scholarly journals Testing general relativity on cosmological scales at redshift z ∼ 1.5 with quasar and CMB lensing

2020 ◽  
Vol 501 (1) ◽  
pp. 1013-1027
Author(s):  
Yucheng Zhang ◽  
Anthony R Pullen ◽  
Shadab Alam ◽  
Sukhdeep Singh ◽  
Etienne Burtin ◽  
...  
Keyword(s):  
General Relativity ◽  
Power Spectrum ◽  
Large Scale ◽  
Sloan Digital Sky Survey ◽  
Gravity Models ◽  
Distortion Parameter ◽  
Angular Power Spectrum ◽  
Sigma Level ◽  
Order Of Magnitude ◽  
Best Fitting

ABSTRACT We test general relativity (GR) at the effective redshift $\bar{z} \sim 1.5$ by estimating the statistic EG, a probe of gravity, on cosmological scales $19 - 190\, h^{-1}{\rm Mpc}$. This is the highest redshift and largest scale estimation of EG so far. We use the quasar sample with redshifts 0.8 < z < 2.2 from Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey Data Release 16 as the large-scale structure (LSS) tracer, for which the angular power spectrum $C_\ell ^{qq}$ and the redshift-space distortion parameter β are estimated. By cross-correlating with the Planck 2018 cosmic microwave background (CMB) lensing map, we detect the angular cross-power spectrum $C_\ell ^{\kappa q}$ signal at $12\, \sigma$ significance. Both jackknife resampling and simulations are used to estimate the covariance matrix (CM) of EG at five bins covering different scales, with the later preferred for its better constraints on the covariances. We find EG estimates agree with the GR prediction at $1\, \sigma$ level over all these scales. With the CM estimated with 300 simulations, we report a best-fitting scale-averaged estimate of $E_G(\bar{z})=0.30\pm 0.05$, which is in line with the GR prediction $E_G^{\rm GR}(\bar{z})=0.33$ with Planck 2018 CMB + BAO matter density fraction Ωm = 0.31. The statistical errors of EG with future LSS surveys at similar redshifts will be reduced by an order of magnitude, which makes it possible to constrain modified gravity models.

scholarly journals Estimating the large-scale angular power spectrum in the presence of systematics: a case study of Sloan Digital Sky Survey quasars

2013 ◽  
Vol 435 (3) ◽  
pp. 1857-1873 ◽  
Author(s):  
Boris Leistedt ◽  
Hiranya V. Peiris ◽  
Daniel J. Mortlock ◽  
Aurélien Benoit-Lévy ◽  
Andrew Pontzen
Keyword(s):  
Power Spectrum ◽  
Large Scale ◽  
Sloan Digital Sky Survey ◽  
Angular Power Spectrum ◽  
Sky Survey

scholarly journals An Accurate Reconstruction of CMB E Mode Signal over Large Angular Scales using Prior Information of CMB Covariance Matrix in ILC Algorithm

2020 ◽  
Author(s):  
Ujjal Purkayastha ◽  
Vipin Sudevan ◽  
Rajib Saha
Keyword(s):  
Power Spectrum ◽  
Linear Combination ◽  
Covariance Matrix ◽  
Large Scale ◽  
Prior Information ◽  
Future Generation ◽  
Temperature Anisotropy ◽  
Satellite Mission ◽  
Angular Power Spectrum ◽  
Accurate Reconstruction

Abstract Recently, the internal-linear-combination (ILC) method was investigated extensively in the context of reconstruction of Cosmic Microwave Background (CMB) temperature anisotropy signal using observations obtained by WMAP and Planck satellite missions. In this article, we, for the first time, apply the ILC method to reconstruct the large scale CMB E mode polarization signal, which could probe the ionization history, using simulated observations of 15 frequency CMB polarization maps of future generation Cosmic Origin Explorer (COrE) satellite mission. We find that the clean power spectra, from the usual ILC, are strongly biased due to non zero CMB-foregrounds chance correlations. In order to address the issues of bias and errors we extend and improve the usual ILC method for CMB E mode reconstruction by incorporating prior information of theoretical E mode angular power spectrum while estimating the weights for linear combination of input maps (Sudevan & Saha 2018b). Using the E mode covariance matrix effectively suppresses the CMB-foreground chance correlation power leading to an accurate reconstruction of cleaned CMB E mode map and its angular power spectrum. We compare the performance of the usual ILC and the new method over large angular scales and show that the later produces significantly statistically improved results than the former. The new E mode CMB angular power spectrum contains neither any significant negative bias at the low multipoles nor any positive foreground bias at relatively higher mutlipoles. The error estimates of the cleaned spectrum agree very well with the cosmic variance induced error.

