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

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

2 Outline 1 Scientific context 2 Planck and Euclid missions 3 Estimators of two-point correlation function 4 Simulation of random cluster catalog 5 Current results 6 Conclusion Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 2 / 16

3 Scientific context Standard model of cosmology The large-scale structure Galaxies, cluster of galaxies, super-clusters and filaments are the largest structures in the universe. Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 3 / 16

4 Planck and Euclid missions Planck mission Euclid mission Credit: ESA. Planck is a space mission by ESA. ( ) Mission: All-sky CMB survey using millimeter wavelengths; Primordial universe (inflation) and dark universe. Credit: ESA. Launch date: Mission: galaxy surveys (1.5 billions galaxies) for studying the dark universe using visible and near infra-red wavelengths. Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 4 / 16

5 Estimators of two-point correlation function Data: Planck SZ cluster catalog Sunyaev-Zel dovich effect Credit: Roman s these Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 5 / 16

6 Estimators of two-point correlation function Data: Planck SZ cluster catalog Planck Sunyaev-Zel dovich cluster catalog (1271 clusters) and the Planck mask map (white area) Planck SZ cluster catalog Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 5 / 16

7 Estimators of two-point correlation function Estimators of two-point correlation function Measure the excess probability respect to the uniform distribution of finding a galaxy in a sphere area S(θ) at an angular separation θ from another galaxy. Peebles & Hauser (1974): Davis & Peebles (1983): Landy and Szalay (1993): 1 + ŵ 1 (θ) = DD RR 1 + ŵ 2 (θ) = DD DR ŵ LS (θ) = DD 2DR + RR RR (1) (2) (3) Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 6 / 16

8 Simulation of random cluster catalog Random galaxy cluster catalogs - Apply the Planck mask to random uniform clusters. - Each random cluster has angular size θ s that corresponds to a noise map σ y500 (32 noise maps of θ s from 0.94 to arcmin) - Keep clusters have generated y > 4 σ y500. Generated θ s and y Planck's ts and y500 Generated ts and y y θs Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 7 / 16

9 Simulation of random cluster catalog Random galaxy cluster catalogs Random uniform cluster catalog Random cluster applied Planck mask and selection function Random uniform catalog Random uniform with Planck mask applied and selection function Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 7 / 16

10 Current results Angular distance of pairs statistics Planck Random uniform Planck and random uniform with mask applied and selection function Fake data and Random uniform both with mask applied and selection function θ [degrees] Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 8 / 16

11 Current results Estimators of Planck catalog and random catalogs Correlation function of Planck catalog and random catalogs with Planck mask applied and selection function. Estimator two-point correlation function Estitmators of Planck and random uniform catalogs applied maskand selection function 0.30 ŵdd/rr ŵdd/dr 0.25 ŵls σŵdd/rr 0.20 σŵdd/rr σŵls Angular distance [degrees] Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 9 / 16

12 Current results Comparing 3 estimators Fake cluster catalog and random cluster catalogs, both with the Planck mask applied and selection function. Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 10 / 16

13 Current results Comparing 3 estimators Planck cluster catalog and random catalogs with the Planck mask applied and selection function Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 11 / 16

14 Current results Expect for detection of Baryon acoustic oscillations Acoustic wave propagating in the early universe due to the counteracting forces of radiation pressure and gravity. The standard ruler for length scale in cosmology. Study the dark energy by constraining cosmological parameters. (SDSS) - Eisenstein et al., 2005 (SDSS) - G. C. Carvalho et al., 2015 Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 12 / 16

15 Current results Expect for detection of Baryon acoustic oscillations Acoustic wave propagating in the early universe due to the counteracting forces of radiation pressure and gravity. The standard ruler for length scale in cosmology. Study the dark energy by constraining cosmological parameters. 140 Redshift distribution of 926 Planck MMF3 clusters (SDSS) - Eisenstein et al., 2005 Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 12 / 16

16 Current results Ongoing work: Two-point correlation at smaller scale High correlation around 10 degrees -> Expect to find the BAO signal Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 13 / 16

17 Conclusion High correlation of clusters at small angular scale. The distribution of Planck cluster catalog produce significant signal from the departure of the uniform distribution. The DD/DR estimator has the smallest dispersion, then following by the estimator DR, and the Landy-Szalay estimator respectively. Expect for the detection of BAO signal at angular scale around 10 degrees. Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 14 / 16

18 Conclusion Future work Estimating the angular correlation function with Euclid requires many steps (as work was needed to produce the Planck cluster catalog) : Calibrate and clean images Find galaxies in images and measure their photometry Measure their distances (or redshift) using spectroscopic and photometric redshift methods. Identify clusters Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 15 / 16

19 Conclusion Thank you for your attention! Study the large-scale structure of the universenovember using galaxy 10, 2016 clusters 16 / 16

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