EUCLID Cosmology Probes

Size: px
Start display at page:

Download "EUCLID Cosmology Probes"

Transcription

1 EUCLID Cosmology Probes Henk Hoekstra & Will Percival on behalf of the EUCLID The presented document is Proprietary information of the. This document shall be used and disclosed by the receiving Party and its related entities (e.g. contractors and subcontractors) only for the purposes of fulfilling the receiving Party's responsibilities under the Project and that identified and marked technical data shall not be disclosed or retransferred to any other entity without prior written permission of the document preparer. Meeting Bologna 7-8 Sept

2 How can we achieve this? These numbers only have meaning if systematic biases are small. is designed to achieve this! Meeting Bologna 7-8 Sept

3 Survey Optimization The FoM increases with increasing area/volume and galaxy number density. This ignores that any survey is limited by cost: time is finite For galaxy clustering a large survey area provides the best bang for your buck. This is not the case for weak lensing. If intrinsic alignments are ignored indeed increasing the survey area is more efficient compared to increasing the number density. However, as the survey becomes shallower, intrinsic alignments become increasingly important. This changes the trade-off between area and depth. Meeting Bologna 7-8 Sept

4 Area requirements Given the nominal survey time this leads to an optimal survey area of 15,000 deg 2 Req. ID Parameter Requirement Goal WL.1-1 & GC.1-1 Survey area >15,000 deg 2 >20,000 deg 2 WL.1-2 Number density >30 arcmin -2 >40 arcmin -2 WL.1-3 Mean redshift >0.8 Meeting Bologna 7-8 Sept

5 Weak gravitational lensing Density fluctuations in the universe affect the propagation of light rays, leading to correlations in the their observable shapes. The statistics of shape correlations as a function of angular scale and redshift can be used to directly infer the statistics of the density fluctuations and consequently cosmology. Meeting Bologna 7-8 Sept

6 What do we need? For each galaxy we need: - Estimate of its shape (corrected for observational effects) - Estimate of its redshift (knowledge of mean and distribution) We need to establish the correlations between the galaxy shapes in the absence of lensing (intrinsic alignments) We need to relate the resulting signal as a function of scale and redshift to cosmological parameters through numerical simulations of structure formation. Meeting Bologna 7-8 Sept

7 Measuring shapes The observed lensing signal may be biased: g obs = (1+ m) g true +c which leads to biases in the ellipticity correlation function (Massey et al., in prep): C true» éë 1+ 2 m ù û C obs + c 2 l l Meeting Bologna 7-8 Sept

8 Measuring shapes We require that the FoM is dominated by the statistical uncertainty, rather than systematic biases (R-WL.1.-4): m< : 2 s sys» c 2 <10-7 : multiplicative bias additive bias This drives the constraints on the space craft and the algorithms used to measure shapes. Meeting Bologna 7-8 Sept

9 Case for space space ground The multiplicative bias m and additive bias σ sys (or c) scale with the square of the PSF: it is much easier to measure shapes when the PSF is small. Weak lensing with is primarily feasible thanks to its small PSF! Meeting Bologna 7-8 Sept

10 Sources of bias Given the PSF size, the multiplicative and additive bias depend on - How well we know the instrumental distortion (knowledge) - How well we can correct for the instrumental distortion (method) - The effective PSF sizes is constrained by the mirror diameter/optics. - The required depth (m AB <24.5) constrains the distribution of galaxy sizes. Results of tests of shape measurement methods (STEP, GREAT 10, etc.) constrain the allocation to the method budget. The remainder of the budget set by R-WL.1-4 determines how well we need to know the instrumental distortions. Meeting Bologna 7-8 Sept

11 Another case for space We need to know the instrumental distortions extremely well, which can only be achieved thanks to the stability provided in space. (see the talk by Jerome Amiaux for a detailed flowdown) 67% multiplicative bias 33% method knowledge R-WL : the multiplicative bias in shape measurements shall be known to an accuracy of σ[μ]<2x10-3 under all observing conditions and all types of galaxies used for weak lensing. Feasible based on GREAT 10 results. R-WL.2.1-9: the relative uncertainty in our knowledge of the PSF size should be: σ[r 2 ]/R 2 <10-3 This has been verified using end-to-end simulations (see talk by Lance Miller) Meeting Bologna 7-8 Sept

12 Another case for space We need to know the instrumental distortions extremely well, which can only be achieved thanks to the stability provided in space. (see the talk by Jerome Amiaux for a detailed flowdown) 11% * additive bias 72% 17% method knowledge margin R-WL : the additive bias in shape measurements shall be known to an accuracy of σ[c]<5x10-4 Feasible based on GREAT 10 results. * Includes cross-term R-WL.2.1-8: the spatio-temporal variation of the ellipticity induced by the PSF should be such that a model can be constructed with residals per component: σ[e inst ]<2x10-4 This has been verified using end-to-end simulations (see talk by Lance Miller). CTI contribution has been verified by Richard Massey. Meeting Bologna 7-8 Sept

13 Need for redshifts The achieve our science goals we need to measure the matter distribution as a function of redshift: weak lensing tomography requires redshifts for the sources. Meeting Bologna 7-8 Sept