scholarly journals The Angular Power Spectrum of Galaxies from Early Sloan Digital Sky Survey Data

2002 ◽  
Vol 571 (1) ◽  
pp. 191-205 ◽  
Author(s):  
Max Tegmark ◽  
Scott Dodelson ◽  
Daniel J. Eisenstein ◽  
Vijay Narayanan ◽  
Roman Scoccimarro ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Survey Data ◽  
Sloan Digital Sky Survey ◽  
Angular Power Spectrum ◽  
Sky Survey

scholarly journals Clustering properties of TGSS radio sources

2019 ◽  
Vol 623 ◽  
pp. A148 ◽  
Author(s):  
Arianna Dolfi ◽  
Enzo Branchini ◽  
Maciej Bilicki ◽  
Andrés Balaguera-Antolínez ◽  
Isabella Prandoni ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Large Scale ◽  
Angular Spectrum ◽  
Radio Sources ◽  
Angular Power Spectrum ◽  
Sky Survey ◽  
Systematic Effects ◽  
Angular Correlation Function ◽  
Multiple Component ◽  
Anomalous Nature

We investigate the clustering properties of radio sources in the Alternative Data Release 1 of the TIFR GMRT Sky Survey (TGSS), focusing on large angular scales, where previous analyses have detected a large clustering signal. After appropriate data selection, the TGSS sample we use contains ∼110 000 sources selected at 150 MHz over ∼70% of the sky. The survey footprint is largely superimposed on that of the NRAO VLA Sky Survey (NVSS) with the majority of TGSS sources having a counterpart in the NVSS sample. These characteristics make TGSS suitable for large-scale clustering analyses and facilitate the comparison with the results of previous studies. In this analysis we focus on the angular power spectrum, although the angular correlation function is also computed to quantify the contribution of multiple-component radio sources. We find that on large angular scales, corresponding to multipoles 2 ≤ ℓ ≤ 30, the amplitude of the TGSS angular power spectrum is significantly larger than that of the NVSS. We do not identify any observational systematic effects that may explain this mismatch. We have produced a number of physically motivated models for the TGSS angular power spectrum and found that all of them fail to match observations, even when taking into account observational and theoretical uncertainties. The same models provide a good fit to the angular spectrum of the NVSS sources. These results confirm the anomalous nature of the TGSS large-scale power, which has no obvious physical origin and seems to indicate that unknown systematic errors are present in the TGSS dataset.

scholarly journals The Sloan Digital Sky Survey Data Release 7 galaxy angular power spectrum

2012 ◽  
Vol 421 (3) ◽  
pp. 2043-2053 ◽  
Author(s):  
Brett Hayes ◽  
Robert Brunner ◽  
Ashley Ross
Keyword(s):  
Power Spectrum ◽  
Survey Data ◽  
Sloan Digital Sky Survey ◽  
Angular Power Spectrum ◽  
Sky Survey ◽  
Data Release

scholarly journals The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the BAO and growth rate of structure of the emission line galaxy sample from the anisotropic power spectrum between redshift 0.6 and 1.1

2020 ◽  
Author(s):  
Arnaud de Mattia ◽  
Vanina Ruhlmann-Kleider ◽  
Anand Raichoor ◽  
Ashley J Ross ◽  
Amélie Tamone ◽  
...  
Keyword(s):  
Growth Rate ◽  
Power Spectrum ◽  
Emission Line ◽  
Large Scale ◽  
Sloan Digital Sky Survey ◽  
Full Data ◽  
Data Set ◽  
Weak Preference ◽  
Galaxy Sample ◽  
Emission Line Galaxies

