BAO analysis from the DR14 QSO sample

BAO analysis from the DR14 QSO sample Héctor Gil-Marín (on behalf of the eboss QC WG) Laboratoire de Physique Nucleaire et de Hautes Energies (LPNHE) Institut Lagrange de Paris (ILP) Understanding Cosmological Observations @ Benasque 1st Aug 2017

Public DR14 data (yesterday!) arxiv:1707.09322 We re very happy to report that the fourteenth data release of SDSS is now live!!! Go have a look at www.sdss.org/dr14, and tell all your friends and colleagues that this awesome data set is now available for them to play with!

The eboss survey : the eboss survey Apache Point Observatory (APO) 2.5-m telescope. SDSS-III project. 2009-2014 BOSS: Baryon Oscillation Spectroscopic Survey SDSS-IV project. 2014-2019 eboss: extended Baryon Oscillation Spectroscopic Survey 3 galaxy clustering programs (ELG, LRG, quasars) + Ly-α new selection algorithms to identify redshift of galaxies BOSS had 99% success rate identifying redshifts of LRGs first eboss tests showed 70% of success rate on LRGs using same BOSS algorithms! Understanding Cosmological Observations @ Benasque, 1st Aug 2017 BAO from the DR14 QSO sample

The eboss survey : the eboss survey eboss survey: ELG, LRG and QSO samples LRG 0.6 < z < 1.0; z eff = 0.71. ELG 0.6 < z < 1.1; z eff = 0.85. QSO 0.8 < z < 2.2; z eff = 1.5. Ly-α z eff = 2.33 [Credit : Anand Raichoor]

The eboss survey : the eboss survey

The eboss survey : the eboss survey 0.7 0.6 assuming Planck ΛCDM cosmology eboss year 6 Planck ΛCDM f σ8(z) 0.5 0.4 0.3 0.2 BOSS DR12 6dFGS SDSS MGS GAMA WiggleZ Vipers 0.2 0.4 0.6 0.8 1.0 1.2 1.4 1.6 z

The eboss survey Low Density of Quasars! Shot noise dominated covariance matrices (traditional) Reconstruction algorithms do not provide much signal gain

The eboss survey : the eboss survey QSO DR14 area 2044 deg 2. quasar range: 0.8 < z < 2.2 (z eff 1.5) Number quasars: 147,000 Low density: 2 10 5 [Mpc/h] 3 3 disconnected areas: 2 SGC & NGC.

The eboss survey : the eboss survey Alphabetical paper Ata et al. 2017 submitted to the Journal arxiv:1705.06373 First in 0.8 z 2.2 D V = 3855 ± 170 r d /r d,fid Mpc at z=1.52 (4.4% precision) 2.5σ BAO significance DR14 Area: 2044 4.4% precision DR16 Area: 5300 2.7% precision eboss is working!

Alcock-Paczynski effect Alcock-Paczynski effect Methodology Measurement Systematic Tests By assuming a wrong cosmological model (Ω m ) we change the line-of-sight clustering respect to the angular clustering, creating a measurable anisotropy: constrains H(z) and D A (z) (or a combination of both). d comov (z) = z 0 cdz H(z ; Ω m ) The BAO scale is determined by the comoving sound horizon at reconvination scale (standard ruler) r s = 1 H 0 Ω 1/2 m a 0 da c s (a + a eq ) 1/2

Baryonic Acoustic Oscillations Alcock-Paczynski effect Methodology Measurement Systematic Tests k α k α = Hfid (z) H(z) k α k α = D A(z) D fid A (z) [Anderson et al. 2014, BOSS DR11] Surveys measure angles and redshifts, and these are affected by the assumed fiducial model. This changes the apparent/observed position of the BAO peak in the power spectrum differently in the radial and angular direction Isotropic Correlation Function / Power Spectrum sensitive to D V (z) = [ ] (1 + z) 2 DA 2 cz 1/3 (z) H(z)

Methodology Alcock-Paczynski effect Methodology Measurement Systematic Tests We perform two complementary and independent analyses on the same dataset using the i) Power Spectrum and ii) Correlation Function. Both observables should contain the same amount of information, but in practice are affected differently by noise and systematic effects. We use mocks (1000 EZ mocks) and (400 QPM mocks) to estimate the covariance matrices and perform systematic tests. We model the broadband shape of the PS/CF phenomenologically and the BAO as linear+damping (Σ nl ) P(k, α) = P sm (k) {1 + [O lin (k/α) 1] e 1 2 Σ2 k2} nl smooth PS: P sm (k) B 2 P lin nw(k) + A 1 k + A 2 + A 3 /k

Measurement Alcock-Paczynski effect Methodology Measurement Systematic Tests DR14 QSO isotropic Power spectrum and Correlation function 1200 1000 SGC, χ 2 /dof =22.1/27 NGC, χ 2 /dof =33.2/27 100 80 60 SGC, χ 2 /dof =28.3/24 NGC, χ 2 /dof =21.0/24 kp0(k) (h 2 Mpc 2 ) 800 600 400 s 2 ξ0(s) (h 2 Mpc 2 ) 40 20 0 20 40 200 0.05 0.10 0.15 0.20 0.25 0.30 k (hmpc 1 ) 60 80 25 50 75 100 125 150 175 200 s (h 1 Mpc) Actual data + diagonal errors from EZ mocks. Dashed lines mean of the EZ-mocks