14 Need for redshifts Tomography can be done using fairly broad bins, and the individual redshifts do not need to be very precise. But the mean redshift in a tomographic bin needs be known to high accuracy: R-WL.1-6: The catastrophic failure fraction (f cat ), shall be less than 10%. R-WL.1-7: The mean of the redshift distribution n(z) in each tomographic redshift bin shall be known to a precision of σ(<z>)/(1+z)<0.002 Tomography Kitching et al. (2008) Meeting Bologna 7-8 Sept

15 External data The VIS and NIR data are not sufficient and therefore we require supporting ground based multi-color data: - PanSTARRS2 (10,000 deg 2 ) - Dark Energy Survey (5000 deg 2 ) - additional data could come from LSST and VST These data are also needed to account to correct galaxy shapes with the correct (wavelength-dependent) PSF. To achieve R-WL.1-7 requires a large calibration sample of ~10 5 galaxies with spectroscopic redshifts. spectroscopy will provide a large sample at z>0.8 adding to results from several ongoing redshift surveys. Meeting Bologna 7-8 Sept

16 Need for redshifts The presence of intrinsic alignments changes this simple picture by placing additional requirements on the precision of the photometric redshifts: R-WL.1-5: The statistical scatter (RMS) of the errors in the measured photometric redshifts, in the range 0.2<z<2.0 shall be σ(z)/(1+z)<0.05 (and with a goal of <0.03). Joachimi et al. Meeting Bologna 7-8 Sept

17 Need for redshifts R-WL.1-5 can be met with by complementing VIS+NISP data with imaging from DES and PanSTARRS2 (assuming nominal survey depths). The use of LSST data allow us to reach the goal of σ(z)/(1+z)<0.03 Abdalla et al. (2008) Meeting Bologna 7-8 Sept

18 Interpretation of the data The largest contribution to the weak lensing power spectrum comes from scales that correspond to groups of galaxies, i.e. non-linear structures. To relate the observations to cosmological parameters we need very accurate predictions from numerical simulations (see talk by Romain Teyssier tomorrow). The lensing signal is sensitive to the total matter power spectrum, not just that of dark matter. If baryons trace the dark matter perfectly then simple n-body simulations might be sufficient, but recent work suggests that feedback processes can redistribute a large fraction of the baryons. Hydro-simulations to infer real C(l) expensive Recipe to convert n-body into real C(l) e.g. Semboloni et al. (2011) Requires better modeling of feedback: data will be extremely useful! Meeting Bologna 7-8 Sept

19 Clusters of galaxies Clusters of galaxies trace the peaks in the density distribution and provide additional information to probe the growth of structure. The data themselves will yield a sample of 60,000 clusters with a S/N>3 between 0.2<z<2 using a conservative optical selection. More than 10 4 of these will be at z>1. The number density of high mass, high redshift clusters is extremely sensitive to any primordial non-gaussianity and deviations from standard dark energy models To reach the projected FoM we need to know: - the masses - selection function Meeting Bologna 7-8 Sept

20 Clusters of galaxies M ass proxies Cluster survey Cosmology? Thanks to no more miracles are needed! Meeting Bologna 7-8 Sept

21 Clusters of galaxies will provide the most accurate masses for the large sample of clusters thanks to its built-in weak lensing analysis. In addition it will probe dark matter density profiles on scales >100 kpc, providing direct and important constraints on numerical simulations. The high resolution imaging also will yield a large number of strong lensing features which provide a unique test of CDM by probing the substructure and small scale density profile (see talk by Massimo Meneghetti). Multi-wavelength analysis (synergy with Planck and erosita, etc.) provide improved constraints on feedback processes, thus improving the fidelity of the numerical simulations and the predicted power spectra. Meeting Bologna 7-8 Sept

22 Galaxy clustering Need angular galaxy positions Need galaxy redshifts For lots of galaxies over a large volume Need to understand population angular completeness radial completeness radial/angular fluctuations This is the hard part Then can go from a density field to an overdensity field, and measure statistics Meeting Bologna 7-8 Sept

23 Using the measured clustering What are the constituents of matter? e.g. neutrino mass, primordial P(k) What is the expansion rate of the Universe? e.g. quintessence, Λ Galaxy Redshift Survey Redshift-Space distortions How does structure form within this background? e.g. modified gravity, GR Understanding acceleration Is the Universe homogeneous on large scales? Copernican principle, Non-Gaussianity How do galaxies form and evolve? semi-analytic models, halo model Meeting Bologna 7-8 Sept

24 Modeling the full P(k) shape There have been significant recent advances modeling the full anisotropic matter power spectrum e.g. Taruya, Nishimichi & Saito 2010; Jennings, Baugh, & Pascoli 2011 There have also been advances in modeling the galaxy power spectrum e.g. Reid & White (2011; arxiv: ) halo power spectra well modeled at z=0.5 everything is simply at higher redshifts! For our predictions, we assume can fit P(k), but take a conservative cut for the range of scale fitted for our predictions consider k<0.2 / hmpc -1 z>1 reduced to k<0.15 / hmpc -1 at z=0.7 Marginalise over galaxy bias Use Figure-of-Merit method developed by Seo & Eisenstein (2007: ApJ, 665, 14) described in Wang et al. (2010: MNRAS, 409, 737). Meeting Bologna 7-8 Sept

25 Area requirements Given the nominal survey time this leads to an optimal survey area of 15,000 deg 2 Meeting Bologna 7-8 Sept