Abstract We analyse the large-scale clustering in Fourier space of emission line galaxies (ELG) from the Data Release 16 of the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey. The ELG sample contains 173,736 galaxies covering 1,170 square degrees in the redshift range 0.6 < z < 1.1. We perform a BAO measurement from the post-reconstruction power spectrum monopole, and study redshift space distortions (RSD) in the first three even multipoles. Photometric variations yield fluctuations of both the angular and radial survey selection functions. Those are directly inferred from data, imposing integral constraints which we model consistently. The full data set has only a weak preference for a BAO feature (1.4σ). At the effective redshift zeff = 0.845 we measure $D_{\rm V}(z_{\rm eff})/r_{\rm drag} = 18.33_{-0.62}^{+0.57}$, with DV the volume-averaged distance and rdrag the comoving sound horizon at the drag epoch. In combination with the RSD measurement, at zeff = 0.85 we find $f\sigma _8(z_{\rm eff}) = 0.289_{-0.096}^{+0.085}$, with f the growth rate of structure and σ8 the normalisation of the linear power spectrum, $D_{\rm H}(z_{\rm eff})/r_{\rm drag} = 20.0_{-2.2}^{+2.4}$ and DM(zeff)/rdrag = 19.17 ± 0.99 with DH and DM the Hubble and comoving angular distances, respectively. These results are in agreement with those obtained in configuration space, thus allowing a consensus measurement of fσ8(zeff) = 0.315 ± 0.095, $D_{\rm H}(z_{\rm eff})/r_{\rm drag} = 19.6_{-2.1}^{+2.2}$ and DM(zeff)/rdrag = 19.5 ± 1.0. This measurement is consistent with a flat ΛCDM model with Planck parameters.

scholarly journals Inflation story: slow-roll and beyond

2021 ◽  
Vol 2021 (12) ◽  
pp. 038
Author(s):  
Dhiraj Kumar Hazra ◽  
Daniela Paoletti ◽  
Ivan Debono ◽  
Arman Shafieloo ◽  
George F. Smoot ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Large Scale ◽  
Microwave Background ◽  
Angular Power Spectrum ◽  
Slow Roll ◽  
Primordial Power Spectrum ◽  
Cosmic Microwave Background Temperature ◽  
Scale Temperature ◽  
Temperature Polarization ◽  
Background Temperature

Abstract We present constraints on inflationary dynamics and features in the primordial power spectrum of scalar perturbations using the Cosmic Microwave Background temperature, polarization data from Planck 2018 data release and updated likelihoods. We constrain the slow-roll dynamics using Hilltop Quartic Potential and Starobinsky R + R 2 model in the Einstein frame using the Planck 2018 binned Plik likelihood. Using the Hilltop as base potential, we construct Whipped Inflation potential to introduce suppression in the scalar power spectrum at large angular scales. We notice marginal (68% C.L.) preference of suppression from the large scale temperature angular power spectrum. However, large-scale E-mode likelihood based on high frequency instrument cross spectrum, does not support this suppression and in the combined data the preference towards the suppression becomes negligible. Based on the Hilltop and Starobinsky model, we construct the Wiggly Whipped Inflation potentials to introduce oscillatory features along with the suppression. We use unbinned data from the recently released CamSpec v12.5 likelihood which updates Planck 2018 results. We compare the Bayesian evidences of the feature models with their baseline slow-roll potentials. We find that the complete slow-roll baseline potential is moderately preferred against potentials which generate features. Compared to Planck 2015 PlikHM bin1 likelihood, we find that the significance of sharp features has decreased owing to the updates in the data analysis pipeline. We also compute the bispectra for the best fit candidates obtained from our analysis.

scholarly journals Unraveling the nature of gravity through our clumpy universe

2014 ◽  
Vol 23 (12) ◽  
pp. 1442025 ◽  
Author(s):  
Shant Baghram ◽  
Saeed Tavasoli ◽  
Farhang Habibi ◽  
Roya Mohayaee ◽  
Joseph Silk
Keyword(s):  
General Relativity ◽  
Large Scale ◽  
Sloan Digital Sky Survey ◽  
Peculiar Velocities ◽  
Large Scale Data ◽  
Cosmological Observations ◽  
Sky Survey ◽  
Scale Data

