Cosmic Homogeneity as standard ruler Pierros Ntelis
Collaborators: J. Rich .97 J.C. Hamilton )=2 H ( J.M. Le Goff 2 R A.Ealet D S. Escoffier A.J. Hawken A. Tilquin
Post Doc Aix-Marseille University, CPPM
P. Ntelis 2nd Colloque National DE, October 2018 s. 1 Cosmic Homogeneity as standard ruler What can fractality tell us about the universe?
Romansco Broccoli, Italy since 16th c.
) Simulation ( )= Euclid (r 2 eBOSS LSST DESI D P. Ntelis 2nd Colloque National DE, October 2018 s. 2 Cosmic Homogeneity as standard ruler Outline ΛCDM Phenomenology Challenges of Cosmological Principle Standard Rulers and Candles Homogeneity scale as a standard Ruler Conclusion and Outlook P. Ntelis 2nd Colloque National DE, October 2018 s. 3 Cosmic Homogeneity as standard ruler Statistical On enough Standard Homogeneity Cosmological Principle = large Phenomenology ΛCDM + scales Isotropy Non Homogeneous + Isotropic Homogeneous + Isotropic M.Stolpovskiy P. Ntelis 2nd Colloque National DE, October 2018 s. 4 Cosmic Homogeneity as standard ruler Standard 4 4 R Least EH = c d xp g Phenomenology ΛCDM S 16⇡G Action Z Principle Gµ⌫ Tµ⌫ Metric Ansatz / Perturbed g g¯ + g Einstein-Boltzmann µ⌫ ' µ⌫ µ⌫ Equations + X, Cosmic Components, (b,CDM,DE,…) f (~x, p,~ t)= [ f (~x, p,~ t)] Dt X C X 8 coupled non linear differential P. Ntelis 2nd Colloque National DE, October 2018 s. 5 Cosmic Homogeneity as standard ruler 5 % 26 % 69 % Perturbed Planck SDSS 2018 ++ Equations Boltzmann-Einstein Cosmological Principle Homogeneous + Isotropic P. Ntelis 2nd Colloque National DE, October 2018 s. 6 Cosmic Homogeneity as standard ruler standard ΛCDM phenomenology Basic aspects of this model: -Initial Conditions: Primordial fluctuations, Inflation? -Expansion -Acceleration -Statistical homogeneity and isotropy on large scales -Baryon Acoustic Oscillations (BAO) Cosmological Constant Problem Can these phenomenological aspects, be described in a better way than standard GR, Λ? P. Ntelis 2nd Colloque National DE, October 2018 s. 7 Cosmic Homogeneity as standard ruler Outline ΛCDM Phenomenology Challenges of Cosmological Principle Standard Rulers and Candles Homogeneity scale as a standard Ruler Conclusion and Outlook P. Ntelis 2nd Colloque National DE, October 2018 s. 8 Cosmic Homogeneity as standard ruler Challenges of Cosmologically Principled Universes: A historical list of large scale structures(LSS): Year Name Size (Mpc) Detection Method Notes Dedication 1983 Webster (5)LQG 100 no-info no-info A.Webster spectro-z, percolation analysis Pisces-Cetus 1987 350 L0=70 h-1 Mpc, 10 members, h=75 R.B.Tully SuperCluster Complex L>L0 no significant 1987 Giand Void 350 L0=200 h-1 Mpc, Spectro-z, FoF Flat, Λ=0, Η0=50km/s/Mpc,q0=0.5 A.I.Kopylov et al. 1989 Great Wall 240 spectro-z blocked by MW gal plain Hunchra & Geller 2003 Sloan Great Wall 420 By comparison of Great Wall Flat J.R.Gott 2006 Newfound Blob 65 FOCAS,Subaru, Lya emitters Flat,0.3,0.70,z~3.1 0510762v1 2007 Super Void 140 NVSS, Waveletes+ISW, Close to cmb cold Spot Rudnick et al. Counts+Brighnes 0704.0908v2 2012 Huge CC (73)LQG 500/1240 SDSS, FoF,L0=100 h70-1Mpc Flat,0.27,0.73,1.0 SGRBM, γ-Ray Bursts, (θφ)-KS test, 2013 Hecules-CoronaBorelis 2.2Gpc h=0.6780 1311.1104 z-independent 2014 Lianakea 160h-1 