26 Galaxy redshift density Req. ID Parameter Requirement Goal GC.1-2 Galaxy sky density 3,500 / deg 2 5,000 / deg 2 GC.1-5 Redshift range 0.7<z<2.05 also gals z<0.7 GC.1-6 Median of redshift distribution >1 >1.1 GC.1-7 Upper quartile of redshifts >1.35 GC Flux limit erg cm -2 s -1 GC Completeness >45% GC Flux limit at all wavelengths <120% of GC Meeting Bologna 7-8 Sept

27 Redshift accuracy Wang et al Req. ID Parameter Requirement Goal GC.1-3 Redshift accuracy σ(z)<0.001(1+z) GC Spectral resolution >250 GC Resolution element sampled by > 2 pixels Meeting Bologna 7-8 Sept

28 Current clustering measurements Percival et al. 2009; arxiv: Meeting Bologna 7-8 Sept

29 clustering measurements 20% of the data, assuming the slitless baseline at z~1 Distance-redshift relation moves P(k) Meeting Bologna 7-8 Sept

30 Slitless spectroscopy from space NIR Slitless spectroscopy would provide a uniform sample of galaxy redshifts based on the H-alpha line emission, with no need to specify a target sample NIR observations are not possible from the ground due to the high background a near-ir survey is much less affected by the dust extinction of our Galaxy H-alpha is less affected by galaxy internal dust extinction than other lines in the blue (e.g. a factor of about 2 less than [OII]3727) the most important emission lines to estimate gas dust extinction, metallicity and ionization properties are in the rest-frame optical (i.e. redshifted in the near-ir for z>0.7) H-alpha is a primary estimator of the star formation rate near-ir spectroscopy provides spectra in the rest-frame optical for z>0.7, hence allowing the best combination with ground-based optical surveys of low redshift galaxies (e.g. SDSS). Meeting Bologna 7-8 Sept

31 1deg 2 of spectroscopy 1 deg2 of the sky simulated and propagated through end-2-end spectroscopic simulation Shows can meet the required n(z), completeness and purity See talk tomorrow by Bianca Garilli Meeting Bologna 7-8 Sept

32 Understanding redshift systematics Slitless spectroscopy leads to redshift failures (purity 1) we need to calibrate the survey Can use a smaller, complete sample to do this The deep-field gives such a sample if rotate dispersion axis (beat confusion) Need wide & deep surveys Req. ID Parameter Requirement Goal GC.1-10 fraction of catastrophic failures f<20% GC.1-11 fraction of catastrophic failures known to 1% GC.1-12 mean redshift in 0.1 redshift bin known to 0.1% GC Subsample of galaxies >140,000 gals, with >99% purity Meeting Bologna 7-8 Sept

33 Using 1 deg 2 sim to test confusion Slitless spectroscopy leads to confusion (density dependent fluctuations in completeness) Isolated galaxies All Confused galaxies Given dispersion in 2 orthogonal directions, we have confusion if another galaxy within cross Meeting Bologna 7-8 Sept

34 100deg 2 sim test of confusion from Durham group Meeting Bologna 7-8 Sept

35 Scientific Synergy between probes Different degeneracies between parameters in standard analyses Direct test of anisotropic stress in the same volume RSD measure time-like metric fluctuations WL measures a combination of time-like and space-like metric fluctuations The deep photo-z catalog will contain many galaxies per halo hosting each spectroscopic galaxy, and we will have WL halo mass estimates providing better weights (Cai et al. 2011) The WL catalog contains many galaxies in the background of the spectroscopic population, which can be used to measure the bias. This breaks galaxy-bias degeneracies in the standard RSD analysis, significantly improving constraints (Bernstein & Cai 2011) Spectroscopic redshift catalog can be used to constrain intrinsic alignment effect for WL measurements Meeting Bologna 7-8 Sept

36 Implementation Synergy The top-level requirements for both GC & WL include large surveys high image quality accessibility to infra-red wavelengths homogeneity of observation, minimum systematics Space mission provides all of this low background stability lack of terrestrial atmospheric effects survey speed Power of is in complementarities at all levels science, analysis, observations, between VIS, NIP, NIS data, and all require space-based observations Meeting Bologna 7-8 Sept

37 Additional cosmological probes (Clusters already covered) Complementing ESA Planck data tightening of parameters given baseline to last scattering surface measurement of Integrated Sachs-Wolfe effect measurement of the lensed CMB sky Type 1a Supernovae in the Deep Field NIR light-curves and colours for 3,000 Type Ia SNe to z~ 1.2 spectroscopy would provide accurate redshifts for many of the host galaxies, although ground-based spectroscopic redshifts would still be required for subset will be the first large- scale NIR search for SNe from space. Meeting Bologna 7-8 Sept

38 Measuring Dark Energy The dark energy equation of state is the ratio of the pressure to density of dark energy p(a) = w(a) ρ(a)c 2. This dependence can be parameterised using a first order Taylor expansion with respect to the scale factor a=1/(1+z), w(a)= w p +(a p a)w a. Detecting w(a)= 1 at any redshift would demonstrate that dark energy is not a cosmological constant, but rather a dynamical field Define a Figure-of-Merit (FoM) FoM = 1/(Δw p Δw a ) Primary probes give a FoM>400, with subdominant systematic uncertainties, matching the DETF definition of a stage-iv mission Meeting Bologna 7-8 Sept