We propose a new probe to test the nature of gravity at various redshifts through large-scale cosmological observations. We use our void catalog, extracted from the Sloan Digital Sky Survey (SDSS, DR10), to trace the distribution of matter along the lines of sight to SNe Ia that are selected from the Union II catalog. We study the relation between SNe Ia luminosities and convergence and also the peculiar velocities of the sources. We show that the effects, on SNe Ia luminosities, of convergence and of peculiar velocities predicted by the theory of general relativity and theories of modified gravities are different and hence provide a new probe of gravity at various redshifts. We show that the present sparse large-scale data does not allow us to determine any statistically-significant deviation from the theory of general relativity but future more comprehensive surveys should provide us with means for such an exploration.

scholarly journals KiDS + GAMA: constraints on horndeski gravity from combined large-scale structure probes

2019 ◽  
Vol 490 (2) ◽  
pp. 2155-2177 ◽  
Author(s):  
A Spurio Mancini ◽  
F Köhlinger ◽  
B Joachimi ◽  
V Pettorino ◽  
B M Schäfer ◽  
...  
Keyword(s):  
Dark Energy ◽  
Large Scale ◽  
Gravity Models ◽  
Dark Energy Density ◽  
Modelling Uncertainty ◽  
Matter Power Spectrum ◽  
Downward Shift ◽  
The Galaxy ◽  
Best Fitting ◽  
Mass Assembly

ABSTRACT We present constraints on Horndeski gravity from a combined analysis of cosmic shear, galaxy–galaxy lensing and galaxy clustering from $450\, \mathrm{deg}^2$ of the Kilo-Degree Survey and the Galaxy And Mass Assembly survey.The Horndeski class of dark energy/modified gravity models includes the majority of universally coupled extensions to ΛCDM with one scalar field in addition to the metric. We study the functions of time that fully describe the evolution of linear perturbations in Horndeski gravity. Our results are compatible throughout with a ΛCDM model. By imposing gravitational wave constraints, we fix the tensor speed excess to zero and consider a subset of models including, e.g. quintessence and f(R) theories. Assuming proportionality of the Horndeski functions αB and αM (kinetic braiding and the Planck mass run rate, respectively) to the dark energy density fraction ΩDE(a) = 1 − Ωm(a), we find for the proportionality coefficients $\hat{\alpha }_\mathrm{ B} = 0.20_{-0.33}^{+0.20} \,$ and $\, \hat{\alpha }_\mathrm{ M} = 0.25_{-0.29}^{+0.19}$. Our value of $S_8 \equiv \sigma _8 \sqrt{\Omega _{\mathrm{m}}/0.3}$ is in better agreement with the Planck estimate when measured in the enlarged Horndeski parameter space than in a pure ΛCDM scenario. In our joint three-probe analysis, we report a downward shift of the S8 best-fitting value from the Planck measurement of $\Delta S_8 = 0.016_{-0.046}^{+0.048}$ in Horndeski gravity, compared to $\Delta S_8 = 0.059_{-0.039}^{+0.040}$ in ΛCDM. Our constraints are robust to the modelling uncertainty of the non-linear matter power spectrum in Horndeski gravity. Our likelihood code for multiprobe analysis in both ΛCDM and Horndeski gravity is publicly available at https://github.com/alessiospuriomancini/KiDSHorndeski.

scholarly journals Model-independent tests of cosmic gravity

2011 ◽  
Vol 369 (1957) ◽  
pp. 4985-4997 ◽  
Author(s):  
Eric V. Linder
Keyword(s):  
General Relativity ◽  
Phase Space ◽  
Large Scale ◽  
Classification Scheme ◽  
Large Scale Structure ◽  
Gravity Models ◽  
Model Independent ◽  
Space Dynamics ◽  
Absolute Criterion ◽  
The Universe

Gravitation governs the expansion and fate of the universe, and the growth of large-scale structure within it, but has not been tested in detail on these cosmic scales. The observed acceleration of the expansion may provide signs of gravitational laws beyond general relativity (GR). Since the form of any such extension is not clear, from either theory or data, we adopt a model-independent approach to parametrizing deviations to the Einstein framework. We explore the phase space dynamics of two key post-GR functions and derive a classification scheme, and an absolute criterion on accuracy necessary for distinguishing classes of gravity models. Future surveys will be able to constrain the post-GR functions' amplitudes and forms to the required precision, and hence reveal new aspects of gravitation.

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