Velocities Wiener Filter no-info 1409.0880v1 2016 BOSS Great Wall 271 h-1 SDSS, 8h-1Mpc smoothing , L>5L0 Flat,0.27,0.73,z~0.47 1602.08498v1 P. Ntelis 2nd Colloque National DE, October 2018 s. 9 Cosmic Homogeneity as standard ruler Challenges of Cosmologically Principled Universes: R.B.Tully et al. 2014 zmax < 0.1 our neighbourhood YOU! P. Ntelis 2nd Colloque National DE, October 2018 s. 10 Cosmic Homogeneity as standard ruler Challenges of Cosmologically Principled Universes: QSO quasi our neighbourhood stellar objects ELG Emission Line Galaxies LRG Luminous Red Galaxies CMASS YOU! Lianakea LRG Luminous 1703.00052 Red Galaxies SDSS-IV SDSS-IV telescope P. Ntelis 2nd Colloque National DE, October 2018 s. 11 Cosmic Homogeneity as standard ruler Challenges of Cosmologically Principled Universes: Fractal Universe and cosmic acceleration arXiv:1810.06318 in a LTB scenario: SN-Ia no Λ, re-analyses UNION2 The projected mass distribution and the arXiv:1810.03539 transition to homogeneity: Gal-Clustering FLRW, re-analyses SDSS DR7 Cosmological Principle is not in the arXiv:1611.02139 sky: Gal-Clustering FLRW, re-analyses SDSS DR7 P. Ntelis 2nd Colloque National DE, October 2018 s. 12 Cosmic Homogeneity as standard ruler Challenges of Cosmologically Principled Universes: Information only on the past lightcone, c finite Cosmology dependence (Redshift ->Distance) Redshift Space Distortions (Gravity, Kaiser, FoG) Inspired by F.Leclercq et al. 2014 Galaxies are biased tracers of matter δ (Cosmic Bias quantifies the -1 galaxy-type r [h Mpc] δtracer = b δmatter selection) YOU! ξtracer = b2 ξmatter By the way RHtracer = bRH RHMatter, NEW! P. Ntelis 2nd Colloque National DE, October 2018 s. 13 Cosmic Homogeneity as standard ruler Outline ΛCDM Phenomenology Challenges of Cosmological Principle Standard Rulers and Candles Homogeneity scale as a standard Ruler Conclusion and Outlook P. Ntelis 2nd Colloque National DE, October 2018 s. 14 Cosmic Homogeneity as standard ruler Standard Candles and Rulers Standard Candles (1998) Standard Rulers (2005) Riess, Schmidt, Perlmutter Eisenstein et al, ++ acceleration 2011 ΔΤ/Τ SN-Ia BAO peak position CMB Same Lmax at explosion z,t at diff z,t Improve Cosmology ,CMB Δρ/ρ wiki 1703.00052 SDSS-IV BAO peak position BAO peak Planck 2015 On Ωk =0 @ % C.L. P. Ntelis 2nd Colloque National DE, October 2018 s. 15 Cosmic Homogeneity as standard ruler Outline ΛCDM Phenomenology Challenges of Cosmological Principle Standard Rulers and Candles Homogeneity scale as a standard Ruler Conclusion and Outlook P. Ntelis 2nd Colloque National DE, October 2018 s. 16 Cosmic Homogeneity as standard ruler Gal Improved cosmological understanding P( Ω , δΩ ) Improved cosmological Constraints CMB HOW? P. Ntelis 2nd Colloque National DE, October 2018 s. 17 Cosmic Homogeneity as standard ruler r D Counts-in-Spheres: N( Homogeneous @ large scales D2(r)=3 Inhomogeneous @ small scales (clustering) D2(r) < 3 Transition to Homogeneity at: D2(RH ) = 3 @ 1% (Arbitrary Choice; Independent of survey) P. Ntelis 2nd Colloque National DE, October 2018 s. 18 Cosmic Homogeneity as standard ruler Measurement: • Use of CMASS galaxy sample of SDSS/BOSS • Small Scale: • clustering • fractality • Large scales: • asymptotic smoothness 1000 