39 Measuring Modified Gravity The growth factor [or its derivative, the growth rate f(z)] quantifies the efficiency with which cosmological structure is built. The growth rate well described by f(z)=ω m (z) γ. A detection of γ= 0.55 would indicate a deviation from General Relativity, and thus a completely different origin of cosmic acceleration, rather than dark energy. can constrain this parameter to 0.01 (where ΛCDM corresponds to γ=0.55). the γ-parameterisation is merely an example. In general, will provide tight constraints on the cosmological growth rate. Meeting Bologna 7-8 Sept

40 Measuring initial conditions Concordance cosmology assumes an initial Gaussian random field of perturbations, with power-law index n s + Planck will provide a factor ~2 improved n s measurement over Planck alone A detection of non-gaussianity would signify a departure from this central assumption of the current standard model. The f NL parameter is a way to quantify the amplitude of this effect. will measure f NL with an accuracy of 2, compared to Planck which measures f NL to an accuracy of 5 with a complementary approach Meeting Bologna 7-8 Sept

41 Measuring Neutrino Masses The total neutrino mass is the sum of the masses of the three known species (electron, muon and tau neutrinos). Massive neutrinos damp structure growth on small scales. The larger the mass, the more damping occurs, leaving a clear signature in the matter power spectrum observed by. particle physics experiments have established that at least two of the three neutrino species have non-zero mass, with the larger mass difference of the order of 0.06 ev will measure Δm ν < 0.03eV, sufficient to determine the neutrino mass hierarchy, if the total mass turns out to be small, m ν <0.1 ev. will show if neutrinos obey a normal (two light neutrinos, one massive neutrino) or inverted (two massive neutrinos, one light neutrino) hierarchy; understanding this will give indications about the mechanism that gave neutrinos their mass. Meeting Bologna 7-8 Sept

42 Summary Major leap forwards in our understanding of the Universe Meeting Bologna 7-8 Sept

EUCLID Spectroscopy. Andrea Cimatti. & the EUCLID-NIS Team. University of Bologna Department of Astronomy

EUCLID Spectroscopy. Andrea Cimatti. & the EUCLID-NIS Team. University of Bologna Department of Astronomy EUCLID Spectroscopy Andrea Cimatti University of Bologna Department of Astronomy & the EUCLID-NIS Team Observing the Dark Universe with EUCLID, ESA ESTEC, 17 November 2009 DARK Universe (73% Dark Energy

More information

Cosmology with the ESA Euclid Mission

Cosmology with the ESA Euclid Mission Cosmology with the ESA Euclid Mission Andrea Cimatti Università di Bologna Dipartimento di Astronomia On behalf of the Euclid Italy Team ESA Cosmic Vision 2015-2025 M-class Mission Candidate Selected in

More information

Euclid. Mapping the Geometry of the Dark Universe. Y. Mellier on behalf of the. Euclid Consortium.

Euclid. Mapping the Geometry of the Dark Universe. Y. Mellier on behalf of the. Euclid Consortium. Mapping the Geometry of the Dark Universe Y. Mellier on behalf of the http://www.euclid-ec.org Instrument Overall WP Breakdown VG :1 The ESA mission: scientific objectives Understand the origin of the

More information

Imaging the Dark Universe with Euclid

Imaging the Dark Universe with Euclid Imaging the Dark Universe with Simon Lilly (ETH Zurich) on behalf of Alexandre Refregier (CEA Saclay) for the Imaging Consortium Conference ESTEC 17/11/09 1 Science Objectives Outstanding questions in

More information

New techniques to measure the velocity field in Universe.

New 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 information

Baryon acoustic oscillations A standard ruler method to constrain dark energy

Baryon 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 information

Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering. Roland de Pu+er JPL/Caltech COSMO- 14

Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering. Roland de Pu+er JPL/Caltech COSMO- 14 Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering Roland de Pu+er JPL/Caltech COSMO- 14 Galaxy Clustering: - 3D maps of galaxies - > 3D power spectrum P(k,mu) - BOSS: V = 4.4 (h-

More information

Are VISTA/4MOST surveys interesting for cosmology? Chris Blake (Swinburne)

Are VISTA/4MOST surveys interesting for cosmology? Chris Blake (Swinburne) Are VISTA/4MOST surveys interesting for cosmology? Chris Blake (Swinburne) Yes! Probes of the cosmological model How fast is the Universe expanding with time? How fast are structures growing within it?

More information

Weak Lensing: Status and Prospects

Weak Lensing: Status and Prospects Weak Lensing: Status and Prospects Image: David Kirkby & the LSST DESC WL working group Image: lsst.org Danielle Leonard Carnegie Mellon University Figure: DES Collaboration 2017 for LSST DESC June 25,

More information

Énergie noire Formation des structures. N. Regnault C. Yèche

Énergie noire Formation des structures. N. Regnault C. Yèche Énergie noire Formation des structures N. Regnault C. Yèche Outline Overview of DE probes (and recent highlights) Hubble Diagram of supernovae Baryon accoustic oscillations Lensing Matter clustering (JLA)

More information

Basic BAO methodology Pressure waves that propagate in the pre-recombination universe imprint a characteristic scale on

Basic BAO methodology Pressure waves that propagate in the pre-recombination universe imprint a characteristic scale on Precision Cosmology With Large Scale Structure, Ohio State University ICTP Cosmology Summer School 2015 Lecture 3: Observational Prospects I have cut this lecture back to be mostly about BAO because I

More information

Euclid and MSE. Y. Mellier IAP and CEA/SAp.

