bernardis, Michael D. Niemack, Rachel Bean [arxiv:1408.6248,
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 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 informationN-body Simulations and Dark energy
N-Body Simulations and models of Dark Energy Elise Jennings Supported by a Marie Curie Early Stage Training Fellowship N-body Simulations and Dark energy elise jennings Introduction N-Body simulations
More informationA kinematical approach to dark energy studies
SLAC-PUB-11882 May 2006 A kinematical approach to dark energy studies David Rapetti 1, Steven W. Allen 1, Mustafa A. Amin 1, Roger D. Blandford 1 1 Kavli Institute for Particle Astrophysics and Cosmology,
More informationLate time cosmology with GWs
Late time cosmology with elisa Institut de Physique Théorique CEA-Saclay CNRS Université Paris-Saclay Outline Standard sirens: Concept and issues Forecast cosmological constraints for elisa: Approach:
More informationModern Cosmology / Scott Dodelson Contents
Modern Cosmology / Scott Dodelson Contents The Standard Model and Beyond p. 1 The Expanding Universe p. 1 The Hubble Diagram p. 7 Big Bang Nucleosynthesis p. 9 The Cosmic Microwave Background p. 13 Beyond
More informationCosmological parameters of modified gravity
Cosmological parameters of modified gravity Levon Pogosian Simon Fraser University Burnaby, BC, Canada In collaborations with R. Crittenden, A. Hojjati, K. Koyama, A. Silvestri, G.-B. Zhao Two questions
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 informationDark Energy: Measuring the Invisible with X-Ray Telescopes
Black holes, Galactic Dark Center Matter and Galactic Center Dark Energy: Measuring the Invisible with X-Ray Telescopes Christine Jones Before 1930 -- only optical observations of the sky Intro Before
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 informationChapter - 3. Analytical solutions of the evolution of mass of black holes and. worm holes immersed in a Generalized Chaplygin Gas model
Chapter - 3 Analytical solutions of the evolution of mass of black holes and worm holes immersed in a Generalized Chaplygin Gas model (Published in International Journal of Pure and Applied Sciences and
More informationarxiv:astro-ph/ v1 6 Mar 2006
Studying the Nature of Dark Energy with Galaxy Clusters Thomas H. Reiprich 1, Daniel S. Hudson 1, Thomas Erben 1, and Craig L. Sarazin 2 arxiv:astro-ph/0603129v1 6 Mar 2006 1 Argelander-Institut für Astronomie,
More informationWhat Can We Learn from Galaxy Clustering 1: Why Galaxy Clustering is Useful for AGN Clustering. Alison Coil UCSD
What Can We Learn from Galaxy Clustering 1: Why Galaxy Clustering is Useful for AGN Clustering Alison Coil UCSD Talk Outline 1. Brief review of what we know about galaxy clustering from observations 2.
More informationCosmic Microwave Background Introduction
Cosmic Microwave Background Introduction Matt Chasse chasse@hawaii.edu Department of Physics University of Hawaii at Manoa Honolulu, HI 96816 Matt Chasse, CMB Intro, May 3, 2005 p. 1/2 Outline CMB, what
More informationTo Lambda or not to Lambda?
To Lambda or not to Lambda? Supratik Pal Indian Statistical Institute Kolkata October 17, 2015 Conclusion We don t know :) Partly based on my works with Dhiraj Hazra, Subha Majumdar, Sudhakar Panda, Anjan
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 informationDark Energy Research at SLAC
Dark Energy Research at SLAC Steven M. Kahn, SLAC / KIPAC Sept 14, 2010 DOE Site Visit: Sept 13-14, 2010 1 Constraining the Properties of Dark Energy The discovery of dark energy in the late 90 s has profound
More informationPhysical Cosmology 4/4/2016. Docente: Alessandro Melchiorri
Physical Cosmology 4/4/2016 Docente: Alessandro Melchiorri alessandro.melchiorri@roma1.infn.it Suggested textbooks Barbara Ryden, Introduction to Cosmology http://www.astro.caltech.edu/~george/ay21/readings/ryden_introcosmo.pdf
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 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 informationClusters and cosmology
Clusters and cosmology The KICP Inaugural Symposium, Dec 12, 2005 Mike Gladders, Carnegie Observatories Clusters Outline: and cosmology Codex Aggereris Caelestise (The Book of celestial Aggregates a primer)
More informationBeyond ΛCDM: Dark energy vs Modified Gravity
Beyond ΛCDM: Dark energy vs Modified Gravity Bhuvnesh Jain University of Pennsylvania References BJ et al, arxiv:1309.5389 (Snowmass) Joyce, BJ, Khoury, Trodden, arxiv:1407.0059 (Review) Cosmology probes:
More informationSome issues in cluster cosmology
Some issues in cluster cosmology Tim McKay University of Michigan Department of Physics 1/30/2002 CFCP Dark Energy Workshop 1 An outline Cluster counting in theory Cluster counting in practice General
More information