Measurement Alcock-Paczynski effect Methodology Measurement Systematic Tests DR14 QSO isotropic Power spectrum and Correlation function 10(P Psmooth)/Psmooth 1.5 1.0 0.5 0.0 0.5 1.0 1.5 0.05 0.10 0.15 0.20 k(hmpc 1 ) 10 3 (ξ[s] ξsmooth) 4 2 0 2 4 25 50 75 100 125 150 175 s (h 1 Mpc) Actual data + diagonal errors from EZ mocks. Solid lines best-fit model

Tests on Mocks Alcock-Paczynski effect Methodology Measurement Systematic Tests Power Spectrum α 1.15 1.10 1.05 1.00 0.95 0.90 DR14 Mocks Power Spectrum σ(α) 0.08 0.07 0.06 0.05 0.04 0.03 0.85 0.85 0.90 0.95 1.00 1.05 1.10 1.15 Correlation Function α 0.02 0.02 0.03 0.04 0.05 0.06 0.07 0.08 Correlation Function σ(α) Correlation coefficient between PS and CF ρ = 0.97. Data is a very typical case of mocks (both in measurement and error).

Tests on Mocks Alcock-Paczynski effect Methodology Measurement Systematic Tests NL effects shift the BAO peak to higher α. 0.1% effect on measured α. Negligible on data!

Tests on data Alcock-Paczynski effect Methodology Measurement Systematic Tests Both P(k) and ξ(s) measurements are very consistent! 16 14 12 ξ(s) P (k) P (k) + ξ(s) χ 2 10 8 3σ 6 4 2 0 2σ 1σ 0.8 0.9 1.0 1.1 1.2 α BAO

Cosmology Alcock-Paczynski effect Methodology Measurement Systematic Tests Fully consistent with LCDM + Planck. Ly-α 2.5 measurement dominates at high z. Further analyses will focus on redshift weighting schemes. Distance/Distance(PlanckΛCDM) 1.05 1.00 0.95 SDSS MGS WiggleZ BOSS DR12 6dFGS DR14 quasars BOSS Lyα 0.0 0.5 1.0 1.5 2.0 2.5 Redshift

BAO Summary Alcock-Paczynski effect Methodology Measurement Systematic Tests Summary, We have a robust BAO isotropic measurement at z 1.5. with 4.4% precision: D V (1.52) = 3855 ± 170 r d /r d,fid Mpc. Very consistent with mocks and between P and ξ observables. Fully consistent with LCDM+Planck

BAO Summary Alcock-Paczynski effect Methodology Measurement Systematic Tests Summary, We have a robust BAO isotropic measurement at z 1.5. with 4.4% precision: D V (1.52) = 3855 ± 170 r d /r d,fid Mpc. Very consistent with mocks and between P and ξ observables. Fully consistent with LCDM+Planck First BAO science result from WG, but not last one. More complex BAO analyses will be done in the forthcoming months (weighting z evolution). Future quasar releases (DR16) will focus on the anisotropic quasar BAO Constrain D A and H. Further information on D V can be extracted from RSD analysis (several papers to be released this Fall)

The main difficulty when performing RSD analyses is controlling the observational systematic effects. Such effects have minor effect on the position of the BAO (given the current errorbars), but they turn to be more important for RSD analyses, Failure rate as a function of the plate position. Spectroscopic errors. Estimate of the quasar redshift using different algorithms.

45 40 35 30 25 20 15 10 5 0 Failure rate in NGC 0 5 10 15 20 25 30 35 40 45 1 0.95 0.9 0.85 0.8 0.75 10% failure rate

45 40 35 30 25 20 15 10 5 0 Failure rate in NGC 0 5 10 15 20 25 30 35 40 45 1 0.98 0.96 0.94 0.92 0.9 0.88 0.86 3.5% failure rate

Why do the quasars always fail at the same plate positions? [Credit: P. Zarrouk]

Even with 3.5% failure rate, applying the nearest angular neighbour reduces the amplitude of the monopole and enhances the quadrupole signal significantly. As a consequence, f σ 8 is affected by 0.7σ. BAO not affected α iso S α f σ 8 S f σ8 N det EZ x i 1.64 ± 0.13-1.43 ± 0.16 - - EZ x i 1.6 ± 4.4 4.8 1.4 ± 4.9 5.5 979 EZ x i w col 1.90 ± 0.13-2.24 ± 0.17 - - EZ x i w col 1.7 ± 4.4 4.6 2.4 ± 5.4 5.4 959 (units of the table in 10 2 ). Better correction than just up-weight the nearest neighbour is needed!

Quasar Clustering Working Group Report Current RSD & BAO projects DR14 QSO sample Gil-Marin et al. Fourier Space Multipoles RSD Hou et al. Configuration Space Wedges RSD Ruggeri et al. Fourier Space Multipoles with z-weights RSD Wang et al. Fourier Space Multipoles with z-weights BAO Zarrouk et al. Configuration Space Multipoles RSD Zhao et al. Fourier Space Multipoles with z-weights RSD Zhu et al. Configuration Space Multipoles with z-weights BAO WG is currently focused on Producing reliable mocks for covariance matrix Building appropriate weighting scheme for correcting redshift failures and close pairs.

Thank you! Understanding Cosmological Observations @ Benasque, 1st Aug 2017 BAO from the DR14 QSO sample