Euclid and MSE. Y. Mellier IAP and CEA/SAp. Euclid and MSE Y. Mellier IAP and CEA/SAp www.euclid-ec.org Euclid and MSE CFHT Users Meeting, Nice 02 May, 2016 Euclid Primary Objectives: the Dark Universe Understand The origin of the Universe s accelerating

More information

BAO errors from past / future surveys. Reid et al. 2015, arxiv:

BAO errors from past / future surveys. Reid et al. 2015, arxiv: BAO errors from past / future surveys Reid et al. 2015, arxiv:1509.06529 Dark Energy Survey (DES) New wide-field camera on the 4m Blanco telescope Survey started, with first year of data in hand Ω = 5,000deg

More information

Galaxy Clusters in Stage 4 and Beyond

Galaxy 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 information

Weak Lensing. Alan Heavens University of Edinburgh UK

Weak Lensing. Alan Heavens University of Edinburgh UK Weak Lensing Alan Heavens University of Edinburgh UK Outline History Theory Observational status Systematics Prospects Weak Gravitational Lensing Coherent distortion of background images Shear, Magnification,

More information

BAO & 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 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 information

Mario Santos (on behalf of the Cosmology SWG) Stockholm, August 24, 2015

Mario 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 information

Concordance Cosmology and Particle Physics. Richard Easther (Yale University)

Concordance 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 information

Recent BAO observations and plans for the future. David Parkinson University of Sussex, UK

Recent BAO observations and plans for the future. David Parkinson University of Sussex, UK Recent BAO observations and plans for the future David Parkinson University of Sussex, UK Baryon Acoustic Oscillations SDSS GALAXIES CMB Comparing BAO with the CMB CREDIT: WMAP & SDSS websites FLAT GEOMETRY

More information

Refining Photometric Redshift Distributions with Cross-Correlations

Refining Photometric Redshift Distributions with Cross-Correlations Refining Photometric Redshift Distributions with Cross-Correlations Alexia Schulz Institute for Advanced Study Collaborators: Martin White Introduction Talk Overview Weak lensing tomography can improve

More information

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 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 information

Beyond BAO: Redshift-Space Anisotropy in the WFIRST Galaxy Redshift Survey

Beyond 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 information

LSST Cosmology and LSSTxCMB-S4 Synergies. Elisabeth Krause, Stanford

LSST Cosmology and LSSTxCMB-S4 Synergies. Elisabeth Krause, Stanford LSST Cosmology and LSSTxCMB-S4 Synergies Elisabeth Krause, Stanford LSST Dark Energy Science Collaboration Lots of cross-wg discussions and Task Force hacks Junior involvement in talks and discussion Three

More information

Jorge Cervantes-Cota, ININ. on behalf of the DESI Collaboration

Jorge 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 information

Weighing the Giants:

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 information

Observing the dark Universe with Euclid

Observing the dark Universe with Euclid Euclid Imaging Instrument Observing the dark Universe with Euclid 18 november 2009 Jerome Amiaux CEA Saclay EIC System Manager On Behalf of the Euclid Imaging Consortium The presented document is Proprietary

More information

From 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 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 information

Cosmology The Road Map

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

More information

Dark 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) 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 information

Cosmological surveys: from Planck to Euclid

Cosmological surveys: from Planck to Euclid Cosmological surveys: from Planck to Nabila Aghanim Institut d'astrophysique Spatiale On behalf of the Consortium The dark universe after Planck A post-planck concordance cosmology with two puzzling ingredients:

More information

New Probe of Dark Energy: coherent motions from redshift distortions Yong-Seon Song (Korea Institute for Advanced Study)

New Probe of Dark Energy: coherent motions from redshift distortions Yong-Seon Song (Korea Institute for Advanced Study) New Probe of Dark Energy: coherent motions from redshift distortions Yong-Seon Song (Korea Institute for Advanced Study) 1 Future wide-deep surveys Photometric wide-deep survey Spectroscopic wide-deep

More information

An Introduction to the Dark Energy Survey

An Introduction to the Dark Energy Survey An Introduction to the Dark Energy Survey A study of the dark energy using four independent and complementary techniques Blanco 4m on Cerro Tololo Galaxy cluster surveys Weak lensing Galaxy angular power

More information

Measuring Neutrino Masses and Dark Energy

Measuring 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 information

LSST, Euclid, and WFIRST

LSST, Euclid, and WFIRST LSST, Euclid, and WFIRST Steven M. Kahn Kavli Institute for Particle Astrophysics and Cosmology SLAC National Accelerator Laboratory Stanford University SMK Perspective I believe I bring three potentially

More information

CMB Lensing Combined with! Large Scale Structure:! Overview / Science Case!

CMB Lensing Combined with! Large Scale Structure:! Overview / Science Case! CMB Lensing Combined with! Large Scale Structure:! Overview / Science Case! X Blake D. Sherwin Einstein Fellow, LBNL Outline! I. Brief Introduction: CMB lensing + LSS as probes of growth of structure II.

More information

Dark Energy with the Euclid Space Mission. Y. Mellier On behalf of the Euclid Consortium. Euclid Consortium.

