Local patch analysis for testing statistical isotropy of the Planck convergence map

Goyal, Priya; Chingangbam, Pravabati

doi:10.1088/1475-7516/2021/08/006

Cited by 9 publications

(3 citation statements)

References 54 publications

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“…The most accurate current measurements of the CMB temperature fluctuations are part of the third public data release of the Planck collaboration [48], precise data that allow to re-examine many interesting features already reported with diverse CMB data sets [2,[18][19][20][21][22][23][24][25][26][27][28][29][30]51]. Further, CMB products combined with data sets from other cosmological tracers are being used to study models alternative to the flat-ΛCDM model (see, e.g.…”

Section: Datamentioning

confidence: 99%

Excess of lensing amplitude in the Planck CMB power spectrum

Mokeddem

Hipólito-Ricaldi

Bernui

2023

J. Cosmol. Astropart. Phys.

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Precise measurements of the Planck cosmic microwave background (CMB) angular power spectrum (APS) at small angles have stimulated accurate statistical analyses of the lensing amplitude parameter A L. To confirm if it satisfies the value expected by the flat-ΛCDM concordance model, i.e. A L = 1, we investigate the spectrum difference obtained as the difference of the measured Planck CMB APS and the Planck best-fit ΛCDM APS model. To know if this residual spectrum corresponds to statistical noise or if it has a hidden signature that can be accounted for with a larger lensing amplitude A L > 1, we apply the Ljung-Box statistical test and find, with high statistical significance, that the spectrum difference is not statistical noise. This spectrum difference is then analysed in detail using simulated APS, based on the Planck ΛCDM best-fit model, where the lensing amplitude is a free parameter. We explore different binnations of the multipole order ℓ and look for the best-fit lensing amplitude parameter that accounts for the spectrum difference in a χ 2 procedure. We find that there is an excess of signal that is well explained by a ΛCDM APS with a non-null lensing amplitude parameter A lens, with values in the interval [0.10,0.29] at 68% confidence level. Furthermore, the lensing parameter in the Planck APS should be 1 + A lens > 1 at ∼ 3σ of statistical confidence. Additionally, we perform statistical tests that confirm the robustness of this result. Important to say that this excess of lensing amplitude, not accounted in the Planck's flat-ΛCDM model, could have an impact on the theoretical expectation of large-scale structures formation once the scales where it was detected correspond to these matter clustering processes.

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Section: Datamentioning

confidence: 99%

Excess of lensing amplitude in the Planck CMB power spectrum

Mokeddem

Hipólito-Ricaldi

Bernui

2023

J. Cosmol. Astropart. Phys.

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“…Subsequently, to explore the large-scale structures in the redshift space as the counterpart of the real space, many powerful statistical measures have been considered by concentrating on the non-Gaussianity and anisotropy (Matsubara 1996;Codis et al 2013;Appleby et al 2018Appleby et al , 2019Appleby et al , 2023. Recently, Minkowski tensors, an extension of scalar MFs (McMullen 1997;Alesker 1999;Beisbart et al 2002;Santaló 2004;Hug et al 2007;Schröder-Turk et al 2013), have been employed on two-and three-dimensional cosmological fields in the real and redshift spaces (Chingangbam et al 2017;Ganesan & Chingangbam 2017;Appleby et al 2018Appleby et al , 2019Appleby et al , 2022Appleby et al , 2023Goyal & Chingangbam 2021).…”

Section: Introductionmentioning

confidence: 99%

Probing the Anisotropy and Non-Gaussianity in the Redshift Space through the Conditional Moments of the First Derivative

Kanafi,

Movahed

2024

ApJ

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Focusing on the redshift space observations with plane-parallel approximation and relying on the rotational dependency of the general definition of excursion sets, we introduce the so-called conditional moments of the first derivative (cmd) measures for the smoothed matter density field in three dimensions. We derive the perturbative expansion of cmd for the real space and redshift space where peculiar velocity disturbs the galaxies’ observed locations. Our criteria can successfully recognize the contribution of linear Kaiser and Finger-of-God effects. Our results demonstrate that the cmd measure has significant sensitivity for pristine constraining the redshift space distortion parameter β = f/b and interestingly, the associated normalized quantity in the Gaussian linear Kaiser limit has only β dependency. Implementation of the synthetic anisotropic Gaussian field approves the consistency between the theoretical and numerical results. Including the first-order contribution of non-Gaussianity perturbatively in the cmd criterion implies that the N-body simulations for the Quijote suite in the redshift space have been mildly skewed with a higher value for the threshold greater than zero. The non-Gaussianity for the perpendicular direction to the line of sight in the redshift space for smoothing scales R ≳ 20 Mpc h −1 is almost the same as in the real space. In contrast, the non-Gaussianity along the line-of-sight direction in the redshift space is magnified. The Fisher forecasts indicate a significant enhancement in constraining the cosmological parameters Ω m , σ 8, and n s when using cmd + cr jointly.

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“…In doing so we implicitly assume that the sampling effect in the observed data and the simulations are similar, and can be subtracted. This method has been applied to CMB temperature, E-mode and lensing convergence data from Planck [10][11][12][13][14].…”

Section: Introductionmentioning

confidence: 99%

The geometrical meaning of statistical isotropy of smooth random fields in two dimensions

Chingangbam,

Goyal,

Yogendran

et al. 2021

Preprint

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We revisit the geometrical meaning of statistical isotropy that is manifest in excursion sets of smooth random fields in two dimensions. Using the contour Minkowski tensor, W1, as our basic tool we first examine geometrical properties of single structures. For simple closed curves in two dimensions we show that W1 is proportional to the identity matrix if the curve has m-fold symmetry, with m ≥ 3. Then we elaborate on how W1 maps any arbitrary shaped simple closed curve to an ellipse that is unique up to translations of its centroid. We also carry out a comparison of the shape parameters, α and β, defined using W1, with the filamentarity parameter defined using two scalar Minkowski functionals -area and contour length. We show that they contain complementary shape information, with W1 containing additional information of orientation of structures. Next, we apply our method to boundaries of excursion sets of random fields and examine what statistical isotropy means for the geometry of the excursion sets. Focusing on Gaussian isotropic fields, and using a semi-numerical approach we quantify the effect of finite sampling of the field on the geometry of the excursion sets. In doing so we obtain an analytic expression for α which takes into account the effect of finite sampling. Finally we derive an analytic expression for the ensemble expectation of W1 for Gaussian anisotropic random fields. Our results provide insights that are useful for designing tests of statistical isotropy using cosmological data.

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Local patch analysis for testing statistical isotropy of the Planck convergence map

Cited by 9 publications

References 54 publications

Excess of lensing amplitude in the Planck CMB power spectrum

Excess of lensing amplitude in the Planck CMB power spectrum

Probing the Anisotropy and Non-Gaussianity in the Redshift Space through the Conditional Moments of the First Derivative

The geometrical meaning of statistical isotropy of smooth random fields in two dimensions

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