QPM catalogues • Confirmation of —> RHth = 62.9 h-1Mpc • ΛCDM model • Cosmological Principle • Exclusion of fractal models @ LSS P.Ntelis et al. arXiv:1702.02159 P. Ntelis 2nd Colloque National DE, October 2018 s. 19 Cosmic Homogeneity as standard ruler P.Ntelis et al. 2017 Euclid 2022 Redshift evolution of homogeneity P. Ntelis 2nd Colloque National DE, October 2018 s. 20 Cosmic Homogeneity as standard ruler QPM-mock for CMASS DR12 of BOSS/SDSS Ameliorate Cosmology! P.Ntelis et al. arXiv:1810.09362 P. Ntelis 2nd Colloque National DE, October 2018 s. 21 Cosmic Homogeneity as standard ruler Outline ΛCDM Phenomenology Challenges of Cosmological Principle Standard Rulers and Candles Homogeneity scale as a standard Ruler Conclusion and Outlook P. Ntelis 2nd Colloque National DE, October 2018 s. 22 Thank you for your Attention! Conclusions -New complementary cosmological ruler, RH! -RH Improves the precision on Ωk , (Ωm,ΩΛ) - D2 Exclude fractal universes at large scales - D2 Exclude inhomogeneous universe at large scales - D2 Confirmation of ΛCDM phenomenology in ~% level - D2 Confirmation of Cosmological Principle P.Ntelis et al. ’18 arXiv:1810.09362 P.Ntelis et al. ’17 arXiv:1702.02159 Outlook RH cosmo-implications analysis is applicable on: - QSO, ELG, (BBH …), … - CMB TT map - Cosmic Web (Nodes, Filaments, Sheets, Voids) - SuperNovae Clustering? - Modifications of Gravity Models, (w, γ, … ) P. Ntelis 2nd Colloque National DE, October 2018 s. 23 Cosmic Homogeneity as standard ruler Back Up P. Ntelis 2nd Colloque National DE, October 2018 s. 24 Cosmic Homogeneity as standard ruler Correlation, r~0.2 |r(z)| <0.3 P. Ntelis 2nd Colloque National DE, October 2018 s. 25 Cosmic Homogeneity as standard ruler Build the chi2 square MCMC method according to: χ2(Α,Β,pT;pF)= (Data) (Theoretical model) with Where dV is the volume distance, pT = (Ωm,ΩΛ) 1+z B and F, stands for Fiducial (fixed parameters) b(z, A, B)=A 1+zm T, stands for the True (parameters we explore) P. Ntelis 2nd Colloque National DE, October 2018 s. 26 Cosmic Homogeneity as standard ruler Bias Dependence Matter < - - - Galaxies gal(r) 3 mat(r)=D2 +3 Precision increase: D2 b2 - M G Smaller Scales M = G 2 D2 D2 + 3(b 1) - Bias Gain RHG = 121 ± 11.4h-1Mpc RHM = 61.9 ± 0.8h-1Mpc P. Ntelis 2nd Colloque National DE, October 2018 s. 27 Cosmic Homogeneity as standard ruler 2 RH 1 @ RH (z) Fij = 2 @✓i@✓j RH gal z X 2 BAO 1 @ rs(z) Fij = 2 @✓i@✓j rs gal z X Error as estimated by CMASS analysis P. Ntelis 2nd Colloque National DE, October 2018 s. 28 Cosmic Homogeneity as standard ruler Fisherology: Results 68 % CMB +RH +BAO δΩΛ 0.06 0.04 0.03 δw0 0.3 0.2 0.2 P. Ntelis 2nd Colloque National DE, October 2018 s. 29 Cosmic Homogeneity as standard ruler Qualitative comparison Black Blue P.Ntelis et al. arXiv:1810.09362 J.Bautista et al., arXiv:1702.00176 P. Ntelis 2nd Colloque National DE, October 2018 s. 30 Cosmic Homogeneity as standard ruler Weak challenging signal of gal-clustering in the back ground of gravitational waves https://journals.aps.org/prd/pdf/10.1103/PhysRevD.86.083512 Why not clustering from BBH? P. Ntelis 2nd Colloque National DE, October 2018 s. 31 Cosmic Homogeneity as standard ruler Back Up P. Ntelis 2nd Colloque National DE, October 2018 s. 32