Dark Energy with the Euclid Space Mission. Y. Mellier On behalf of the Euclid Consortium. Euclid Consortium. Dark Energy with the Space Mission Y. Mellier On behalf of the http://www.euclid-ec.org Instrument Overall WP Breakdown VG :1 Itzykson, IPhT-CEA Saclay June 18-20, 2012 Objective of the Mission Instrument

More information

Elise Jennings University of Chicago

Elise Jennings University of Chicago Pacific 2014 Testing gravity with large scale structure dynamics Elise Jennings University of Chicago THE UNIVERSITY OF CHICAGO THE ENRICO FERMI INSTITUTE EJ, B. Li, C.M. Baugh, G. Zhao, K. Kazuya 2013

More information

Galaxies 626. Lecture 3: From the CMBR to the first star

Galaxies 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 information

Constraining Dark Energy and Modified Gravity with the Kinetic SZ effect

Constraining 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 information

Baryon Acoustic Oscillations Part I

Baryon 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 information

BAO and Lyman-α with BOSS

BAO 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 information

The 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 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 information

The State of Tension Between the CMB and LSS

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

More information

Mapping the dark universe with cosmic magnification

Mapping the dark universe with cosmic magnification Mapping the dark universe with cosmic magnification 张鹏杰 Zhang, Pengjie 中科院上海天文台 Shanghai Astronomical Observatory (SHAO) Chinese Academy of Sciences All the hard works are done by my student Yang Xinjuan

More information

EUCLID galaxy clustering and weak lensing at high redshift

EUCLID galaxy clustering and weak lensing at high redshift EUCLID galaxy clustering and weak lensing at high redshift Luca Amendola INAF/Osservatorio Astronomico di Roma Observations are converging to an unexpected universe The dark energy problem F g μν 1 R μν

More information

Baryon Acoustic Oscillations and Beyond: Galaxy Clustering as Dark Energy Probe

Baryon 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 information

WL and BAO Surveys and Photometric Redshifts

WL and BAO Surveys and Photometric Redshifts WL and BAO Surveys and Photometric Redshifts Lloyd Knox University of California, Davis Yong-Seon Song (U Chicago) Tony Tyson (UC Davis) and Hu Zhan (UC Davis) Also: Chris Fassnacht, Vera Margoniner and

More information

Weak Gravitational Lensing. Gary Bernstein, University of Pennsylvania KICP Inaugural Symposium December 10, 2005

Weak Gravitational Lensing. Gary Bernstein, University of Pennsylvania KICP Inaugural Symposium December 10, 2005 Weak Gravitational Lensing Gary Bernstein, University of Pennsylvania KICP Inaugural Symposium December 10, 2005 astrophysics is on the 4th floor... President Amy Gutmann 215 898 7221 Physics Chair Tom

More information

Cosmology with Galaxy bias

Cosmology with Galaxy bias Cosmology with Galaxy bias Enrique Gaztañaga, M.Eriksen (PhD in progress...) www.ice.cat/mice Figure of Merit (FoM): Expansion x Growth w(z) -> Expansion History (background metric) we will use w0 and

More information

Clusters of Galaxies with Euclid

Clusters of Galaxies with Euclid Clusters of Galaxies with Euclid Figure by L. Caridà A. Biviano (INAF-OATS) largely based on Sartoris, AB, Fedeli et al. 2016 Euclid: ESA medium class A&A mission, selected Oct 2011, to be launched in

More information

Cosmology with Wide Field Astronomy

Cosmology with Wide Field Astronomy M. Moniez To cite this version: M. Moniez.. 35th International Conference on High Energy Physics (ICHEP2010), Jul 2010, Paris, France. Proceedings of Science, 441 (4 p.), 2010. HAL Id:

More information

RADIO-OPTICAL-cmb SYNERGIES. Alkistis Pourtsidou ICG Portsmouth

RADIO-OPTICAL-cmb SYNERGIES. Alkistis Pourtsidou ICG Portsmouth RADIO-OPTICAL-cmb SYNERGIES Alkistis Pourtsidou ICG Portsmouth Image credit: Hayden Planetarium, 2014 New Frontiers in Observational Cosmology [Planck 2015] 95% of our Universe is very strange - new physics!

More information

What 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 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 information

Cosmological 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 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 information

Supernovae with Euclid

Supernovae with Euclid Supernovae with Euclid Isobel Hook University of Oxford and INAF (Obs. Roma) Thanks to R. Nichol, M. Della Valle, F. Mannucci, A. Goobar, P. Astier, B. Leibundgut, A. Ealet Euclid Conference 17 18 Nov

More information

Results from the Baryon Oscillation Spectroscopic Survey (BOSS)

Results 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 information

Probing growth of cosmic structure using galaxy dynamics: a converging picture of velocity bias. Hao-Yi Wu University of Michigan

Probing growth of cosmic structure using galaxy dynamics: a converging picture of velocity bias. Hao-Yi Wu University of Michigan Probing growth of cosmic structure using galaxy dynamics: a converging picture of velocity bias Hao-Yi Wu University of Michigan Galaxies are not necessarily test particles Probing dark energy with growth

More information

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 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 information

The impact of relativistic effects on cosmological parameter estimation

The 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

EIC Simulations. Thomas Kitching, EIC Weak Lensing & Simulation Working Groups

EIC Simulations. Thomas Kitching, EIC Weak Lensing & Simulation Working Groups EIC Simulations Thomas Kitching A. Amara, S. Bridle, O. Boulade, B. Dobke, A. Fontana, A. Grazian, A. Heavens, A. Kiessling, M. Meneghetti, S. Paulin-Henriksson, J. Rhodes, A. Refregier, A. Taylor, R.

More information

Xiuyuan Yang (Columbia University and BNL) Jan Kratochvil (University of Miami)

Xiuyuan Yang (Columbia University and BNL) Jan Kratochvil (University of Miami) Xiuyuan Yang (Columbia University and BNL) Jan Kratochvil (University of Miami) Advisors: Morgan May (Brookhaven National Lab) Zoltan Haiman (Columbia University) Introduction Large surveys such as LSST

More information

Large Imaging Surveys for Cosmology:

Large Imaging Surveys for Cosmology: Large Imaging Surveys for Cosmology: cosmic magnification AND photometric calibration Alexandre Boucaud Thesis work realized at APC under the supervision of James G. BARTLETT and Michel CRÉZÉ Outline Introduction

More information

The Euclid space mission and the origin of the accelerating Universe

The Euclid space mission and the origin of the accelerating Universe The Euclid space mission and the origin of the accelerating Universe Yannick Mellier Institut d Astrophysique de Paris and CEA/IRFU Service d Astrophysique Saclay On behalf of the Euclid Collaboration

More information

Weak Lensing: a Probe of Dark Matter and Dark Energy. Alexandre Refregier (CEA Saclay)

Weak Lensing: a Probe of Dark Matter and Dark Energy. Alexandre Refregier (CEA Saclay) Weak Lensing: a Probe of Dark Matter and Dark Energy Alexandre Refregier (CEA Saclay) SLAC August 2004 Concordance ΛCDM Model Outstanding questions: initial conditions (inflation?) nature of the dark matter

More information

Brief Introduction to Cosmology

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

More information

EUCLID Legacy with Spectroscopy

EUCLID Legacy with Spectroscopy EUCLID Legacy with Spectroscopy Gianni Zamorani INAF - Bologna Astronomical Observatory (on behalf of the E-NIS Team) Observing the Dark Universe with Euclid 17-18 November 2009 ESTEC, The Netherlands

More information

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 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 information

Testing gravity on cosmological scales with the observed abundance of massive clusters

Testing gravity on cosmological scales with the observed abundance of massive clusters 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

More information

STUDY OF THE LARGE-SCALE STRUCTURE OF THE UNIVERSE USING GALAXY CLUSTERS

STUDY OF THE LARGE-SCALE STRUCTURE OF THE UNIVERSE USING GALAXY CLUSTERS STUDY OF THE LARGE-SCALE STRUCTURE OF THE UNIVERSE USING GALAXY CLUSTERS BÙI VĂN TUẤN Advisors: Cyrille Rosset, Michel Crézé, James G. Bartlett ASTROPARTICLE AND COSMOLOGY LABORATORY PARIS DIDEROT UNIVERSITY

More information

Tesla Jeltema. Assistant Professor, Department of Physics. Observational Cosmology and Astroparticle Physics

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

More information

Cosmology and Large Scale Structure

Cosmology and Large Scale Structure Cosmology and Large Scale Structure Alexandre Refregier PASCOS13 Taipei 11.22.2013 Matter Baryons Dark Matter Radiation Inflation Dark Energy Gravity Measuring the Dark Universe Geometry Growth of structure

More information

HI and Continuum Cosmology

HI and Continuum Cosmology HI and Continuum Cosmology Radiometry Equation snr 1 2 A For SKA, eff S[ ] kt rms sys 1/ 2 for each 100 mjy 1/ 2 [ ] polarizati on, two polarizati ons Filipe B. Abdalla Cosmology: Concordance Model Heavy

More information

Baryon 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 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 information

Kinetic Sunyaev-Zel dovich effect: Dark Energy, Modified gravity, Massive Neutrinos

Kinetic 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 information

Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 1 / 16

Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 1 / 16 Study the large-scale structure of the universe using galaxy clusters Bùi Văn Tuấn Advisors: Cyrille Rosset Michel Crézé Director: Volker Beckmann Astroparticle and Cosmology Laboratory Université Paris

More information

The 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 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 information

Present and future redshift survey David Schlegel, Berkeley Lab

Present and future redshift survey David Schlegel, Berkeley Lab Present and future redshift survey David Schlegel, Berkeley Lab David Schlegel, COSMO-17 @Paris, 30 Aug 2017 1 Redshift surveys = one of ~few probes of inflationary epoch Inflation-era parameters: non-gaussianity,

More information

Gravitational Lensing of the CMB

Gravitational 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 information

Neutrinos and cosmology

Neutrinos 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 information

Precision Cosmology from Redshift-space galaxy Clustering

Precision Cosmology from Redshift-space galaxy Clustering 27th June-1st July, 2011 WKYC2011@KIAS Precision Cosmology from Redshift-space galaxy Clustering ~ Progress of high-precision template for BAOs ~ Atsushi Taruya RESearch Center for the Early Universe (RESCEU),

More information

Cosmology and Astrophysics with Galaxy Clusters Recent Advances and Future Challenges

Cosmology 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 information

Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background

Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Cross-Correlation of Cosmic Shear and Extragalactic Gamma-ray Background Masato Shirasaki (Univ. of Tokyo) with Shunsaku Horiuchi (UCI), Naoki Yoshida (Univ. of Tokyo, IPMU) Extragalactic Gamma-Ray Background

More information

Correlations between the Cosmic Microwave Background and Infrared Galaxies

Correlations between the Cosmic Microwave Background and Infrared Galaxies Correlations between the Cosmic Microwave Background and Infrared Galaxies Brett Scheiner & Jake McCoy Based on work by Goto, Szapudi and Granett (2012) http://cdsads.u-strasbg.fr/abs/2012mnras.422l..77g

More information

Science with EUCLID. 30 Avril 2014

Science with EUCLID. 30 Avril 2014 Françoise Combes On behalf of Euclid Consortium Science with EUCLID 30 Avril 2014 1 Cosmology, Dark energy Kowalski et al 2008 Concordance model, between CMB, Supernovae Ia, Large-scale structure (weak

More information

Controlling intrinsic alignments in weak lensing statistics

Controlling intrinsic alignments in weak lensing statistics Controlling intrinsic alignments in weak lensing statistics Benjamin Joachimi, Peter Schneider joachimi@astro.uni-bonn.de Bonn University, Germany ADA6, Monastir, Tunisia May 6th 2010 Outline Intrinsic

More information

Constraining Dark Energy: First Results from the SDSS-II Supernova Survey

Constraining Dark Energy: First Results from the SDSS-II Supernova Survey Constraining Dark Energy: First Results from the SDSS-II Supernova Survey J. Craig Wheeler Department of Astronomy University of Texas at Austin (adapted from presentation by Josh Frieman) Texas Cosmology

More information

Mapping the Universe spectroscopic surveys for BAO measurements Meeting on fundamental cosmology, june 2016, Barcelona, Spain Johan Comparat

Mapping the Universe spectroscopic surveys for BAO measurements Meeting on fundamental cosmology, june 2016, Barcelona, Spain Johan Comparat Mapping the Universe spectroscopic surveys for BAO measurements Meeting on fundamental cosmology, june 2016, Barcelona, Spain Johan Comparat 1 Baryonic acoustic oscillations The acoustic length scale is

More information

Weak lensing measurements of Dark Matter Halos around galaxies

Weak lensing measurements of Dark Matter Halos around galaxies Weak lensing measurements of Dark Matter Halos around galaxies Rachel Mandelbaum Carnegie Mellon University 1 Image credits: NASA, ESA, S. Beckwith (STScI), the HUDF Team 2 Image credit: ESA/Planck 3 The

More information

Luminous Quasars and AGN Surveys with ELTs

Luminous Quasars and AGN Surveys with ELTs Luminous Quasars and AGN Surveys with ELTs Roberto J. Assef Núcleo de Astronomía Universidad Diego Portales This Talk Will focus on two topics: 1. The most luminous (obscured) quasars 2. AGN surveys Big

More information

Challenges of low and intermediate redshift supernova surveys

Challenges of low and intermediate redshift supernova surveys Challenges of low and intermediate redshift supernova surveys Ribamar R. R. Reis Image credit: ESO / M. Kornmesser Introduction Type Ia supernovae (SNeIa) are thermonuclear explosions of CO white dwarfs

More information

Large Scale Structure with the Lyman-α Forest

Large 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 information

arxiv: v1 [astro-ph.co] 3 Apr 2019

arxiv: 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 information

Imprint of Scalar Dark Energy on CMB polarization

Imprint of Scalar Dark Energy on CMB polarization Imprint of Scalar Dark Energy on CMB polarization Kin-Wang Ng ( 吳建宏 ) Institute of Physics & Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan Cosmology and Gravity Pre-workshop NTHU, Apr

More information

Euclid Legacy Science

Euclid Legacy Science Euclid Legacy Science Simona Mei GEPI Observatory of Paris University of Paris 7 Denis Diderot James G. Bartlett APC - University of Paris 7 Denis Diderot on the basis of the work of legacy coordinators

More information

Mapping Dark Matter with the Dark Energy Survey

Mapping Dark Matter with the Dark Energy Survey Mapping Dark Matter with the Dark Energy Survey Tim Eifler On behalf of many people in the DES collaboration DaMaSC IV: Beyond WIMP Dark Matter Aug. 30, 2017 Disclaimer DES has recently published Year

More information

THE PAU (BAO) SURVEY. 1 Introduction

THE PAU (BAO) SURVEY. 1 Introduction THE PAU (BAO) SURVEY E. Fernández Department of Physics, Universitat Autònoma de Barcelona/IFAE, Campus UAB, Edif. Cn, 08193 Bellaterra, Barcelona, Spain In this talk we present a proposal for a new galaxy

More information

Shear Power of Weak Lensing. Wayne Hu U. Chicago

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

More information

Really, really, what universe do we live in?

Really, really, what universe do we live in? Really, really, what universe do we live in? Fluctuations in cosmic microwave background Origin Amplitude Spectrum Cosmic variance CMB observations and cosmological parameters COBE, balloons WMAP Parameters

More information

The rise of galaxy surveys and mocks (DESI progress and challenges) Shaun Cole Institute for Computational Cosmology, Durham University, UK

The rise of galaxy surveys and mocks (DESI progress and challenges) Shaun Cole Institute for Computational Cosmology, Durham University, UK The rise of galaxy surveys and mocks (DESI progress and challenges) Shaun Cole Institute for Computational Cosmology, Durham University, UK Mock Santiago Welcome to Mock Santiago The goal of this workshop

More information

Precision Cosmology with X-ray and SZE Galaxy Cluster Surveys?

Precision 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 information